%0 Electronic Article %T To high redshift and low mass: exploring the emergence of quenched galaxies and their environments at $33$. %R 10.48550/arXiv.2312.12207 %= eprint: arXiv:2312.12207 %0 Electronic Article %T Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic Star-Formation Rate Density 300 Myr after the Big Bang %A Robertson, Brant %A Johnson, Benjamin D. %A Tacchella, Sandro %A Eisenstein, Daniel J. %A Hainline, Kevin %A Arribas, Santiago %A Baker, William M. %A Bunker, Andrew J. %A Carniani, Stefano %A Carreira, Courtney %A Cargile, Phillip A. %A Charlot, Stéphane %A Chevallard, Jacopo %A Curti, Mirko %A Curtis-Lake, Emma %A D'Eugenio, Francesco %A Egami, Eiichi %A Hausen, Ryan %A Helton, Jakob M. %A Jakobsen, Peter %A Ji, Zhiyuan %A Jones, Gareth C. %A Maiolino, Roberto %A Maseda, Michael V. %A Nelson, Erica %A Pérez-González, Pablo G. %A Puskás, Dávid %A Rieke, Marcia %A Smit, Renske %A Sun, Fengwu %A Übler, Hannah %A Whitler, Lily %A Willmer, Christopher N. A. %A Willott, Chris %A Witstok, Joris %J arXiv e-prints %D 2023 %8 December 01, 2023 %P arXiv:2312.10033 %K Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023arXiv231210033R %Z 33 pages, 21 figures. Submitted to AAS Journals %X We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters spanning $0.4-0.9\mu\mathrm{m}$) and novel JWST images with 14 filters spanning $0.8-5\mu\mathrm{m}$, including 7 medium-band filters, and reaching total exposure times of up to 46 hours per filter. We combine all the imaging data at $>2\mu\mathrm{m}$ to construct the deepest imaging ever taken at these wavelengths, reaching as deep as $\approx31.4$ AB mag in the stack and 30.1-30.8 AB mag ($5\sigma$, $r=0.1"$ circular aperture) in individual filters. We measure photometric redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts $z=11.5-15$. These objects show compact half-light radii of $R_{1/2}\sim50-200$pc, stellar masses of $M_\star\sim10^7-10^8M_\odot$, and star-formation rates of $\mathrm{SFR}\sim0.1-1~M_\odot~\mathrm{yr}^{-1}$. Our search finds no candidates at $153$ the standard optical diagnostic diagrams (N2-BPT or S2-VO87) become unable to distinguish many AGN from other sources of photoionisation. Therefore, we also use high ionisation lines, such as HeII$\lambda$4686, HeII$\lambda$1640, NeIV$\lambda$2422, NeV$\lambda$3420, and NV$\lambda$1240, also in combination with other UV transitions, to trace the presence of AGN. Out of a parent sample of 209 galaxies, we identify 42 type-2 AGN (although 10 of them are tentative), giving a fraction of galaxies in JADES hosting type-2 AGN of about $20\pm3$\%, which does not evolve significantly in the redshift range between 2 and 10. The selected type-2 AGN have estimated bolometric luminosities of $10^{41.3-44.9}$ erg s$^{-1}$ and host-galaxy stellar masses of $10^{7.2-9.3}$ M$_{\odot}$. The star formation rates of the selected AGN host galaxies are consistent with those of the star-forming main sequence. The AGN host galaxies at z=4-6 contribute $\sim$8-30 \% to the UV luminosity function, slightly increasing with UV luminosity. %R 10.48550/arXiv.2311.18731 %= eprint: arXiv:2311.18731 %0 Electronic Article %T JADES: Carbon enrichment 350 Myr after the Big Bang in a gas-rich galaxy %A D'Eugenio, Francesco %A Maiolino, Roberto %A Carniani, Stefano %A Curtis-Lake, Emma %A Witstok, Joris %A Chevallard, Jacopo %A Charlot, Stephane %A Baker, William M. %A Arribas, Santiago %A Boyett, Kristan %A Bunker, Andrew J. %A Curti, Mirko %A Eisenstein, Daniel J. %A Hainline, Kevin %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Looser, Tobias J. %A Nakajima, Kimihiko %A Nelson, Erica %A Rieke, Marcia %A Robertson, Brant %A Scholtz, Jan %A Smit, Renske %A Venturi, Giacomo %A Tacchella, Sandro %A Uebler, Hannah %A Willmer, Christopher N. A. %A Willott, Chris %J arXiv e-prints %D 2023 %8 November 01, 2023 %P arXiv:2311.09908 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv231109908D %Z 13 pages, 8 figures. Submitted to Astronomy & Astrophysics %X Finding the emergence of the first generation of metals in the early Universe, and identifying their origin, are some of the most important goals of modern astrophysics. We present deep JWST/NIRSpec spectroscopy of GS-z12, a galaxy at z=12.5, in which we report the detection of C III]${\lambda}{\lambda}$1907,1909 nebular emission. This is the most distant detection of a metal transition and the most distant redshift determination via emission lines. In addition, we report tentative detections of [O II]${\lambda}{\lambda}$3726,3729 and [Ne III]${\lambda}$3869, and possibly O III]${\lambda}{\lambda}$1661,1666. By using the accurate redshift from C III], we can model the Ly${\alpha}$ drop to reliably measure an absorbing column density of hydrogen of $N_{HI} \approx 10^{22}$ cm$^{-2}$ - too high for an IGM origin and implying abundant ISM in GS-z12 or CGM around it. We infer a lower limit for the neutral gas mass of about $10^7$ MSun which, compared with a stellar mass of $\approx4 \times 10^7$ MSun inferred from the continuum fitting, implies a gas fraction higher than about 0.1-0.5. We derive a solar or even super-solar carbon-to-oxygen ratio, tentatively [C/O]>0.15. This is higher than the C/O measured in galaxies discovered by JWST at z=6-9, and higher than the C/O arising from Type-II supernovae enrichment, while AGB stars cannot contribute to carbon enrichment at these early epochs and low metallicities. Such a high C/O in a galaxy observed 350 Myr after the Big Bang may be explained by the yields of extremely metal poor stars, and may even be the heritage of the first generation of supernovae from Population III progenitors. %R 10.48550/arXiv.2311.09908 %= eprint: arXiv:2311.09908 %0 Electronic Article %T The galaxies missed by Hubble and ALMA: the contribution of extremely red galaxies to the cosmic census at 33$ that were previously missing from galaxy census estimates. The data indicate the existence of abundant, dusty and post-starburst-like galaxies down to $10^8$M$_\odot$, below the sensitivity limit of Spitzer and ALMA. Modeling the NIRCam and HST photometry of these red sources can result in extreme, high values for both stellar mass and star formation rate (SFR); however, including 7 MIRI filters out to 21$\mu$m results in decreased mass (median 0.6 dex for log$_{10}$M$^*$/M$_{\odot}>$10), and SFR (median 10$\times$ for SFR$>$100 M$_{\odot}$/yr). At $z>6$, our sample includes a high fraction of little red dots (LRDs; NIRCam-selected dust-reddened AGN candidates). We significantly measure older stellar populations in the LRDs out to rest-frame 3$\mu$m (the stellar bump) and rule out a dominant contribution from hot dust emission, a signature of AGN contamination to stellar population measurements. This allows us to measure their contribution to the cosmic census at $z>3$, below the typical detection limits of ALMA ($L_{\rm IR}<10^{12}L_\odot$). We find that these sources, which are overwhelmingly missed by HST and ALMA, could effectively double the obscured fraction of the star formation rate density at $4 = 7.955$ and $\left< z_{\mathrm{\,spec}} \right> = 8.222$ (representing densities around $\sim 6$ and $\sim 12$ times that of a random volume). We estimate the total halo mass of these large-scale structures to be $11.5 \leq \mathrm{log}_{10}\left(M_{\mathrm{halo}}/M_{\odot}\right) \leq 13.4$ using an empirical stellar mass to halo mass relation, which are likely underestimates as a result of incompleteness. These protocluster candidates are expected to evolve into massive galaxy clusters with $\mathrm{log}_{10}\left(M_{\mathrm{halo}}/M_{\odot}\right) rsim 14$ by $z = 0$. %R 10.48550/arXiv.2311.04270 %= eprint: arXiv:2311.04270 %0 Journal Article %T First detection of the BAO signal from early DESI data %A Moon, Jeongin %A Valcin, David %A Rashkovetskyi, Michael %A Saulder, Christoph %A Aguilar, Jessica Nicole %A Ahlen, Steven %A Alam, Shadab %A Bailey, Stephen %A Baltay, Charles %A Blum, Robert %A Brooks, David %A Burtin, Etienne %A Chaussidon, Edmond %A Dawson, Kyle %A de la Macorra, Axel %A de M attia, Arnaud %A Dhungana, Govinda %A Eisenstein, Daniel %A Flaugher, Brenna %A Font-Ribera, Andreu %A Forero-Romero, Jaime E. %A Garcia-Quintero, Cristhian %A Gontcho A Gontcho, Satya %A Guy, Julien %A Hanif, Malik Muhammad Sikandar %A Honscheid, Klaus %A Ishak, Mustapha %A Kehoe, Robert %A Kim, Sumi %A Kisner, Theodore %A Kremin, Anthony %A Landriau, Martin %A Le Guillou, Laurent %A Levi, Michael %A Manera, Marc %A Martini, Paul %A McDonald, Patrick %A Meisner, Aaron %A Miquel, Ramon %A Moustakas, John %A Myers, Adam %A Nadathur, Seshadri %A Neveux, Richard %A Newman, Jeffrey A. %A Nie, Jundan %A Padmanabhan, Nikhil %A Palanque-Delabrouille, Nathalie %A Percival, Will %A Pérez Fernández, Alejandro %A Poppett, Claire %A Prada, Francisco %A Raichoor, Anand %A Ross, Ashley J. %A Rossi, Graziano %A Samushia, Lado %A Schlegel, David %A Seo, Hee-Jong %A Tarlé, Gregory %A Vargas Magana, Mariana %A Variu, Andrei %A Weaver, Benjamin Alan %A White, Martin J. %A Yèche, Christophe %A Yuan, Sihan %A Zhao, Cheng %A Zhou, Rongpu %A Zhou, Zhimin %A Zou, Hu %+ AA(Sejong University, Seoul, Korea), AB(Ohio University, Department of Physics and Astronomy), AC(Harvard Smithsonian Center for Astrophysics), AD(Korea Astronomy and Space Science Institute), AE(Lawrence Berkeley National Laboratory, California), AF(Boston University, Department of Physics), AG(Tata Institute of Fundamental Research, India), AH(Lawrence Berkeley National Laboratory, California), AI(Physics Department, Yale University, PO Box 208120, New Haven, CT 06511, USA), AJ(National Optical Astronomy Observatory, Arizona), AK(University College London, Department of Physics and Astronomy), AL(Institut de Recherche sur les Lois Fondamentales de l'Universe), AM(Institut de Recherche sur les Lois Fondamentales de l'Universe), AN(University of Utah, Department of Physics and Astronomy), AO(UNAM, Institute of Physics), AP(Institut de Recherche sur les Lois Fondamentales de l'Universe), AQ(Southern Methodist University, Texas), AR(Harvard Smithsonian Center for Astrophysics), AS(Fermi National Accelerator Laboratory, Illinois), AT(Institute for High Energy Physics, Barcelona), AU(University of the Andes, Colombia), AV(University of Texas, Dallas, Department of Physics), AW(Lawrence Berkeley National Laboratory, California), AX(Lawrence Berkeley National Laboratory, California), AY(University of Michigan), AZ(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), BA(University of Texas, Dallas, Department of Physics), BB(Southern Methodist University, Texas), BC(Natural Science Research Institute, University of Seoul, 163 Seoulsiripdae-ro, Dongdaemun-gu, Seoul 02504, South Korea), BD(Lawrence Berkeley National Laboratory, California), BE(Lawrence Berkeley National Laboratory, California), BF(Lawrence Berkeley National Laboratory, California), BG(Laboratoire de Physique Nucleaire et de Hautes Energies), BH(Lawrence Berkeley National Laboratory, California), BI(Departament de Física, Serra Húnter, Universitat Autònoma de Barcelona, E-08193 Bellaterra (Barcelona), Spain), BJ(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), BK(Lawrence Berkeley National Laboratory, California), BL(National Optical Astronomy Observatory, Arizona), BM(Institute for High Energy Physics, Barcelona; Institucio Catalona de Recerca i Estudis Avancats), BN(Siena College, New York), BO(University of Wyoming, Department of Physics and Astronomy), BP(University of Portsmouth, Institute of Cosmology and Gravitation), BQ(Royal Observatory Edinburgh), BR(University of Pittsburgh, Department of Physics and Astronomy), BS(CAS, National Astronomical Observatories), BT(Physics Department, Yale University, PO Box 208120, New Haven, CT 06511, USA;), BU(Lawrence Berkeley National Laboratory, California; Institut de Recherche sur les Lois Fondamentales de l'Universe), BV(University of Waterloo, Canada; Perimeter Institute for Theoretical Physics, Canada), BW(UNAM, Institute of Physics), BX(University of California, Berkeley, Space Sciences Laboratory; Lawrence Berkeley National Laboratory, California), BY(Institute of Astrophysics of Andalusia), BZ(Lawrence Berkeley National Laboratory, California), CA(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), CB(Sejong University, Seoul, Korea), CC(Kansas State University, Department of Physics), CD(Lawrence Berkeley National Laboratory, California), CE(Ohio University, Department of Physics and Astronomy), CF(University of Michigan), CG(UNAM, Institute of Physics), CH(Ecole Polytechnique Federale de Lausanne), CI(National Optical Astronomy Observatory, Arizona), CJ(University of California, Berkeley, Department of Physics), CK(Institut de Recherche sur les Lois Fondamentales de l'Universe), CL(Stanford Linear Accelerator Center), CM(Ecole Polytechnique Federale de Lausanne), CN(Lawrence Berkeley National Laboratory, California), CO(CAS, National Astronomical Observatories), CP(CAS, National Astronomical Observatories) %J Monthly Notices of the Royal Astronomical Society %V 525 %D 2023 %8 November 01, 2023 %P 5406-5422 %K galaxies: statistics; cosmology: large-scale structure of Universe; observations; dark energy; methods: data analysis; statistical; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.525.5406M %X We present the first detection of the baryon acoustic oscillations (BAOs) signal obtained using unblinded data collected during the initial 2 months of operations of the Stage-IV ground-based Dark Energy Spectroscopic Instrument (DESI). From a selected sample of 261 291 luminous red galaxies spanning the redshift interval 0.4 < z < 1.1 and covering 1651 square degrees with a 57.9 per cent completeness level, we report a ~5σ level BAO detection and the measurement of the BAO location at a precision of 1.7 per cent. Using a bright galaxy sample of 109 523 galaxies in the redshift range 0.1 < z < 0.5, over 3677 square degrees with a 50.0 per cent completeness, we also detect the BAO feature at ~3σ significance with a 2.6 per cent precision. These first BAO measurements represent an important milestone, acting as a quality control on the optimal performance of the complex robotically actuated, fibre-fed DESI spectrograph, as well as an early validation of the DESI spectroscopic pipeline and data management system. Based on these first promising results, we forecast that DESI is on target to achieve a high-significance BAO detection at sub-per cent precision with the completed 5-yr survey data, meeting the top-level science requirements on BAO measurements. This exquisite level of precision will set new standards in cosmology and confirm DESI as the most competitive BAO experiment for the remainder of this decade. %R 10.1093/mnras/stad2618 %= eprint: arXiv:2304.08427 %@ 0035-8711 %0 Journal Article %T Synthetic light-cone catalogues of modern redshift and weak lensing surveys waith ABACUSSUMMIT %A Hadzhiyska, Boryana %A Yuan, S. %A Blake, C. %A Eisenstein, D. J. %A Aguilar, J. %A Ahlen, S. %A Brooks, D. %A Claybaugh, T. %A de la Macorra, A. %A Doel, P. %A Emas, N. %A Forero-Romero, J. E. %A Garcia-Quintero, C. %A Ishak, M. %A Joudaki, S. %A Jullo, E. %A Kehoe, R. %A Kisner, T. %A Kremin, A. %A Krolewski, A. %A Landriau, M. %A Lange, J. U. %A Manera, M. %A Miquel, R. %A Nie, Jundan %A Poppett, C. %A Porredon, A. %A Rossi, G. %A Ruggeri, R. %A Saulder, C. %A Schubnell, M. %A Tarlé, G. %A Weaver, B. A. %A Xhakaj, E. %A Zhou, Zhimin %+ AA(Lawrence Berkeley National Laboratory, California; -; Stanford Linear Accelerator Center), AB(Stanford Linear Accelerator Center), AC(Swinburne University of Technology, Center for Astrophysics and Supercomputing), AD(Harvard Smithsonian Center for Astrophysics), AE(Lawrence Berkeley National Laboratory, California), AF(Boston University, Department of Physics), AG(University College London, Department of Physics and Astronomy), AH(Lawrence Berkeley National Laboratory, California), AI(UNAM, Institute of Physics), AJ(University College London, Department of Physics and Astronomy), AK(Swinburne University of Technology, Center for Astrophysics and Supercomputing), AL(University of the Andes, Colombia), AM(University of Texas, Dallas, Department of Physics), AN(University of Texas, Dallas, Department of Physics), AO(University of Waterloo, Department of Physics and Astronomy), AP(Aix-Marseille Universite, Laboratoire d'Astrophysique), AQ(Southern Methodist University, Texas), AR(Lawrence Berkeley National Laboratory, California), AS(Lawrence Berkeley National Laboratory, California), AT(University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada; University of Waterloo, Canada), AU(Lawrence Berkeley National Laboratory, California), AV(University of Michigan, Department of Physics), AW(Institute for High Energy Physics, Barcelona), AX(Institute for High Energy Physics, Barcelona; Institucio Catalona de Recerca i Estudis Avancats), AY(CAS, National Astronomical Observatories), AZ(Lawrence Berkeley National Laboratory, California; -; University of California, Berkeley, Space Sciences Laboratory), BA(Royal Observatory Edinburgh; The Ohio State University, Department of Physics), BB(Sejong University, Department of Astronomy), BC(Swinburne University of Technology, Center for Astrophysics and Supercomputing; University of Queensland, School of Mathematics and Physics), BD(Korea Astronomy and Space Science Institute), BE(University of Michigan, Department of Physics), BF(University of Michigan, Department of Physics), BG(National Optical Astronomy Observatory, Arizona), BH(University of California, Santa Cruz, Department of Astronomy and Astrophysics), BI(CAS, National Astronomical Observatories) %J Monthly Notices of the Royal Astronomical Society %V 525 %D 2023 %8 November 01, 2023 %P 4367-4387 %K gravitational lensing: weak; methods: numerical; galaxies: haloes; cosmic background radiation; large-scale structure of Universe; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.525.4367H %X The joint analysis of different cosmological probes, such as galaxy clustering and weak lensing, can potentially yield invaluable insights into the nature of the primordial Universe, dark energy, and dark matter. However, the development of high-fidelity theoretical models is a necessary stepping stone. Here, we present public high-resolution weak lensing maps on the light-cone, generated using the N-body simulation suite ABACUSSUMMIT, and accompanying weak lensing mock catalogues, tuned to the Early Data Release small-scale clustering measurements of the Dark Energy Spectroscopic Instrument. Available in this release are maps of the cosmic shear, deflection angle, and convergence fields at source redshifts ranging from z = 0.15 to 2.45 as well as cosmic microwave background convergence maps for each of the 25 base-resolution simulations ($L_{\rm box} = 2000\, h^{-1}\, {\rm Mpc}$ and Npart = 69123) as well as for the two huge simulations ($L_{\rm box} = 7500\, h^{-1}\, {\rm Mpc}$ and Npart = 86403) at the fiducial ABACUSSUMMIT cosmology. The pixel resolution of each map is 0.21 arcmin, corresponding to a HEALPIX Nside of 16 384. The sky coverage of the base simulations is an octant until z ≈ 0.8 (decreasing to about 1800 deg2 at z ≈ 2.4), whereas the huge simulations offer full-sky coverage until z ≈ 2.2. Mock lensing source catalogues are sampled matching the ensemble properties of the Kilo-Degree Survey, Dark Energy Survey, and Hyper Suprime-Cam data sets. The mock catalogues are validated against theoretical predictions for various clustering and lensing statistics, such as correlation multipoles, galaxy-shear, and shear-shear, showing excellent agreement. All products can be downloaded via a Globus endpoint (see Data Availability section). %R 10.1093/mnras/stad2563 %= eprint: arXiv:2305.11935 %@ 0035-8711 %0 Journal Article %T JADES Initial Data Release for the Hubble Ultra Deep Field: Revealing the Faint Infrared Sky with Deep JWST NIRCam Imaging %A Rieke, Marcia J. %A Robertson, Brant %A Tacchella, Sandro %A Hainline, Kevin %A Johnson, Benjamin D. %A Hausen, Ryan %A Ji, Zhiyuan %A Willmer, Christopher N. A. %A Eisenstein, Daniel J. %A Puskás, Dávid %A Alberts, Stacey %A Arribas, Santiago %A Baker, William M. %A Baum, Stefi %A Bhatawdekar, Rachana %A Bonaventura, Nina %A Boyett, Kristan %A Bunker, Andrew J. %A Cameron, Alex J. %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Chen, Zuyi %A Curti, Mirko %A Curtis-Lake, Emma %A Danhaive, A. Lola %A DeCoursey, Christa %A Dressler, Alan %A Egami, Eiichi %A Endsley, Ryan %A Helton, Jakob M. %A Hviding, Raphael E. %A Kumari, Nimisha %A Looser, Tobias J. %A Lyu, Jianwei %A Maiolino, Roberto %A Maseda, Michael V. %A Nelson, Erica J. %A Rieke, George %A Rix, Hans-Walter %A Sandles, Lester %A Saxena, Aayush %A Sharpe, Katherine %A Shivaei, Irene %A Skarbinski, Maya %A Smit, Renske %A Stark, Daniel P. %A Stone, Meredith %A Suess, Katherine A. %A Sun, Fengwu %A Topping, Michael %A Übler, Hannah %A Villanueva, Natalia C. %A Wallace, Imaan E. B. %A Williams, Christina C. %A Willott, Chris %A Whitler, Lily %A Witstok, Joris %A Woodrum, Charity %+ AA(University of Arizona, Department of Astronomy and Steward Observatory), AB(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AC(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK), AD(University of Arizona, Department of Astronomy and Steward Observatory), AE(Harvard Smithsonian Center for Astrophysics), AF(Johns Hopkins University, Department of Physics and Astronomy), AG(University of Arizona, Department of Astronomy and Steward Observatory), AH(University of Arizona, Department of Astronomy and Steward Observatory), AI(Harvard Smithsonian Center for Astrophysics), AJ(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK), AK(University of Arizona, Department of Astronomy and Steward Observatory), AL(Center for Astrobiology, Madrid), AM(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK), AN(University of Manitoba, Department of Physics and Astronomy), AO(European Space Research and Technology Centre), AP(University of Arizona, Department of Astronomy and Steward Observatory), AQ(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics), AR(University of Oxford, Department of Physics), AS(University of Oxford, Department of Physics), AT(Scuola Normale Superiore, Pisa, Italy), AU(Institut d'Astrophysique de Paris), AV(University of Oxford, Department of Physics), AW(University of Arizona, Department of Astronomy and Steward Observatory), AX(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK), AY(University of Hertfordshire, School of Physics, Astronomy and Mathematics), AZ(Kavli Institute for Cosmology, UK), BA(University of Arizona, Department of Astronomy and Steward Observatory), BB(Carnegie Institution of Washington, Observatories, California), BC(University of Arizona, Department of Astronomy and Steward Observatory), BD(University of Texas, Austin, Department of Astronomy), BE(University of Arizona, Department of Astronomy and Steward Observatory), BF(University of Arizona, Department of Astronomy and Steward Observatory; Max-Planck-Institute for Astronomy, Heidelberg), BG(AURA for European Space Agency, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), BH(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK), BI(University of Arizona, Department of Astronomy and Steward Observatory), BJ(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK; University College London, Department of Physics and Astronomy), BK(University of Wisconsin, Madison, Department of Astronomy), BL(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), BM(University of Arizona, Department of Astronomy and Steward Observatory), BN(Max-Planck-Institute for Astronomy, Heidelberg), BO(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK), BP(University College London, Department of Physics and Astronomy), BQ(Harvard Smithsonian Center for Astrophysics), BR(University of Arizona, Department of Astronomy and Steward Observatory; Center for Astrobiology, Madrid), BS(Harvard Smithsonian Center for Astrophysics), BT(Liverpool John Moores University, Astrophysics Research Institute), BU(University of Arizona, Department of Astronomy and Steward Observatory), BV(University of Arizona, Department of Astronomy and Steward Observatory), BW(University of California, Santa Cruz, Department of Astronomy and Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology, California), BX(University of Arizona, Department of Astronomy and Steward Observatory), BY(University of Arizona, Department of Astronomy and Steward Observatory), BZ(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK), CA(Harvard Smithsonian Center for Astrophysics), CB(University of Oxford, Department of Physics), CC(National Optical Astronomy Observatory, Arizona), CD(Herzberg Institute for Astronomy and Astrophysics), CE(University of Arizona, Department of Astronomy and Steward Observatory), CF(University of Cambridge, Institute of Astronomy; Kavli Institute for Cosmology, UK), CG(University of Arizona, Department of Astronomy and Steward Observatory) %J The Astrophysical Journal Supplement Series %V 269 %D 2023 %8 November 01, 2023 %P 16 %K High-redshift galaxies; 734; Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023ApJS..269...16R %X JWST has revolutionized the field of extragalactic astronomy with its sensitive and high-resolution infrared view of the distant Universe. Adding to the new legacy of JWST observations, we present the first NIRCam imaging data release from the JWST Advanced Deep Extragalactic Survey (JADES), providing nine filters of infrared imaging of ~25 arcmin2 covering the Hubble Ultra Deep Field and portions of Great Observatories Origins Deep Survey South. Utilizing 87 on-sky dual-filter hours of exposure time, these images reveal the deepest ever near-infrared view of this iconic field. We supply carefully constructed nine-band mosaics of the JADES bands, as well as matching reductions of five additional bands from the JWST Extragalactic Medium-band Survey. Combining with existing Hubble Space Telescope imaging, we provide 23-band space-based photometric catalogs and photometric redshifts for ≈47,500 sources. To promote broad engagement with JADES, we have created an interactive FitsMap website to provide an interface for professional researchers and the public to experience these JWST data sets. Combined with the first JADES NIRSpec data release, these public JADES imaging and spectroscopic data sets provide a new foundation for discoveries of the infrared Universe by the worldwide scientific community. %R 10.3847/1538-4365/acf44d %= eprint: arXiv:2306.02466 %@ 0067-0049 %0 Electronic Article %T JADES: Using NIRCam Photometry to Investigate the Dependence of Stellar Mass Inferences on the IMF in the Early Universe %A Woodrum, Charity %A Rieke, Marcia %A Ji, Zhiyuan %A Baker, William M. %A Bhatawdekar, Rachana %A Bunker, Andrew J. %A Charlot, Stéphane %A Curtis-Lake, Emma %A Eisenstein, Daniel J. %A Hainline, Kevin %A Hausen, Ryan %A Helton, Jakob M. %A Hviding, Raphael E. %A Johnson, Benjamin D. %A Robertson, Brant %A Sun, Fengwu %A Tacchella, Sandro %A Whitler, Lily %A Williams, Christina C. %A Willmer, Christopher N. A. %J arXiv e-prints %D 2023 %8 October 01, 2023 %P arXiv:2310.18464 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv231018464W %Z The Significance statement is required for PNAS submission %X The detection of numerous and relatively bright galaxies at redshifts z > 9 has prompted new investigations into the star-forming properties of high-redshift galaxies. Using local forms of the initial mass function (IMF) to estimate stellar masses of these galaxies from their light output leads to galaxy masses that are at the limit allowed for the state of the LambdaCDM Universe at their redshift. We explore how varying the IMF assumed in studies of galaxies in the early universe changes the inferred values for the stellar masses of these galaxies. We infer galaxy properties with the SED fitting code Prospector using varying IMF parameterizations for a sample of 102 galaxies from the JWST Advanced Deep Extragalactic Survey (JADES) spectroscopically confirmed to be at z > 6.7, with additional photometry from the JWST Extragalactic Medium Band Survey (JEMS) for twenty-one galaxies. We demonstrate that models with stellar masses reduced by a factor of three or more do not affect the modeled spectral energy distribution (SED). %R 10.48550/arXiv.2310.18464 %= eprint: arXiv:2310.18464 %0 Electronic Article %T The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release %A Eisenstein, Daniel J. %A Johnson, Benjamin D. %A Robertson, Brant %A Tacchella, Sandro %A Hainline, Kevin %A Jakobsen, Peter %A Maiolino, Roberto %A Bonaventura, Nina %A Bunker, Andrew J. %A Cameron, Alex J. %A Cargile, Phillip A. %A Curtis-Lake, Emma %A Hausen, Ryan %A Puskás, Dávid %A Rieke, Marcia %A Sun, Fengwu %A Willmer, Christopher N. A. %A Willott, Chris %A Alberts, Stacey %A Arribas, Santiago %A Baker, William M. %A Baum, Stefi %A Bhatawdekar, Rachana %A Carniani, Stefano %A Charlot, Stephane %A Chen, Zuyi %A Chevallard, Jacopo %A Curti, Mirko %A DeCoursey, Christa %A D'Eugenio, Francesco %A de Graaff, Anna %A Egami, Eiichi %A Helton, Jakob M. %A Ji, Zhiyuan %A Jones, Gareth C. %A Kumari, Nimisha %A Lützgendorf, Nora %A Laseter, Isaac %A Looser, Tobias J. %A Lyu, Jianwei %A Maseda, Michael V. %A Nelson, Erica %A Parlanti, Eleonora %A Rauscher, Bernard J. %A Rawle, Tim %A Rieke, George %A Rix, Hans-Walter %A Rujopakarn, Wiphu %A Sandles, Lester %A Saxena, Aayush %A Scholtz, Jan %A Sharpe, Katherine %A Shivaei, Irene %A Simmonds, Charlotte %A Smit, Renske %A Topping, Michael W. %A Übler, Hannah %A Venturi, Giacomo %A Williams, Christina C. %A Witstok, Joris %A Woodrum, Charity %J arXiv e-prints %D 2023 %8 October 01, 2023 %P arXiv:2310.12340 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv231012340E %Z Submitted to ApJ Supplement. Images and catalogs are available at https://archive.stsci.edu/hlsp/jades . A FITSmap portal to view the images is at https://jades.idies.jhu.edu %X We summarize the properties and initial data release of the JADES Origins Field (JOF), which will soon be the deepest imaging field yet observed with the James Webb Space Telescope (JWST). This field falls within the GOODS-S region about 8' south-west of the Hubble Ultra Deep Field (HUDF), where it was formed initially in Cycle 1 as a parallel field of HUDF spectroscopic observations within the JWST Advanced Deep Extragalactic Survey (JADES). This imaging will be greatly extended in Cycle 2 program 3215, which will observe the JOF for 5 days in six medium-band filters, seeking robust candidates for z>15 galaxies. This program will also include ultra-deep parallel NIRSpec spectroscopy (up to 104 hours on-source, summing over the dispersion modes) on the HUDF. Cycle 3 observations from program 4540 will add 20 hours of NIRCam slitless spectroscopy to the JOF. With these three campaigns, the JOF will be observed for 380 open-shutter hours with NIRCam using 15 imaging filters and 2 grism bandpasses. Further, parts of the JOF have deep 43 hr MIRI observations in F770W. Taken together, the JOF will soon be one of the most compelling deep fields available with JWST and a powerful window into the early Universe. This paper presents the second data release from JADES, featuring the imaging and catalogs from the year 1 JOF observations. %R 10.48550/arXiv.2310.12340 %= eprint: arXiv:2310.12340 %0 Electronic Article %T AGN Selection and Demographics: A New Age with JWST/MIRI %A Lyu, Jianwei %A Alberts, Stacey %A Rieke, George H. %A Shivaei, Irene %A Perez-Gonzalez, Pablo G. %A Sun, Fengwu %A Hainline, Kevin N. %A Baum, Stefi %A Bonaventura, Nina %A Bunker, Andrew J. %A Egami, Eiichi %A Eisenstein, Daniel J. %A Florian, Michael %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Morrison, Jane %A Rieke, Marcia %A Robertson, Brant %A Rujopakarn, Wiphu %A Tacchella, Sandro %A Scholtz, Jan %A Willmer, Christopher N. A. %J arXiv e-prints %D 2023 %8 October 01, 2023 %P arXiv:2310.12330 %K Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023arXiv231012330L %Z 32 pages, 21 figures, submitted to ApJ %X Understanding the co-evolution of supermassive black holes (SMBHs) and their host systems requires a comprehensive census of active galactic nuclei (AGN) behavior across a wide range of redshift, luminosity, obscuration level and galaxy properties. We report significant progress with JWST towards this goal from the Systematic Mid-infrared Instrument Legacy Extragalactic Survey (SMILES). Based on comprehensive SED analysis of 3273 MIRI-detected sources, we identify 217 AGN candidates over a survey area of $\sim$34 arcmin$^2$, including a primary sample of 111 AGNs in normal massive galaxies ($M_{*}>10^{9.5}~M_\odot$) at $z\sim$0--4, an extended sample of 86 AGN {\it candidates} in low-mass galaxies ($M_{*}<10^{9.5}~M_\odot$) and a high-$z$ sample of 20 AGN {\it candidates} at $z\sim$4--8.4. Notably, about 80\% of our MIRI-selected AGN candidates are new discoveries despite the extensive pre-JWST AGN searches. Even among the massive galaxies where the previous AGN search is believed to be thorough, 34\% of the MIRI AGN identifications are new, highlighting the impact of obscuration on previous selections. By combining our results with the efforts at other wavelengths, we build the most complete AGN sample to date and examine the relative performance of different selection techniques. We find the obscured AGN fraction increases from $L_{\rm AGN, bol}\sim10^{10}~L_\odot$ to $10^{11}~L_\odot$ and then drops towards higher luminosity. Additionally, the obscured AGN fraction gradually increases from $z\sim0$ to $z\sim4$ with most high-$z$ AGNs obscured. We discuss how AGN obscuration, intrinsic SED variations, galaxy contamination, survey depth and selection techniques complicate the construction of a complete AGN sample. %R 10.48550/arXiv.2310.12330 %= eprint: arXiv:2310.12330 %0 Electronic Article %T FRESCO: An extended, massive, rapidly rotating galaxy at z=5.3 %A Nelson, Erica J. %A Brammer, Gabriel %A Gimenez-Arteaga, Clara %A Oesch, Pascal A. %A Ubler, Hannah %A de Graaff, Anna %A Matharu, Jasleen %A Naidu, Rohan P. %A Shapley, Alice E. %A Whitaker, Katherine E. %A Wisnioski, Emily %A Forster Schreiber, Natascha M. %A Smit, Renske %A van Dokkum, Pieter %A Chisholm, John %A Endsley, Ryan %A Hartley, Abigail I. %A Gibson, Justus %A Giovinazzo, Emma %A Illingworth, Garth %A Labbe, Ivo %A Maseda, Michael V. %A Matthee, Jorryt %A Covelo Paz, Alba %A Price, Sedona H. %A Reddy, Naveen A. %A Shivaei, Irene %A Weibel, Andrea %A Wuyts, Stijn %A Xiao, Mengyuan %A Alberts, Stacey %A Baker, William M. %A Bunker, Andrew J. %A Cameron, Alex J. %A Charlot, Stephane %A Eisenstein, Daniel J. %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Jones, Gareth C. %A Maiolino, Roberto %A Robertson, Brant %A Sandles, Lester %A Suess, Katherine A. %A Tacchella, Sandro %A Williams, Christina C. %A Witstok, Joris %J arXiv e-prints %D 2023 %8 October 01, 2023 %P arXiv:2310.06887 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv231006887N %Z Fig. 3 shows the main result %X With the remarkable sensitivity and resolution of JWST in the infrared, measuring rest-optical kinematics of galaxies at $z>5$ has become possible for the first time. This study pilots a new method for measuring galaxy dynamics for highly multiplexed, unbiased samples by combining FRESCO NIRCam grism spectroscopy and JADES medium-band imaging. Here we present one of the first JWST kinematic measurements for a galaxy at $z>5$. We find a significant velocity gradient, which, if interpreted as rotation yields $V_{rot} = 240\pm50$km/s and we hence refer to this galaxy as Twister-z5. With a rest-frame optical effective radius of $r_e=2.25$kpc, the high rotation velocity in this galaxy is not due to a compact size as may be expected in the early universe but rather a high total mass, ${\rm log(M}_{dyn}/{\rm M}_\odot)=11.0\pm0.2$. This is a factor of roughly 4x higher than the stellar mass within the effective radius. We also observe that the radial H$\alpha$ equivalent width profile and the specific star formation rate map from resolved stellar population modeling is centrally depressed by a factor of $\sim1.5$ from the center to $r_e$. Combined with the morphology of the line-emitting gas in comparison to the continuum, this centrally suppressed star formation is consistent with a star-forming disk surrounding a bulge growing inside-out. While large, rapidly rotating disks are common to z~2, the existence of one after only 1Gyr of cosmic time, shown for the first time in ionized gas, adds to the growing evidence that some galaxies matured earlier than expected in the history of the universe. %R 10.48550/arXiv.2310.06887 %= eprint: arXiv:2310.06887 %0 Journal Article %T Constraining accuracy of the pairwise velocities in N-body simulations using scale-free models %A Maleubre, Sara %A Eisenstein, Daniel J. %A Garrison, Lehman H. %A Joyce, Michael %+ AA(Laboratoire de Physique Nucleaire et de Hautes Energies; Max-Planck-Institute for Extraterrestrial Physics, Garching), AB(Harvard Smithsonian Center for Astrophysics), AC(Center for Computational Astrophysics, Flatiron Institute, New York; -), AD(Laboratoire de Physique Nucleaire et de Hautes Energies) %J Monthly Notices of the Royal Astronomical Society %V 525 %D 2023 %8 October 01, 2023 %P 1039-1052 %K methods: numerical; large-scale structure of Universe; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.525.1039M %X We present a continuation of an analysis that aims to quantify resolution of N-body simulations by exploiting large (up to N = 40963) simulations of scale-free cosmologies run using ABACUS. Here, we focus on radial pairwise velocities of the matter field, both by direct estimation and through the cumulative two-point correlation function (using the pair conservation equation). We find that convergence at the 1 per cent level of the mean relative pairwise velocity can be demonstrated over a range of scales, evolving from a few times the grid spacing at early times to slightly below this scale at late times. We show the analysis of two different box sizes as well as from averaging results from the smaller boxes, and compare the power of the two aforementioned estimators in constraining accuracy at each scale. Down to scales of the order of the smoothing parameter, convergence is obtained at ~$5~{{\rm per\, cent}}$ precision, and shows a behaviour indicating asymptotic stable clustering. We also infer for LCDM simulations conservative estimates on the evolution of the lower cut-off to resolution (at 1 and 5 per cent precision) as a function of redshift. %R 10.1093/mnras/stad2388 %= eprint: arXiv:2211.07607 %@ 0035-8711 %0 Journal Article %T On the impact of the galaxy window function on cosmological parameter estimation %A Karim, Tanveer %A Rezaie, Mehdi %A Singh, Sukhdeep %A Eisenstein, Daniel %+ AA(Center for Astrophysics | Harvard & Smithsonian, 60 Garden St, MS 10, Cambridge, MA 02138, USA;), AB(Kansas State University, Department of Physics; The Ohio State University, Department of Astronomy), AC(Carnegie Mellon University, Department of Physics), AD(Center for Astrophysics | Harvard & Smithsonian, 60 Garden St, MS 10, Cambridge, MA 02138, USA;) %J Monthly Notices of the Royal Astronomical Society %V 525 %D 2023 %8 October 01, 2023 %P 311-324 %K methods: data analysis; methods: statistical; cosmological parameters; large-scale structure of the Universe; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.525..311K %X One important source of systematics in galaxy redshift surveys comes from the estimation of the galaxy window function. Up until now, the impact of the uncertainty in estimating the galaxy window function on parameter inference has not been properly studied. In this paper, we show that the uncertainty and the bias in estimating the galaxy window function will be salient for ongoing and next-generation galaxy surveys using a simulation-based approach. With a specific case study of cross-correlating emission-line galaxies from the DESI Legacy Imaging Surveys and the Planck cosmic microwave background lensing map, we show that neural network-based regression approaches to modelling the window function are superior in comparison to linear regression-based models. We additionally show that the definition of the galaxy overdensity estimator can impact the overall signal-to-noise of observed power spectra. Finally, we show that the additive biases coming from the window functions can significantly bias the modes of the inferred parameters and also degrade their precision. Thus, a careful understanding of the window functions will be essential to conduct cosmological experiments. %R 10.1093/mnras/stad2210 %= eprint: arXiv:2305.11956 %@ 0035-8711 %0 Journal Article %T The DESI One-Percent survey: exploring the Halo Occupation Distribution of Emission Line Galaxies with ABACUSSUMMIT simulations %A Rocher, Antoine %A Ruhlmann-Kleider, Vanina %A Burtin, Etienne %A Yuan, Sihan %A de Mattia, Arnaud %A Ross, Ashley J. %A Aguilar, Jessica %A Ahlen, Steven %A Alam, Shadab %A Bianchi, Davide %A Brooks, David %A Cole, Shaun %A Dawson, Kyle %A de la Macorra, Axel %A Doel, Peter %A Eisenstein, Daniel J. %A Fanning, Kevin %A Forero-Romero, Jaime E. %A Garrison, Lehman H. %A Gontcho A Gontcho, Satya %A Gonzalez-Perez, Violeta %A Guy, Julien %A Hadzhiyska, Boryana %A Hahn, ChangHoon %A Honscheid, Klaus %A Kisner, Theodore %A Landriau, Martin %A Lasker, James %A E. Levi, Michael %A Manera, Marc %A Meisner, Aaron %A Miquel, Ramon %A Moustakas, John %A Mueller, Eva-Maria %A Newman, Jeffrey A. %A Nie, Jundan %A Percival, Will J. %A Poppett, Claire %A Qin, Fei %A Rossi, Graziano %A Samushia, Lado %A Sanchez, Eusebio %A Schlegel, David %A Schubnell, Michael %A Seo, Hee-Jong %A Tarlé, Gregory %A Vargas-Magaña, Mariana %A Weaver, Benjamin A. %A Yu, Jiaxi %A Zhang, Hanyu %A Zheng, Zheng %A Zhou, Zhimin %A Zou, Hu %+ AA(Institut de Recherche sur les Lois Fondamentales de l'Universe), AB(Institut de Recherche sur les Lois Fondamentales de l'Universe), AC(Institut de Recherche sur les Lois Fondamentales de l'Universe), AD(SLAC National Accelerator Laboratory, Menlo Park, CA 94305, U.S.A.), AE(Institut de Recherche sur les Lois Fondamentales de l'Universe), AF(The Ohio State University, Department of Physics; -; -), AG(Lawrence Berkeley National Laboratory, California), AH(Physics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, U.S.A.), AI(Tata Institute of Fundamental Research, India), AJ(University of Milan, Department of Physics), AK(University College London, Department of Physics and Astronomy), AL(Durham University, Department of Physics), AM(Department of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, U.S.A.), AN(UNAM, Institute of Physics), AO(University College London, Department of Physics and Astronomy), AP(Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, U.S.A.), AQ(The Ohio State University, Columbus, 43210 OH, U.S.A.), AR(University of the Andes, Colombia; -), AS(Center for Computational Astrophysics, Flatiron Institute, 162 5 th Avenue, New York, NY 10010, U.S.A.), AT(Lawrence Berkeley National Laboratory, California), AU(Centro de Investigación Avanzada en Física Fundamental (CIAFF), Facultad de Ciencias, Universidad Autónoma de Madrid, ES-28049 Madrid, Spain; Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049, Madrid, Spain), AV(Lawrence Berkeley National Laboratory, California), AW(Lawrence Berkeley National Laboratory, California; -), AX(Princeton University, Department of Astrophysical Sciences), AY(The Ohio State University, Department of Physics; The Ohio State University, Department of Physics; -), AZ(Lawrence Berkeley National Laboratory, California), BA(Lawrence Berkeley National Laboratory, California), BB(Department of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, U.S.A.), BC(Lawrence Berkeley National Laboratory, California), BD(Institute for High Energy Physics, Barcelona), BE(NSF's NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.A.), BF(Institucio Catalona de Recerca i Estudis Avancats; Institute for High Energy Physics, Barcelona), BG(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, U.S.A.), BH(University of Sussex, Department of Physics and Astronomy), BI(Department of Physics & Astronomy and Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, U.S.A.), BJ(CAS, National Astronomical Observatories), BK(University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada; University of Waterloo, Canada), BL(Lawrence Berkeley National Laboratory, California; -; -), BM(Korea Astronomy and Space Science Institute), BN(Sejong University, Seoul, Korea), BO(Abastumani Astrophysical Observatory; Kansas State University, Department of Physics; Ilia State University, Georgia), BP(Centro de Investigaciones Energeticas Medioambientales y Tecnologicas, Spain), BQ(Lawrence Berkeley National Laboratory, California), BR(University of Michigan, Department of Physics; University of Michigan), BS(Ohio University, Department of Physics and Astronomy), BT(University of Michigan), BU(UNAM, Institute of Physics), BV(NSF's NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.A.), BW(Ecole Polytechnique Federale de Lausanne), BX(Kansas State University, Department of Physics), BY(Department of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, U.S.A.), BZ(CAS, National Astronomical Observatories), CA(CAS, National Astronomical Observatories) %J Journal of Cosmology and Astroparticle Physics %V 2023 %D 2023 %8 October 01, 2023 %P 016 %K cosmological simulations; dark energy experiments; galaxy clustering; redshift surveys; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023JCAP...10..016R %X The One-Percent survey of the Dark Energy Spectroscopic Instrument collected ~ 270k emission line galaxies (ELGs) at 0.8 < z < 1.6. The high completeness of the sample allowed the clustering to be measured down to scales never probed before, 0.04 Mpc/h in rp for the projected 2-point correlation function (2PCF) and 0.17 Mpc/h in galaxy pair separation s for the 2PCF monopole and quadrupole. The most striking feature of the measurements is a strong signal at the smallest scales, below 0.2 Mpc/h in rp and 1 Mpc/h in s. We analyse these data in the halo occupation distribution framework. We consider different distributions for central galaxies, a standard power law for satellites with no condition on the presence of a central galaxy and explore several extensions of these models. For all considered models, the mean halo mass of the sample is found to be log10 ⟨Mh ⟩ ~ 11.9. We obtain a satellite mean occupation function which agrees with physically motivated ELG models only if we introduce central-satellite conformity, meaning that the satellite occupation is conditioned by the presence of central galaxies of the same type. To achieve in addition a good modelling of the clustering between 0.1 and 1 Mpc/h in rp , we allow for ELG positioning outside of the halo virial radius and find 0.5% of ELGs residing in the outskirts of halos. Furthermore, the satellite velocity dispersion inside halos is found to be ~ 30% larger than that of the halo dark matter particles. These are the main findings of our work. We investigate assembly bias as a function of halo concentration, local density or local density anisotropies and observe no significant change in our results. We split the data sample in two redshift bins and report no significant evolution with redshift. Lastly, changing the cosmology in the modelling impacts only slightly our results. %R 10.1088/1475-7516/2023/10/016 %= eprint: arXiv:2306.06319 %@ 1475-7516 %0 Journal Article %T JEMS: A Deep Medium-band Imaging Survey in the Hubble Ultra Deep Field with JWST NIRCam and NIRISS %A Williams, Christina C. %A Tacchella, Sandro %A Maseda, Michael V. %A Robertson, Brant E. %A Johnson, Benjamin D. %A Willott, Chris J. %A Eisenstein, Daniel J. %A Willmer, Christopher N. A. %A Ji, Zhiyuan %A Hainline, Kevin N. %A Helton, Jakob M. %A Alberts, Stacey %A Baum, Stefi %A Bhatawdekar, Rachana %A Boyett, Kristan %A Bunker, Andrew J. %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Curtis-Lake, Emma %A de Graaff, Anna %A Egami, Eiichi %A Franx, Marijn %A Kumari, Nimisha %A Maiolino, Roberto %A Nelson, Erica J. %A Rieke, Marcia J. %A Sandles, Lester %A Shivaei, Irene %A Simmonds, Charlotte %A Smit, Renske %A Suess, Katherine A. %A Sun, Fengwu %A Übler, Hannah %A Witstok, Joris %+ AA(National Optical Astronomy Observatory, Arizona; University of Arizona, Department of Astronomy and Steward Observatory), AB(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AC(University of Wisconsin, Madison, Department of Astronomy), AD(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AE(Harvard Smithsonian Center for Astrophysics), AF(Herzberg Institute for Astronomy and Astrophysics), AG(Harvard Smithsonian Center for Astrophysics), AH(University of Arizona, Department of Astronomy and Steward Observatory), AI(University of Arizona, Department of Astronomy and Steward Observatory), AJ(University of Arizona, Department of Astronomy and Steward Observatory), AK(University of Arizona, Department of Astronomy and Steward Observatory), AL(University of Arizona, Department of Astronomy and Steward Observatory), AM(Dept. of Physics & Astronomy, University of Manitoba, 30A Sifton Road, Winnipeg, MB R3T 2N2 Canada), AN(European Science and Astronomy Center), AO(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics), AP(University of Oxford, Department of Physics), AQ(Scuola Normale Superiore, Pisa, Italy), AR(Institut d'Astrophysique de Paris), AS(University of Oxford, Department of Physics), AT(University of Hertfordshire, School of Physics, Astronomy and Mathematics), AU(Max-Planck-Institute for Astronomy, Heidelberg), AV(University of Arizona, Department of Astronomy and Steward Observatory), AW(Leiden Observatory), AX(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AY(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AZ(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), BA(University of Arizona, Department of Astronomy and Steward Observatory), BB(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BC(University of Arizona, Department of Astronomy and Steward Observatory), BD(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BE(Liverpool John Moores University, Astrophysics Research Institute), BF(University of California, Santa Cruz, Department of Astronomy and Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology, California), BG(University of Arizona, Department of Astronomy and Steward Observatory), BH(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BI(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy) %J The Astrophysical Journal Supplement Series %V 268 %D 2023 %8 October 01, 2023 %P 64 %K Emission line galaxies; High-redshift galaxies; Redshift surveys; Extragalactic astronomy; 459; 734; 1378; 506; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023ApJS..268...64W %X We present JWST Extragalactic Medium-band Survey, the first public medium-band imaging survey carried out using JWST/NIRCam and NIRISS. These observations use ~2 and ~4 μm medium-band filters (NIRCam F182M, F210M, F430M, F460M, F480M; and NIRISS F430M and F480M in parallel) over 15.6 arcmin2 in the Hubble Ultra Deep Field (UDF), thereby building on the deepest multiwavelength public data sets available anywhere on the sky. We describe our science goals, survey design, NIRCam and NIRISS image reduction methods, and describe our first data release of the science-ready mosaics, which reach 5σ point-source limits (AB mag) of ~29.3-29.4 in 2 μm filters and ~28.2-28.7 at 4 μm. Our chosen filters create a JWST imaging survey in the UDF that enables novel analysis of a range of spectral features potentially across the redshift range of 0.3 < z < 20, including Paschen-α, Hα+[N II], and [O III]+Hβ emission at high spatial resolution. We find that our JWST medium-band imaging efficiently identifies strong line emitters (medium-band colors >1 mag) across redshifts 1.5 < z < 9.3, most prominently Hα+[N II] and [O III]+Hβ. We present our first data release including science-ready mosaics of each medium-band image available to the community, adding to the legacy value of past and future surveys in the UDF. This survey demonstrates the power of medium-band imaging with JWST, informing future extragalactic survey strategies using JWST observations. %R 10.3847/1538-4365/acf130 %= eprint: arXiv:2301.09780 %@ 0067-0049 %0 Journal Article %T Minor Merger Growth in Action: JWST Detects Faint Blue Companions around Massive Quiescent Galaxies at 0.5 ≤ z ≤ 3.0 %A Suess, Katherine A. %A Williams, Christina C. %A Robertson, Brant %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Nelson, Erica %A Alberts, Stacey %A Hainline, Kevin %A D'Eugenio, Francesco %A Übler, Hannah %A Rieke, Marcia %A Rieke, George %A Bunker, Andrew J. %A Carniani, Stefano %A Charlot, Stephane %A Eisenstein, Daniel J. %A Maiolino, Roberto %A Stark, Daniel P. %A Tacchella, Sandro %A Willott, Chris %+ AA(Kavli Institute for Particle Astrophysics and Cosmology, California), AB(National Optical Astronomy Observatory, Arizona), AC(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AD(University of Arizona, Department of Astronomy and Steward Observatory), AE(Harvard Smithsonian Center for Astrophysics), AF(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), AG(University of Arizona, Department of Astronomy and Steward Observatory), AH(University of Arizona, Department of Astronomy and Steward Observatory), AI(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AJ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AK(University of Arizona, Department of Astronomy and Steward Observatory), AL(Steward Observatory and Dept of Planetary Sciences, University of Arizona 933 N. Cherry Avenue Tucson, AZ 85721, USA), AM(University of Oxford, Department of Physics), AN(Scuola Normale Superiore, Pisa, Italy), AO(Institut d'Astrophysique de Paris), AP(Harvard Smithsonian Center for Astrophysics), AQ(Kavli Institute for Cosmology, UK; University of Cambridge, Department of Physics; University College London, Department of Physics and Astronomy), AR(University of Arizona, Department of Astronomy and Steward Observatory), AS(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AT(Herzberg Institute for Astronomy and Astrophysics) %J The Astrophysical Journal %V 956 %D 2023 %8 October 01, 2023 %P L42 %K Galaxy evolution; Galaxy formation; Galaxy structure; Elliptical galaxies; High-redshift galaxies; 594; 595; 622; 456; 734; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023ApJ...956L..42S %X Minor mergers are thought to drive the structural evolution of massive quiescent galaxies; however, existing Hubble Space Telescope (HST) imaging is primarily sensitive to stellar mass ratios ≳1:10. Here, we report the discovery of a large population of low-mass companions within 35 kpc of known $\mathrm{log}{M}_{* }/{M}_{\odot }rsim 10.5$ quiescent galaxies at 0.5 ≤ z ≤ 3. While massive companions like those identified by HST are rare, JWST imaging from the JWST Advanced Deep Extragalactic Survey reveals that the average massive quiescent galaxy hosts approximately five nearby companions with stellar mass ratios <1:10. Despite a median stellar mass ratio of just 1:900, these tiny companions are so numerous that they represent at least 30% of the total mass being added to quiescent galaxies via minor mergers. While relatively massive companions have colors similar to their hosts, companions with mass ratios <1:10 typically have bluer colors and lower mass-to-light ratios than their host galaxies at similar radii. The accretion of these tiny companions is likely to drive evolution in the color gradients and stellar population properties of the host galaxies. Our results suggest that the well-established "minor merger growth" model for quiescent galaxies extends down to very low mass ratios of ≲1:100, and demonstrates the power of JWST to constrain both the spatially resolved properties of massive galaxies and the properties of low-mass companions beyond the local Universe. %R 10.3847/2041-8213/acf5e6 %= eprint: arXiv:2307.14209 %@ 0004-637X %0 Journal Article %T Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane %A Kent, S. %A Neilsen, E. %A Honscheid, K. %A Rabinowitz, D. %A Schlafly, E. F. %A Guy, J. %A Schlegel, D. %A García-Bellido, J. %A Li, T. S. %A Sanchez, E. %A Silber, J. %A Aguilar, J. %A Ahlen, S. %A Brooks, D. %A Claybaugh, T. %A de la Macorra, A. %A Doel, P. %A Eisenstein, D. J. %A Fanning, K. %A Font-Ribera, A. %A Forero-Romero, J. E. %A Gontcho, S. Gontcho A. %A Jimenez, J. %A Kirkby, D. %A Kisner, T. %A Kremin, A. %A Landriau, M. %A Le Guillou, L. %A Levi, M. E. %A Magneville, C. %A Manera, M. %A Martini, P. %A Meisner, A. %A Miquel, R. %A Moustakas, J. %A Nie, J. %A Palanque-Delabrouille, N. %A Percival, W. J. %A Poppett, C. %A Rezaie, M. %A Ross, A. J. %A Rossi, G. %A Schubnell, M. %A Seo, H. %A Tarlé, Gregory %A Weaver, B. A. %A Zhou, R. %A Zhou, Z. %A Zou, H. %+ AA(Fermi National Accelerator Laboratory, Illinois; University of Chicago, Department of Astronomy and Astrophysics), AB(Fermi National Accelerator Laboratory, Illinois), AC(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Physics), AD(Physics Department, Yale University, P.O. Box 208120, New Haven, CT 06511, USA), AE(Space Telescope Science Institute, Baltimore, Maryland), AF(Lawrence Berkeley National Laboratory, California), AG(Lawrence Berkeley National Laboratory, California), AH(Autonomous University of Madrid, Department of Physics), AI(University of Toronto, Department of Astronomy and Astrophysics), AJ(Centro de Investigaciones Energeticas Medioambientales y Tecnologicas, Spain), AK(Lawrence Berkeley National Laboratory, California), AL(Lawrence Berkeley National Laboratory, California), AM(Boston University, Department of Physics), AN(University College London, Department of Physics and Astronomy), AO(Lawrence Berkeley National Laboratory, California), AP(UNAM, Institute of Physics), AQ(University College London, Department of Physics and Astronomy), AR(Harvard Smithsonian Center for Astrophysics), AS(The Ohio State University), AT(Institute for High Energy Physics, Barcelona), AU(University of the Andes, Colombia; -), AV(Lawrence Berkeley National Laboratory, California), AW(Institute for High Energy Physics, Barcelona), AX(University of California, Irvine, Department of Physics and Astronomy), AY(Lawrence Berkeley National Laboratory, California), AZ(Lawrence Berkeley National Laboratory, California), BA(Lawrence Berkeley National Laboratory, California), BB(Laboratoire de Physique Nucleaire et de Hautes Energies), BC(Lawrence Berkeley National Laboratory, California), BD(Institut de Recherche sur les Lois Fondamentales de l'Universe), BE(Institute for High Energy Physics, Barcelona; Autonomous University of Barcelona, Department of Physics), BF(The Ohio State University, Department of Astronomy; The Ohio State University; The Ohio State University, Department of Astronomy), BG(National Optical Astronomy Observatory, Arizona), BH(Institute for High Energy Physics, Barcelona; Institucio Catalona de Recerca i Estudis Avancats), BI(Siena College, New York), BJ(CAS, National Astronomical Observatories), BK(Lawrence Berkeley National Laboratory, California; Institut de Recherche sur les Lois Fondamentales de l'Universe), BL(University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada; University of Waterloo, Canada), BM(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory; University of California, Berkeley), BN(Kansas State University, Department of Physics), BO(The Ohio State University, Department of Astronomy; The Ohio State University; The Ohio State University, Department of Astronomy), BP(Sejong University, Department of Astronomy), BQ(University of Michigan, Department of Physics; University of Michigan), BR(Ohio University, Department of Physics and Astronomy), BS(University of Michigan), BT(National Optical Astronomy Observatory, Arizona), BU(Lawrence Berkeley National Laboratory, California), BV(CAS, National Astronomical Observatories), BW(CAS, National Astronomical Observatories) %J The Astronomical Journal %V 166 %D 2023 %8 October 01, 2023 %P 177 %K Astronomical techniques; Wide-field telescopes; Calibration; 1684; 1800; 2179; Astrophysics - Instrumentation and Methods for Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023AJ....166..177K %X The Dark Energy Spectroscopic Instrument, consisting of 5020 robotic fiber positioners and associated systems on the Mayall telescope at Kitt Peak, Arizona, is carrying out a survey to measure the spectra of 40 million galaxies and quasars and produce the largest 3D map of the universe to date. The primary science goal is to use baryon acoustic oscillations to measure the expansion history of the universe and the time evolution of dark energy. A key function of the online control system is to position each fiber on a particular target in the focal plane with an accuracy of 11 μm rms 2D. This paper describes the set of software programs used to perform this function along with the methods used to validate their performance. %R 10.3847/1538-3881/acf7c3 %= eprint: arXiv:2307.06238 %@ 0004-6256 %0 Journal Article %T JADES: Discovery of extremely high equivalent width Lyman-α emission from a faint galaxy within an ionized bubble at z = 7.3 %A Saxena, Aayush %A Robertson, Brant E. %A Bunker, Andrew J. %A Endsley, Ryan %A Cameron, Alex J. %A Charlot, Stephane %A Simmonds, Charlotte %A Tacchella, Sandro %A Witstok, Joris %A Willott, Chris %A Carniani, Stefano %A Curtis-Lake, Emma %A Ferruit, Pierre %A Jakobsen, Peter %A Arribas, Santiago %A Chevallard, Jacopo %A Curti, Mirko %A D'Eugenio, Francesco %A De Graaff, Anna %A Jones, Gareth C. %A Looser, Tobias J. %A Maseda, Michael V. %A Rawle, Tim %A Rix, Hans-Walter %A Del Pino, Bruno Rodríguez %A Smit, Renske %A Übler, Hannah %A Eisenstein, Daniel J. %A Hainline, Kevin %A Hausen, Ryan %A Johnson, Benjamin D. %A Rieke, Marcia %A Williams, Christina C. %A Willmer, Christopher N. A. %A Baker, William M. %A Bhatawdekar, Rachana %A Bowler, Rebecca %A Boyett, Kristan %A Chen, Zuyi %A Egami, Eiichi %A Ji, Zhiyuan %A Kumari, Nimisha %A Nelson, Erica %A Perna, Michele %A Sandles, Lester %A Scholtz, Jan %A Shivaei, Irene %+ AA(University of Oxford, Department of Physics; University College London, Department of Physics and Astronomy), AB(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AC(University of Oxford, Department of Physics), AD(University of Texas, Austin, Department of Astronomy), AE(University of Oxford, Department of Physics), AF(Institut d'Astrophysique de Paris), AG(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AH(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AI(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AJ(Herzberg Institute for Astronomy and Astrophysics), AK(Scuola Normale Superiore, Pisa, Italy), AL(Center for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatfield, AL10 9AB, UK), AM(European Science and Astronomy Center), AN(Niels Bohr Institute for Astronomy, Physics and Geophysics; Niels Bohr Institute for Astronomy, Physics and Geophysics), AO(Center for Astrobiology, Madrid), AP(University of Oxford, Department of Physics), AQ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; European Southern Observatory, Germany), AR(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AS(Max-Planck-Institute for Astronomy, Heidelberg), AT(University of Oxford, Department of Physics), AU(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AV(University of Wisconsin, Madison, Department of Astronomy), AW(European Space Agency, Space Telescope Science Institute, Baltimore, MA, USA), AX(Max-Planck-Institute for Astronomy, Heidelberg), AY(Center for Astrobiology, Madrid), AZ(Liverpool John Moores University, Astrophysics Research Institute), BA(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BB(Centre for Astrophysics, Harvard & Smithsonian, 60 Garden St., Cambridge, MA, 02138, USA), BC(University of Arizona, Department of Astronomy and Steward Observatory), BD(Johns Hopkins University, Department of Physics and Astronomy), BE(Centre for Astrophysics, Harvard & Smithsonian, 60 Garden St., Cambridge, MA, 02138, USA), BF(University of Arizona, Department of Astronomy and Steward Observatory), BG(National Optical Astronomy Observatory, Arizona), BH(University of Arizona, Department of Astronomy and Steward Observatory), BI(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BJ(European Science and Astronomy Center; European Space Research and Technology Centre), BK(Jodrell Bank Centre for Astrophysics), BL(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics in 3D), BM(University of Arizona, Department of Astronomy and Steward Observatory), BN(University of Arizona, Department of Astronomy and Steward Observatory), BO(University of Arizona, Department of Astronomy and Steward Observatory), BP(AURA for European Space Agency, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21210, USA), BQ(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), BR(Center for Astrobiology, Madrid), BS(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BT(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), BU(University of Arizona, Department of Astronomy and Steward Observatory) %J Astronomy and Astrophysics %V 678 %D 2023 %8 October 01, 2023 %P A68 %K dark ages; reionization; first stars; galaxies: high-redshift; galaxies: evolution; galaxies: star formation; Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023A&A...678A..68S %X We report the discovery of a remarkable Lyα emitting galaxy at z = 7.2782, JADES-GS+53.16746−27.7720 (shortened to JADES-GS-z7-LA), with rest-frame equivalent width, EW0(Lyα) = 388.0 ± 88.8 Å and UV magnitude −17.0. The spectroscopic redshift is confirmed via rest-frame optical lines [O II], Hβ and [O III] in its JWST/NIRSpec Micro-Shutter Assembly (MSA) spectrum. The Lyα line is detected in both lower resolution (R ∼ 100) PRISM as well as medium resolution (R ∼ 1000) G140M grating spectra. The line spread function-deconvolved Lyα full width at half maximum in the grating is 383.9 ± 56.2 km s−1 and the Lyα velocity offset compared to the systemic redshift is 113.3 ± 80.0 km s−1, indicative of very little neutral gas or dust within the galaxy. We estimate the Lyα escape fraction to be > 70%. JADES-GS-z7-LA has a [O III]/[O II] ratio (O32) of 11.1 ± 2.2 and a ([O III] + [O II])/Hβ ratio (R23) of 11.2 ± 2.6, consistent with low metallicity and high ionization parameters. Deep NIRCam imaging also revealed a close companion source (separated by 0.23″), which exhibits similar photometry to that of JADES-GS-z7-LA, with a photometric excess in the F410M NIRCam image consistent with [O III] + Hβ emission at the same redshift. The spectral energy distribution of JADES-GS-z7-LA indicates a "bursty" star formation history, with a low stellar mass of ≈107 M⊙. Assuming that the Lyα transmission through the intergalactic medium is the same as its measured escape fraction, an ionized region of size > 1.5 pMpc is needed to explain the high Lyα EW and low velocity offset compared to systemic seen in JADES-GS-z7-LA. Owing to its UV-faintness, we show that it is incapable of single-handedly ionizing a region large enough to explain its Lyα emission. Therefore, we suggest that JADES-GS-z7-LA (and possibly the companion source) may be a part of a larger overdensity, presenting direct evidence of overlapping ionized bubbles at z > 7. %R 10.1051/0004-6361/202346245 %= eprint: arXiv:2302.12805 %@ 0004-6361 %0 Electronic Article %T Cosmological constraints from density-split clustering in the BOSS CMASS galaxy sample %A Paillas, Enrique %A Cuesta-Lazaro, Carolina %A Percival, Will J. %A Nadathur, Seshadri %A Cai, Yan-Chuan %A Yuan, Sihan %A Beutler, Florian %A de Mattia, Arnaud %A Eisenstein, Daniel %A Forero-Sanchez, Daniel %A Padilla, Nelson %A Pinon, Mathilde %A Ruhlmann-Kleider, Vanina %A Sánchez, Ariel G. %A Valogiannis, Georgios %A Zarrouk, Pauline %J arXiv e-prints %D 2023 %8 September 01, 2023 %P arXiv:2309.16541 %K Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023arXiv230916541P %Z Submitted to MNRAS. Source code to generate the figures available in the captions. Updated to add missing references and fix legend of Fig. 6 %X We present a clustering analysis of the BOSS DR12 CMASS galaxy sample, combining measurements of the galaxy two-point correlation function and density-split clustering down to a scale of $1\,h^{-1}{\rm Mpc}$. Our theoretical framework is based on emulators trained on high-fidelity mock galaxy catalogues that forward model the cosmological dependence of the clustering statistics within an extended-$\Lambda$CDM framework, including redshift-space and Alcock-Paczynski distortions. Our base-$\Lambda$CDM analysis finds $\omega_{\rm cdm} = 0.1201\pm 0.0022$, $\sigma_8 = 0.792\pm 0.034$, and $n_s = 0.970\pm 0.018$, corresponding to $f\sigma_8 = 0.462\pm 0.020$ at $z \approx 0.525$, which is in agreement with Planck 2018 predictions and various clustering studies in the literature. We test single-parameter extensions to base-$\Lambda$CDM, varying the running of the spectral index, the dark energy equation of state, and the density of massless relic neutrinos, finding no compelling evidence for deviations from the base model. We model the galaxy-halo connection using a halo occupation distribution framework, finding signatures of environment-based assembly bias in the data. We validate our pipeline against mock catalogues that match the clustering and selection properties of CMASS, showing that we can recover unbiased cosmological constraints even with a volume 84 times larger than the one used in this study. %R 10.48550/arXiv.2309.16541 %= eprint: arXiv:2309.16541 %0 Electronic Article %T SUNBIRD: A simulation-based model for full-shape density-split clustering %A Cuesta-Lazaro, Carolina %A Paillas, Enrique %A Yuan, Sihan %A Cai, Yan-Chuan %A Nadathur, Seshadri %A Percival, Will J. %A Beutler, Florian %A de Mattia, Arnaud %A Eisenstein, Daniel %A Forero-Sanchez, Daniel %A Padilla, Nelson %A Pinon, Mathilde %A Ruhlmann-Kleider, Vanina %A Sánchez, Ariel G. %A Valogiannis, Georgios %A Zarrouk, Pauline %J arXiv e-prints %D 2023 %8 September 01, 2023 %P arXiv:2309.16539 %K Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023arXiv230916539C %Z Submitted to MNRAS. Source code to generate the figures available in the captions. Updated to add missing references %X Combining galaxy clustering information from regions of different environmental densities can help break cosmological parameter degeneracies and access non-Gaussian information from the density field that is not readily captured by the standard two-point correlation function (2PCF) analyses. However, modelling these density-dependent statistics down to the non-linear regime has so far remained challenging. We present a simulation-based model that is able to capture the cosmological dependence of the full shape of the density-split clustering (DSC) statistics down to intra-halo scales. Our models are based on neural-network emulators that are trained on high-fidelity mock galaxy catalogues within an extended-$\Lambda$CDM framework, incorporating the effects of redshift-space, Alcock-Paczynski distortions and models of the halo-galaxy connection. Our models reach sub-percent level accuracy down to $1\,h^{-1}{\rm Mpc}$ and are robust against different choices of galaxy-halo connection modelling. When combined with the galaxy 2PCF, DSC can tighten the constraints on $\omega_{\rm cdm}$, $\sigma_8$, and $n_s$ by factors of 2.9, 1.9, and 2.1, respectively, compared to a 2PCF-only analysis. DSC additionally puts strong constraints on environment-based assembly bias parameters. Our code is made publicly available on Github. %R 10.48550/arXiv.2309.16539 %= eprint: arXiv:2309.16539 %0 Electronic Article %T Brown Dwarf Candidates in the JADES and CEERS Extragalactic Surveys %A Hainline, Kevin N. %A Helton, Jakob M. %A Johnson, Benjamin D. %A Sun, Fengwu %A Topping, Michael W. %A Leisenring, Jarron M. %A Baker, William M. %A Eisenstein, Daniel J. %A Hausen, Ryan %A Hviding, Raphael E. %A Lyu, Jianwei %A Robertson, Brant %A Tacchella, Sandro %A Williams, Christina C. %A Willmer, Christopher N. A. %A Roellig, Thomas L. %J arXiv e-prints %D 2023 %8 September 01, 2023 %P arXiv:2309.03250 %K Astrophysics - Solar and Stellar Astrophysics; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230903250H %Z 22 pages, 9 figures, accepted by ApJ (January 18, 2024) %X By combining the JWST/NIRCam JADES and CEERS extragalactic datasets, we have uncovered a sample of twenty-one T and Y brown dwarf candidates at best-fit distances between 0.1 - 4.2 kpc. These sources were selected by targeting the blue 1$\mu$m - 2.5$\mu$m colors and red 3$\mu$m - 4.5$\mu$m colors that arise from molecular absorption in the atmospheres of T$_{\mathrm{eff}} < $ 1300K brown dwarfs. We fit these sources using multiple models of low-mass stellar atmospheres and present the resulting fluxes, sizes, effective temperatures and other derived properties for the sample. If confirmed, these fits place the majority of the sources in the Milky Way thick disk and halo. We observe proper motion for seven of the candidate brown dwarfs with directions in agreement with the plane of our galaxy, providing evidence that they are not extragalactic in nature. We demonstrate how the colors of these sources differ from selected high-redshift galaxies, and explore the selection of these sources in planned large-area JWST NIRCam surveys. Deep imaging with JWST/NIRCam presents an an excellent opportunity for finding and understanding these very cold low-mass stars at kpc distances. %R 10.48550/arXiv.2309.03250 %= eprint: arXiv:2309.03250 %0 Journal Article %T Carbonaceous dust grains seen in the first billion years of cosmic time %A Witstok, Joris %A Shivaei, Irene %A Smit, Renske %A Maiolino, Roberto %A Carniani, Stefano %A Curtis-Lake, Emma %A Ferruit, Pierre %A Arribas, Santiago %A Bunker, Andrew J. %A Cameron, Alex J. %A Charlot, Stephane %A Chevallard, Jacopo %A Curti, Mirko %A de Graaff, Anna %A D'Eugenio, Francesco %A Giardino, Giovanna %A Looser, Tobias J. %A Rawle, Tim %A Rodríguez del Pino, Bruno %A Willott, Chris %A Alberts, Stacey %A Baker, William M. %A Boyett, Kristan %A Egami, Eiichi %A Eisenstein, Daniel J. %A Endsley, Ryan %A Hainline, Kevin N. %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Kumari, Nimisha %A Lyu, Jianwei %A Nelson, Erica %A Perna, Michele %A Rieke, Marcia %A Robertson, Brant E. %A Sandles, Lester %A Saxena, Aayush %A Scholtz, Jan %A Sun, Fengwu %A Tacchella, Sandro %A Williams, Christina C. %A Willmer, Christopher N. A. %+ AA(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AB(University of Arizona, Department of Astronomy and Steward Observatory), AC(Liverpool John Moores University, Astrophysics Research Institute), AD(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), AE(Scuola Normale Superiore, Pisa, Italy), AF(University of Hertfordshire, School of Physics, Astronomy and Mathematics), AG(European Science and Astronomy Center), AH(Center for Astrobiology, Madrid), AI(University of Oxford, Department of Physics), AJ(University of Oxford, Department of Physics), AK(Institut d'Astrophysique de Paris), AL(University of Oxford, Department of Physics), AM(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; European Southern Observatory, Germany), AN(Max-Planck-Institute for Astronomy, Heidelberg), AO(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AP(European Space Research and Technology Centre), AQ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AR(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AS(Center for Astrobiology, Madrid), AT(Herzberg Institute for Astronomy and Astrophysics), AU(University of Arizona, Department of Astronomy and Steward Observatory), AV(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AW(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics), AX(University of Arizona, Department of Astronomy and Steward Observatory), AY(Harvard Smithsonian Center for Astrophysics), AZ(University of Texas, Austin, Department of Astronomy), BA(University of Arizona, Department of Astronomy and Steward Observatory), BB(University of Arizona, Department of Astronomy and Steward Observatory), BC(Harvard Smithsonian Center for Astrophysics), BD(AURA for European Space Agency, Space Telescope Science Institute, Baltimore, MD, USA), BE(University of Arizona, Department of Astronomy and Steward Observatory), BF(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), BG(Center for Astrobiology, Madrid), BH(University of Arizona, Department of Astronomy and Steward Observatory), BI(University of California, Santa Cruz, Department of Astronomy and Astrophysics), BJ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BK(University College London, Department of Physics and Astronomy; University of Oxford, Department of Physics), BL(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BM(University of Arizona, Department of Astronomy and Steward Observatory), BN(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BO(National Optical Astronomy Observatory, Arizona), BP(University of Arizona, Department of Astronomy and Steward Observatory) %J Nature %V 621 %D 2023 %8 September 01, 2023 %P 267-270 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023Natur.621..267W %X Large dust reservoirs (up to approximately 108 M⊙) have been detected1-3 in galaxies out to redshift z ≃ 8, when the age of the Universe was only about 600 Myr. Generating substantial amounts of dust within such a short timescale has proven challenging for theories of dust formation4,5 and has prompted the revision of the modelling of potential sites of dust production6-8, such as the atmospheres of asymptotic giant branch stars in low-metallicity environments, supernova ejecta and the accelerated growth of grains in the interstellar medium. However, degeneracies between different evolutionary pathways remain when the total dust mass of galaxies is the only available observable. Here we report observations of the 2,175 Å dust attenuation feature, which is well known in the Milky Way and galaxies at z ≲ 3 (refs. 9-11), in the near-infrared spectra of galaxies up to z ≃ 7, corresponding to the first billion years of cosmic time. The relatively short timescale implied for the formation of carbonaceous grains giving rise to this feature12 suggests a rapid production process, possibly in Wolf-Rayet stars or supernova ejecta. %R 10.1038/s41586-023-06413-w %= eprint: arXiv:2302.05468 %@ 0028-0836 %0 Journal Article %T Validation of semi-analytical, semi-empirical covariance matrices for two-point correlation function for early DESI data %A Rashkovetskyi, Michael %A Eisenstein, Daniel J. %A Aguilar, Jessica Nicole %A Brooks, David %A Claybaugh, Todd %A Cole, Shaun %A Dawson, Kyle %A de la Macorra, Axel %A Doel, Peter %A Fanning, Kevin %A Font-Ribera, Andreu %A Forero-Romero, Jaime E. %A Gontcho A Gontcho, Satya %A Hahn, ChangHoon %A Honscheid, Klaus %A Kehoe, Robert %A Kisner, Theodore %A Landriau, Martin %A Levi, Michael %A Manera, Marc %A Miquel, Ramon %A Moon, Jeongin %A Nadathur, Seshadri %A Nie, Jundan %A Poppett, Claire %A Ross, Ashley J. %A Rossi, Graziano %A Sanchez, Eusebio %A Saulder, Christoph %A Schubnell, Michael %A Seo, Hee-Jong %A Tarle, Gregory %A Valcin, David %A Weaver, Benjamin Alan %A Zhao, Cheng %A Zhou, Zhimin %A Zou, Hu %+ AA(Harvard Smithsonian Center for Astrophysics), AB(Harvard Smithsonian Center for Astrophysics), AC(Lawrence Berkeley National Laboratory, California), AD(University College London, Department of Physics and Astronomy), AE(Lawrence Berkeley National Laboratory, California), AF(Durham University, Department of Physics), AG(University of Utah, Department of Physics and Astronomy), AH(UNAM, Institute of Physics), AI(University College London, Department of Physics and Astronomy), AJ(The Ohio State University, Department of Astronomy), AK(Institute for High Energy Physics, Barcelona), AL(Departamento de Física & Observatorio Astronómico, Universidad de los Andes, Cra. 1 No. 18A-10, Edificio Ip, CP 111711, Bogotá, Colombia), AM(Lawrence Berkeley National Laboratory, California), AN(Princeton University, Department of Astrophysical Sciences), AO(The Ohio State University, Department of Astronomy), AP(Southern Methodist University, Texas), AQ(Lawrence Berkeley National Laboratory, California), AR(Lawrence Berkeley National Laboratory, California), AS(Lawrence Berkeley National Laboratory, California), AT(Institute for High Energy Physics, Barcelona), AU(Institute for High Energy Physics, Barcelona; Institucio Catalona de Recerca i Estudis Avancats), AV(Sejong University, Seoul, Korea; Max-Planck-Institute for Astrophysics, Garching), AW(University of Portsmouth, Institute of Cosmology and Gravitation), AX(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, PR China), AY(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory), AZ(The Ohio State University, Department of Astronomy), BA(Sejong University, Seoul, Korea), BB(Centro de Investigaciones Energeticas Medioambientales y Tecnologicas, Spain), BC(Korea Astronomy and Space Science Institute), BD(University of Michigan, Department of Physics), BE(Ohio University, Department of Physics and Astronomy), BF(University of Michigan, Department of Physics), BG(Ohio University, Department of Physics and Astronomy), BH(National Optical Astronomy Observatory, Arizona), BI(Department of Astronomy, Tsinghua University, 30 Shuangqing Road, Haidian District, Beijing, 100190, China; Ecole Polytechnique Fédérale de Lausanne, CH-1015 Lausanne, Switzerland), BJ(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, PR China), BK(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100012, PR China) %J Monthly Notices of the Royal Astronomical Society %V 524 %D 2023 %8 September 01, 2023 %P 3894-3911 %K methods: statistical; surveys; software: data analysis; galaxies: statistics; large-scale structure of Universe; cosmology: theory; Astrophysics - Cosmology and Nongalactic Astrophysics; Mathematics - Statistics Theory; Physics - Data Analysis; Statistics and Probability %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.3894R %X We present an extended validation of semi-analytical, semi-empirical covariance matrices for the two-point correlation function (2PCF) on simulated catalogs representative of luminous red galaxies (LRGs) data collected during the initial 2 months of operations of the Stage-IV ground-based Dark Energy Spectroscopic Instrument (DESI). We run the pipeline on multiple effective Zel'dovich (EZ) mock galaxy catalogs with the corresponding cuts applied and compare the results with the mock sample covariance to assess the accuracy and its fluctuations. We propose an extension of the previously developed formalism for catalogs processed with standard reconstruction algorithms. We consider methods for comparing covariance matrices in detail, highlighting their interpretation and statistical properties caused by sample variance, in particular, non-trivial expectation values of certain metrics even when the external covariance estimate is perfect. With improved mocks and validation techniques, we confirm a good agreement between our predictions and sample covariance. This allows one to generate covariance matrices for comparable data sets without the need to create numerous mock galaxy catalogs with matching clustering, only requiring 2PCF measurements from the data itself. The code used in this paper is publicly available at https://github.com/oliverphilcox/RascalC. %R 10.1093/mnras/stad2078 %= eprint: arXiv:2306.06320 %@ 0035-8711 %0 Journal Article %T The MillenniumTNG Project: refining the one-halo model of red and blue galaxies at different redshifts %A Hadzhiyska, Boryana %A Hernquist, Lars %A Eisenstein, Daniel %A Delgado, Ana Maria %A Bose, Sownak %A Kannan, Rahul %A Pakmor, Rüdiger %A Springel, Volker %A Contreras, Sergio %A Barrera, Monica %A Ferlito, Fulvio %A Hernández-Aguayo, César %A White, Simon D. M. %A Frenk, Carlos %+ AA(Harvard Smithsonian Center for Astrophysics; University of California, Berkeley; Lawrence Berkeley National Laboratory, Physics Division), AB(Harvard Smithsonian Center for Astrophysics), AC(Harvard Smithsonian Center for Astrophysics), AD(Harvard Smithsonian Center for Astrophysics), AE(Durham University, Department of Physics), AF(Harvard Smithsonian Center for Astrophysics; York University, Department of Physics and Astronomy), AG(Max-Planck-Institute for Astrophysics, Garching), AH(Max-Planck-Institute for Astrophysics, Garching), AI(Donostia International Physics Center, Manuel Lardizabal Ibilbidea, 4, 20018 Donostia, Gipuzkoa, Spain), AJ(Max-Planck-Institute for Astrophysics, Garching), AK(Max-Planck-Institute for Astrophysics, Garching), AL(Max-Planck-Institute for Astrophysics, Garching; Max Planck Society for the Advancement of Science, Germany), AM(York University, Department of Physics and Astronomy), AN(Durham University, Department of Physics) %J Monthly Notices of the Royal Astronomical Society %V 524 %D 2023 %8 September 01, 2023 %P 2524-2538 %K galaxies: haloes; large-scale structure of Universe; cosmology: theory; Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.2524H %X Luminous red galaxies (LRGs) and blue star-forming emission-line galaxies (ELGs) are key tracers of large-scale structure used by cosmological surveys. Theoretical predictions for such data are often done via simplistic models for the galaxy-halo connection. In this work, we use the large, high-fidelity hydrodynamical simulation of the MillenniumTNG project (MTNG) to inform a new phenomenological approach for obtaining an accurate and flexible galaxy-halo model on small scales. Our aim is to study LRGs and ELGs at two distinct epochs, z = 1 and z = 0, and recover their clustering down to very small scales, $r \sim 0.1 \ h^{-1}\, {\rm Mpc}$, i.e. the one-halo regime, while a companion paper extends this to a two-halo model for larger distances. The occupation statistics of ELGs in MTNG inform us that (1) the satellite occupations exhibit a slightly super-Poisson distribution, contrary to commonly made assumptions, and (2) that haloes containing at least one ELG satellite are twice as likely to host a central ELG. We propose simple recipes for modelling these effects, each of which calls for the addition of a single free parameter to simpler halo occupation models. To construct a reliable satellite population model, we explore the LRG and ELG satellite radial and velocity distributions and compare them with those of subhaloes and particles in the simulation. We find that ELGs are anisotropically distributed within haloes, which together with our occupation results provides strong evidence for cooperative galaxy formation (manifesting itself as one-halo galaxy conformity); i.e. galaxies with similar properties form in close proximity to each other. Our refined galaxy-halo model represents a useful improvement of commonly used analysis tools and thus can be of help to increase the constraining power of large-scale structure surveys. %R 10.1093/mnras/stad279 %= eprint: arXiv:2210.10068 %@ 0035-8711 %0 Journal Article %T The MillenniumTNG Project: an improved two-halo model for the galaxy-halo connection of red and blue galaxies %A Hadzhiyska, Boryana %A Eisenstein, Daniel %A Hernquist, Lars %A Pakmor, Rüdiger %A Bose, Sownak %A Delgado, Ana Maria %A Contreras, Sergio %A Kannan, Rahul %A White, Simon D. M. %A Springel, Volker %A Frenk, Carlos %A Hernández-Aguayo, César %A Barrera, Fulvio Ferlito %A Monica %+ AA(Harvard Smithsonian Center for Astrophysics; University of California, Berkeley; Lawrence Berkeley National Laboratory, Physics Division), AB(Harvard Smithsonian Center for Astrophysics), AC(Harvard Smithsonian Center for Astrophysics), AD(Max-Planck-Institute for Astrophysics, Garching), AE(Durham University, Department of Physics), AF(Harvard Smithsonian Center for Astrophysics), AG(Donostia International Physics Center (DIPC), Donostia-San Sebastian, Manuel Lardizabal Ibilbidea, 4, 20018, Spain), AH(Harvard Smithsonian Center for Astrophysics; York University, Department of Physics and Astronomy), AI(Max-Planck-Institute for Astrophysics, Garching), AJ(Max-Planck-Institute for Astrophysics, Garching), AK(Durham University, Department of Physics), AL(Max-Planck-Institute for Astrophysics, Garching; Max Planck Society for the Advancement of Science, Germany), AM(Max-Planck-Institute for Astrophysics, Garching) %J Monthly Notices of the Royal Astronomical Society %V 524 %D 2023 %8 September 01, 2023 %P 2507-2523 %K galaxies: haloes; large-scale structure of Universe; cosmology: theory; Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.2507H %X Approximate methods to populate dark-matter haloes with galaxies are of great utility to galaxy surveys. However, the limitations of simple halo occupation models (HODs) preclude a full use of small-scale galaxy clustering data and call for more sophisticated models. We study two galaxy populations, luminous red galaxies (LRGs) and star-forming emission-line galaxies (ELGs), at two epochs, z = 1 and z = 0, in the large-volume, high-resolution hydrodynamical simulation of the MillenniumTNG project. In a partner study we concentrated on the small-scale, one-halo regime down to r ~ 0.1 h-1 Mpc, while here we focus on modelling galaxy assembly bias in the two-halo regime, r ≳ 1 h-1 Mpc. Interestingly, the ELG signal exhibits scale dependence out to relatively large scales (r ~ 20 h-1 Mpc), implying that the linear bias approximation for this tracer is invalid on these scales, contrary to common assumptions. The 10-15 per cent discrepancy is only reconciled when we augment our halo occupation model with a dependence on extrinsic halo properties ('shear' being the best-performing one) rather than intrinsic ones (e.g. concentration, peak mass). We argue that this fact constitutes evidence for two-halo galaxy conformity. Including tertiary assembly bias (i.e. a property beyond mass and 'shear') is not an essential requirement for reconciling the galaxy assembly bias signal of LRGs, but the combination of external and internal properties is beneficial for recovering ELG the clustering. We find that centrals in low-mass haloes dominate the assembly bias signal of both populations. Finally, we explore the predictions of our model for higher order statistics such as nearest neighbour counts. The latter supplies additional information about galaxy assembly bias and can be used to break degeneracies between halo model parameters. %R 10.1093/mnras/stad731 %= eprint: arXiv:2210.10072 %@ 0035-8711 %0 Journal Article %T Planting a Lyman alpha forest on ABACUSSUMMIT %A Hadzhiyska, Boryana %A Font-Ribera, A. %A Cuceu, A. %A Chabanier, S. %A Aguilar, J. %A Brooks, D. %A de la Macorra, A. %A Doel, P. %A Eisenstein, D. J. %A Forero-Romero, J. E. %A Gontcho A Gontcho, S. %A Honscheid, K. %A Kehoe, R. %A Landriau, M. %A Miquel, R. %A Nie, Jundan %A Percival, W. J. %A Rossi, G. %A Tarlé, Gregory %A Zhou, Zhimin %+ AA(Lawrence Berkeley National Laboratory, California; University of California, Berkeley), AB(Institute for High Energy Physics, Barcelona), AC(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Physics; The Ohio State University), AD(Lawrence Berkeley National Laboratory, California), AE(Lawrence Berkeley National Laboratory, California), AF(University College London, Department of Physics and Astronomy), AG(Instituto de Física, Universidad Nacional Autónoma de México, Sendero Bicipuma, C.U., Coyoacán, 04510, Ciudad de México, CDMX, México), AH(University College London, Department of Physics and Astronomy), AI(Harvard Smithsonian Center for Astrophysics), AJ(University of the Andes, Colombia), AK(Lawrence Berkeley National Laboratory, California), AL(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Physics; The Ohio State University), AM(Southern Methodist University, Texas), AN(Lawrence Berkeley National Laboratory, California), AO(Institute for High Energy Physics, Barcelona; Institucio Catalona de Recerca i Estudis Avancats), AP(CAS, National Astronomical Observatories), AQ(University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada; University of Waterloo, Canada), AR(Sejong University, Seoul, Korea), AS(University of Michigan), AT(CAS, National Astronomical Observatories) %J Monthly Notices of the Royal Astronomical Society %V 524 %D 2023 %8 September 01, 2023 %P 1008-1024 %K methods: numerical; quasars: absorption lines; cosmology: theory; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.1008H %X The full-shape correlations of the Lyman alpha (Ly α) forest contain a wealth of cosmological information through the Alcock-Paczyński effect. However, these measurements are challenging to model without robustly testing and verifying the theoretical framework used for analysing them. Here, we leverage the accuracy and volume of the N-body simulation suite ABACUSSUMMIT to generate high-resolution Ly α skewers and quasi-stellar object (QSO) catalogues. One of the main goals of our mocks is to aid in the full-shape Ly α analysis planned by the Dark Energy Spectroscopic Instrument (DESI) team. We provide optical depth skewers for six of the fiducial cosmology base-resolution simulations ($L_{\rm box} = 2\, h^{-1}\, {\rm Gpc}$, N = 69123) at z = 2.5. We adopt a simple recipe based on the Fluctuating Gunn-Peterson Approximation (FGPA) for constructing these skewers from the matter density in an N-body simulation and calibrate it against the 1D and 3D Ly α power spectra extracted from the hydrodynamical simulation IllustrisTNG (TNG; $L_{\rm box} = 205\, h^{-1}\, {\rm Mpc}$, N = 25003). As an important application, we study the non-linear broadening of the baryon acoustic oscillation (BAO) peak and show the cross-correlation between DESI-like QSOs and our Ly α forest skewers. We find differences on small scales between the Kaiser approximation prediction and our mock measurements of the Ly α × QSO cross-correlation, which would be important to account for in upcoming analyses. The ABACUSSUMMIT Ly α forest mocks open up the possibility for improved modelling of cross-correlations between Ly α and cosmic microwave background (CMB) lensing and Ly α and QSOs, and for forecasts of the 3-point Ly α correlation function. Our catalogues and skewers are publicly available on Globus via the National Energy Research Scientific Computing Center (NERSC) (full link under the section 'Data Availability'). %R 10.1093/mnras/stad1920 %= eprint: arXiv:2305.08899 %@ 0035-8711 %0 Journal Article %T JADES: Probing interstellar medium conditions at z ∼ 5.5-9.5 with ultra-deep JWST/NIRSpec spectroscopy %A Cameron, Alex J. %A Saxena, Aayush %A Bunker, Andrew J. %A D'Eugenio, Francesco %A Carniani, Stefano %A Maiolino, Roberto %A Curtis-Lake, Emma %A Ferruit, Pierre %A Jakobsen, Peter %A Arribas, Santiago %A Bonaventura, Nina %A Charlot, Stephane %A Chevallard, Jacopo %A Curti, Mirko %A Looser, Tobias J. %A Maseda, Michael V. %A Rawle, Tim %A Rodríguez Del Pino, Bruno %A Smit, Renske %A Übler, Hannah %A Willott, Chris %A Witstok, Joris %A Egami, Eiichi %A Eisenstein, Daniel J. %A Johnson, Benjamin D. %A Hainline, Kevin %A Rieke, Marcia %A Robertson, Brant E. %A Stark, Daniel P. %A Tacchella, Sandro %A Williams, Christina C. %A Willmer, Christopher N. A. %A Bhatawdekar, Rachana %A Bowler, Rebecca %A Boyett, Kristan %A Circosta, Chiara %A Helton, Jakob M. %A Jones, Gareth C. %A Kumari, Nimisha %A Ji, Zhiyuan %A Nelson, Erica %A Parlanti, Eleonora %A Sandles, Lester %A Scholtz, Jan %A Sun, Fengwu %+ AA(University of Oxford, Department of Physics), AB(University of Oxford, Department of Physics; University College London, Department of Physics and Astronomy), AC(University of Oxford, Department of Physics), AD(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AE(Scuola Normale Superiore, Pisa, Italy), AF(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), AG(University of Hertfordshire, School of Physics, Astronomy and Mathematics), AH(European Science and Astronomy Center), AI(Niels Bohr Institute for Astronomy, Physics and Geophysics; Niels Bohr Institute for Astronomy, Physics and Geophysics), AJ(Center for Astrobiology, Madrid), AK(Niels Bohr Institute for Astronomy, Physics and Geophysics; Niels Bohr Institute for Astronomy, Physics and Geophysics), AL(Institut d'Astrophysique de Paris), AM(University of Oxford, Department of Physics), AN(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; European Southern Observatory, Germany), AO(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AP(University of Wisconsin, Madison, Department of Astronomy), AQ(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AR(Center for Astrobiology, Madrid), AS(Liverpool John Moores University, Astrophysics Research Institute), AT(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AU(Herzberg Institute for Astronomy and Astrophysics), AV(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AW(University of Arizona, Department of Astronomy and Steward Observatory), AX(Harvard Smithsonian Center for Astrophysics), AY(Harvard Smithsonian Center for Astrophysics), AZ(University of Arizona, Department of Astronomy and Steward Observatory), BA(University of Arizona, Department of Astronomy and Steward Observatory), BB(University of California, Santa Cruz, Department of Astronomy and Astrophysics), BC(University of Arizona, Department of Astronomy and Steward Observatory), BD(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BE(National Optical Astronomy Observatory, Arizona), BF(University of Arizona, Department of Astronomy and Steward Observatory), BG(European Science and Astronomy Center; European Space Research and Technology Centre), BH(Jodrell Bank Centre for Astrophysics), BI(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics in 3D), BJ(European Science and Astronomy Center), BK(University of Arizona, Department of Astronomy and Steward Observatory), BL(University of Oxford, Department of Physics), BM(AURA for European Space Agency, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21210, USA), BN(University of Arizona, Department of Astronomy and Steward Observatory), BO(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), BP(Scuola Normale Superiore, Pisa, Italy), BQ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BR(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), BS(University of Arizona, Department of Astronomy and Steward Observatory) %J Astronomy and Astrophysics %V 677 %D 2023 %8 September 01, 2023 %P A115 %K galaxies: evolution; galaxies: high-redshift; galaxies: ISM; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023A&A...677A.115C %X We present emission-line ratios from a sample of 27 Lyman-break galaxies from z ∼ 5.5 − 9.5 with −17.0 < M1500 < −20.4, measured from ultra-deep JWST/NIRSpec multi-object spectroscopy from the JWST Advanced Deep Extragalactic Survey (JADES). We used a combination of 28 h deep PRISM/CLEAR and 7 h deep G395M/F290LP observations to measure, or place strong constraints on, ratios of widely studied rest-frame optical emission lines including Hα, Hβ, [O II] λλ3726, 3729, [Ne III] λ3869, [O III] λ4959, [O III] λ5007, [O I] λ6300, [N II] λ6583, and [S II] λλ6716, 6731 in individual z > 5.5 spectra. We find that the emission-line ratios exhibited by these z ∼ 5.5 − 9.5 galaxies occupy clearly distinct regions of line-ratio space compared to typical z ∼ 0 − 3 galaxies, instead being more consistent with extreme populations of lower-redshift galaxies. This is best illustrated by the [O III]/[O II] ratio, tracing interstellar medium (ISM) ionisation, in which we observe more than half of our sample to have [O III]/[O II] > 10. Our high signal-to-noise spectra reveal more than an order of magnitude of scatter in line ratios such as [O II]/Hβ and [O III]/[O II], indicating significant diversity in the ISM conditions within the sample. We find no convincing detections of [N II] λ6583 in our sample, either in individual galaxies, or a stack of all G395M/F290LP spectra. The emission-line ratios observed in our sample are generally consistent with galaxies with extremely high ionisation parameters (log U ∼ −1.5), and a range of metallicities spanning from ∼0.1 × Z⊙ to higher than ∼0.3 × Z⊙, suggesting we are probing low-metallicity systems undergoing periods of rapid star formation, driving strong radiation fields. These results highlight the value of deep observations in constraining the properties of individual galaxies, and hence probing diversity within galaxy population. %R 10.1051/0004-6361/202346107 %= eprint: arXiv:2302.04298 %@ 0004-6361 %0 Journal Article %T JADES NIRSpec Spectroscopy of GN-z11: Lyman-α emission and possible enhanced nitrogen abundance in a z = 10.60 luminous galaxy %A Bunker, Andrew J. %A Saxena, Aayush %A Cameron, Alex J. %A Willott, Chris J. %A Curtis-Lake, Emma %A Jakobsen, Peter %A Carniani, Stefano %A Smit, Renske %A Maiolino, Roberto %A Witstok, Joris %A Curti, Mirko %A D'Eugenio, Francesco %A Jones, Gareth C. %A Ferruit, Pierre %A Arribas, Santiago %A Charlot, Stephane %A Chevallard, Jacopo %A Giardino, Giovanna %A de Graaff, Anna %A Looser, Tobias J. %A Lützgendorf, Nora %A Maseda, Michael V. %A Rawle, Tim %A Rix, Hans-Walter %A Del Pino, Bruno Rodríguez %A Alberts, Stacey %A Egami, Eiichi %A Eisenstein, Daniel J. %A Endsley, Ryan %A Hainline, Kevin %A Hausen, Ryan %A Johnson, Benjamin D. %A Rieke, George %A Rieke, Marcia %A Robertson, Brant E. %A Shivaei, Irene %A Stark, Daniel P. %A Sun, Fengwu %A Tacchella, Sandro %A Tang, Mengtao %A Williams, Christina C. %A Willmer, Christopher N. A. %A Baker, William M. %A Baum, Stefi %A Bhatawdekar, Rachana %A Bowler, Rebecca %A Boyett, Kristan %A Chen, Zuyi %A Circosta, Chiara %A Helton, Jakob M. %A Ji, Zhiyuan %A Kumari, Nimisha %A Lyu, Jianwei %A Nelson, Erica %A Parlanti, Eleonora %A Perna, Michele %A Sandles, Lester %A Scholtz, Jan %A Suess, Katherine A. %A Topping, Michael W. %A Übler, Hannah %A Wallace, Imaan E. B. %A Whitler, Lily %+ AA(University of Oxford, Department of Physics), AB(University of Oxford, Department of Physics; University College London, Department of Physics and Astronomy), AC(University of Oxford, Department of Physics), AD(Herzberg Institute for Astronomy and Astrophysics), AE(University of Hertfordshire, School of Physics, Astronomy and Mathematics), AF(Niels Bohr Institute for Astronomy, Physics and Geophysics; Niels Bohr Institute for Astronomy, Physics and Geophysics), AG(Scuola Normale Superiore, Pisa, Italy), AH(Liverpool John Moores University, Astrophysics Research Institute), AI(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), AJ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AK(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; European Southern Observatory, Germany), AL(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AM(University of Oxford, Department of Physics), AN(European Science and Astronomy Center), AO(Centro de Astrobiología (CAB), CSIC-INTA, Cra. de Ajalvir Km. 4, 28850, Torrej'on de Ardoz, Madrid, Spain), AP(Institut d'Astrophysique de Paris), AQ(University of Oxford, Department of Physics), AR(European Space Research and Technology Centre), AS(Max-Planck-Institute for Astronomy, Heidelberg), AT(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AU(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AV(University of Wisconsin, Madison, Department of Astronomy), AW(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AX(Max-Planck-Institute for Astronomy, Heidelberg), AY(Centro de Astrobiología (CAB), CSIC-INTA, Cra. de Ajalvir Km. 4, 28850, Torrej'on de Ardoz, Madrid, Spain), AZ(University of Arizona, Department of Astronomy and Steward Observatory), BA(University of Arizona, Department of Astronomy and Steward Observatory), BB(Harvard Smithsonian Center for Astrophysics), BC(University of Texas, Austin, Department of Astronomy), BD(University of Arizona, Department of Astronomy and Steward Observatory), BE(Johns Hopkins University, Department of Physics and Astronomy), BF(Harvard Smithsonian Center for Astrophysics), BG(University of Arizona, Department of Astronomy and Steward Observatory), BH(University of Arizona, Department of Astronomy and Steward Observatory), BI(University of California, Santa Cruz, Department of Astronomy and Astrophysics), BJ(University of Arizona, Department of Astronomy and Steward Observatory), BK(University of Arizona, Department of Astronomy and Steward Observatory), BL(University of Arizona, Department of Astronomy and Steward Observatory), BM(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BN(University of Arizona, Department of Astronomy and Steward Observatory), BO(National Optical Astronomy Observatory, Arizona; University of Arizona, Department of Astronomy and Steward Observatory), BP(University of Arizona, Department of Astronomy and Steward Observatory), BQ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BR(University of Manitoba, Department of Physics and Astronomy), BS(European Science and Astronomy Center; European Space Research and Technology Centre), BT(Jodrell Bank Centre for Astrophysics), BU(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics), BV(University of Arizona, Department of Astronomy and Steward Observatory), BW(European Science and Astronomy Center), BX(University of Arizona, Department of Astronomy and Steward Observatory), BY(University of Arizona, Department of Astronomy and Steward Observatory), BZ(AURA for European Space Agency, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21210, USA), CA(University of Arizona, Department of Astronomy and Steward Observatory), CB(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), CC(Scuola Normale Superiore, Pisa, Italy), CD(Centro de Astrobiología (CAB), CSIC-INTA, Cra. de Ajalvir Km. 4, 28850, Torrej'on de Ardoz, Madrid, Spain), CE(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), CF(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), CG(University of California, Santa Cruz, Department of Astronomy and Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology, California), CH(University of Arizona, Department of Astronomy and Steward Observatory), CI(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), CJ(University of Oxford, Department of Physics), CK(University of Arizona, Department of Astronomy and Steward Observatory) %J Astronomy and Astrophysics %V 677 %D 2023 %8 September 01, 2023 %P A88 %K galaxies: high-redshift; galaxies: evolution; galaxies: groups: individual: GN-z11; galaxies: abundances; Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023A&A...677A..88B %X We present JADES JWST/NIRSpec spectroscopy of GN-z11, the most luminous candidate z > 10 Lyman break galaxy in the GOODS-North field with MUV = −21.5. We derive a redshift of z = 10.603 (lower than previous determinations) based on multiple emission lines in our low and medium resolution spectra over 0.7 − 5.3 μm. We significantly detect the continuum and measure a blue rest-UV spectral slope of β = −2.4. Remarkably, we see spatially extended Lyman-α in emission (despite the highly neutral intergalactic medium expected at this early epoch), offset 555 km s−1 redwards of the systemic redshift. From our measurements of collisionally excited lines of both low and high ionisation (including [O II] λ3727, [Ne III] λ3869, and C III] λ1909), we infer a high ionisation parameter (log U ∼ −2). We detect the rarely seen N IV] λ1486 and N III] λ1748 lines in both our low and medium resolution spectra, with other high ionisation lines seen in the low resolution spectrum, such as He II (blended with O III]) and C IV (with a possible P-Cygni profile). Based on the observed rest-UV line ratios, we cannot conclusively rule out photoionisation from an active galactic nucleus (AGN), although the high C III]/He II and N III]/He II ratios are compatible with a star formation explanation. If the observed emission lines are powered by star formation, then the strong N III] λ1748 observed may imply an unusually high N/O abundance. Balmer emission lines (Hγ, Hδ) are also detected, and if powered by star formation rather than an AGN, we infer a star formation rate of ∼20 − 30 M⊙ yr−1 (depending on the initial mass function) and low dust attenuation. Our NIRSpec spectroscopy confirms that GN-z11 is a remarkable galaxy with extreme properties seen 430 Myr after the Big Bang. %R 10.1051/0004-6361/202346159 %= eprint: arXiv:2302.07256 %@ 0004-6361 %0 Electronic Article %T Ionised gas kinematics and dynamical masses of $zrsim6$ galaxies from JADES/NIRSpec high-resolution spectroscopy %A de Graaff, Anna %A Rix, Hans-Walter %A Carniani, Stefano %A Suess, Katherine A. %A Charlot, Stéphane %A Curtis-Lake, Emma %A Arribas, Santiago %A Baker, William M. %A Boyett, Kristan %A Bunker, Andrew J. %A Cameron, Alex J. %A Chevallard, Jacopo %A Curti, Mirko %A Eisenstein, Daniel J. %A Franx, Marijn %A Hainline, Kevin %A Hausen, Ryan %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Jones, Gareth C. %A Maiolino, Roberto %A Maseda, Michael V. %A Nelson, Erica %A Parlanti, Eleonora %A Rawle, Tim %A Robertson, Brant %A Tacchella, Sandro %A Übler, Hannah %A Williams, Christina C. %A Willmer, Christopher N. A. %A Willott, Chris %J arXiv e-prints %D 2023 %8 August 01, 2023 %P arXiv:2308.09742 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230809742D %Z Accepted for publication in A&A. Software for JWST/NIRSpec MSA modelling (slit losses, 1D LSFs and 2D model fitting) publicly available at https://github.com/annadeg/jwst-msafit %X We explore the kinematic gas properties of six $5.51$ thus far. The cold gas masses implied by the observed star formation rates are $\sim 10\times$ larger than the stellar masses. We find that their ionised gas is spatially resolved by JWST, with evidence for broadened lines and spatial velocity gradients. Using a simple thin-disc model, we fit these data with a novel forward modelling software that accounts for the complex geometry, point spread function, and pixellation of the NIRSpec instrument. We find the sample to include both rotation- and dispersion-dominated structures, as we detect velocity gradients of $v(r_{\rm e})\approx100-150\,{\rm km\,s^{-1}}$, and find velocity dispersions of $\sigma_0\approx 30-70\,{\rm km\,s^{-1}}$ that are comparable to those at cosmic noon. The dynamical masses implied by these models ($M_{\rm dyn}\sim10^{9-10}\,{\rm M_\odot}$) are larger than the stellar masses by up to a factor 40, and larger than the total baryonic mass (gas + stars) by a factor of $\sim 3$. Qualitatively, this result is robust even if the observed velocity gradients reflect ongoing mergers rather than rotating discs. Unless the observed emission line kinematics is dominated by outflows, this implies that the centres of these galaxies are dark-matter dominated or that star formation is $3\times$ less efficient, leading to higher inferred gas masses. %R 10.48550/arXiv.2308.09742 %= eprint: arXiv:2308.09742 %0 Electronic Article %T JADES. The diverse population of infant Black Holes at 4 10^44 erg/s, among galaxies in the redshift range 4 10%. %R 10.48550/arXiv.2308.01230 %= eprint: arXiv:2308.01230 %0 Journal Article %T The ionizing photon production efficiency at z 6 for Lyman-alpha emitters using JEMS and MUSE %A Simmonds, C. %A Tacchella, S. %A Maseda, M. %A Williams, C. C. %A Baker, W. M. %A Witten, C. E. C. %A Johnson, B. D. %A Robertson, B. %A Saxena, A. %A Sun, F. %A Witstok, J. %A Bhatawdekar, R. %A Boyett, K. %A Bunker, A. J. %A Charlot, S. %A Curtis-Lake, E. %A Egami, E. %A Eisenstein, D. J. %A Ji, Z. %A Maiolino, R. %A Sandles, L. %A Smit, R. %A Übler, H. %A Willott, C. J. %+ AA(The Kavli Institute for Cosmology (KICC), University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK), AB(The Kavli Institute for Cosmology (KICC), University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK), AC(University of Wisconsin, Madison, Department of Astronomy), AD(National Optical Astronomy Observatory, Arizona; University of Arizona, Department of Astronomy and Steward Observatory), AE(The Kavli Institute for Cosmology (KICC), University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK), AF(University of Cambridge, Institute of Astronomy; -), AG(Harvard Smithsonian Center for Astrophysics), AH(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AI(University of Oxford, Department of Physics; University College London, Department of Physics and Astronomy), AJ(University of Arizona, Department of Astronomy and Steward Observatory), AK(The Kavli Institute for Cosmology (KICC), University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK), AL(European Science and Astronomy Center; European Space Research and Technology Centre), AM(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics in 3D), AN(University of Oxford, Department of Physics), AO(Institut d'Astrophysique de Paris), AP(University of Hertfordshire, School of Physics, Astronomy and Mathematics), AQ(University of Arizona, Department of Astronomy and Steward Observatory), AR(Harvard Smithsonian Center for Astrophysics), AS(University of Arizona, Department of Astronomy and Steward Observatory), AT(The Kavli Institute for Cosmology (KICC), University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK; Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK), AU(The Kavli Institute for Cosmology (KICC), University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK), AV(Liverpool John Moores University, Astrophysics Research Institute), AW(The Kavli Institute for Cosmology (KICC), University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK), AX(Herzberg Institute for Astronomy and Astrophysics) %J Monthly Notices of the Royal Astronomical Society %V 523 %D 2023 %8 August 01, 2023 %P 5468-5486 %K galaxies: high-redshift; galaxies: evolution; galaxies: general; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.5468S %X We study the ionizing photon production efficiency at the end of the Epoch of Reionization (z ~ 5.4 - 6.6) for a sample of 30 Ly α emitters. This is a crucial quantity to infer the ionizing photon budget of the universe. These objects were selected to have reliable spectroscopic redshifts, assigned based on the profile of their Ly α emission line, detected in the MUSE deep fields. We exploit medium-band observations from the JWST Extragalactic Medium-band Survey (JEMS) to find the flux excess corresponding to the redshifted Hα emission line. We estimate the ultraviolet (UV) luminosity by fitting the full JEMS photometry, along with several HST photometric points, with Prospector. We find a median UV continuum slope of $\beta = -2.09^{+0.23}_{-0.21}$, indicating young stellar populations with little-to-no dust attenuation. Supported by this, we derive ξion,0 with no dust attenuation and find a median value of log$\frac{\xi _{ion,0}}{\text{Hz erg}^{-1}} = 25.44^{+0.21}_{-0.15}$. If we perform dust attenuation corrections and assume a Calzetti attenuation law, our values are lowered by ~0.1 dex. Our results suggest Ly α emitters at the Epoch of Reionization have slightly enhanced ξion,0 compared to previous estimations from literature, in particular, when compared to the non-Ly α emitting population. This initial study provides a promising outlook on the characterization of ionizing photon production in the early universe. In the future, a more extensive study will be performed on the entire data set provided by the JWST Advanced Deep Extragalactic Survey (JADES). Thus, for the first time, allowing us to place constraints on the wider galaxy populations driving reionization. %R 10.1093/mnras/stad1749 %= eprint: arXiv:2303.07931 %@ 0035-8711 %0 Journal Article %T First Sample of Hα+[O III]λ5007 Line Emitters at z > 6 Through JWST/NIRCam Slitless Spectroscopy: Physical Properties and Line-luminosity Functions %A Sun, Fengwu %A Egami, Eiichi %A Pirzkal, Nor %A Rieke, Marcia %A Baum, Stefi %A Boyer, Martha %A Boyett, Kristan %A Bunker, Andrew J. %A Cameron, Alex J. %A Curti, Mirko %A Eisenstein, Daniel J. %A Gennaro, Mario %A Greene, Thomas P. %A Jaffe, Daniel %A Kelly, Doug %A Koekemoer, Anton M. %A Kumari, Nimisha %A Maiolino, Roberto %A Maseda, Michael %A Perna, Michele %A Rest, Armin %A Robertson, Brant E. %A Schlawin, Everett %A Smit, Renske %A Stansberry, John %A Sunnquist, Ben %A Tacchella, Sandro %A Williams, Christina C. %A Willmer, Christopher N. A. %+ AA(University of Arizona, Department of Astronomy and Steward Observatory), AB(University of Arizona, Department of Astronomy and Steward Observatory), AC(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AD(University of Arizona, Department of Astronomy and Steward Observatory), AE(University of Manitoba, Department of Physics and Astronomy), AF(Space Telescope Science Institute, Baltimore, Maryland), AG(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics), AH(University of Oxford, Department of Physics, Denys Wilkinson Building, Keble Road, Oxford OX13RH, UK), AI(University of Oxford, Department of Astrophysics), AJ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AK(Harvard Smithsonian Center for Astrophysics), AL(Space Telescope Science Institute, Baltimore, Maryland; Johns Hopkins University, Department of Physics and Astronomy), AM(NASA Ames Research Center), AN(University of Texas, Austin, Department of Astronomy), AO(University of Arizona, Department of Astronomy and Steward Observatory), AP(Space Telescope Science Institute, Baltimore, Maryland), AQ(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AR(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), AS(University of Wisconsin, Madison, Department of Astronomy), AT(Center for Astrobiology, Madrid), AU(Space Telescope Science Institute, Baltimore, Maryland; Johns Hopkins University, Department of Physics and Astronomy), AV(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AW(University of Arizona, Department of Astronomy and Steward Observatory), AX(Liverpool John Moores University, Astrophysics Research Institute), AY(Space Telescope Science Institute, Baltimore, Maryland), AZ(Space Telescope Science Institute, Baltimore, Maryland), BA(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BB(University of Arizona, Department of Astronomy and Steward Observatory; National Optical Astronomy Observatory, Arizona), BC(University of Arizona, Department of Astronomy and Steward Observatory) %J The Astrophysical Journal %V 953 %D 2023 %8 August 01, 2023 %P 53 %K Emission line galaxies; High-redshift galaxies; James Webb Space Telescope; Starburst galaxies; Galaxy spectroscopy; 459; 734; 2291; 1570; 2171; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023ApJ...953...53S %X We present a sample of four emission-line galaxies at z = 6.11-6.35 that were serendipitously discovered using the commissioning data for the James Webb Space Telescope (JWST)/NIRCam wide-field slitless spectroscopy mode. One of them (at z = 6.11) has been reported previously, while the others are new discoveries. These sources are selected by the secure detections of both [O III] λ5007 and Hα lines with other fainter lines, which were tentatively detected in some cases (e.g., [O II] λ3727, [O III] λ4959). In the [O III]/Hβ-[N II]/Hα Baldwin-Phillips-Terlevich diagram, these galaxies occupy the same parameter space as that of z ~ 2 star-forming galaxies, indicating that they have been enriched rapidly to subsolar metallicities (~0.4 Z ⊙), similar to galaxies with comparable stellar masses at much lower redshifts. The detection of strong Hα lines suggests a higher ionizing photon production efficiency within galaxies in the early universe. We find brightening of the [O III] λ5007 line-luminosity function (LF) from z = 3 to 6, and weak or no redshift evolution of the Hα line LF from z = 2 to 6. Both LFs are underpredicted at z ~ 6 by a factor of ~10 in certain cosmological simulations. This further indicates a global Lyα photon escape fraction of 7%-10% at z ~ 6, which is slightly lower than previous estimates through the comparison of the UV-derived star formation rate density and Lyα luminosity density. Our sample recovers ${66}_{-44}^{+128}$ % of z = 6.0-6.6 galaxies in the survey volume with stellar masses greater than 5 × 108 M ⊙, suggesting the ubiquity of strong Hα and [O III] line emitters in the Epoch of Reionization, which will be further uncovered in the era of JWST. %R 10.3847/1538-4357/acd53c %= eprint: arXiv:2209.03374 %@ 0004-637X %0 Electronic Article %T The UV Continuum Slopes of Early Star-Forming Galaxies in JADES %A Topping, Michael W. %A Stark, Daniel P. %A Endsley, Ryan %A Whitler, Lily %A Hainline, Kevin %A Johnson, Benjamin D. %A Robertson, Brant %A Tacchella, Sandro %A Chen, Zuyi %A Alberts, Stacey %A Baker, William M. %A Bunker, Andrew J. %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Curtis-Lake, Emma %A DeCoursey, Christa %A Egami, Eiichi %A Eisenstein, Daniel J. %A Ji, Zhiyuan %A Maiolino, Roberto %A Williams, Christina C. %A Willmer, Christopher N. A. %A Willott, Chris %A Witstok, Joris %J arXiv e-prints %D 2023 %8 July 01, 2023 %P arXiv:2307.08835 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230708835T %Z 17 pages, 13 figures; submitted to MNRAS %X The power-law slope of the rest-UV continuum ($f_{\lambda}\propto\lambda^{\beta}$) is a key metric of early star forming galaxies, providing one of our only windows into the stellar populations and physical conditions of $z>10$ galaxies. Expanding upon previous studies with limited sample sizes, we leverage deep imaging from JADES to investigate the UV slopes of 179 $z>9$ galaxies with apparent magnitudes of $m_{\rm F200W}=26-31$, which display a median UV slope of $\beta=-2.4$. We compare to a statistical sample of $z=5-9$ galaxies, finding a shift toward bluer rest-UV colors at all $\rm~M_{UV}$. The most UV-luminous $z>9$ galaxies are significantly bluer than their lower-redshift counterparts, representing a dearth of moderately-red galaxies in the first $500~$Myr. At yet earlier times, the $z>11$ galaxy population exhibits very blue UV slopes, implying very low attenuation from dust. We identify a robust sample of 44 galaxies with $\beta<-2.8$, which have SEDs requiring models of density-bounded HII regions and median ionizing photon escape fractions of $0.51$ to reproduce. Their rest-optical colors imply that this sample has weaker emission lines (median $m_{\rm F356W}-m_{\rm F444W}=0.19$ mag) than typical galaxies (median $m_{\rm F356W}-m_{\rm F444W}=0.39$ mag), consistent with the inferred escape fractions. This sample has relatively low stellar masses (median $\log(M/M_{\odot})=7.5$), and specific star-formation rates (median$=79\rm/Gyr$) nearly twice that of our full sample (median$=44\rm/Gyr$), suggesting they are more common among systems experiencing a recent upturn in star formation. We demonstrate that the shutoff of star formation provides an alternative solution for modelling of extremely blue UV colors, making distinct predictions for the rest-optical emission of these galaxies. Future spectroscopy will be required to distinguish between these physical pictures. %R 10.48550/arXiv.2307.08835 %= eprint: arXiv:2307.08835 %0 Electronic Article %T JADES: deep spectroscopy of a low-mass galaxy at redshift 2.3 quenched by environment %A Sandles, Lester %A D'Eugenio, Francesco %A Helton, Jakob M. %A Maiolino, Roberto %A Hainline, Kevin %A Baker, William M. %A Williams, Christina C. %A Alberts, Stacey %A Bunker, Andrew J. %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Curti, Mirko %A Curtis-Lake, Emma %A Eisenstein, Daniel J. %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Looser, Tobias J. %A Rawle, Tim %A Robertson, Brant %A Rodríguez Del Pino, Bruno %A Tacchella, Sandro %A Übler, Hannah %A Willmer, Christopher N. A. %A Willott, Chris %J arXiv e-prints %D 2023 %8 July 01, 2023 %P arXiv:2307.08633 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230708633S %Z Submitted to A&A %X We report the discovery of a quiescent galaxy at $z=2.34$ with a stellar mass of only $M_\star = 9.5^{+1.8}_{-1.2} \times 10^{8} \mathrm{M}_\odot$, based on deep JWST/NIRSpec spectroscopy. This is the least massive quiescent galaxy found so far at high redshift. We use a Bayesian approach to model the spectrum and photometry, and find the target to have been quiescent for 0.6 Gyr with a mass-weighted average stellar age of 0.8-1.7 Gyr (dominated by systematics). The galaxy displays an inverse colour gradient with radius, consistent with environment-driven quenching. Based on a combination of spectroscopic and robust (medium- and broad-band) photometric redshifts, we identify a galaxy overdensity near the location of the target (5-$\sigma$ above the background level at this redshift). We stress that had we been specifically targetting galaxies within overdensities, the main target would not have been selected on photometry alone; therefore, environment studies based on photometric redshifts are biased against low-mass quiescent galaxies. The overdensity contains three spectroscopically confirmed, massive, old galaxies ($M_\star = 8-17 \times 10^{10} \mathrm{M}_\odot$). The presence of these evolved systems points to accelerated galaxy evolution in overdensities at redshifts z > 2, in agreement with previous works. In projection, our target lies only 35 pkpc away from the most massive galaxy in this overdensity (spectroscopic redshift z = 2.349) which is located close to overdensity's centre. This suggests the low-mass galaxy was quenched by environment, making it possibly the earliest evidence for environment-driven quenching to date. %R 10.48550/arXiv.2307.08633 %= eprint: arXiv:2307.08633 %0 Journal Article %T JWST NIRCam + NIRSpec: interstellar medium and stellar populations of young galaxies with rising star formation and evolving gas reservoirs %A Tacchella, Sandro %A Johnson, Benjamin D. %A Robertson, Brant E. %A Carniani, Stefano %A D'Eugenio, Francesco %A Kumari, Nimisha %A Maiolino, Roberto %A Nelson, Erica J. %A Suess, Katherine A. %A Übler, Hannah %A Williams, Christina C. %A Adebusola, Alabi %A Alberts, Stacey %A Arribas, Santiago %A Bhatawdekar, Rachana %A Bonaventura, Nina %A Bowler, Rebecca A. A. %A Bunker, Andrew J. %A Cameron, Alex J. %A Curti, Mirko %A Egami, Eiichi %A Eisenstein, Daniel J. %A Frye, Brenda %A Hainline, Kevin %A Helton, Jakob M. %A Ji, Zhiyuan %A Looser, Tobias J. %A Lyu, Jianwei %A Perna, Michele %A Rawle, Timothy %A Rieke, George %A Rieke, Marcia %A Saxena, Aayush %A Sandles, Lester %A Shivaei, Irene %A Simmonds, Charlotte %A Sun, Fengwu %A Willmer, Christopher N. A. %A Willott, Chris J. %A Witstok, Joris %+ AA(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AB(Harvard Smithsonian Center for Astrophysics), AC(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AD(Scuola Normale Superiore, Pisa, Italy), AE(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AF(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AG(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), AH(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), AI(Kavli Institute for Particle Astrophysics and Cosmology, California), AJ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AK(National Optical Astronomy Observatory, Arizona), AL(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AM(University of Arizona, Department of Astronomy and Steward Observatory), AN(Center for Astrobiology, Madrid), AO(European Space Research and Technology Centre), AP(Niels Bohr Institute for Astronomy, Physics and Geophysics), AQ(Jodrell Bank Centre for Astrophysics), AR(University of Oxford, Department of Physics), AS(University of Oxford, Department of Physics), AT(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AU(University of Arizona, Department of Astronomy and Steward Observatory), AV(Harvard Smithsonian Center for Astrophysics), AW(University of Arizona, Department of Astronomy and Steward Observatory), AX(University of Arizona, Department of Astronomy and Steward Observatory), AY(University of Arizona, Department of Astronomy and Steward Observatory), AZ(UMass Amherst), BA(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BB(University of Arizona, Department of Astronomy and Steward Observatory), BC(Center for Astrobiology, Madrid), BD(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), BE(University of Arizona, Department of Astronomy and Steward Observatory), BF(University of Arizona, Department of Astronomy and Steward Observatory), BG(University College London, Department of Physics and Astronomy), BH(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BI(University of Arizona, Department of Astronomy and Steward Observatory), BJ(University of Geneva, Astronomical Observatory), BK(University of Arizona, Department of Astronomy and Steward Observatory), BL(University of Arizona, Department of Astronomy and Steward Observatory), BM(Herzberg Institute for Astronomy and Astrophysics), BN(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy) %J Monthly Notices of the Royal Astronomical Society %V 522 %D 2023 %8 July 01, 2023 %P 6236-6249 %K galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: star formation; early Universe; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.6236T %X We present an interstellar medium and stellar population analysis of three spectroscopically confirmed z > 7 galaxies in the Early Release Observations JWST/NIRCam and JWST/NIRSpec data of the SMACS J0723.3-7327 cluster. We use the Bayesian spectral energy distribution-fitting code PROSPECTOR with a flexible star formation history (SFH), a variable dust attenuation law, and a self-consistent model of nebular emission (continuum and emission lines). Importantly, we self-consistently fit both the emission line fluxes from JWST/NIRSpec and the broad-band photometry from JWST/NIRCam, taking into account slit-loss effects. We find that these three z=7.6-8.5 galaxies (M⋆ ≈ 108 M⊙) are young with rising SFHs and mass-weighted ages of 3-4 Myr, though we find indications for underlying older stellar populations. The inferred gas-phase metallicities broadly agree with the direct metallicity estimates from the auroral lines. The galaxy with the lowest gas-phase metallicity (Zgas= 0.06 Z⊙) has a steeply rising SFH, is very compact (<0.2 kpc), and has a high star formation rate surface density (ΣSFR ≈ 22 M⊙ yr-1 kpc-2), consistent with rapid gas accretion. The two other objects with higher gas-phase metallicities show more complex multicomponent morphologies on kpc scales, indicating that their recent increase in star formation rate is driven by mergers or internal, gravitational instabilities. We discuss effects of assuming different SFH priors or only fitting the photometric data. Our analysis highlights the strength and importance of combining JWST imaging and spectroscopy for fully assessing the nature of galaxies at the earliest epochs. %R 10.1093/mnras/stad1408 %= eprint: arXiv:2208.03281 %@ 0035-8711 %0 Journal Article %T JADES Imaging of GN-z11: Revealing the Morphology and Environment of a Luminous Galaxy 430 Myr after the Big Bang %A Tacchella, Sandro %A Eisenstein, Daniel J. %A Hainline, Kevin %A Johnson, Benjamin D. %A Baker, William M. %A Helton, Jakob M. %A Robertson, Brant %A Suess, Katherine A. %A Chen, Zuyi %A Nelson, Erica %A Puskás, Dávid %A Sun, Fengwu %A Alberts, Stacey %A Egami, Eiichi %A Hausen, Ryan %A Rieke, George %A Rieke, Marcia %A Shivaei, Irene %A Williams, Christina C. %A Willmer, Christopher N. A. %A Bunker, Andrew %A Cameron, Alex J. %A Carniani, Stefano %A Charlot, Stephane %A Curti, Mirko %A Curtis-Lake, Emma %A Looser, Tobias J. %A Maiolino, Roberto %A Maseda, Michael V. %A Rawle, Tim %A Rix, Hans-Walter %A Smit, Renske %A Übler, Hannah %A Willott, Chris %A Witstok, Joris %A Baum, Stefi %A Bhatawdekar, Rachana %A Boyett, Kristan %A Danhaive, A. Lola %A de Graaff, Anna %A Endsley, Ryan %A Ji, Zhiyuan %A Lyu, Jianwei %A Sandles, Lester %A Saxena, Aayush %A Scholtz, Jan %A Topping, Michael W. %A Whitler, Lily %+ AA(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AB(Harvard Smithsonian Center for Astrophysics), AC(University of Arizona, Department of Astronomy and Steward Observatory), AD(Harvard Smithsonian Center for Astrophysics), AE(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AF(University of Arizona, Department of Astronomy and Steward Observatory), AG(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AH(University of California, Santa Cruz, Department of Astronomy and Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology, California), AI(University of Arizona, Department of Astronomy and Steward Observatory), AJ(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), AK(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AL(University of Arizona, Department of Astronomy and Steward Observatory), AM(University of Arizona, Department of Astronomy and Steward Observatory), AN(University of Arizona, Department of Astronomy and Steward Observatory), AO(Johns Hopkins University, Department of Physics and Astronomy), AP(University of Arizona, Department of Astronomy and Steward Observatory), AQ(University of Arizona, Department of Astronomy and Steward Observatory), AR(University of Arizona, Department of Astronomy and Steward Observatory), AS(University of Arizona, Department of Astronomy and Steward Observatory; National Optical Astronomy Observatory, Arizona), AT(University of Arizona, Department of Astronomy and Steward Observatory), AU(University of Oxford, Department of Physics), AV(University of Oxford, Department of Physics), AW(Scuola Normale Superiore, Pisa, Italy), AX(Institut d'Astrophysique de Paris), AY(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; -), AZ(University of Hertfordshire, School of Physics, Astronomy and Mathematics), BA(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BB(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), BC(University of Wisconsin, Madison, Department of Astronomy), BD(European Space Agency, Space Telescope Science Institute, Baltimore, MD 21218, US), BE(Max-Planck-Institute for Astronomy, Heidelberg), BF(Liverpool John Moores University, Astrophysics Research Institute), BG(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BH(Herzberg Institute for Astronomy and Astrophysics), BI(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BJ(University of Manitoba, Department of Physics and Astronomy), BK(European Space Agency, ESAC/ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; European Space Agency, ESA/ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, NL, The Netherlands), BL(School of Physics, University of Melbourne, Parkville 3010, VIC 3010, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia), BM(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BN(Max-Planck-Institute for Astronomy, Heidelberg), BO(University of Texas, Austin, Department of Astronomy), BP(University of Arizona, Department of Astronomy and Steward Observatory), BQ(University of Arizona, Department of Astronomy and Steward Observatory), BR(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BS(University of Oxford, Department of Physics; University College London, Department of Physics and Astronomy), BT(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BU(University of Arizona, Department of Astronomy and Steward Observatory), BV(University of Arizona, Department of Astronomy and Steward Observatory) %J The Astrophysical Journal %V 952 %D 2023 %8 July 01, 2023 %P 74 %K Galaxy evolution; Galaxy formation; Galaxy structure; High-redshift galaxies; Star formation; 594; 595; 622; 734; 1569; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023ApJ...952...74T %X We present JWST NIRCam nine-band near-infrared imaging of the luminous z = 10.6 galaxy GN-z11 from the JWST Advanced Deep Extragalactic Survey of the GOODS-N field. We find a spectral energy distribution (SED) entirely consistent with the expected form of a high-redshift galaxy: a clear blue continuum from 1.5 to 4 μm with a complete dropout in F115W. The core of GN-z11 is extremely compact in JWST imaging. We analyze the image with a two-component model, using a point source and a Sérsic profile that fits to a half-light radius of 200 pc and an index n = 0.9. We find a low-surface-brightness haze about 0.″4 to the northeast of the galaxy, which is most likely a foreground object but might be a more extended component of GN-z11. At a spectroscopic redshift of 10.60 (Bunker et al. 2023), the comparison of the NIRCam F410M and F444W images spans the Balmer jump. From population-synthesis modeling, here assuming no light from an active galactic nucleus, we reproduce the SED of GN-z11, finding a stellar mass of ~109 M ⊙, a star formation rate of ~20 M ⊙ yr-1, and a young stellar age of ~20 Myr. Since massive galaxies at high redshift are likely to be highly clustered, we search for faint neighbors of GN-z11, finding nine galaxies out to ~5 comoving Mpc transverse with photometric redshifts consistent with z = 10.6, and a tenth more tentative dropout only 3″ away. This is consistent with GN-z11 being hosted by a massive dark-matter halo (≈8 × 1010 M ⊙), though lower halo masses cannot be ruled out. %R 10.3847/1538-4357/acdbc6 %= eprint: arXiv:2302.07234 %@ 0004-637X %0 Electronic Article %T JADES: The incidence rate and properties of galactic outflows in low-mass galaxies across 3 < z < 9 %A Carniani, Stefano %A Venturi, Giacomo %A Parlanti, Eleonora %A de Graaff, Anna %A Maiolino, Roberto %A Arribas, Santiago %A Bonaventura, Nina %A Boyett, Kristan %A Bunker, Andrew J. %A Cameron, Alex J. %A Charlot, Stephane %A Chevallard, Jacopo %A Curti, Mirko %A Curtis-Lake, Emma %A Eisenstein, Daniel J. %A Giardino, Giovanna %A Hausen, Ryan %A Kumari, Nimisha %A Maseda, Michael V. %A Nelson, Erica %A Perna, Michele %A Rix, Hans-Walter %A Robertson, Brant %A Rodríguez Del Pino, Bruno %A Sandles, Lester %A Scholtz, Jan %A Simmonds, Charlotte %A Smit, Renske %A Tacchella, Sandro %A Übler, Hannah %A Williams, Christina C. %A Willott, Chris %A Witstok, Joris %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.11801 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230611801C %Z 16 pages, 3 tables, Submitted to A&A %X We investigate the incidence and properties of ionized gas outflows in a sample of 52 galaxies with stellar mass between $10^7$ M$_{\odot}$ and $10^9$ M$_{\odot}$ observed with ultra-deep JWST/NIRSpec MSA spectroscopy as part of the JWST Advanced Deep Extragalactic Survey (JADES). The high-spectral resolution (R2700) NIRSpec observations allowed us to identify for the first time the signature of outflows in the rest-frame optical nebular lines in low-mass galaxies at $z>3$. The incidence fraction of ionized outflows, traced by broad components, is about 25-40$\%$ depending on the intensity of the emission lines. The low incidence fraction might be due to both the sensitivity limit and the fact that outflows are not isotropic but have a limited opening angle which results in a detection only when this is directed toward our line of sight. Evidence for outflows increases slightly with stellar mass and star-formation rate. The median velocity and mass loading factor (i.e., the ratio between mass outflow rate and star formation rate) of the outflowing ionized gas are 500 km s$^{-1}$ and $\eta=2.1^{+2.5}_{-1.6}$, respectively. These are two and 100 times higher, respectively than the typical values observed in local dwarf galaxies. These outflows are able to escape the gravitational potential of the galaxy and enrich the circum-galactic medium and, potentially, the inter-galactic medium. Our results indicate that outflows can significantly impact the star formation activity in low-mass galaxies within the first 2 Gyr of the Universe. %R 10.48550/arXiv.2306.11801 %= eprint: arXiv:2306.11801 %0 Electronic Article %T GN-z11: The environment of an AGN at $z=$10.603 %A Scholtz, Jan %A Witten, Callum %A Laporte, Nicolas %A Ubler, Hannah %A Perna, Michele %A Maiolino, Roberto %A Arribas, Santiago %A Baker, William %A Bennett, Jake %A D'Eugenio, Francesco %A Tacchella, Sandro %A Witstok, Joris %A Bunker, Andrew %A Carniani, Stefano %A Charlot, Stephane %A Curtis-Lake, Emma %A Eisenstein, Daniel %A Robertson, Brant %A Rodriguez Del Pino, Bruno %A Simmonds, Charlotte %A Smit, Renske %A Venturi, Giacomo %A Williams, Christina %A Willmer, Christopher %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.09142 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230609142S %Z Submitted to A&A. 8 pages, 5 figures %X Recent observations with the \textit{James Webb} Space Telescope (JWST) have further refined the spectroscopic redshift of GN-z11, one of the most distant galaxies identified with the \textit{Hubble} Space Telescope (HST) at $z=10.603$. The presence of extremely dense gas ($>10^{10}$ cm$^{-3}$), the detection of high-ionisation lines and of CII*1335 emission, as well as the presence of an ionisation cone, indicate that GN-z11 also hosts an Active Galactic Nucleus (AGN). Further photometric and spectroscopic follow-up demonstrates that it lies in a large-scale, overdense structure with possible signatures of Population III (PopIII) stars in its halo. Surprisingly, Ly$\alpha$ has also been detected despite the expected largely neutral inter-galactic medium at such a redshift. We exploit recent JWST/NIRSpec IFU observations to demonstrate that the Ly$\alpha$ emission in GN-z11 is part of an extended halo with a minimum size of 0.8--3.2 kpc, depending on the definition used to derive the halo size. The surface brightness of the Ly$\alpha$ halo around GN-z11 appears consistent with Ly$\alpha$ halos observed around $z\sim6$ quasars. At the wavelength of Ly$\alpha$ at $z\sim$10.6, we identify three other emission line candidates within the IFU Field-of-View with no UV rest-frame counterpart visible in deep images from the JWST/NIRCam. If confirmed, this could be the first evidence that the local region of GN-z11 represents a candidate protocluster core, forming just 400 Myr after the Big Bang. We give a first estimate of the dark matter halo mass of this structure ($M_h$=2.96$^{+0.44}_{-0.39} \times$10$^{10}$ M$_{\odot}$), consistent with a Coma-like cluster progenitor. %R 10.48550/arXiv.2306.09142 %= eprint: arXiv:2306.09142 %0 Electronic Article %T The Optical Corrector for the Dark Energy Spectroscopic Instrument %A Miller, Timothy N. %A Doel, Peter %A Gutierrez, Gaston %A Besuner, Robert %A Brooks, David %A Gallo, Giuseppe %A Heetderks, Henry %A Jelinsky, Patrick %A Kent, Stephen M. %A Lampton, Michael %A Levi, Michael %A Liang, Ming %A Meisner, Aaron %A Sholl, Michael J. %A Silber, Joseph Harry %A Sprayberry, David %A Aguilar, Jessica Nicole %A de la Macorra, Axel %A Eisenstein, Daniel %A Fanning, Kevin %A Font-Ribera, Andreu %A Gaztanaga, Enrique %A Gontcho, Satya Gontcho A %A Honscheid, Klaus %A Jimenez, Jorge %A Joyce, Dick %A Kehoe, Robert %A Kisner, Theodore %A Kremin, Anthony %A Landriau, Martin %A Le Guillou, Laurent %A Magneville, Christophe %A Martini, Paul %A Miquel, Ramon %A Moustakas, John %A Nie, Jundan %A Percival, Will %A Poppett, Claire %A Prada, Francisco %A Rossi, Graziano %A Schlegel, David %A Schubnell, Michael %A Seo, Hee-Jong %A Sharples, Ray %A Tarle, Gregory %A Vargas-Magana, Mariana %A Zhou, Zhimin %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.06310 %K Astrophysics - Instrumentation and Methods for Astrophysics; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023arXiv230606310M %Z 68 pages, 56 figures, 22 tables. Submitted to the Astronomical Journal %X The Dark Energy Spectroscopic Instrument (DESI) is currently measuring the spectra of 40\,million galaxies and quasars, the largest such survey ever made to probe the nature of cosmological dark energy. The 4-meter Mayall telescope at Kitt Peak National Observatory has been adapted for DESI, including the construction of a 3.2-degree diameter prime focus corrector that focuses astronomical light onto a 0.8-meter diameter focal surface with excellent image quality over the DESI bandpass of 360-980nm. The wide-field corrector includes six lenses, as large as 1.1-meters in diameter and as heavy as 237\,kilograms, including two counter-rotating wedged lenses that correct for atmospheric dispersion over Zenith angles from 0 to 60 degrees. The lenses, cells, and barrel assembly all meet precise alignment tolerances on the order of tens of microns. The barrel alignment is maintained throughout a range of observing angles and temperature excursions in the Mayall dome by use of a hexapod, which is itself supported by a new cage, ring, and truss structure. In this paper we describe the design, fabrication, and performance of the new corrector and associated structure, focusing on how they meet DESI requirements. In particular we describe the prescription and specifications of the lenses, design choices and error budgeting of the barrel assembly, stray light mitigations, and integration and test at the Mayall telescope. We conclude with some validation highlights that demonstrate the successful corrector on-sky performance, and list some lessons learned during the multi-year fabrication phase. %R 10.48550/arXiv.2306.06310 %= eprint: arXiv:2306.06310 %0 Electronic Article %T The Early Data Release of the Dark Energy Spectroscopic Instrument %A DESI Collaboration %A Adame, A. G. %A Aguilar, J. %A Ahlen, S. %A Alam, S. %A Aldering, G. %A Alexander, D. M. %A Alfarsy, R. %A Allende Prieto, C. %A Alvarez, M. %A Alves, O. %A Anand, A. %A Andrade-Oliveira, F. %A Armengaud, E. %A Asorey, J. %A Avila, S. %A Aviles, A. %A Bailey, S. %A Balaguera-Antolínez, A. %A Ballester, O. %A Baltay, C. %A Bault, A. %A Bautista, J. %A Behera, J. %A Beltran, S. F. %A BenZvi, S. %A Beraldo e Silva, L. %A Bermejo-Climent, J. R. %A Berti, A. %A Besuner, R. %A Beutler, F. %A Bianchi, D. %A Blake, C. %A Blum, R. %A Bolton, A. S. %A Brieden, S. %A Brodzeller, A. %A Brooks, D. %A Brown, Z. %A Buckley-Geer, E. %A Burtin, E. %A Cabayol-Garcia, L. %A Cai, Z. %A Canning, R. %A Cardiel-Sas, L. %A Carnero Rosell, A. %A Castander, F. J. %A Cervantes-Cota, J. L. %A Chabanier, S. %A Chaussidon, E. %A Chaves-Montero, J. %A Chen, S. %A Chuang, C. %A Claybaugh, T. %A Cole, S. %A Cooper, A. P. %A Cuceu, A. %A Davis, T. M. %A Dawson, K. %A de Belsunce, R. %A de la Cruz, R. %A de la Macorra, A. %A de Mattia, A. %A Demina, R. %A Demirbozan, U. %A DeRose, J. %A Dey, A. %A Dey, B. %A Dhungana, G. %A Ding, J. %A Ding, Z. %A Doel, P. %A Doshi, R. %A Douglass, K. %A Edge, A. %A Eftekharzadeh, S. %A Eisenstein, D. J. %A Elliott, A. %A Escoffier, S. %A Fagrelius, P. %A Fan, X. %A Fanning, K. %A Fawcett, V. A. %A Ferraro, S. %A Ereza, J. %A Flaugher, B. %A Font-Ribera, A. %A Forero-Sánchez, D. %A Forero-Romero, J. E. %A Frenk, C. S. %A Gänsicke, B. T. %A García, L. Á. %A García-Bellido, J. %A Garcia-Quintero, C. %A Garrison, L. H. %A Gil-Marín, H. %A Golden-Marx, J. %A Gontcho, S. Gontcho A %A Gonzalez-Morales, A. X. %A Gonzalez-Perez, V. %A Gordon, C. %A Graur, O. %A Green, D. %A Gruen, D. %A Guy, J. %A Hadzhiyska, B. %A Hahn, C. %A Han, J. J. %A Hanif, M. M. S %A Herrera-Alcantar, H. K. %A Honscheid, K. %A Hou, J. %A Howlett, C. %A Huterer, D. %A Iršič, V. %A Ishak, M. %A Jacques, A. %A Jana, A. %A Jiang, L. %A Jimenez, J. %A Jing, Y. P. %A Joudaki, S. %A Jullo, E. %A Juneau, S. %A Kizhuprakkat, N. %A Karaçaylı, N. G. %A Karim, T. %A Kehoe, R. %A Kent, S. %A Khederlarian, A. %A Kim, S. %A Kirkby, D. %A Kisner, T. %A Kitaura, F. %A Kneib, J. %A Koposov, S. E. %A Kovács, A. %A Kremin, A. %A Krolewski, A. %A L'Huillier, B. %A Lambert, A. %A Lamman, C. %A Lan, T. -W. %A Landriau, M. %A Lang, D. %A Lange, J. U. %A Lasker, J. %A Le Guillou, L. %A Leauthaud, A. %A Levi, M. E. %A Li, T. S. %A Linder, E. %A Lyons, A. %A Magneville, C. %A Manera, M. %A Manser, C. J. %A Margala, D. %A Martini, P. %A McDonald, P. %A Medina, G. E. %A Medina-Varela, L. %A Meisner, A. %A Mena-Fernández, J. %A Meneses-Rizo, J. %A Mezcua, M. %A Miquel, R. %A Montero-Camacho, P. %A Moon, J. %A Moore, S. %A Moustakas, J. %A Mueller, E. %A Mundet, J. %A Muñoz-Gutiérrez, A. %A Myers, A. D. %A Nadathur, S. %A Napolitano, L. %A Neveux, R. %A Newman, J. A. %A Nie, J. %A Nikutta, R. %A Niz, G. %A Norberg, P. %A Noriega, H. E. %A Paillas, E. %A Palanque-Delabrouille, N. %A Palmese, A. %A Zhiwei, P. %A Parkinson, D. %A Penmetsa, S. %A Percival, W. J. %A Pérez-Fernández, A. %A Pérez-Ràfols, I. %A Pieri, M. %A Poppett, C. %A Porredon, A. %A Pothier, S. %A Prada, F. %A Pucha, R. %A Raichoor, A. %A Ramírez-Pérez, C. %A Ramirez-Solano, S. %A Rashkovetskyi, M. %A Ravoux, C. %A Rocher, A. %A Rockosi, C. %A Ross, A. J. %A Rossi, G. %A Ruggeri, R. %A Ruhlmann-Kleider, V. %A Sabiu, C. G. %A Said, K. %A Saintonge, A. %A Samushia, L. %A Sanchez, E. %A Saulder, C. %A Schaan, E. %A Schlafly, E. F. %A Schlegel, D. %A Scholte, D. %A Schubnell, M. %A Seo, H. %A Shafieloo, A. %A Sharples, R. %A Sheu, W. %A Silber, J. %A Sinigaglia, F. %A Siudek, M. %A Slepian, Z. %A Smith, A. %A Sprayberry, D. %A Stephey, L. %A Suárez-Pérez, J. %A Sun, Z. %A Tan, T. %A Tarlé, G. %A Tojeiro, R. %A Ureña-López, L. A. %A Vaisakh, R. %A Valcin, D. %A Valdes, F. %A Valluri, M. %A Vargas-Magaña, M. %A Variu, A. %A Verde, L. %A Walther, M. %A Wang, B. %A Wang, M. S. %A Weaver, B. A. %A Weaverdyck, N. %A Wechsler, R. H. %A White, M. %A Xie, Y. %A Yang, J. %A Yèche, C. %A Yu, J. %A Yuan, S. %A Zhang, H. %A Zhang, Z. %A Zhao, C. %A Zheng, Z. %A Zhou, R. %A Zhou, Z. %A Zou, H. %A Zou, S. %A Zu, Y. %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.06308 %K Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023arXiv230606308D %Z 43 pages, 7 figures, 17 tables, submitted to AJ, DESI EDR references added; doi:10.5281/zenodo.7964161 %X The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes good-quality spectral information from 466,447 objects targeted as part of the Milky Way Survey, 428,758 as part of the Bright Galaxy Survey, 227,318 as part of the Luminous Red Galaxy sample, 437,664 as part of the Emission Line Galaxy sample, and 76,079 as part of the Quasar sample. In addition, the release includes spectral information from 137,148 objects that expand the scope beyond the primary samples as part of a series of secondary programs. Here, we describe the spectral data, data quality, data products, Large-Scale Structure science catalogs, access to the data, and references that provide relevant background to using these spectra. %R 10.48550/arXiv.2306.06308 %= eprint: arXiv:2306.06308 %0 Electronic Article %T The Star-forming and Ionizing Properties of Dwarf z~6-9 Galaxies in JADES: Insights on Bursty Star Formation and Ionized Bubble Growth %A Endsley, Ryan %A Stark, Daniel P. %A Whitler, Lily %A Topping, Michael W. %A Johnson, Benjamin D. %A Robertson, Brant %A Tacchella, Sandro %A Alberts, Stacey %A Baker, William M. %A Bhatawdekar, Rachana %A Boyett, Kristan %A Bunker, Andrew J. %A Cameron, Alex J. %A Carniani, Stefano %A Charlot, Stéphane %A Chen, Zuyi %A Chevallard, Jacopo %A Curtis-Lake, Emma %A Danhaive, A. Lola %A Egami, Eiichi %A Eisenstein, Daniel J. %A Hainline, Kevin %A Helton, Jakob M. %A Ji, Zhiyuan %A Looser, Tobias J. %A Maiolino, Roberto %A Nelson, Erica %A Puskás, Dávid %A Rieke, George %A Rieke, Marcia %A Rix, Hans-Walter %A Sandles, Lester %A Saxena, Aayush %A Simmonds, Charlotte %A Smit, Renske %A Sun, Fengwu %A Williams, Christina C. %A Willmer, Christopher N. A. %A Willott, Chris %A Witstok, Joris %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.05295 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230605295E %Z Minor updates to references and typo corrections. 29 pages, 16 figures. Submitted to MNRAS. Comments welcome %X Reionization is thought to be driven by faint star-forming galaxies, but characterizing this population in detail has long remained very challenging. Here we utilize deep nine-band NIRCam imaging from JADES to study the star-forming and ionizing properties of 756 $z\sim6-9$ galaxies, including hundreds of very UV-faint objects ($M_\mathrm{UV}>-18$). The faintest ($m\sim30$) galaxies in our sample typically have stellar masses of $M_\ast\sim(1-3)\times10^7$ $M_\odot$ and young light-weighted ages ($\sim$50 Myr), though some show strong Balmer breaks implying much older ages ($\sim$500 Myr). We find no evidence for extremely massive galaxies ($>3\times10^{10}$ $M_\odot$) in our sample. We infer a strong (factor $>$2) decline in the typical [OIII]$+$H$\beta$ EWs towards very faint $z\sim6-9$ galaxies, yet a weak UV luminosity dependence on the H$\alpha$ EWs at $z\sim6$. We demonstrate that these EW trends can be explained if fainter galaxies have systematically lower metallicities as well as more recently-declining star formation histories relative to the most UV-luminous galaxies in our sample. Our data provide evidence that the brightest galaxies are frequently experiencing a recent strong upturn in SFR. We also discuss how the EW trends may be influenced by a strong correlation between $M_\mathrm{UV}$ and Lyman continuum escape fraction. This alternative explanation has dramatically different implications for the contribution of galaxies along the luminosity function to cosmic reionization, highlighting the need for deep spectroscopic follow-up. Finally, we quantify the photometric overdensities around two $z>7$ strong Ly$\alpha$ emitters in the JADES footprint. One Ly$\alpha$ emitter lies close to a strong photometric overdensity while the other shows no significant nearby overdensity, perhaps implying that not all strong $z>7$ Ly$\alpha$ emitters reside in large ionized bubbles. %R 10.48550/arXiv.2306.05295 %= eprint: arXiv:2306.05295 %0 Electronic Article %T JADES: The production and escape of ionizing photons from faint Lyman-alpha emitters in the epoch of reionization %A Saxena, Aayush %A Bunker, Andrew J. %A Jones, Gareth C. %A Stark, Daniel P. %A Cameron, Alex J. %A Witstok, Joris %A Arribas, Santiago %A Baker, William M. %A Baum, Stefi %A Bhatawdekar, Rachana %A Bowler, Rebecca %A Boyett, Kristan %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Curti, Mirko %A Curtis-Lake, Emma %A Eisenstein, Daniel J. %A Endsley, Ryan %A Hainline, Kevin %A Helton, Jakob M. %A Johnson, Benjamin D. %A Kumari, Nimisha %A Looser, Tobias J. %A Maiolino, Roberto %A Rieke, Marcia %A Rix, Hans-Walter %A Robertson, Brant E. %A Sandles, Lester %A Simmonds, Charlotte %A Smit, Renske %A Tacchella, Sandro %A Williams, Christina C. %A Willmer, Christopher N. A. %A Willott, Chris %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.04536 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230604536S %Z Submitted to A&A. 22 pages, 13 figures, spectra presented in the appendix %X We present the properties of 16 faint Lyman-$\alpha$ emitting galaxies (LAEs) at $z>5.8$ from the JWST Advanced Deep Extragalactic Survey (JADES) spectroscopic data in the Hubble Ultra Deep Field/GOODS-S. These LAEs span a redshift range $z\approx5.8-8.0$ and UV magnitude range $M_{\textrm{UV}} \approx -17$ to $-20.6$, with Ly$\alpha$ equivalent width (EW) in the range $\approx 25-350$ Å. The detection of other rest-optical emission lines in the spectra of these LAEs enables the determination of accurate systemic redshifts and Ly$\alpha$ velocity offsets, as well as the physical and chemical composition of their stars and interstellar media. These faint LAEs are consistent with metal-poor systems with high ionization parameters, similar to the general galaxy population at $z>6$. We measure an average ionizing photon production efficiency, log($\xi_{\textrm{ion}}$/erg$^{-1}$ Hz) $\approx 25.56$ across our LAEs, which does not evolve strongly with redshift. We report an anti-correlation between Ly$\alpha$ escape fraction and velocity offset from systemic, consistent with model expectations. We further find that the strength and velocity offset of Ly$\alpha$ are not correlated with galaxy spectroscopic properties nor with $\xi_{\textrm{ion}}$. We find a decrease in Ly$\alpha$ escape fractions with redshift, indicative of decreasing sizes of ionized bubbles around LAEs at high redshifts. We use a range of galaxy properties to predict Lyman continuum escape fractions for our LAEs, finding that the ionizing photon output into the intergalactic medium from our LAEs remains roughly constant across the observed UV magnitude and Ly$\alpha$ equivalent width, showing a mild increase with redshift. We derive correlations between the ionizing photon output from LAEs and UV magnitude Ly$\alpha$ strengths and redshift, which can be used to build realistic reionization models. %R 10.48550/arXiv.2306.04536 %= eprint: arXiv:2306.04536 %0 Electronic Article %T JADES: Balmer Decrement Measurements at redshifts 4 < z < 7 %A Sandles, Lester %A D'Eugenio, Francesco %A Maiolino, Roberto %A Looser, Tobias J. %A Arribas, Santiago %A Baker, William M. %A Bonaventura, Nina %A Bunker, Andrew J. %A Cameron, Alex J. %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Curti, Mirko %A Curtis-Lake, Emma %A de Graaff, Anna %A Eisenstein, Daniel J. %A Hainline, Kevin %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Jones, Gareth C. %A Kumari, Nimisha %A Nelson, Erica %A Perna, Michele %A Rawle, Tim %A Rix, Hans-Walter %A Robertson, Brant %A Rodriguez Del Pino, Bruno %A Scholtz, Jan %A Shivaei, Irene %A Smit, Renske %A Sun, Fengwu %A Tacchella, Sandro %A Uebler, Hannah %A Williams, Christina C. %A Willott, Chris %A Witstok, Joris %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.03931 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230603931S %X We present Balmer decrement H$\alpha$/ H$\beta$ measurements for a sample of 51 galaxies at redshifts z = 4-7 observed with the JWST/NIRSpec MSA, as part of the JADES survey. Leveraging 28-hour long exposures and the efficiency of the prism/clear configuration (but also using information from the medium-resolution gratings), we are able to probe directly the low-mass end of the galaxy population, reaching stellar masses Mstar as low as 10^7 Msun . We find that the correlation between Balmer decrement and Mstar is already established at these high redshifts, indicating a rapid build up of dust in moderately massive galaxies at such early epochs. The lowest-mass galaxies in our sample (Mstar = 1-3 x 10^7 Msun ) display a remarkably low Balmer decrement of 2.88 $\pm$ 0.08, consistent with case B, suggesting very little dust content. However, we warn that such a low observed Balmer decrement may also partly be a consequence of an intrinsically lower H$\alpha$/ H$\beta$, resulting from the extreme conditions of the ionized gas in these primeval and unevolved systems. We further compare the Balmer decrement to continuum-derived star-formation rates (SFR), finding tentative evidence of a correlation, which likely traces the underlying connection between SFR and mass of cold gas. However, we note that larger samples are required to distinguish between direct and primary correlations from indirect and secondary dependencies at such high redshifts. %R 10.48550/arXiv.2306.03931 %= eprint: arXiv:2306.03931 %0 Electronic Article %T JADES: Detecting [OIII]$\lambda 4363$ Emitters and Testing Strong Line Calibrations in the High-$z$ Universe with Ultra-deep JWST/NIRSpec Spectroscopy up to $z \sim 9.5$ %A Laseter, Isaac H. %A Maseda, Michael V. %A Curti, Mirko %A Maiolino, Roberto %A D'Eugenio, Francesco %A Cameron, Alex J. %A Looser, Tobias J. %A Arribas, Santiago %A Baker, William M. %A Bhatawdekar, Rachana %A Boyett, Kristan %A Bunker, Andrew J. %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Curtis-lake, Emma %A Egami, Eiichi %A Eisenstein, Daniel J. %A Hainline, Kevin %A Hausen, Ryan %A Ji, Zhiyuan %A Kumari, Nimisha %A Perna, Michele %A Rawle, Tim %A Rix, Hans-Walter %A Robertson, Brant %A Rodríguez Del Pino, Bruno %A Sandles, Lester %A Scholtz, Jan %A Smit, Renske %A Tacchella, Sandro %A Übler, Hannah %A Williams, Christina C. %A Willott, Chris %A Witstok, Joris %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.03120 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230603120L %Z 28 pages, 13 figures; A&A 681, A70 (2024); doi:10.1051/0004-6361/202347133 %X We present 10 novel [OIII]$\lambda 4363$ auroral line detections up to $z\sim 9.5$ measured from ultra-deep JWST/NIRSpec MSA spectroscopy from the JWST Advanced Deep Extragalactic Survey (JADES). We leverage the deepest spectroscopic observations yet taken with NIRSpec to determine electron temperatures and oxygen abundances using the direct T$_e$ method. We directly compare against a suite of locally calibrated strong-line diagnostics and recent high-$z$ calibrations. We find the calibrations fail to simultaneously match our JADES sample, thus warranting a self-consistent revision of these calibrations for the high-$z$ Universe. We find weak dependence between R2 and O3O2 with metallicity, thus suggesting these line-ratios are ineffective in the high-$z$ Universe as metallicity diagnostics and degeneracy breakers. We find R3 and R23 still correlate with metallicity, but we find tentative flattening of these diagnostics, thus suggesting future difficulties when applying these strong-line ratios as metallicity indicators in the high-$z$ Universe. We also propose and test an alternative diagnostic based on a different combination of R3 and R2 with a higher dynamic range. We find a reasonably good agreement (median offset of 0.002 dex, median absolute offset of 0.13 dex) with the JWST sample at low metallicity. Our sample demonstrates higher ionization/excitation ratios than local galaxies with rest-frame EWs(H$\beta$) $\approx 200 -300$ Angstroms. However, we find the median rest-frame EWs(H$\beta$) of our sample to be $\sim 2\text{x}$ less than the galaxies used for the local calibrations. This EW discrepancy combined with the high ionization of our galaxies does not present a clear description of [OIII]$\lambda 4363$ production in the high-$z$ Universe, thus warranting a much deeper examination into the factors affecting production. %R 10.48550/arXiv.2306.03120 %= eprint: arXiv:2306.03120 %0 Electronic Article %T Inside-out growth in the early Universe: a core in a vigorously star-forming disc %A Baker, William M. %A Tacchella, Sandro %A Johnson, Benjamin D. %A Nelson, Erica %A Suess, Katherine A. %A D'Eugenio, Francesco %A Curti, Mirko %A de Graaff, Anna %A Ji, Zhiyuan %A Maiolino, Roberto %A Robertson, Brant %A Scholtz, Jan %A Alberts, Stacey %A Arribas, Santiago %A Boyett, Kristan %A Bunker, Andrew J. %A Carniani, Stefano %A Charlot, Stephane %A Chen, Zuyi %A Chevallard, Jacopo %A Curtis-Lake, Emma %A Danhaive, A. Lola %A DeCoursey, Christa %A Egami, Eiichi %A Eisenstein, Daniel J. %A Endsley, Ryan %A Hausen, Ryan %A Helton, Jakob M. %A Kumari, Nimisha %A Looser, Tobias J. %A Maseda, Michael V. %A Puskás, Dávid %A Rieke, Marcia %A Sandles, Lester %A Sun, Fengwu %A Übler, Hannah %A Williams, Christina C. %A Willmer, Christopher N. A. %A Witstok, Joris %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.02472 %K Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023arXiv230602472B %Z 49 pages, 15 figures, submitted to Nature Astronomy %X The physical processes that establish the morphological evolution and the structural diversity of galaxies are key unknowns in extragalactic astrophysics. Here we report the finding of the morphologically-mature galaxy JADES-GS+53.18343-27.79097, which existed within the first 700 million years of the Universe's history. This star-forming galaxy with a stellar mass of $10^{8.6}$ solar masses consists of three components, a highly-compact core with a half-light radius of 144 pc, a strongly star-forming disc with a radius of 468 pc, and a star-forming clump, which all show distinctive star-formation histories. The central stellar mass density of this galaxy is within a factor of two of the most massive present-day ellipticals, while being globally 1000 times less massive. The radial profile of the specific star-formation rate is strongly rising toward the outskirts. This evidence strongly suggests the first detection of inside-out growth of a galaxy as a proto-bulge and a star-forming disc in the Epoch of Reionization. %R 10.48550/arXiv.2306.02472 %= eprint: arXiv:2306.02472 %0 Electronic Article %T JADES: The emergence and evolution of Ly$\alpha$ emission and constraints on the IGM neutral fraction %A Jones, Gareth C. %A Bunker, Andrew J. %A Saxena, Aayush %A Witstok, Joris %A Stark, Daniel P. %A Arribas, Santiago %A Baker, William M. %A Bhatawdekar, Rachana %A Bowler, Rebecca %A Boyett, Kristan %A Cameron, Alex J. %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Curti, Mirko %A Curtis-Lake, Emma %A Eisenstein, Daniel J. %A Hainline, Kevin %A Hausen, Ryan %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Kumari, Nimisha %A Looser, Tobias J. %A Maiolino, Roberto %A Maseda, Michael V. %A Parlanti, Eleonora %A Rix, Hans-Walter %A Robertson, Brant E. %A Sandles, Lester %A Scholtz, Jan %A Smit, Renske %A Tacchella, Sandro %A Ubler, Hannah %A Williams, Christina C. %A Willott, Chris %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.02471 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230602471J %Z 18 pages, 10 figures. Accepted for publication in A&A %X The rest-frame UV recombination emission line Ly$\alpha$ can be powered by ionising photons from young massive stars in star forming galaxies, but its ability to be resonantly scattered by neutral gas complicates its interpretation. For reionization era galaxies, a neutral intergalactic medium (IGM) will scatter Ly$\alpha$ from the line of sight, making Ly$\alpha$ a useful probe of the neutral fraction evolution. Here, we explore Ly$\alpha$ in JWST/NIRSpec spectra from the ongoing JADES programme, which targets hundreds of galaxies in the well-studied GOODS-S and GOODS-N fields. These sources are UV-faint ($-20.4<\rm M_{\rm UV}<-16.4$), and thus represent a poorly-explored class of galaxies. The low spectral resolution ($R\sim100$) spectra of a subset of 84 galaxies in GOODS-S with $z_{spec}>5.6$ (as derived with optical lines) are fit with line and continuum models, in order to search for significant line emission. Through exploration of the R100 data, we find evidence for Ly$\alpha$ in 17 sources. This sample allows us to place observational constraints on the fraction of galaxies with Ly$\alpha$ emission in the redshift range $5.6 8 in GOODS-S and GOODS-N %A Hainline, Kevin N. %A Johnson, Benjamin D. %A Robertson, Brant %A Tacchella, Sandro %A Helton, Jakob M. %A Sun, Fengwu %A Eisenstein, Daniel J. %A Simmonds, Charlotte %A Topping, Michael W. %A Whitler, Lily %A Willmer, Christopher N. A. %A Rieke, Marcia %A Suess, Katherine A. %A Hviding, Raphael E. %A Cameron, Alex J. %A Alberts, Stacey %A Baker, William M. %A Bhatawdekar, Rachana %A Boyett, Kristan %A Bunker, Andrew J. %A Carniani, Stefano %A Charlot, Stephane %A Chen, Zuyi %A Curti, Mirko %A Curtis-Lake, Emma %A D'Eugenio, Francesco %A Egami, Eiichi %A Endsley, Ryan %A Hausen, Ryan %A Ji, Zhiyuan %A Looser, Tobias J. %A Lyu, Jianwei %A Maiolino, Roberto %A Nelson, Erica %A Puskas, David %A Rawle, Tim %A Sandles, Lester %A Saxena, Aayush %A Smit, Renske %A Stark, Daniel P. %A Williams, Christina C. %A Willott, Chris %A Witstok, Joris %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.02468 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230602468H %Z v2: 43 pages, 20 figures, accepted by The Astrophysical Journal, full online data catalog found at https://doi.org/10.5281/zenodo.7996499 %X We present a catalog of 717 candidate galaxies at $z > 8$ selected from 125 square arcminutes of NIRCam imaging as part of the JWST Advanced Deep Extragalactic Survey (JADES). We combine the full JADES imaging dataset with data from the JEMS and FRESCO JWST surveys along with extremely deep existing observations from HST/ACS for a final filter set that includes fifteen JWST/NIRCam filters and five HST/ACS filters. The high-redshift galaxy candidates were selected from their estimated photometric redshifts calculated using a template fitting approach, followed by visual inspection from seven independent reviewers. We explore these candidates in detail, highlighting interesting resolved or extended sources, sources with very red long-wavelength slopes, and our highest redshift candidates, which extend to $z_{phot} = 18$. We also investigate potential contamination by stellar objects, and do not find strong evidence from SED fitting that these faint high-redshift galaxy candidates are low-mass stars. Over 93\% of the sources are newly identified from our deep JADES imaging, including 31 new galaxy candidates at $z_{phot} > 12$. Using 42 sources in our sample with measured spectroscopic redshifts from NIRSpec and FRESCO, we find excellent agreement to our photometric redshift estimates, with no catastrophic outliers and an average difference of $\langle \Delta z = z_{phot}- z_{spec} \rangle= 0.26$. These sources comprise one of the most robust samples for probing the early buildup of galaxies within the first few hundred million years of the Universe's history. %R 10.48550/arXiv.2306.02468 %= eprint: arXiv:2306.02468 %0 Electronic Article %T JADES NIRSpec Initial Data Release for the Hubble Ultra Deep Field: Redshifts and Line Fluxes of Distant Galaxies from the Deepest JWST Cycle 1 NIRSpec Multi-Object Spectroscopy %A Bunker, Andrew J. %A Cameron, Alex J. %A Curtis-Lake, Emma %A Jakobsen, Peter %A Carniani, Stefano %A Curti, Mirko %A Witstok, Joris %A Maiolino, Roberto %A D'Eugenio, Francesco %A Looser, Tobias J. %A Willott, Chris %A Bonaventura, Nina %A Hainline, Kevin %A Uebler, Hannah %A Willmer, Christopher N. A. %A Saxena, Aayush %A Smit, Renske %A Alberts, Stacey %A Arribas, Santiago %A Baker, William M. %A Baum, Stefi %A Bhatawdekar, Rachana %A Bowler, Rebecca A. A. %A Boyett, Kristan %A Charlot, Stephane %A Chen, Zuyi %A Chevallard, Jacopo %A Circosta, Chiara %A DeCoursey, Christa %A de Graaff, Anna %A Egami, Eiichi %A Eisenstein, Daniel J. %A Endsley, Ryan %A Ferruit, Pierre %A Giardino, Giovanna %A Hausen, Ryan %A Helton, Jakob M. %A Hviding, Raphael E. %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Jones, Gareth C. %A Kumari, Nimisha %A Laseter, Isaac %A Luetzgendorf, Nora %A Maseda, Michael V. %A Nelson, Erica %A Parlanti, Eleonora %A Perna, Michele %A Rawle, Tim %A Rix, Hans-Walter %A Rieke, Marcia %A Robertson, Brant %A Rodriguez Del Pino, Bruno %A Sandles, Lester %A Scholtz, Jan %A Sharpe, Katherine %A Skarbinski, Maya %A Stark, Daniel P. %A Sun, Fengwu %A Tacchella, Sandro %A Topping, Michael W. %A Villanueva, Natalia C. %A Wallace, Imaan E. B. %A Williams, Christina C. %A Woodrum, Charity %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.02467 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230602467B %Z Submitted to A&A. Data products available from https://archive.stsci.edu/hlsp/jades %X We describe the NIRSpec component of the JWST Deep Extragalactic Survey (JADES), and provide deep spectroscopy of 253 sources targeted with the NIRSpec micro-shutter assembly in the Hubble Ultra Deep Field and surrounding GOODS-South. The multi-object spectra presented here are the deepest so far obtained with JWST, amounting to up to 28 hours in the low-dispersion ($R\sim 30-300$) prism, and up to 7 hours in each of the three medium-resolution $R\approx 1000$ gratings and one high-dispersion grating, G395H ($R\approx2700$). Our low-dispersion and medium-dispersion spectra cover the wavelength range $0.6-5.3\mu$m. We describe the selection of the spectroscopic targets, the strategy for the allocation of targets to micro-shutters, and the design of the observations. We present the public release of the reduced 2D and 1D spectra, and a description of the reduction and calibration process. We measure spectroscopic redshifts for 178 of the objects targeted extending up to $z=13.2$. We present a catalog of all emission lines detected at $S/N>5$, and our redshift determinations for the targets. Combined with the first JADES NIRCam data release, these public JADES spectroscopic and imaging datasets provide a new foundation for discoveries of the infrared universe by the worldwide scientific community. %R 10.48550/arXiv.2306.02467 %= eprint: arXiv:2306.02467 %0 Electronic Article %T Overview of the JWST Advanced Deep Extragalactic Survey (JADES) %A Eisenstein, Daniel J. %A Willott, Chris %A Alberts, Stacey %A Arribas, Santiago %A Bonaventura, Nina %A Bunker, Andrew J. %A Cameron, Alex J. %A Carniani, Stefano %A Charlot, Stephane %A Curtis-Lake, Emma %A D'Eugenio, Francesco %A Endsley, Ryan %A Ferruit, Pierre %A Giardino, Giovanna %A Hainline, Kevin %A Hausen, Ryan %A Jakobsen, Peter %A Johnson, Benjamin D. %A Maiolino, Roberto %A Rieke, Marcia %A Rieke, George %A Rix, Hans-Walter %A Robertson, Brant %A Stark, Daniel P. %A Tacchella, Sandro %A Williams, Christina C. %A Willmer, Christopher N. A. %A Baker, William M. %A Baum, Stefi %A Bhatawdekar, Rachana %A Boyett, Kristan %A Chen, Zuyi %A Chevallard, Jacopo %A Circosta, Chiara %A Curti, Mirko %A Danhaive, A. Lola %A DeCoursey, Christa %A de Graaff, Anna %A Dressler, Alan %A Egami, Eiichi %A Helton, Jakob M. %A Hviding, Raphael E. %A Ji, Zhiyuan %A Jones, Gareth C. %A Kumari, Nimisha %A Lützgendorf, Nora %A Laseter, Isaac %A Looser, Tobias J. %A Lyu, Jianwei %A Maseda, Michael V. %A Nelson, Erica %A Parlanti, Eleonora %A Perna, Michele %A Puskás, Dávid %A Rawle, Tim %A Rodríguez Del Pino, Bruno %A Sandles, Lester %A Saxena, Aayush %A Scholtz, Jan %A Sharpe, Katherine %A Shivaei, Irene %A Silcock, Maddie S. %A Simmonds, Charlotte %A Skarbinski, Maya %A Smit, Renske %A Stone, Meredith %A Suess, Katherine A. %A Sun, Fengwu %A Tang, Mengtao %A Topping, Michael W. %A Übler, Hannah %A Villanueva, Natalia C. %A Wallace, Imaan E. B. %A Whitler, Lily %A Witstok, Joris %A Woodrum, Charity %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.02465 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230602465E %Z 33 pages, submitted to ApJ Supplement. The JADES Collaboration web site is at https://jades-survey.github.io, and the initial data release is available at https://archive.stsci.edu/hlsp/jades with a viewer at http://jades.idies.jhu.edu %X We present an overview of the James Webb Space Telescope (JWST) Advanced Deep Extragalactic Survey (JADES), an ambitious program of infrared imaging and spectroscopy in the GOODS-S and GOODS-N deep fields, designed to study galaxy evolution from high redshift to cosmic noon. JADES uses about 770 hours of Cycle 1 guaranteed time largely from the Near-Infrared Camera (NIRCam) and Near-Infrared Spectrograph (NIRSpec) instrument teams. In GOODS-S, in and around the Hubble Ultra Deep Field and Chandra Deep Field South, JADES produces a deep imaging region of ~45 arcmin$^2$ with an average of 130 hrs of exposure time spread over 9 NIRCam filters. This is extended at medium depth in GOODS-S and GOODS-N with NIRCam imaging of ~175 arcmin$^2$ with an average exposure time of 20 hrs spread over 8-10 filters. In both fields, we conduct extensive NIRSpec multi-object spectroscopy, including 2 deep pointings of 55 hrs exposure time, 14 medium pointings of ~12 hrs, and 15 shallower pointings of ~4 hrs, targeting over 5000 HST and JWST-detected faint sources with 5 low, medium, and high-resolution dispersers covering 0.6-5.3 microns. Finally, JADES extends redward via coordinated parallels with the JWST Mid-Infrared Instrument (MIRI), featuring ~9 arcmin$^2$ with 43 hours of exposure at 7.7 microns and twice that area with 2-6.5 hours of exposure at 12.8 microns For nearly 30 years, the GOODS-S and GOODS-N fields have been developed as the premier deep fields on the sky; JADES is now providing a compelling start on the JWST legacy in these fields. %R 10.48550/arXiv.2306.02465 %= eprint: arXiv:2306.02465 %0 Electronic Article %T JWST-JADES. Possible Population III signatures at z=10.6 in the halo of GN-z11 %A Maiolino, Roberto %A Uebler, Hannah %A Perna, Michele %A Scholtz, Jan %A D'Eugenio, Francesco %A Witten, Callum %A Laporte, Nicolas %A Witstok, Joris %A Carniani, Stefano %A Tacchella, Sandro %A Baker, William %A Arribas, Santiago %A Nakajima, Kimihiko %A Eisenstein, Daniel %A Bunker, Andrew %A Charlot, Stephane %A Cresci, Giovanni %A Curti, Mirko %A Curtis-Lake, Emma %A de Graaff, Anna %A Ji, Zhiyuan %A Johnson, Benjamin D. %A Kumari, Nimisha %A Looser, Tobias J. %A Maseda, Michael %A Robertson, Brant %A Rodriguez Del Pino, Bruno %A Sandles, Lester %A Simmonds, Charlotte %A Smit, Renske %A Sun, Fengwu %A Venturi, Giacomo %A Williams, Christina %A Willmer, Christopher %J arXiv e-prints %D 2023 %8 June 01, 2023 %P arXiv:2306.00953 %K Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023arXiv230600953M %Z Submitted to A&A, 13 pages, 8 figures; some typos corrected and some minor additional information added to match submitted version %X Finding the first generation of stars formed out of pristine gas in the early Universe, known as Population III (PopIII) stars, is one of the most important goals of modern astrophysics. Recent models suggest that PopIII stars may form in pockets of pristine gas in the halo of more evolved galaxies. Here we present NIRSpec-IFU and NIRSpec-MSA observations of the region around GN-z11, an exceptionally luminous galaxy at $z=10.6$, which reveal a $>$5$\sigma$ detection of a feature consistent with being HeII$\lambda$1640 emission at the redshift of GN-z11. The very high equivalent width of the putative HeII emission in this clump (170 A), and the lack of metal lines, can be explained in terms of photoionisation by PopIII stars, while photoionisation by PopII stars is inconsistent with the data. It would also indicate that the putative PopIII stars likely have a top-heavy initial mass function (IMF), with an upper cutoff reaching at least 500 M$_\odot$. The PopIII bolometric luminosity inferred from the HeII line would be $\sim 2\times 10^{10}~L_\odot$, which (with a top-heavy IMF) would imply a total stellar mass formed in the burst of $\sim 6\times 10^{5}~M_\odot$. We find that photoionisation by the Active Galactic Nucleus (AGN) in GN-z11 cannot account for the HeII luminosity observed in the clump, but can potentially be responsible for additional HeII emission observed closer to GN-z11. We also consider the possibility of in-situ photoionisation by an accreting Direct Collapse Black Hole (DCBH) hosted by the HeII clump; we find that this scenario is less favoured, but it remains a possible alternative interpretation. We also report the detection of a Ly$\alpha$ halo stemming out of GN-z11 and extending out to $\sim$2 kpc, as well as resolved, funnel-shaped CIII] emission, likely tracing the ionisation cone of the AGN. %R 10.48550/arXiv.2306.00953 %= eprint: arXiv:2306.00953 %0 Journal Article %T The James Webb Space Telescope Mission %A Gardner, Jonathan P. %A Mather, John C. %A Abbott, Randy %A Abell, James S. %A Abernathy, Mark %A Abney, Faith E. %A Abraham, John G. %A Abraham, Roberto %A Abul-Huda, Yasin M. %A Acton, Scott %A Adams, Cynthia K. %A Adams, Evan %A Adler, David S. %A Adriaensen, Maarten %A Aguilar, Jonathan Albert %A Ahmed, Mansoor %A Ahmed, Nasif S. %A Ahmed, Tanjira %A Albat, Rüdeger %A Albert, Loïc %A Alberts, Stacey %A Aldridge, David %A Allen, Mary Marsha %A Allen, Shaune S. %A Altenburg, Martin %A Altunc, Serhat %A Alvarez, Jose Lorenzo %A Álvarez-Márquez, Javier %A Alves de Oliveira, Catarina %A Ambrose, Leslie L. %A Anandakrishnan, Satya M. %A Andersen, Gregory C. %A Anderson, Harry James %A Anderson, Jay %A Anderson, Kristen %A Anderson, Sara M. %A Aprea, Julio %A Archer, Benita J. %A Arenberg, Jonathan W. %A Argyriou, Ioannis %A Arribas, Santiago %A Artigau, Étienne %A Arvai, Amanda Rose %A Atcheson, Paul %A Atkinson, Charles B. %A Averbukh, Jesse %A Aymergen, Cagatay %A Bacinski, John J. %A Baggett, Wayne E. %A Bagnasco, Giorgio %A Baker, Lynn L. %A Balzano, Vicki Ann %A Banks, Kimberly A. %A Baran, David A. %A Barker, Elizabeth A. %A Barrett, Larry K. %A Barringer, Bruce O. %A Barto, Allison %A Bast, William %A Baudoz, Pierre %A Baum, Stefi %A Beatty, Thomas G. %A Beaulieu, Mathilde %A Bechtold, Kathryn %A Beck, Tracy %A Beddard, Megan M. %A Beichman, Charles %A Bellagama, Larry %A Bely, Pierre %A Berger, Timothy W. %A Bergeron, Louis E. %A Bernier, Antoine-Darveau %A Bertch, Maria D. %A Beskow, Charlotte %A Betz, Laura E. %A Biagetti, Carl P. %A Birkmann, Stephan %A Bjorklund, Kurt F. %A Blackwood, James D. %A Blazek, Ronald Paul %A Blossfeld, Stephen %A Bluth, Marcel %A Boccaletti, Anthony %A Boegner, Martin E., Jr. %A Bohlin, Ralph C. %A Boia, John Joseph %A Böker, Torsten %A Bonaventura, N. %A Bond, Nicholas A. %A Bosley, Kari Ann %A Boucarut, Rene A. %A Bouchet, Patrice %A Bouwman, Jeroen %A Bower, Gary %A Bowers, Ariel S. %A Bowers, Charles W. %A Boyce, Leslye A. %A Boyer, Christine T. %A Boyer, Martha L. %A Boyer, Michael %A Boyer, Robert %A Bradley, Larry D. %A Brady, Gregory R. %A Brandl, Bernhard R. %A Brannen, Judith L. %A Breda, David %A Bremmer, Harold G. %A Brennan, David %A Bresnahan, Pamela A. %A Bright, Stacey N. %A Broiles, Brian J. %A Bromenschenkel, Asa %A Brooks, Brian H. %A Brooks, Keira J. %A Brown, Bob %A Brown, Bruce %A Brown, Thomas M. %A Bruce, Barry W. %A Bryson, Jonathan G. %A Bujanda, Edwin D. %A Bullock, Blake M. %A Bunker, A. J. %A Bureo, Rafael %A Burt, Irving J. %A Bush, James Aaron %A Bushouse, Howard A. %A Bussman, Marie C. %A Cabaud, Olivier %A Cale, Steven %A Calhoon, Charles D. %A Calvani, Humberto %A Canipe, Alicia M. %A Caputo, Francis M. %A Cara, Mihai %A Carey, Larkin %A Case, Michael Eli %A Cesari, Thaddeus %A Cetorelli, Lee D. %A Chance, Don R. %A Chandler, Lynn %A Chaney, Dave %A Chapman, George N. %A Charlot, S. %A Chayer, Pierre %A Cheezum, Jeffrey I. %A Chen, Bin %A Chen, Christine H. %A Cherinka, Brian %A Chichester, Sarah C. %A Chilton, Zachary S. %A Chittiraibalan, Dharini %A Clampin, Mark %A Clark, Charles R. %A Clark, Kerry W. %A Clark, Stephanie M. %A Claybrooks, Edward E. %A Cleveland, Keith A. %A Cohen, Andrew L. %A Cohen, Lester M. %A Colón, Knicole D. %A Coleman, Benee L. %A Colina, Luis %A Comber, Brian J. %A Comeau, Thomas M. %A Comer, Thomas %A Conde Reis, Alain %A Connolly, Dennis C. %A Conroy, Kyle E. %A Contos, Adam R. %A Contreras, James %A Cook, Neil J. %A Cooper, James L. %A Cooper, Rachel Aviva %A Correia, Michael F. %A Correnti, Matteo %A Cossou, Christophe %A Costanza, Brian F. %A Coulais, Alain %A Cox, Colin R. %A Coyle, Ray T. %A Cracraft, Misty M. %A Crew, Keith A. %A Curtis, Gary J. %A Cusveller, Bianca %A Da Costa Maciel, Cleyciane %A Dailey, Christopher T. %A Daugeron, Frédéric %A Davidson, Greg S. %A Davies, James E. %A Davis, Katherine Anne %A Davis, Michael S. %A Day, Ratna %A de Chambure, Daniel %A de Jong, Pauline %A De Marchi, Guido %A Dean, Bruce H. %A Decker, John E. %A Delisa, Amy S. %A Dell, Lawrence C. %A Dellagatta, Gail %A Dembinska, Franciszka %A Demosthenes, Sandor %A Dencheva, Nadezhda M. %A Deneu, Philippe %A DePriest, William W. %A Deschenes, Jeremy %A Dethienne, Nathalie %A Detre, Örs Hunor %A Diaz, Rosa Izela %A Dicken, Daniel %A DiFelice, Audrey S. %A Dillman, Matthew %A Disharoon, Maureen O. %A Dixon, William V. %A Doggett, Jesse B. %A Dominguez, Keisha L. %A Donaldson, Thomas S. %A Doria-Warner, Cristina M. %A Santos, Tony Dos %A Doty, Heather %A Douglas, Robert E., Jr. %A Doyon, René %A Dressler, Alan %A Driggers, Jennifer %A Driggers, Phillip A. %A Dunn, Jamie L. %A DuPrie, Kimberly C. %A Dupuis, Jean %A Durning, John %A Dutta, Sanghamitra B. %A Earl, Nicholas M. %A Eccleston, Paul %A Ecobichon, Pascal %A Egami, Eiichi %A Ehrenwinkler, Ralf %A Eisenhamer, Jonathan D. %A Eisenhower, Michael %A Eisenstein, Daniel J. %A El Hamel, Zaky %A Elie, Michelle L. %A Elliott, James %A Elliott, Kyle Wesley %A Engesser, Michael %A Espinoza, Néstor %A Etienne, Odessa %A Etxaluze, Mireya %A Evans, Leah %A Fabreguettes, Luce %A Falcolini, Massimo %A Falini, Patrick R. %A Fatig, Curtis %A Feeney, Matthew %A Feinberg, Lee D. %A Fels, Raymond %A Ferdous, Nazma %A Ferguson, Henry C. %A Ferrarese, Laura %A Ferreira, Marie-Héléne %A Ferruit, Pierre %A Ferry, Malcolm %A Filippazzo, Joseph Charles %A Firre, Daniel %A Fix, Mees %A Flagey, Nicolas %A Flanagan, Kathryn A. %A Fleming, Scott W. %A Florian, Michael %A Flynn, James R. %A Foiadelli, Luca %A Fontaine, Mark R. %A Fontanella, Erin Marie %A Forshay, Peter Randolph %A Fortner, Elizabeth A. %A Fox, Ori D. %A Framarini, Alexandro P. %A Francisco, John I. %A Franck, Randy %A Franx, Marijn %A Franz, David E. %A Friedman, Scott D. %A Friend, Katheryn E. %A Frost, James R. %A Fu, Henry %A Fullerton, Alexander W. %A Gaillard, Lionel %A Galkin, Sergey %A Gallagher, Ben %A Galyer, Anthony D. %A García Marín, Macarena %A Gardner, Lisa E. %A Garland, Dennis %A Garrett, Bruce Albert %A Gasman, Danny %A Gáspár, András %A Gastaud, René %A Gaudreau, Daniel %A Gauthier, Peter Timothy %A Geers, Vincent %A Geithner, Paul H. %A Gennaro, Mario %A Gerber, John %A Gereau, John C. %A Giampaoli, Robert %A Giardino, Giovanna %A Gibbons, Paul C. %A Gilbert, Karoline %A Gilman, Larry %A Girard, Julien H. %A Giuliano, Mark E. %A Gkountis, Konstantinos %A Glasse, Alistair %A Glassmire, Kirk Zachary %A Glauser, Adrian Michael %A Glazer, Stuart D. %A Goldberg, Joshua %A 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Hashimoto, Ryan %A Haskins, Sujee J. %A Hawkins, Robert Edward %A Hayden, Brian %A Hayden, William L. %A Healy, Mike %A Hecht, Karen %A Heeg, Vince J. %A Hejal, Reem %A Helm, Kristopher A. %A Hengemihle, Nicholas J. %A Henning, Thomas %A Henry, Alaina %A Henry, Ronald L. %A Henshaw, Katherine %A Hernandez, Scarlin %A Herrington, Donald C. %A Heske, Astrid %A Hesman, Brigette Emily %A Hickey, David L. %A Hilbert, Bryan N. %A Hines, Dean C. %A Hinz, Michael R. %A Hirsch, Michael %A Hitcho, Robert S. %A Hodapp, Klaus %A Hodge, Philip E. %A Hoffman, Melissa %A Holfeltz, Sherie T. %A Holler, Bryan Jason %A Hoppa, Jennifer Rose %A Horner, Scott %A Howard, Joseph M. %A Howard, Richard J. %A Huber, Jean M. %A Hunkeler, Joseph S. %A Hunter, Alexander %A Hunter, David Gavin %A Hurd, Spencer W. %A Hurst, Brendan J. %A Hutchings, John B. %A Hylan, Jason E. %A Ignat, Luminita Ilinca %A Illingworth, Garth %A Irish, Sandra M. %A Isaacs, John C., III %A Jackson, Wallace C., Jr. %A Jaffe, Daniel T. %A Jahic, Jasmin %A Jahromi, Amir %A Jakobsen, Peter %A James, Bryan %A James, John C. %A James, LeAndrea Rae %A Jamieson, William Brian %A Jandra, Raymond D. %A Jayawardhana, Ray %A Jedrzejewski, Robert %A Jeffers, Basil S. %A Jensen, Peter %A Joanne, Egges %A Johns, Alan T. %A Johnson, Carl A. %A Johnson, Eric L. %A Johnson, Patricia %A Johnson, Phillip Stephen %A Johnson, Thomas K. %A Johnson, Timothy W. %A Johnstone, Doug %A Jollet, Delphine %A Jones, Danny P. %A Jones, Gregory S. %A Jones, Olivia C. %A Jones, Ronald A. %A Jones, Vicki %A Jordan, Ian J. %A Jordan, Margaret E. %A Jue, Reginald %A Jurkowski, Mark H. %A Justis, Grant %A Justtanont, Kay %A Kaleida, Catherine C. %A Kalirai, Jason S. %A Kalmanson, Phillip Cabrales %A Kaltenegger, Lisa %A Kammerer, Jens %A Kan, Samuel K. %A Kanarek, Graham Childs %A Kao, Shaw-Hong %A Karakla, Diane M. %A Karl, Hermann %A Kassin, Susan A. %A Kauffman, David D. %A Kavanagh, Patrick %A Kelley, Leigh L. %A Kelly, Douglas M. %A Kendrew, Sarah %A Kennedy, Herbert V. %A Kenny, Deborah A. %A Keski-Kuha, Ritva A. %A Keyes, Charles D. %A Khan, Ali %A Kidwell, Richard C. %A Kimble, Randy A. %A King, James S. %A King, Richard C. %A Kinzel, Wayne M. %A Kirk, Jeffrey R. %A Kirkpatrick, Marc E. %A Klaassen, Pamela %A Klingemann, Lana %A Klintworth, Paul U. %A Knapp, Bryan Adam %A Knight, Scott %A Knollenberg, Perry J. %A Knutsen, Daniel Mark %A Koehler, Robert %A Koekemoer, Anton M. %A Kofler, Earl T. %A Kontson, Vicki L. %A Kovacs, Aiden Rose %A Kozhurina-Platais, Vera %A Krause, Oliver %A Kriss, Gerard A. %A Krist, John %A Kristoffersen, Monica R. %A Krogel, Claudia %A Krueger, Anthony P. %A Kulp, Bernard A. %A Kumari, Nimisha %A Kwan, Sandy W. %A Kyprianou, Mark %A Labador, Aurora Gadiano %A Labiano, Álvaro %A Lafrenière, David %A Lagage, Pierre-Olivier %A Laidler, Victoria G. %A Laine, Benoit %A Laird, Simon %A Lajoie, Charles-Philippe %A Lallo, Matthew D. %A Lam, May Yen %A LaMassa, Stephanie Marie %A Lambros, Scott D. %A Lampenfield, Richard Joseph %A Lander, Matthew Ed %A Langston, James Hutton %A Larson, Kirsten %A Larson, Melora %A LaVerghetta, Robert Joseph %A Law, David R. %A Lawrence, Jon F. %A Lee, David W. %A Lee, Janice %A Lee, Yat-Ning Paul %A Leisenring, Jarron %A Leveille, Michael Dunlap %A Levenson, Nancy A. %A Levi, Joshua S. %A Levine, Marie B. %A Lewis, Dan %A Lewis, Jake %A Lewis, Nikole %A Libralato, Mattia %A Lidon, Norbert %A Liebrecht, Paula Louisa %A Lightsey, Paul %A Lilly, Simon %A Lim, Frederick C. %A Lim, Pey Lian %A Ling, Sai-Kwong %A Link, Lisa J. %A Link, Miranda Nicole %A Lipinski, Jamie L. %A Liu, XiaoLi %A Lo, Amy S. %A Lobmeyer, Lynette %A Logue, Ryan M. %A Long, Chris A. %A Long, Douglas R. %A Long, Ilana D. %A Long, Knox S. %A López-Caniego, Marcos %A Lotz, Jennifer M. %A Love-Pruitt, Jennifer M. %A Lubskiy, Michael %A Luers, Edward B. %A Luetgens, Robert A. %A Luevano, Annetta J. %A Lui, Sarah Marie G. 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C. %A Slocum, Christine E. %A Slowinski, Steven E. %A Smith, Corbett T. %A Smith, Eric P. %A Smith, Erin C. %A Smith, Koby %A Smith, Robert %A Smith, Stephanie J. %A Smolik, John L. %A Soderblom, David R. %A Sohn, Sangmo Tony %A Sokol, Jeff %A Sonneborn, George %A Sontag, Christopher D. %A Sooy, Peter R. %A Soummer, Remi %A Southwood, Dana M. %A Spain, Kay %A Sparmo, Joseph %A Speer, David T. %A Spencer, Richard %A Sprofera, Joseph D. %A Stallcup, Scott S. %A Stanley, Marcia K. %A Stansberry, John A. %A Stark, Christopher C. %A Starr, Carl W. %A Stassi, Diane Y. %A Steck, Jane A. %A Steeley, Christine D. %A Stephens, Matthew A. %A Stephenson, Ralph J. %A Stewart, Alphonso C. %A Stiavelli, Massimo %A , Stockman, Hervey Jr. %A Strada, Paolo %A Straughn, Amber N. %A Streetman, Scott %A Strickland, David Kendal %A Strobele, Jingping F. %A Stuhlinger, Martin %A Stys, Jeffrey Edward %A Such, Miguel %A Sukhatme, Kalyani %A Sullivan, Joseph F. %A Sullivan, Pamela C. %A Sumner, Sandra M. %A Sun, Fengwu %A Sunnquist, Benjamin Dale %A Swade, Daryl Allen %A Swam, Michael S. %A Swenton, Diane F. %A Swoish, Robby A. %A Tam Litten, Oi In %A Tamas, Laszlo %A Tao, Andrew %A Taylor, David K. %A Taylor, Joanna M. %A te Plate, Maurice %A Van Tea, Mason %A Teague, Kelly K. %A Telfer, Randal C. %A Temim, Tea %A Texter, Scott C. %A Thatte, Deepashri G. %A Thompson, Christopher Lee %A Thompson, Linda M. %A Thomson, Shaun R. %A Thronson, Harley %A Tierney, C. M. %A Tikkanen, Tuomo %A Tinnin, Lee %A Tippet, William Thomas %A Todd, Connor William %A Tran, Hien D. %A Trauger, John %A Trejo, Edwin Gregorio %A Vinh Truong, Justin Hoang %A Tsukamoto, Christine L. %A Tufail, Yasir %A Tumlinson, Jason %A Tustain, Samuel %A Tyra, Harrison %A Ubeda, Leonardo %A Underwood, Kelli %A Uzzo, Michael A. %A Vaclavik, Steven %A Valenduc, Frida %A Valenti, Jeff A. %A Van Campen, Julie %A van de Wetering, Inge %A Van Der Marel, Roeland P. %A van Haarlem, Remy %A Vandenbussche, Bart %A van Dishoeck, Ewine F. %A Vanterpool, Dona D. %A Vernoy, Michael R. %A Vila Costas, Maria Begoña %A Volk, Kevin %A Voorzaat, Piet %A Voyton, Mark F. %A Vydra, Ekaterina %A Waddy, Darryl J. %A Waelkens, Christoffel %A Wahlgren, Glenn Michael %A Walker, Frederick E., Jr. %A Wander, Michel %A Warfield, Christine K. %A Warner, Gerald %A Wasiak, Francis C. %A Wasiak, Matthew F. %A Wehner, James %A Weiler, Kevin R. %A Weilert, Mark %A Weiss, Stanley B. %A Wells, Martyn %A Welty, Alan D. %A Wheate, Lauren %A Wheeler, Thomas P. %A White, Christy L. %A Whitehouse, Paul %A Whiteleather, Jennifer Margaret %A Whitman, William Russell %A Williams, Christina C. %A Willmer, Christopher N. 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Cherry Avenue, Tucson, AZ 85719, USA), ALI(University of Arizona, Department of Astronomy and Steward Observatory), ALJ(Herzberg Institute for Astronomy and Astrophysics), ALK(Northrop Grumman Aerospace, Redondo Beach), ALL(Honeywell Aerospace #100, 303 Terry Fox Drive, Ottawa, ON K2K 3J1, Canada), ALM(University of Arizona, Department of Astronomy and Steward Observatory), ALN(NASA Goddard Space Flight Center, Maryland), ALO(Arizona State University, School of Earth and Space Exploration), ALP(Space Telescope Science Institute, Baltimore, Maryland), ALQ(Space Telescope Science Institute, Baltimore, Maryland), ALR(Space Telescope Science Institute, Baltimore, Maryland), ALS(University of Arizona, Department of Astronomy and Steward Observatory), ALT(European Space Agency, Centre Spatial Guyanais, BP816-Route Nationale 1, 97388 Kourou CEDEX, French Guiana, France), ALU(Northrop Grumman Aerospace, Redondo Beach), ALV(Northrop Grumman Aerospace, Redondo Beach), ALW(Ball Aerospace and Technologies Corporation, Colorado), ALX(Space Telescope Science Institute, Baltimore, Maryland), ALY(Royal Observatory Edinburgh), ALZ(NASA Goddard Space Flight Center, Maryland), AMA(Space Telescope Science Institute, Baltimore, Maryland), AMB(Northrop Grumman Aerospace, Redondo Beach), AMC(Space Telescope Science Institute, Baltimore, Maryland), AMD(Space Telescope Science Institute, Baltimore, Maryland), AME(NASA Goddard Space Flight Center, Maryland), AMF(Northrop Grumman Aerospace, Redondo Beach), AMG(Space Telescope Science Institute, Baltimore, Maryland), AMH(Space Telescope Science Institute, Baltimore, Maryland), AMI(Space Telescope Science Institute, Baltimore, Maryland), AMJ(Universities Space Research Association, 425 3rd Street Southwest, Suite 950, Washington DC 20024, USA), AMK(Northrop Grumman Aerospace, Redondo Beach), AML(Northrop Grumman Aerospace, Redondo Beach), AMM(Space Telescope Science Institute, Baltimore, Maryland), AMN(Space Telescope Science Institute, Baltimore, Maryland), AMO(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AMP(Space Telescope Science Institute, Baltimore, Maryland), AMQ(Honeywell Aerospace #100, 303 Terry Fox Drive, Ottawa, ON K2K 3J1, Canada), AMR(NASA Goddard Space Flight Center, Maryland), AMS(Space Telescope Science Institute, Baltimore, Maryland), AMT(European Space Research and Technology Centre) %J Publications of the Astronomical Society of the Pacific %V 135 %D 2023 %8 June 01, 2023 %P 068001 %K Space vehicle instruments; Astronomical instrumentation; Infrared astronomy; Infrared observatories; Space observatories; History of astronomy; 1548; 799; 786; 791; 1543; 1868; Astrophysics - Instrumentation and Methods for Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023PASP..135f8001G %X Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least 4 m. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the 6.5 m James Webb Space Telescope. A generation of astronomers will celebrate their accomplishments for the life of the mission, potentially as long as 20 yr, and beyond. This report and the scientific discoveries that follow are extended thank-you notes to the 20,000 team members. The telescope is working perfectly, with much better image quality than expected. In this and accompanying papers, we give a brief history, describe the observatory, outline its objectives and current observing program, and discuss the inventions and people who made it possible. We cite detailed reports on the design and the measured performance on orbit. %R 10.1088/1538-3873/acd1b5 %= eprint: arXiv:2304.04869 %@ 0004-6280 %0 Journal Article %T Intrinsic alignment as an RSD contaminant in the DESI survey %A Lamman, Claire %A Eisenstein, Daniel %A Aguilar, Jessica Nicole %A Brooks, David %A de la Macorra, Axel %A Doel, Peter %A Font-Ribera, Andreu %A Gontcho A Gontcho, Satya %A Honscheid, Klaus %A Kehoe, Robert %A Kisner, Theodore %A Kremin, Anthony %A Landriau, Martin %A Levi, Michael %A Miquel, Ramon %A Moustakas, John %A Palanque-Delabrouille, Nathalie %A Poppett, Claire %A Schubnell, Michael %A Tarlé, Gregory %+ AA(Harvard Smithsonian Center for Astrophysics), AB(Harvard Smithsonian Center for Astrophysics), AC(Lawrence Berkeley National Laboratory, California), AD(University College London, Department of Physics and Astronomy), AE(UNAM, Institute of Physics), AF(University College London, Department of Physics and Astronomy), AG(Institut de Física de'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, Spain;), AH(Lawrence Berkeley National Laboratory, California), AI(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Physics), AJ(Southern Methodist University, Texas), AK(Lawrence Berkeley National Laboratory, California), AL(Lawrence Berkeley National Laboratory, California), AM(Lawrence Berkeley National Laboratory, California), AN(Lawrence Berkeley National Laboratory, California), AO(Institut de Física de'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, Spain; Institució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys, 23, E-08010 Barcelona, Spain), AP(Siena College, New York), AQ(Lawrence Berkeley National Laboratory, California; Institut de Recherche sur les Lois Fondamentales de l'Universe), AR(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory; University of California, Berkeley, Space Sciences Laboratory), AS(University of Michigan, Department of Physics), AT(University of Michigan, Department of Physics) %J Monthly Notices of the Royal Astronomical Society %V 522 %D 2023 %8 June 01, 2023 %P 117-129 %K methods: data analysis; dark energy; large-scale structure of Universe; cosmology: observations; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.522..117L %X We measure the tidal alignment of the major axes of luminous red galaxies (LRGs) from the Legacy Imaging Survey and use it to infer the artificial redshift-space distortion signature that will arise from an orientation-dependent, surface-brightness selection in the Dark Energy Spectroscopic Instrument (DESI) survey. Using photometric redshifts to downweight the shape-density correlations due to weak lensing, we measure the intrinsic tidal alignment of LRGs. Separately, we estimate the net polarization of LRG orientations from DESI's fibre-magnitude target selection to be of order 10-2 along the line of sight. Using these measurements and a linear tidal model, we forecast a 0.5 per cent fractional decrease on the quadrupole of the two-point correlation function for projected separations of 40-80 h-1 Mpc. We also use a halo catalogue from the ABACUSSUMMIT cosmological simulation suite to reproduce this false quadrupole. %R 10.1093/mnras/stad950 %= eprint: arXiv:2209.03949 %@ 0035-8711 %0 Journal Article %T The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation %A Hahn, ChangHoon %A Wilson, Michael J. %A Ruiz-Macias, Omar %A Cole, Shaun %A Weinberg, David H. %A Moustakas, John %A Kremin, Anthony %A Tinker, Jeremy L. %A Smith, Alex %A Wechsler, Risa H. %A Ahlen, Steven %A Alam, Shadab %A Bailey, Stephen %A Brooks, David %A Cooper, Andrew P. %A Davis, Tamara M. %A Dawson, Kyle %A Dey, Arjun %A Dey, Biprateep %A Eftekharzadeh, Sarah %A Eisenstein, Daniel J. %A Fanning, Kevin %A Forero-Romero, Jaime E. %A Frenk, Carlos S. %A Gaztañaga, Enrique %A Gontcho A Gontcho, Satya %A Guy, Julien %A Honscheid, Klaus %A Ishak, Mustapha %A Juneau, Stéphanie %A Kehoe, Robert %A Kisner, Theodore %A Lan, Ting-Wen %A Landriau, Martin %A Le Guillou, Laurent %A Levi, Michael E. %A Magneville, Christophe %A Martini, Paul %A Meisner, Aaron %A Myers, Adam D. %A Nie, Jundan %A Norberg, Peder %A Palanque-Delabrouille, Nathalie %A Percival, Will J. %A Poppett, Claire %A Prada, Francisco %A Raichoor, Anand %A Ross, Ashley J. %A Safonova, Sasha %A Saulder, Christoph %A Schlafly, Eddie %A Schlegel, David %A Sierra-Porta, David %A Tarle, Gregory %A Weaver, Benjamin A. %A Yèche, Christophe %A Zarrouk, Pauline %A Zhou, Rongpu %A Zhou, Zhimin %A Zou, Hu %+ AA(Princeton University, Department of Astrophysical Sciences; Lawrence Berkeley National Laboratory, California), AB(Lawrence Berkeley National Laboratory, California; Durham University, Department of Physics), AC(Durham University, Department of Physics), AD(Durham University, Department of Physics), AE(The Ohio State University, Department of Astronomy), AF(Siena College, New York), AG(Lawrence Berkeley National Laboratory, California), AH(New York University, Department of Physics/CCPP), AI(Durham University, Department of Physics; Institut de Recherche sur les Lois Fondamentales de l'Universe; Royal Observatory Edinburgh), AJ(Stanford University, Department of Physics; Kavli Institute for Particle Astrophysics and Cosmology, California; Stanford Linear Accelerator Center), AK(Physics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, USA), AL(Royal Observatory Edinburgh), AM(Lawrence Berkeley National Laboratory, California), AN(University College London, Department of Physics and Astronomy), AO(National Tsing-Hua University, Taiwan, Department of Physics), AP(School of Mathematics and Physics, University of Queensland, 4101, Australia), AQ(University of Utah, Department of Physics and Astronomy), AR(National Optical Astronomy Observatory, Arizona), AS(University of Pittsburgh, Department of Physics and Astronomy), AT(Universities Space Research Association, NASA Ames Research Centre, USA), AU(Harvard Smithsonian Center for Astrophysics), AV(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), AW(University of the Andes, Colombia), AX(Durham University, Department of Physics), AY(Institut de Cìencies de l'Espai, IEEC-CSIC, Campus UAB, Carrer de Can Magrans s/n, E-08913 Bellaterra, Barcelona, Spain), AZ(Lawrence Berkeley National Laboratory, California; University of Rochester, Department of Physics and Astronomy), BA(Lawrence Berkeley National Laboratory, California), BB(The Ohio State University, Department of Physics), BC(University of Texas, Dallas, Department of Physics), BD(National Optical Astronomy Observatory, Arizona), BE(Southern Methodist University, Texas), BF(Lawrence Berkeley National Laboratory, California), BG(National Taiwan University, Department of Physics; National Taiwan University, Institute of Astrophysics), BH(Lawrence Berkeley National Laboratory, California), BI(Laboratoire de Physique Nucleaire et de Hautes Energies), BJ(Lawrence Berkeley National Laboratory, California), BK(Atomic Energy Commission, Saclay), BL(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), BM(National Optical Astronomy Observatory, Arizona), BN(University of Wyoming, Department of Physics and Astronomy), BO(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100101, People's Republic of China), BP(Durham University, Department of Physics; Durham University, Department of Physics), BQ(Lawrence Berkeley National Laboratory, California; Atomic Energy Commission, Saclay), BR(University of Waterloo, Canada; University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada), BS(Lawrence Berkeley National Laboratory, California), BT(Institute of Astrophysics of Andalusia), BU(Lawrence Berkeley National Laboratory, California), BV(The Ohio State University, Department of Astronomy), BW(Physics Department, Yale University, P.O. Box 208120, New Haven, CT 06511, USA), BX(Korea Astronomy and Space Science Institute), BY(Lawrence Livermore National Laboratory, California), BZ(Lawrence Berkeley National Laboratory, California), CA(University of the Andes, Colombia; -), CB(University of Michigan, Department of Physics), CC(National Optical Astronomy Observatory, Arizona), CD(Atomic Energy Commission, Saclay), CE(Laboratoire de Physique Nucleaire et de Hautes Energies), CF(Lawrence Berkeley National Laboratory, California), CG(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100101, People's Republic of China), CH(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100101, People's Republic of China) %J The Astronomical Journal %V 165 %D 2023 %8 June 01, 2023 %P 253 %K Observational cosmology; Cosmology; Redshift surveys; Galaxies; Galactic and extragalactic astronomy; Galaxy spectroscopy; Spectrophotometry; 1146; 343; 1378; 573; 563; 2171; 1556; Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023AJ....165..253H %X Over the next 5 yr, the Dark Energy Spectroscopic Instrument (DESI) will use 10 spectrographs with 5000 fibers on the 4 m Mayall Telescope at Kitt Peak National Observatory to conduct the first Stage IV dark energy galaxy survey. At z < 0.6, the DESI Bright Galaxy Survey (BGS) will produce the most detailed map of the universe during the dark-energy-dominated epoch with redshifts of >10 million galaxies spanning 14,000 deg2. In this work, we present and validate the final BGS target selection and survey design. From the Legacy Surveys, BGS will target an r < 19.5 mag limited sample (BGS Bright), a fainter 19.5 < r < 20.175 color-selected sample (BGS Faint), and a smaller low-z quasar sample. BGS will observe these targets using exposure times scaled to achieve homogeneous completeness and cover the footprint three times. We use observations from the Survey Validation programs conducted prior to the main survey along with simulations to show that BGS can complete its strategy and make optimal use of "bright" time. BGS targets have stellar contamination <1%, and their densities do not depend strongly on imaging properties. BGS Bright will achieve >80% fiber assignment efficiency. Finally, BGS Bright and BGS Faint will achieve >95% redshift success over any observing condition. BGS meets the requirements for an extensive range of scientific applications. BGS will yield the most precise baryon acoustic oscillation and redshift-space distortion measurements at z < 0.4. It presents opportunities for new methods that require highly complete and dense samples (e.g., N-point statistics, multitracers). BGS further provides a powerful tool to study galaxy populations and the relations between galaxies and dark matter. %R 10.3847/1538-3881/accff8 %= eprint: arXiv:2208.08512 %@ 0004-6256 %0 Electronic Article %T JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5 %A Ji, Zhiyuan %A Williams, Christina C. %A Tacchella, Sandro %A Suess, Katherine A. %A Baker, William M. %A Alberts, Stacey %A Bunker, Andrew J. %A Johnson, Benjamin D. %A Robertson, Brant %A Sun, Fengwu %A Eisenstein, Daniel J. %A Rieke, Marcia %A Maseda, Michael V. %A Hainline, Kevin %A Hausen, Ryan %A Rieke, George %A Willmer, Christopher N. A. %A Egami, Eiichi %A Shivaei, Irene %A Carniani, Stefano %A Charlot, Stephane %A Chevallard, Jacopo %A Curtis-Lake, Emma %A Looser, Tobias J. %A Maiolino, Roberto %A Willott, Chris %A Chen, Zuyi %A Helton, Jakob M. %A Lyu, Jianwei %A Nelson, Erica %A Bhatawdekar, Rachana %A Boyett, Kristan %A Sandles, Lester %J arXiv e-prints %D 2023 %8 May 01, 2023 %P arXiv:2305.18518 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230518518J %Z 32 pages, 16 figures, submitted to ApJ. Comments are welcome %X We present a spatially resolved study of stellar populations in 6 galaxies with stellar masses $M_*\sim10^{10}M_\odot$ at $z\sim3.7$ using 14-filter JWST/NIRCam imaging from the JADES and JEMS surveys. The 6 galaxies are visually selected to have clumpy substructures with distinct colors over rest-frame $3600-4100$Å, including a bright dominant stellar core that is close to their stellar-light centroids. With 23-filter photometry from HST to JWST, we measure the stellar-population properties of individual structural components via SED fitting using Prospector. We find that the central stellar cores are $rsim2$ times more massive than the Toomre mass, indicating they may not form via in-situ fragmentation. The stellar cores have stellar ages of $0.4-0.7$ Gyr that are similar to the timescale of clump inward migration due to dynamical friction, suggesting that they likely instead formed through the coalescence of giant stellar clumps. While they have not yet quenched, the 6 galaxies are below the star-forming main sequence by $0.2-0.7$ dex. Within each galaxy, we find that the specific star formation rate is lower in the central stellar core, and the stellar-mass surface density of the core is already similar to quenched galaxies of the same masses and redshifts. Meanwhile, the stellar ages of the cores are either comparable to or younger than the extended, smooth parts of the galaxies. Our findings are consistent with model predictions of the gas-rich compaction scenario for the buildup of galaxies' central regions at high redshifts. We are likely witnessing the coeval formation of dense central cores, along with the onset of galaxy-wide quenching at $z>3$. %R 10.48550/arXiv.2305.18518 %= eprint: arXiv:2305.18518 %0 Electronic Article %T A small and vigorous black hole in the early Universe %A Maiolino, Roberto %A Scholtz, Jan %A Witstok, Joris %A Carniani, Stefano %A D'Eugenio, Francesco %A de Graaff, Anna %A Uebler, Hannah %A Tacchella, Sandro %A Curtis-Lake, Emma %A Arribas, Santiago %A Bunker, Andrew %A Charlot, Stéphane %A Chevallard, Jacopo %A Curti, Mirko %A Looser, Tobias J. %A Maseda, Michael V. %A Rawle, Tim %A Rodriguez Del Pino, Bruno %A Willott, Chris J. %A Egami, Eiichi %A Eisenstein, Daniel %A Hainline, Kevin %A Robertson, Brant %A Williams, Christina C. %A Willmer, Christopher N. A. %A Baker, William M. %A Boyett, Kristan %A DeCoursey, Christa %A Fabian, Andrew C. %A Helton, Jakob M. %A Ji, Zhiyuan %A Jones, Gareth C. %A Kumari, Nimisha %A Laporte, Nicolas %A Nelson, Erica %A Perna, Michele %A Sandles, Lester %A Shivaei, Irene %A Sun, Fengwu %J arXiv e-prints %D 2023 %8 May 01, 2023 %P arXiv:2305.12492 %K Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - High Energy Astrophysical Phenomena %U https://ui.adsabs.harvard.edu/abs/2023arXiv230512492M %Z 9 figures, 2 tables, published in Nature, replaced to match the accepted version %X Multiple theories have been proposed to describe the formation of black hole seeds in the early Universe and to explain the emergence of very massive black holes observed in the first billion years after Big Bang. Models consider different seeding and accretion scenarios, which require the detection and characterisation of black holes in the first few hundred million years after Big Bang to be validated. Here we present an extensive analysis of the JWST-NIRSpec spectrum of GN-z11, an exceptionally luminous galaxy at z=10.6, revealing the detection of the [NeIV]2423 and CII*1335 transitions (typical of Active Galactic Nuclei, AGN), as well as semi-forbidden nebular lines tracing gas densities higher than 10^9 cm-3, typical of the Broad Line Region of AGN. These spectral features indicate that GN-z11 hosts an accreting black hole. The spectrum also reveals a deep and blueshifted CIV1549 absorption trough, tracing an outflow with velocity 800-1000 km/s, likely driven by the AGN. Assuming local virial relations, we derive a black hole mass of log(M_BH/Msun) = 6.2 +- 0.3, accreting at about 5 times the Eddington rate. These properties are consistent with both heavy seeds scenarios, or scenarios envisaging intermediate/light seeds experiencing episodic super-Eddington phases. Our finding naturally explains the high luminosity of GN-z11 and can also provide an explanation for its exceptionally high nitrogen abundance. %R 10.48550/arXiv.2305.12492 %= eprint: arXiv:2305.12492 %0 Journal Article %T Spectroscopic confirmation of four metal-poor galaxies at z = 10.3-13.2 %A Curtis-Lake, Emma %A Carniani, Stefano %A Cameron, Alex %A Charlot, Stephane %A Jakobsen, Peter %A Maiolino, Roberto %A Bunker, Andrew %A Witstok, Joris %A Smit, Renske %A Chevallard, Jacopo %A Willott, Chris %A Ferruit, Pierre %A Arribas, Santiago %A Bonaventura, Nina %A Curti, Mirko %A D'Eugenio, Francesco %A Franx, Marijn %A Giardino, Giovanna %A Looser, Tobias J. %A Lützgendorf, Nora %A Maseda, Michael V. %A Rawle, Tim %A Rix, Hans-Walter %A Rodríguez del Pino, Bruno %A Übler, Hannah %A Sirianni, Marco %A Dressler, Alan %A Egami, Eiichi %A Eisenstein, Daniel J. %A Endsley, Ryan %A Hainline, Kevin %A Hausen, Ryan %A Johnson, Benjamin D. %A Rieke, Marcia %A Robertson, Brant %A Shivaei, Irene %A Stark, Daniel P. %A Tacchella, Sandro %A Williams, Christina C. %A Willmer, Christopher N. A. %A Bhatawdekar, Rachana %A Bowler, Rebecca %A Boyett, Kristan %A Chen, Zuyi %A de Graaff, Anna %A Helton, Jakob M. %A Hviding, Raphael E. %A Jones, Gareth C. %A Kumari, Nimisha %A Lyu, Jianwei %A Nelson, Erica %A Perna, Michele %A Sandles, Lester %A Saxena, Aayush %A Suess, Katherine A. %A Sun, Fengwu %A Topping, Michael W. %A Wallace, Imaan E. B. %A Whitler, Lily %+ AA(University of Hertfordshire, School of Physics, Astronomy and Mathematics), AB(Scuola Normale Superiore, Pisa, Italy), AC(University of Oxford, Department of Physics), AD(Institut d'Astrophysique de Paris), AE(Niels Bohr Institute for Astronomy, Physics and Geophysics; Niels Bohr Institute for Astronomy, Physics and Geophysics), AF(Kavli Institute for Cosmology, UK; -; University College London, Department of Physics and Astronomy), AG(University of Oxford, Department of Physics), AH(Kavli Institute for Cosmology, UK; -), AI(Liverpool John Moores University, Astrophysics Research Institute), AJ(University of Oxford, Department of Physics), AK(Herzberg Institute for Astronomy and Astrophysics), AL(European Science and Astronomy Center), AM(Center for Astrobiology, Madrid), AN(Niels Bohr Institute for Astronomy, Physics and Geophysics; Niels Bohr Institute for Astronomy, Physics and Geophysics), AO(Kavli Institute for Cosmology, UK; -), AP(Kavli Institute for Cosmology, UK; -), AQ(Leiden Observatory), AR(European Space Research and Technology Centre), AS(Kavli Institute for Cosmology, UK; -), AT(European Space Agency (ESA), ESA Office, STScI, Baltimore, MD, USA), AU(University of Wisconsin, Madison, Department of Astronomy), AV(European Space Agency (ESA), ESA Office, STScI, Baltimore, MD, USA), AW(Max-Planck-Institute for Astronomy, Heidelberg), AX(Center for Astrobiology, Madrid), AY(Kavli Institute for Cosmology, UK; -), AZ(European Space Agency (ESA), ESA Office, STScI, Baltimore, MD, USA), BA(Carnegie Institution of Washington, Observatories, California), BB(University of Arizona, Department of Astronomy and Steward Observatory), BC(Harvard Smithsonian Center for Astrophysics), BD(University of Texas, Austin, Department of Astronomy), BE(University of Arizona, Department of Astronomy and Steward Observatory), BF(Johns Hopkins University, Department of Physics and Astronomy), BG(Harvard Smithsonian Center for Astrophysics), BH(University of Arizona, Department of Astronomy and Steward Observatory), BI(University of California, Santa Cruz, Department of Astronomy and Astrophysics), BJ(University of Arizona, Department of Astronomy and Steward Observatory), BK(University of Arizona, Department of Astronomy and Steward Observatory), BL(Kavli Institute for Cosmology, UK; -), BM(National Optical Astronomy Observatory, Arizona), BN(University of Arizona, Department of Astronomy and Steward Observatory), BO(European Space Research and Technology Centre), BP(Jodrell Bank Centre for Astrophysics), BQ(University of Melbourne, Department of Physics; ANU, Research School of Astronomy and Astrophysics), BR(University of Arizona, Department of Astronomy and Steward Observatory), BS(Max-Planck-Institute for Astronomy, Heidelberg), BT(University of Arizona, Department of Astronomy and Steward Observatory), BU(University of Arizona, Department of Astronomy and Steward Observatory), BV(University of Oxford, Department of Physics), BW(AURA for European Space Agency, Space Telescope Science Institute, Baltimore, MD, USA), BX(University of Arizona, Department of Astronomy and Steward Observatory), BY(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), BZ(Center for Astrobiology, Madrid), CA(Kavli Institute for Cosmology, UK; -), CB(University of Oxford, Department of Physics; University College London, Department of Physics and Astronomy), CC(University of California, Santa Cruz, Department of Astronomy and Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology, California), CD(University of Arizona, Department of Astronomy and Steward Observatory), CE(University of Arizona, Department of Astronomy and Steward Observatory), CF(University of Oxford, Department of Physics), CG(University of Arizona, Department of Astronomy and Steward Observatory) %J Nature Astronomy %V 7 %D 2023 %8 May 01, 2023 %P 622-632 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023NatAs...7..622C %X Finding and characterizing the first galaxies that illuminated the early universe at cosmic dawn is pivotal to understand the physical conditions and the processes that led to the formation of the first stars. In the first few months of operations, imaging from the James Webb Space Telescope (JWST) has been used to identify tens of candidates of galaxies at redshift (z) greater than 10, less than 450 million years after the Big Bang. However, none of such candidates has yet been confirmed spectroscopically, leaving open the possibility that they are actually low-redshift interlopers. Here we present spectroscopic confirmation and analysis of four galaxies unambiguously detected at redshift 10.3 ≤ z ≤ 13.2, previously selected from JWST Near Infrared Camera imaging. The spectra reveal that these primeval galaxies are metal poor, have masses on the order of about 107-108 solar masses and young ages. The damping wings that shape the continuum close to the Lyman edge provide constraints on the neutral hydrogen fraction of the intergalactic medium from normal star-forming galaxies. These findings demonstrate the rapid emergence of the first generations of galaxies at cosmic dawn. %R 10.1038/s41550-023-01918-w %= eprint: arXiv:2212.04568 %@ 2397-3366 %0 Journal Article %T Identification and properties of intense star-forming galaxies at redshifts z > 10 %A Robertson, B. E. %A Tacchella, S. %A Johnson, B. D. %A Hainline, K. %A Whitler, L. %A Eisenstein, D. J. %A Endsley, R. %A Rieke, M. %A Stark, D. P. %A Alberts, S. %A Dressler, A. %A Egami, E. %A Hausen, R. %A Rieke, G. %A Shivaei, I. %A Williams, C. C. %A Willmer, C. N. A. %A Arribas, S. %A Bonaventura, N. %A Bunker, A. %A Cameron, A. J. %A Carniani, S. %A Charlot, S. %A Chevallard, J. %A Curti, M. %A Curtis-Lake, E. %A D'Eugenio, F. %A Jakobsen, P. %A Looser, T. J. %A Lützgendorf, N. %A Maiolino, R. %A Maseda, M. V. %A Rawle, T. %A Rix, H. -W. %A Smit, R. %A Übler, H. %A Willott, C. %A Witstok, J. %A Baum, S. %A Bhatawdekar, R. %A Boyett, K. %A Chen, Z. %A de Graaff, A. %A Florian, M. %A Helton, J. M. %A Hviding, R. E. %A Ji, Z. %A Kumari, N. %A Lyu, J. %A Nelson, E. %A Sandles, L. %A Saxena, A. %A Suess, K. A. %A Sun, F. %A Topping, M. %A Wallace, I. E. B. %+ AA(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AB(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AC(Harvard Smithsonian Center for Astrophysics), AD(University of Arizona, Department of Astronomy and Steward Observatory), AE(University of Arizona, Department of Astronomy and Steward Observatory), AF(Harvard Smithsonian Center for Astrophysics), AG(University of Texas, Austin, Department of Astronomy), AH(University of Arizona, Department of Astronomy and Steward Observatory), AI(University of Arizona, Department of Astronomy and Steward Observatory), AJ(University of Arizona, Department of Astronomy and Steward Observatory), AK(Carnegie Institution of Washington, Observatories, California), AL(University of Arizona, Department of Astronomy and Steward Observatory), AM(Johns Hopkins University, Department of Physics and Astronomy), AN(University of Arizona, Department of Astronomy and Steward Observatory), AO(University of Arizona, Department of Astronomy and Steward Observatory), AP(National Optical Astronomy Observatory, Arizona), AQ(University of Arizona, Department of Astronomy and Steward Observatory), AR(Centre for Astrobiology (CAB), CSIC-INTA, Torrejón de Ardoz, Madrid, Spain), AS(Niels Bohr Institute for Astronomy, Physics and Geophysics; Niels Bohr Institute for Astronomy, Physics and Geophysics), AT(University of Oxford, Department of Physics), AU(University of Oxford, Department of Physics), AV(Scuola Normale Superiore, Pisa, Italy), AW(Institut d'Astrophysique de Paris), AX(University of Oxford, Department of Physics), AY(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AZ(University of Hertfordshire, School of Physics, Astronomy and Mathematics), BA(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BB(Niels Bohr Institute for Astronomy, Physics and Geophysics; Niels Bohr Institute for Astronomy, Physics and Geophysics), BC(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BD(Space Telescope Science Institute, European Space Agency, Baltimore, MD, USA), BE(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy; University College London, Department of Physics and Astronomy), BF(University of Wisconsin, Madison, Department of Astronomy), BG(Space Telescope Science Institute, European Space Agency, Baltimore, MD, USA), BH(Max-Planck-Institute for Astronomy, Heidelberg), BI(Liverpool John Moores University, Astrophysics Research Institute), BJ(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BK(Herzberg Institute for Astronomy and Astrophysics), BL(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BM(University of Manitoba, Department of Physics and Astronomy), BN(European Space Research and Technology Centre), BO(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics in 3D), BP(University of Arizona, Department of Astronomy and Steward Observatory), BQ(Max-Planck-Institute for Astronomy, Heidelberg), BR(University of Arizona, Department of Astronomy and Steward Observatory), BS(University of Arizona, Department of Astronomy and Steward Observatory), BT(University of Arizona, Department of Astronomy and Steward Observatory), BU(University of Arizona, Department of Astronomy and Steward Observatory), BV(Space Telescope Science Institute, AURA for European Space Agency, Baltimore, MD, USA), BW(University of Arizona, Department of Astronomy and Steward Observatory), BX(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), BY(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), BZ(University of Oxford, Department of Physics; University College London, Department of Physics and Astronomy), CA(University of California, Santa Cruz, Department of Astronomy and Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology, California), CB(University of Arizona, Department of Astronomy and Steward Observatory), CC(University of Arizona, Department of Astronomy and Steward Observatory), CD(University of Oxford, Department of Physics) %J Nature Astronomy %V 7 %D 2023 %8 May 01, 2023 %P 611-621 %K Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023NatAs...7..611R %X Surveys with the James Webb Space Telescope (JWST) have discovered candidate galaxies in the first 400 Myr of cosmic time. Preliminary indications have suggested these candidate galaxies may be more massive and abundant than previously thought. However, without confirmed distances, their inferred properties remain uncertain. Here we identify four galaxies located in the JWST Advanced Deep Extragalactic Survey Near-Infrared Camera imaging with photometric redshifts z of roughly 10-13. These galaxies include the first redshift z > 12 systems discovered with distances spectroscopically confirmed by JWST in a companion paper. Using stellar population modelling, we find the galaxies typically contain 100 million solar masses in stars, in stellar populations that are less than 100 million years old. The moderate star-formation rates and compact sizes suggest elevated star-formation rate surface densities, a key indicator of their formation pathways. Taken together, these measurements show that the first galaxies contributing to cosmic reionization formed rapidly and with intense internal radiation fields. %R 10.1038/s41550-023-01921-1 %= eprint: arXiv:2212.04480 %@ 2397-3366 %0 Journal Article %T Non-parametric Lagrangian biasing from the insights of neural nets %A Wu, Xiaohan %A Muñoz, Julian B. %A Eisenstein, Daniel J. %+ AA(Harvard Smithsonian Center for Astrophysics; Canadian Institute for Theoretical Astrophysics), AB(Harvard Smithsonian Center for Astrophysics), AC(Harvard Smithsonian Center for Astrophysics) %J Journal of Cosmology and Astroparticle Physics %V 2023 %D 2023 %8 May 01, 2023 %P 040 %K cosmic web; redshift surveys; cosmological simulations; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023JCAP...05..040W %X We present a Lagrangian model of galaxy clustering bias in which we train a neural net using the local properties of the smoothed initial density field to predict the late-time mass-weighted halo field. By fitting the mass-weighted halo field in the ABACUSSUMMIT simulations at z = 0.5, we find that including three coarsely spaced smoothing scales gives the best recovery of the halo power spectrum. Adding more smoothing scales may lead to 2-5% underestimation of the large-scale power and can cause the neural net to overfit. We find that the fitted halo-to-mass ratio can be well described by two directions in the original high-dimension feature space. Projecting the original features into these two principal components and re-training the neural net either reproduces the original training result, or outperforms it with a better match of the halo power spectrum. The elements of the principal components are unlikely to be assigned physical meanings, partly owing to the features being highly correlated between different smoothing scales. Our work illustrates a potential need to include multiple smoothing scales when studying galaxy bias, and this can be done easily with machine-learning methods that can take in high dimensional input feature space. %R 10.1088/1475-7516/2023/05/040 %= eprint: arXiv:2212.08095 %@ 1475-7516 %0 Journal Article %T JWST Reveals a Population of Ultrared, Flattened Galaxies at 2 ≲ z ≲ 6 Previously Missed by HST %A Nelson, Erica J. %A Suess, Katherine A. %A Bezanson, Rachel %A Price, Sedona H. %A van Dokkum, Pieter %A Leja, Joel %A Wang, Bingjie %A Whitaker, Katherine E. %A Labbé, Ivo %A Barrufet, Laia %A Brammer, Gabriel %A Eisenstein, Daniel J. %A Gibson, Justus %A Hartley, Abigail I. %A Johnson, Benjamin D. %A Heintz, Kasper E. %A Mathews, Elijah %A Miller, Tim B. %A Oesch, Pascal A. %A Sandles, Lester %A Setton, David J. %A Speagle, Joshua S. %A Tacchella, Sandro %A Tadaki, Ken-ichi %A Übler, Hannah %A Weaver, John. R. %+ AA(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), AB(University of California, Santa Cruz, Department of Astronomy and Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology, California), AC(University of Pittsburgh, Department of Physics and Astronomy), AD(Max-Planck-Institute for Extraterrestrial Physics, Garching), AE(Yale University, Department of Astronomy), AF(Pennsylvania State University, Department of Astronomy; Pennsylvania State University; Pennsylvania State University, Institute for Gravitation and the Cosmos), AG(Pennsylvania State University, Department of Astronomy; Pennsylvania State University; Pennsylvania State University, Institute for Gravitation and the Cosmos), AH(UMass Amherst; Niels Bohr Institute for Astronomy, Physics and Geophysics), AI(Swinburne University of Technology, Center for Astrophysics and Supercomputing), AJ(University of Geneva, Astronomical Observatory), AK(Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Jagtvej 128, Kø benhavn N, DK-2200, Denmark), AL(Harvard Smithsonian Center for Astrophysics), AM(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), AN(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), AO(Harvard Smithsonian Center for Astrophysics), AP(Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Jagtvej 128, Kø benhavn N, DK-2200, Denmark), AQ(Pennsylvania State University, Department of Astronomy; Pennsylvania State University; Pennsylvania State University, Institute for Gravitation and the Cosmos), AR(Yale University, Department of Astronomy), AS(University of Geneva, Astronomical Observatory; -), AT(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AU(University of Pittsburgh, Department of Physics and Astronomy), AV(University of Toronto, Department of Astronomy and Astrophysics; University of Toronto, Dunlap Institute; University of Toronto, Canada), AW(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AX(National Astronomical Observatory of Japan), AY(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AZ(UMass Amherst) %J The Astrophysical Journal %V 948 %D 2023 %8 May 01, 2023 %P L18 %K Galaxy evolution; Galaxy structure; Galaxy formation; 594; 622; 595; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023ApJ...948L..18N %X With just a month of data, JWST is already transforming our view of the universe, revealing and resolving starlight in unprecedented populations of galaxies. Although "HST-dark" galaxies have previously been detected at long wavelengths, these observations generally suffer from a lack of spatial resolution, which limits our ability to characterize their sizes and morphologies. Here we report on a first view of starlight from a subset of the HST-dark population that is bright with JWST/NIRCam (4.4 μm < 24.5 mag) and very faint or even invisible with HST (<1.6 μm). In this Letter we focus on a dramatic and unanticipated population of physically extended galaxies (≳0.″25). These 12 galaxies have photometric redshifts 2 < z < 6, high stellar masses M ⋆ ≳ 1010 M ⊙, and significant dust-attenuated star formation. Surprisingly, the galaxies have elongated projected axis ratios at 4.4 μm, suggesting that the population is disk dominated or prolate and we hence refer to them as ultrared flattened objects. Most of the galaxies appear red at all radii, suggesting significant dust attenuation throughout. With R e (F444W) ~ 1-2 kpc, the galaxies are similar in size to compact massive galaxies at z ~ 2 and the cores of massive galaxies and S0s at z ~ 0. The stellar masses, sizes, and morphologies of the sample suggest that some could be progenitors of lenticular or fast-rotating galaxies in the local universe. The existence of this population suggests that our previous censuses of the universe may have missed massive, dusty edge-on disks, in addition to dust-obscured starbursts. %R 10.3847/2041-8213/acc1e1 %= eprint: arXiv:2208.01630 %@ 0004-637X %0 Journal Article %T JWST Observations of the Enigmatic Y-Dwarf WISE 1828+2650. I. Limits to a Binary Companion %A De Furio, Matthew %A Lew, Ben %A Beichman, Charles %A Roellig, Thomas %A Bryden, Geoffrey %A Ciardi, David %A Meyer, Michael %A Rieke, Marcia %A Greenbaum, Alexandra %A Leisenring, Jarron %A Llop-Sayson, Jorge %A Ygouf, Marie %A Albert, Loic %A Boyer, Martha %A Eisenstein, Daniel %A Hodapp, Klaus %A Horner, Scott %A Johnstone, Doug %A Kelly, Doug %A Misselt, Karl %A Rieke, George %A Stansberry, John %A Young, Erick %+ AA(University of Michigan, Department of Astronomy), AB(NASA Ames Research Center; NASA Ames Research Center), AC(NASA Exoplanet Science Institute, Infrared Processing and Analysis Center (IPAC), Pasadena, CA​, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91125, USA), AD(NASA Ames Research Center), AE(Jet Propulsion Laboratory), AF(NASA Exoplanet Science Institute, Infrared Processing and Analysis Center (IPAC), Pasadena, CA​, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91125, USA), AG(University of Michigan, Department of Astronomy), AH(University of Arizona, Department of Astronomy and Steward Observatory), AI(Infrared Processing and Analysis Center), AJ(University of Arizona, Department of Astronomy and Steward Observatory), AK(California Institute of Technology), AL(Jet Propulsion Laboratory), AM(University of Montreal, Canada), AN(Space Telescope Science Institute, Baltimore, Maryland), AO(Harvard Smithsonian Center for Astrophysics), AP(University of Hawaii, Hilo), AQ(NASA Ames Research Center), AR(Herzberg Institute for Astronomy and Astrophysics; University of Victoria, Department of Physics and Astronomy), AS(University of Arizona, Department of Astronomy and Steward Observatory), AT(University of Arizona, Department of Astronomy and Steward Observatory), AU(University of Arizona, Department of Astronomy and Steward Observatory), AV(Space Telescope Science Institute, Baltimore, Maryland), AW(Universities Space Research Association, 425 3rd St. SW, Suite 950, Washington, DC 20024, USA) %J The Astrophysical Journal %V 948 %D 2023 %8 May 01, 2023 %P 92 %K Brown dwarfs; Y dwarfs; Visual binary stars; Binary stars; James Webb Space Telescope; Theoretical models; Infrared spectroscopy; 185; 1827; 1777; 154; 2291; 2107; 2285; Astrophysics - Solar and Stellar Astrophysics; Astrophysics - Earth and Planetary Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023ApJ...948...92D %X The Y-dwarf WISE 1828+2650 is one of the coldest known brown dwarfs with an effective temperature of ~300 K. Located at a distance of just 10 pc, previous model-based estimates suggest WISE1828+2650 has a mass of ~5-10 M J, making it a valuable laboratory for understanding the formation, evolution, and physical characteristics of gas giant planets. However, previous photometry and spectroscopy have presented a puzzle, with the near impossibility of simultaneously fitting both the short- (0.9-2.0 μm) and long-wavelength (3-5 μm) data. A potential solution to this problem has been the suggestion that WISE 1828+2650 is a binary system whose composite spectrum might provide a better match to the data. Alternatively, new models being developed to fit JWST/NIRSpec, and MIRI spectroscopy might provide new insights. This article describes JWST/NIRCam observations of WISE 1828+2650 in six filters to address the binarity question and to provide new photometry to be used in model fitting. We also report adaptive optics imaging with the Keck I0 m telescope. We find no evidence for multiplicity for a companion beyond 0.5 au with either JWST or Keck. Companion articles will present low- and high-resolution spectra of WISE 1828 obtained with both NIRSpec and MIRI. %R 10.3847/1538-4357/acbf1e %= eprint: arXiv:2302.12723 %@ 0004-637X %0 Electronic Article %T JADES: Insights on the low-mass end of the mass--metallicity--star-formation rate relation at $3 < z < 10$ from deep JWST/NIRSpec spectroscopy %A Curti, Mirko %A Maiolino, Roberto %A Curtis-Lake, Emma %A Chevallard, Jacopo %A Carniani, Stefano %A D'Eugenio, Francesco %A Looser, Tobias J. %A Scholtz, Jan %A Charlot, Stephane %A Cameron, Alex %A Übler, Hannah %A Witstok, Joris %A Boyett, Kristian %A Laseter, Isaac %A Sandles, Lester %A Arribas, Santiago %A Bunker, Andrew %A Giardino, Giovanna %A Maseda, Michael V. %A Rawle, Tim %A Rodríguez Del Pino, Bruno %A Smit, Renske %A Willott, Chris J. %A Eisenstein, Daniel J. %A Hausen, Ryan %A Johnson, Benjamin %A Rieke, Marcia %A Robertson, Brant %A Tacchella, Sandro %A Williams, Christina C. %A Willmer, Christopher %A Baker, William M. %A Bhatawdekar, Rachana %A Egami, Eiichi %A Helton, Jakob M. %A Ji, Zhiyuan %A Kumari, Nimisha %A Perna, Michele %A Shivaei, Irene %A Sun, Fengwu %J arXiv e-prints %D 2023 %8 April 01, 2023 %P arXiv:2304.08516 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230408516C %Z Re-submitted to A&A after revision %X We analyse the gas-phase metallicity properties of a sample of low stellar mass (log M*/M_sun <= 9) galaxies at 3 < z < 10, observed with JWST/NIRSpec as part of the JADES programme in its deep GOODS-S tier. By combining this sample with more massive galaxies at similar redshifts from other programmes, we study the scaling relations between stellar mass, oxygen abundance (O/H), and star-formation rate (SFR) for 146 galaxies, spanning across three orders of magnitude in stellar mass and out to the epoch of early galaxy assembly. We find evidence for a shallower slope at the low-mass-end of the mass-metallicity relation (MZR), with 12 + log(O/H) = (7.72+-0.02) + (0.17+-0.03) log(M* / 10^8 M_sun), in good agreement with the MZR probed by local analogues of high-redshift systems like 'Green Pea' and 'Blueberry' galaxies. The inferred slope is well matched by models including 'momentum-driven' SNe winds, suggesting that feedback mechanisms in dwarf galaxies (and at high-z) might be different from those in place at higher masses. The evolution in the normalisation is observed to be relatively mild compared to previous determinations of the MZR at z~3 (~ 0.1 - 0.2 dex across the explored mass regime). We observe a deviation from the local fundamental metallicity relation (FMR) for our sample at high redshift, especially at z > 6, with galaxies significantly less enriched (with a median offset in log(O/H) of ~ 0.5 dex, significant at ~ 5 sigma) than predicted given their M* and SFR. These observations are consistent with an enhanced stochasticity in the star-formation history, and/or with an increased efficiency in metal removals by outflows, prompting us to reconsider the nature of the relationship between M*, O/H, and SFR in the early Universe. %R 10.48550/arXiv.2304.08516 %= eprint: arXiv:2304.08516 %0 Journal Article %T Reconstructing cosmological initial conditions from late-time structure with convolutional neural networks %A Shallue, Christopher J. %A Eisenstein, Daniel J. %+ AA(Harvard Smithsonian Center for Astrophysics), AB(Harvard Smithsonian Center for Astrophysics) %J Monthly Notices of the Royal Astronomical Society %V 520 %D 2023 %8 April 01, 2023 %P 6256-6267 %K methods: data analysis; early Universe; large-scale structure of Universe; Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - Instrumentation and Methods for Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023MNRAS.520.6256S %X We present a method to reconstruct the initial linear-regime matter density field from the late-time non-linearly evolved density field in which we channel the output of standard first-order reconstruction to a convolutional neural network (CNN). Our method shows dramatic improvement over the reconstruction of either component alone. We show why CNNs are not well-suited for reconstructing the initial density directly from the late-time density: CNNs are local models, but the relationship between initial and late-time density is not local. Our method leverages standard reconstruction as a preprocessing step, which inverts bulk gravitational flows sourced over very large scales, transforming the residual reconstruction problem from long-range to local and making it ideally suited for a CNN. We develop additional techniques to account for redshift distortions, which warp the density fields measured by galaxy surveys. Our method improves the range of scales of high-fidelity reconstruction by a factor of 2 in wavenumber above standard reconstruction, corresponding to a factor of 8 increase in the number of well-reconstructed modes. In addition, our method almost completely eliminates the anisotropy caused by redshift distortions. As galaxy surveys continue to map the Universe in increasingly greater detail, our results demonstrate the opportunity offered by CNNs to untangle the non-linear clustering at intermediate scales more accurately than ever before. %R 10.1093/mnras/stad528 %= eprint: arXiv:2207.12511 %@ 0035-8711 %0 Journal Article %T Overview of the DESI Milky Way Survey %A Cooper, Andrew P. %A Koposov, Sergey E. %A Allende Prieto, Carlos %A Manser, Christopher J. %A Kizhuprakkat, Namitha %A Myers, Adam D. %A Dey, Arjun %A Gänsicke, Boris T. %A Li, Ting S. %A Rockosi, Constance %A Valluri, Monica %A Najita, Joan %A Deason, Alis %A Raichoor, Anand %A Wang, M. -Y. %A Ting, Y. -S. %A Kim, Bokyoung %A Carrillo, Andreia %A Wang, Wenting %A Beraldo e Silva, Leandro %A Han, Jiwon Jesse %A Ding, Jiani %A Sánchez-Conde, Miguel %A Aguilar, Jessica N. %A Ahlen, Steven %A Bailey, Stephen %A Belokurov, Vasily %A Brooks, David %A Cunha, Katia %A Dawson, Kyle %A de la Macorra, Axel %A Doel, Peter %A Eisenstein, Daniel J. %A Fagrelius, Parker %A Fanning, Kevin %A Font-Ribera, Andreu %A Forero-Romero, Jaime E. %A Gaztañaga, Enrique %A Gontcho a Gontcho, Satya %A Guy, Julien %A Honscheid, Klaus %A Kehoe, Robert %A Kisner, Theodore %A Kremin, Anthony %A Landriau, Martin %A Levi, Michael E. %A Martini, Paul %A Meisner, Aaron M. %A Miquel, Ramon %A Moustakas, John %A Nie, Jundan J. D. %A Palanque-Delabrouille, Nathalie %A Percival, Will J. %A Poppett, Claire %A Prada, Francisco %A Rehemtulla, Nabeel %A Schlafly, Edward %A Schlegel, David %A Schubnell, Michael %A Sharples, Ray M. %A Tarlé, Gregory %A Wechsler, Risa H. %A Weinberg, David H. %A Zhou, Zhimin %A Zou, Hu %+ AA(National Tsing-Hua University, Taiwan, Department of Physics; -; National Center for Theoretical Sciences, Taiwan), AB(Royal Observatory Edinburgh; University of Cambridge, Institute of Astronomy), AC(Astrophysical Institute of the Canaries; University of La Laguna, Department of Astrophysics), AD(Imperial College, London), AE(National Tsing-Hua University, Taiwan, Department of Physics; -), AF(University of Wyoming, Department of Physics and Astronomy), AG(National Optical Astronomy Observatory, Arizona), AH(University of Warwick, Department of Physics), AI(University of Toronto, Department of Astronomy and Astrophysics), AJ(University of California, Santa Cruz, Department of Astronomy and Astrophysics; University of California System), AK(University of Michigan, Department of Astronomy), AL(National Optical Astronomy Observatory, Arizona), AM(Institute for Computational Cosmology, Department of Physics, Durham University, South Rd., Durham DH1 3LE, UK), AN(Lawrence Berkeley National Laboratory, California), AO(Carnegie Mellon University, Pennsylvania), AP(ANU, Research School of Astronomy and Astrophysics; Australian National University, Canberra), AQ(Royal Observatory Edinburgh), AR(Institute for Computational Cosmology, Department of Physics, Durham University, South Rd., Durham DH1 3LE, UK), AS(Shanghai Jiaotong University, China), AT(University of Michigan, Department of Astronomy), AU(Harvard Smithsonian Center for Astrophysics), AV(University of California, Santa Cruz, Department of Astronomy and Astrophysics; University of California System), AW(Autonomous University of Madrid, Department of Physics), AX(Lawrence Berkeley National Laboratory, California), AY(Physics Dept., Boston University, 590 Commonwealth Ave., Boston, MA 02215, USA), AZ(Lawrence Berkeley National Laboratory, California), BA(University of Cambridge, Institute of Astronomy; Center for Computational Astrophysics, Flatiron Institute, New York), BB(University College London, Department of Physics and Astronomy), BC(University of Arizona, Department of Astronomy and Steward Observatory), BD(University of Utah, Department of Physics and Astronomy), BE(UNAM, Institute of Physics), BF(University College London, Department of Physics and Astronomy), BG(Harvard Smithsonian Center for Astrophysics), BH(National Optical Astronomy Observatory, Arizona), BI(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), BJ(Institute for High Energy Physics, Barcelona), BK(University of the Andes, Colombia), BL(Institute of Space Studies, Catalona; Institute of Space Studies, Catalona), BM(Lawrence Berkeley National Laboratory, California; -), BN(Lawrence Berkeley National Laboratory, California), BO(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), BP(Department of Physics, Southern Methodist University, 3215 Daniel Ave., Dallas, TX 75275, USA), BQ(Lawrence Berkeley National Laboratory, California), BR(Lawrence Berkeley National Laboratory, California), BS(Lawrence Berkeley National Laboratory, California), BT(Lawrence Berkeley National Laboratory, California), BU(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), BV(National Optical Astronomy Observatory, Arizona), BW(Institute for High Energy Physics, Barcelona; Institucio Catalona de Recerca i Estudis Avancats), BX(Siena College, New York), BY(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100101, People's Republic of China), BZ(Lawrence Berkeley National Laboratory, California; Institut de Recherche sur les Lois Fondamentales de l'Universe), CA(University of Waterloo, Canada; University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada), CB(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory; University of California, Berkeley), CC(Institute of Astrophysics of Andalusia), CD(University of Michigan, Department of Astronomy), CE(Lawrence Livermore National Laboratory, California), CF(Lawrence Berkeley National Laboratory, California), CG(University of Michigan, Department of Physics), CH(Institute for Computational Cosmology, Department of Physics, Durham University, South Rd., Durham DH1 3LE, UK; Centre for Advanced Instrumentation, Department of Physics, Durham University, South Rd., Durham DH1 3LE, UK), CI(University of Michigan, Department of Physics), CJ(Kavli Institute for Particle Astrophysics and Cosmology, California; Stanford University, Department of Physics; Stanford Linear Accelerator Center), CK(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), CL(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100101, People's Republic of China), CM(National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing, 100101, People's Republic of China) %J The Astrophysical Journal %V 947 %D 2023 %8 April 01, 2023 %P 37 %K Milky Way stellar halo; Dwarf galaxies; Milky Way evolution; Milky Way Galaxy; Milky Way dark matter halo; Milky Way dynamics; Surveys; Milky Way Galaxy physics; Spectroscopy; Radial velocity; Stellar abundances; Galaxy formation; 1060; 416; 1052; 1054; 1049; 1051; 1671; 1056; 1558; 1332; 1577; 595; Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023ApJ...947...37C %X We describe the Milky Way Survey (MWS) that will be undertaken with the Dark Energy Spectroscopic Instrument (DESI) on the Mayall 4 m telescope at the Kitt Peak National Observatory. Over the next 5 yr DESI MWS will observe approximately seven million stars at Galactic latitudes |b| > 20°, with an inclusive target selection scheme focused on the thick disk and stellar halo. MWS will also include several high-completeness samples of rare stellar types, including white dwarfs, low-mass stars within 100 pc of the Sun, and horizontal branch stars. We summarize the potential of DESI to advance understanding of the Galactic structure and stellar evolution. We introduce the final definitions of the main MWS target classes and estimate the number of stars in each class that will be observed. We describe our pipelines for deriving radial velocities, atmospheric parameters, and chemical abundances. We use ≃500,000 spectra of unique stellar targets from the DESI Survey Validation program (SV) to demonstrate that our pipelines can measure radial velocities to ≃1 km s-1 and [Fe/H] accurate to ≃0.2 dex for typical stars in our main sample. We find the stellar parameter distributions from ≈100 deg2 of SV observations with ≳90% completeness on our main sample are in good agreement with expectations from mock catalogs and previous surveys. %R 10.3847/1538-4357/acb3c0 %= eprint: arXiv:2208.08514 %@ 0004-637X %0 Journal Article %T The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument %A Guy, J. %A Bailey, S. %A Kremin, A. %A Alam, Shadab %A Alexander, D. M. %A Allende Prieto, C. %A BenZvi, S. %A Bolton, A. S. %A Brooks, D. %A Chaussidon, E. %A Cooper, A. P. %A Dawson, K. %A de la Macorra, A. %A Dey, A. %A Dey, Biprateep %A Dhungana, G. %A Eisenstein, D. J. %A Font-Ribera, A. %A Forero-Romero, J. E. %A Gaztañaga, E. %A Gontcho A Gontcho, S. %A Green, D. %A Honscheid, K. %A Ishak, M. %A Kehoe, R. %A Kirkby, D. %A Kisner, T. %A Koposov, Sergey E. %A Lan, Ting-Wen %A Landriau, M. %A Le Guillou, L. %A Levi, Michael E. %A Magneville, C. %A Manser, Christopher J. %A Martini, P. %A Meisner, Aaron M. %A Miquel, R. %A Moustakas, J. %A Myers, Adam D. %A Newman, Jeffrey A. %A Nie, Jundan %A Palanque-Delabrouille, N. %A Percival, W. J. %A Poppett, C. %A Prada, F. %A Raichoor, A. %A Ravoux, C. %A Ross, A. J. %A Schlafly, E. F. %A Schlegel, D. %A Schubnell, M. %A Sharples, Ray M. %A Tarlé, Gregory %A Weaver, B. A. %A Yéche, Christophe %A Zhou, Rongpu %A Zhou, Zhimin %A Zou, H. %+ AA(Lawrence Berkeley National Laboratory, California), AB(Lawrence Berkeley National Laboratory, California), AC(Lawrence Berkeley National Laboratory, California), AD(Royal Observatory Edinburgh), AE(Durham University, Department of Physics), AF(Instituto de Astrofísica de Canarias, C/ Vía Láctea, s/n, E-38205 La Laguna, Tenerife, Spain Universidad de La Laguna, Dept. de Astrofísica, E-38206 La Laguna, Tenerife, Spain), AG(University of Rochester, Department of Physics and Astronomy), AH(National Optical Astronomy Observatory, Arizona), AI(University College London, Department of Physics and Astronomy), AJ(Institut de Recherche sur les Lois Fondamentales de l'Universe), AK(Institute of Astronomy and Department of Physics, National Tsing Hua University, 101 Kuang-Fu Road Sec. 2, Hsinchu 30013, Taiwan), AL(University of Utah, Department of Physics and Astronomy), AM(UNAM, Institute of Physics), AN(National Optical Astronomy Observatory, Arizona), AO(University of Pittsburgh, Department of Physics and Astronomy), AP(Southern Methodist University, Texas), AQ(Harvard Smithsonian Center for Astrophysics), AR(Institut de Física dAltes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, Spain), AS(University of the Andes, Colombia), AT(Institute of Space Studies, Catalona; Institute of Space Studies, Catalona), AU(Lawrence Berkeley National Laboratory, California), AV(University of California, Irvine, Department of Physics and Astronomy), AW(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Physics; The Ohio State University), AX(University of Texas, Dallas, Department of Physics), AY(Southern Methodist University, Texas), AZ(University of California, Irvine, Department of Physics and Astronomy), BA(Lawrence Berkeley National Laboratory, California), BB(Royal Observatory Edinburgh), BC(Graduate Institute of Astrophysics and Department of Physics, National Taiwan University, No. 1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan), BD(Lawrence Berkeley National Laboratory, California), BE(Laboratoire de Physique Nucleaire et de Hautes Energies), BF(Lawrence Berkeley National Laboratory, California), BG(Institut de Recherche sur les Lois Fondamentales de l'Universe), BH(University of Warwick, Department of Physics), BI(The Ohio State University, Department of Astronomy; The Ohio State University; The Ohio State University, Department of Astronomy), BJ(National Optical Astronomy Observatory, Arizona), BK(Institut de Física dAltes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, Spain; Institució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys, 23, E-08010 Barcelona, Spain), BL(Siena College, New York), BM(University of Wyoming, Department of Physics and Astronomy), BN(University of Pittsburgh, Department of Physics and Astronomy), BO(CAS, National Astronomical Observatories), BP(Lawrence Berkeley National Laboratory, California; Institut de Recherche sur les Lois Fondamentales de l'Universe), BQ(University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada; University of Waterloo, Canada), BR(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory; University of California, Berkeley), BS(Institute of Astrophysics of Andalusia), BT(Lawrence Berkeley National Laboratory, California), BU(Institut de Recherche sur les Lois Fondamentales de l'Universe), BV(The Ohio State University, Department of Astronomy; The Ohio State University; The Ohio State University, Department of Astronomy), BW(Space Telescope Science Institute, Baltimore, Maryland), BX(Lawrence Berkeley National Laboratory, California), BY(University of Michigan, Department of Physics; University of Michigan), BZ(Durham University, Department of Physics; Durham University, Department of Physics), CA(University of Michigan), CB(National Optical Astronomy Observatory, Arizona), CC(Institut de Recherche sur les Lois Fondamentales de l'Universe), CD(Lawrence Berkeley National Laboratory, California), CE(CAS, National Astronomical Observatories), CF(CAS, National Astronomical Observatories) %J The Astronomical Journal %V 165 %D 2023 %8 April 01, 2023 %P 144 %K Galaxy spectroscopy; High-redshift galaxies; Redshift surveys; 2171; 734; 1378; Astrophysics - Instrumentation and Methods for Astrophysics; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023AJ....165..144G %X We describe the spectroscopic data processing pipeline of the Dark Energy Spectroscopic Instrument (DESI), which is conducting a redshift survey of about 40 million galaxies and quasars using a purpose-built instrument on the 4 m Mayall Telescope at Kitt Peak National Observatory. The main goal of DESI is to measure with unprecedented precision the expansion history of the universe with the baryon acoustic oscillation technique and the growth rate of structure with redshift space distortions. Ten spectrographs with three cameras each disperse the light from 5000 fibers onto 30 CCDs, covering the near-UV to near-infrared (3600-9800 Å) with a spectral resolution ranging from 2000 to 5000. The DESI data pipeline generates wavelength- and flux-calibrated spectra of all the targets, along with spectroscopic classifications and redshift measurements. Fully processed data from each night are typically available to the DESI collaboration the following morning. We give details about the pipeline's algorithms, and provide performance results on the stability of the optics, the quality of the sky background subtraction, and the precision and accuracy of the instrumental calibration. This pipeline has been used to process the DESI Survey Validation data set, and has exceeded the project's requirements for redshift performance, with high efficiency and a purity greater than 99% for all target classes. %R 10.3847/1538-3881/acb212 %= eprint: arXiv:2209.14482 %@ 0004-6256 %0 Journal Article %T Target Selection and Validation of DESI Emission Line Galaxies %A Raichoor, A. %A Moustakas, J. %A Newman, Jeffrey A. %A Karim, T. %A Ahlen, S. %A Alam, Shadab %A Bailey, S. %A Brooks, D. %A Dawson, K. %A de la Macorra, A. %A de Mattia, A. %A Dey, A. %A Dey, Biprateep %A Dhungana, G. %A Eftekharzadeh, S. %A Eisenstein, D. J. %A Fanning, K. %A Font-Ribera, A. %A García-Bellido, J. %A Gaztañaga, E. %A A Gontcho, S. Gontcho %A Guy, J. %A Honscheid, K. %A Ishak, M. %A Kehoe, R. %A Kisner, T. %A Kremin, Anthony %A Lan, Ting-Wen %A Landriau, M. %A Le Guillou, L. %A Levi, Michael E. %A Magneville, C. %A Manera, M. %A Martini, P. %A Meisner, Aaron M. %A Myers, Adam D. %A Nie, Jundan %A Palanque-Delabrouille, N. %A Percival, W. J. %A Poppett, C. %A Prada, F. %A Ross, A. J. %A Ruhlmann-Kleider, V. %A Sabiu, C. G. %A Schlafly, E. F. %A Schlegel, D. %A Tarlé, Gregory %A Weaver, B. A. %A Yèche, Christophe %A Zhou, Rongpu %A Zhou, Zhimin %A Zou, H. %+ AA(Lawrence Berkeley National Laboratory, California), AB(Siena College, New York), AC(University of Pittsburgh, Department of Physics and Astronomy), AD(Harvard Smithsonian Center for Astrophysics), AE(Physics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, USA), AF(Royal Observatory Edinburgh), AG(Lawrence Berkeley National Laboratory, California), AH(University College London, Department of Physics and Astronomy), AI(University of Utah, Department of Physics and Astronomy), AJ(UNAM, Institute of Physics), AK(Institut de Recherche sur les Lois Fondamentales de l'Universe), AL(National Optical Astronomy Observatory, Arizona), AM(University of Pittsburgh, Department of Physics and Astronomy), AN(Southern Methodist University, Texas), AO(Universities Space Research Association, NASA Ames Research Centre, USA), AP(Harvard Smithsonian Center for Astrophysics), AQ(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), AR(Institute for High Energy Physics, Barcelona), AS(Autonomous University of Madrid, Department of Physics), AT(Institute of Space Studies, Catalona; Institute of Space Studies, Catalona), AU(Lawrence Berkeley National Laboratory, California), AV(Lawrence Berkeley National Laboratory, California), AW(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), AX(University of Texas, Dallas, Department of Physics), AY(Southern Methodist University, Texas), AZ(Lawrence Berkeley National Laboratory, California), BA(Lawrence Berkeley National Laboratory, California), BB(Graduate Institute of Astrophysics and Department of Physics, National Taiwan University, No. 1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan), BC(Lawrence Berkeley National Laboratory, California), BD(Laboratoire de Physique Nucleaire et de Hautes Energies), BE(Lawrence Berkeley National Laboratory, California), BF(Institut de Recherche sur les Lois Fondamentales de l'Universe), BG(Institute for High Energy Physics, Barcelona; -), BH(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), BI(National Optical Astronomy Observatory, Arizona), BJ(University of Wyoming, Department of Physics and Astronomy), BK(CAS, National Astronomical Observatories), BL(Lawrence Berkeley National Laboratory, California; Institut de Recherche sur les Lois Fondamentales de l'Universe), BM(University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada; University of Waterloo, Canada), BN(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory; University of California, Berkeley), BO(Institute of Astrophysics of Andalusia), BP(The Ohio State University, Department of Astronomy), BQ(Institut de Recherche sur les Lois Fondamentales de l'Universe), BR(Natural Science Research Institute, University of Seoul, 163 Seoulsiripdae-ro, Dongdaemun-gu, Seoul, Republic of Korea), BS(Space Telescope Science Institute, Baltimore, Maryland), BT(Lawrence Berkeley National Laboratory, California), BU(University of Michigan), BV(National Optical Astronomy Observatory, Arizona), BW(Institut de Recherche sur les Lois Fondamentales de l'Universe), BX(Lawrence Berkeley National Laboratory, California), BY(CAS, National Astronomical Observatories), BZ(CAS, National Astronomical Observatories) %J The Astronomical Journal %V 165 %D 2023 %8 March 01, 2023 %P 126 %K Emission line galaxies; Surveys; Large-scale structure of the universe; 459; 1671; 902; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023AJ....165..126R %X The Dark Energy Spectroscopic Instrument (DESI) will precisely constrain cosmic expansion and the growth of structure by collecting ~40 million extragalactic redshifts across ~80% of cosmic history and one-third of the sky. The Emission Line galaxy (ELG) sample, which will comprise about one-third of all DESI tracers, will be used to probe the universe over the 0.6 < z < 1.6 range, including the 1.1 < z < 1.6 range, which is expected to provide the tightest constraints. We present the target selection for the DESI Survey Validation (SV) and Main Survey ELG samples, which relies on the imaging of the Legacy Surveys. The Main ELG selection consists of a g-band magnitude cut and a (g - r) versus (r - z) color box, while the SV selection explores extensions of the Main selection boundaries. The Main ELG sample is composed of two disjoint subsamples, which have target densities of about 1940 deg-2 and 460 deg-2, respectively. We first characterize their photometric properties and density variations across the footprint. We then analyze the DESI spectroscopic data that have been obtained from 2020 December to 2021 December in the SV and Main Survey. We establish a preliminary criterion for selecting reliable redshifts, based on the [O II] flux measurement, and assess its performance. Using this criterion, we are able to present the spectroscopic efficiency of the Main ELG selection, along with its redshift distribution. We thus demonstrate that the Main selection 1940 deg-2 subsample alone should provide 400 deg-2 and 460 deg-2 reliable redshifts in the 0.6 < z < 1.1 and the 1.1 < z < 1.6 ranges, respectively. %R 10.3847/1538-3881/acb213 %= eprint: arXiv:2208.08513 %@ 0004-6256 %0 Electronic Article %T Discovery of a quiescent galaxy at z=7.3 %A Looser, Tobias J. %A D'Eugenio, Francesco %A Maiolino, Roberto %A Witstok, Joris %A Sandles, Lester %A Curtis-Lake, Emma %A Chevallard, Jacopo %A Tacchella, Sandro %A Johnson, Benjamin D. %A Baker, William M. %A Suess, Katherine A. %A Carniani, Stefano %A Ferruit, Pierre %A Arribas, Santiago %A Bonaventura, Nina %A Bunker, Andrew J. %A Cameron, Alex J. %A Charlot, Stephane %A Curti, Mirko %A de Graaff, Anna %A Maseda, Michael V. %A Rawle, Tim %A Rix, Hans-Walter %A Rodriguez Del Pino, Bruno %A Smit, Renske %A Übler, Hannah %A Willott, Chris %A Alberts, Stacey %A Egami, Eiichi %A Eisenstein, Daniel J. %A Endsley, Ryan %A Hausen, Ryan %A Rieke, Marcia %A Robertson, Brant %A Shivaei, Irene %A Williams, Christina C. %A Boyett, Kristan %A Chen, Zuyi %A Ji, Zhiyuan %A Jones, Gareth J. %A Kumari, Nimisha %A Nelson, Erica %A Perna, Michele %A Saxena, Aayush %A Scholtz, Jan %J arXiv e-prints %D 2023 %8 February 01, 2023 %P arXiv:2302.14155 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230214155L %X Local galaxies are known to broadly follow a bimodal distribution: actively star forming and quiescent systems (i.e. galaxies with no or negligible star formation activity at the epoch of observation). Why, when and how such bimodality was established, and whether it has been associated with different processes at different cosmic epochs, is still a key open question in extragalactic astrophysics. Directly observing early quiescent galaxies in the primordial Universe is therefore of utmost importance to constraining models of galaxy formation and transformation. Early quiescent galaxies have been identified out to redshift $z < 5$, and these are all found to be massive ($M_{*}>10^{10}~M_{\odot}$). Here we report the discovery of a quiescent galaxy at z$=$7.3, when the Universe was only 700 Myr old - about 5% of its current age. The JWST/NIRSpec spectrum of this galaxy from our JADES programme exhibits a complete absence of nebular emission lines, while the Balmer break and Ly$\alpha$ drop are unambiguously detected. We infer that this galaxy experienced a short and intense burst of star formation followed by rapid quenching, about 10-20 Myr before the epoch of observation. Particularly interesting is that the mass of this quiescent galaxy is only $\sim$4-6$\times 10^8~M_{\odot}$. This mass range is sensitive to various feedback mechanisms that can result in temporary or permanent quiescence. Therefore this galaxy represents a unique opportunity to learn more about galaxy formation and transformation in the early Universe. %R 10.48550/arXiv.2302.14155 %= eprint: arXiv:2302.14155 %0 Electronic Article %T The JWST Advanced Deep Extragalactic Survey: Discovery of an Extreme Galaxy Overdensity at $z = 5.4$ with JWST/NIRCam in GOODS-S %A Helton, Jakob M. %A Sun, Fengwu %A Woodrum, Charity %A Hainline, Kevin N. %A Willmer, Christopher N. A. %A Rieke, George H. %A Rieke, Marcia J. %A Tacchella, Sandro %A Robertson, Brant %A Johnson, Benjamin D. %A Alberts, Stacey %A Eisenstein, Daniel J. %A Hausen, Ryan %A Bonaventura, Nina R. %A Bunker, Andrew %A Charlot, Stephane %A Curti, Mirko %A Curtis-Lake, Emma %A Looser, Tobias J. %A Maiolino, Roberto %A Willott, Chris %A Witstok, Joris %A Boyett, Kristan %A Chen, Zuyi %A Egami, Eiichi %A Endsley, Ryan %A Hviding, Raphael E. %A Jaffe, Daniel T. %A Ji, Zhiyuan %A Lyu, Jianwei %A Sandles, Lester %J arXiv e-prints %D 2023 %8 February 01, 2023 %P arXiv:2302.10217 %K Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023arXiv230210217H %Z Resubmitted to ApJ based on reviewer report; main text has 15 pages, 6 figures and 1 table; appendix has 1 page, 2 figure sets, and 2 tables %X We report the discovery of an extreme galaxy overdensity at $z = 5.4$ in the GOODS-S field using JWST/NIRCam imaging from JADES and JEMS alongside JWST/NIRCam wide field slitless spectroscopy from FRESCO. We identified potential members of the overdensity using HST+JWST photometry spanning $\lambda = 0.4-5.0\ \mu\mathrm{m}$. These data provide accurate and well-constrained photometric redshifts down to $m \approx 29-30\,\mathrm{mag}$. We subsequently confirmed $N = 81$ galaxies at $5.2 < z < 5.5$ using JWST slitless spectroscopy over $\lambda = 3.9-5.0\ \mu\mathrm{m}$ through a targeted line search for $\mathrm{H} \alpha$ around the best-fit photometric redshift. We verified that $N = 42$ of these galaxies reside in the field while $N = 39$ galaxies reside in a density around $\sim 10$ times that of a random volume. Stellar populations for these galaxies were inferred from the photometry and used to construct the star-forming main sequence, where protocluster members appeared more massive and exhibited earlier star formation (and thus older stellar populations) when compared to their field galaxy counterparts. We estimate the total halo mass of this large-scale structure to be $12.6 \lesssim \mathrm{log}_{10} \left( M_{\mathrm{halo}}/M_{\odot} \right) \lesssim 12.8$ using an empirical stellar mass to halo mass relation, which is likely an underestimate as a result of incompleteness. Our discovery demonstrates the power of JWST at constraining dark matter halo assembly and galaxy formation at very early cosmic times. %R 10.48550/arXiv.2302.10217 %= eprint: arXiv:2302.10217 %0 Journal Article %T Performance of NIRCam on JWST in Flight %A Rieke, Marcia J. %A Kelly, Douglas M. %A Misselt, Karl %A Stansberry, John %A Boyer, Martha %A Beatty, Thomas %A Egami, Eiichi %A Florian, Michael %A Greene, Thomas P. %A Hainline, Kevin %A Leisenring, Jarron %A Roellig, Thomas %A Schlawin, Everett %A Sun, Fengwu %A Tinnin, Lee %A Williams, Christina C. %A Willmer, Christopher N. A. %A Wilson, Debra %A Clark, Charles R. %A Rohrbach, Scott %A Brooks, Brian %A Canipe, Alicia %A Correnti, Matteo %A DiFelice, Audrey %A Gennaro, Mario %A Girard, Julien H. %A Hartig, George %A Hilbert, Bryan %A Koekemoer, Anton M. %A Nikolov, Nikolay K. %A Pirzkal, Norbert %A Rest, Armin %A Robberto, Massimo %A Sunnquist, Ben %A Telfer, Randal %A Wu, Chi Rai %A Ferry, Malcolm %A Lewis, Dan %A Baum, Stefi %A Beichman, Charles %A Doyon, René %A Dressler, Alan %A Eisenstein, Daniel J. %A Ferrarese, Laura %A Hodapp, Klaus %A Horner, Scott %A Jaffe, Daniel T. %A Johnstone, Doug %A Krist, John %A Martin, Peter %A McCarthy, Donald W. %A Meyer, Michael %A Rieke, George H. %A Trauger, John %A Young, Erick T. %+ AA(University of Arizona, Department of Astronomy and Steward Observatory), AB(University of Arizona, Department of Astronomy and Steward Observatory), AC(University of Arizona, Department of Astronomy and Steward Observatory), AD(Space Telescope Science Institute, Baltimore, Maryland), AE(Space Telescope Science Institute, Baltimore, Maryland), AF(University of Wisconsin, Madison, Department of Astronomy), AG(University of Arizona, Department of Astronomy and Steward Observatory), AH(University of Arizona, Department of Astronomy and Steward Observatory), AI(NASA Ames Research Center), AJ(University of Arizona, Department of Astronomy and Steward Observatory), AK(University of Arizona, Department of Astronomy and Steward Observatory), AL(NASA Ames Research Center), AM(University of Arizona, Department of Astronomy and Steward Observatory), AN(University of Arizona, Department of Astronomy and Steward Observatory), AO(University of Arizona, Department of Astronomy and Steward Observatory), AP(National Optical-Infrared Research Laboratory, 950 N Cherry Avenue, Tucson, AZ 85719, USA), AQ(University of Arizona, Department of Astronomy and Steward Observatory), AR(University of Arizona, Department of Astronomy and Steward Observatory), AS(NASA Goddard Space Flight Center, Maryland), AT(NASA Goddard Space Flight Center, Maryland), AU(Space Telescope Science Institute, Baltimore, Maryland), AV(Space Telescope Science Institute, Baltimore, Maryland), AW(Astronomical Observatory of Rome; ASI Science Data Center), AX(Space Telescope Science Institute, Baltimore, Maryland), AY(Space Telescope Science Institute, Baltimore, Maryland), AZ(Space Telescope Science Institute, Baltimore, Maryland), BA(Space Telescope Science Institute, Baltimore, Maryland), BB(Space Telescope Science Institute, Baltimore, Maryland), BC(Space Telescope Science Institute, Baltimore, Maryland), BD(Space Telescope Science Institute, Baltimore, Maryland), BE(Space Telescope Science Institute, Baltimore, Maryland), BF(Space Telescope Science Institute, Baltimore, Maryland; Johns Hopkins University, Department of Physics and Astronomy), BG(Space Telescope Science Institute, Baltimore, Maryland; Johns Hopkins University, Maryland), BH(Space Telescope Science Institute, Baltimore, Maryland), BI(Space Telescope Science Institute, Baltimore, Maryland), BJ(Space Telescope Science Institute, Baltimore, Maryland), BK(Lockheed Martin, Palo Alto), BL(Lockheed Martin, Palo Alto), BM(Faculty of Science, 230 Machray Hall, 186 Dysart Road, University of Manitoba, Winnipeg, MB R3T 2N2, Canada), BN(Jet Propulsion Laboratory), BO(University of Montreal, Department of Physics), BP(Carnegie Institution of Washington, Observatories, California), BQ(Harvard Smithsonian Center for Astrophysics), BR(Herzberg Institute for Astronomy and Astrophysics), BS(University of Hawaii, Manoa, Institute for Astronomy), BT(881 Spinosa Drive, Sunnyvale, CA 94087, USA), BU(University of Texas, Austin, Department of Astronomy), BV(Herzberg Institute for Astronomy and Astrophysics; University of Victoria, Department of Physics and Astronomy), BW(Jet Propulsion Laboratory), BX(Canadian Institute for Theoretical Astrophysics), BY(University of Arizona, Department of Astronomy and Steward Observatory), BZ(University of Michigan, Department of Astronomy), CA(University of Arizona, Department of Astronomy and Steward Observatory), CB(Jet Propulsion Laboratory), CC(USRA, Mountain View, CA, USA) %J Publications of the Astronomical Society of the Pacific %V 135 %D 2023 %8 February 01, 2023 %P 028001 %K Infrared telescopes; Space observatories; Space telescopes; 794; 1543; 1547; Astrophysics - Instrumentation and Methods for Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023PASP..135b8001R %X The Near Infrared Camera for the James Webb Space Telescope (JWST) is delivering the imagery that astronomers have hoped for ever since JWST was proposed back in the 1990s. In the Commissioning Period that extended from right after launch to early 2022 July, NIRCam has been subjected to a number of performance tests and operational checks. The camera is exceeding prelaunch expectations in virtually all areas, with very few surprises discovered in flight. NIRCam also delivered the imagery needed by the Wavefront Sensing Team for use in aligning the telescope mirror segments. %R 10.1088/1538-3873/acac53 %= eprint: arXiv:2212.12069 %@ 0004-6280 %0 Journal Article %T Target Selection and Validation of DESI Quasars %A Chaussidon, Edmond %A Yèche, Christophe %A Palanque-Delabrouille, Nathalie %A Alexander, David M. %A Yang, Jinyi %A Ahlen, Steven %A Bailey, Stephen %A Brooks, David %A Cai, Zheng %A Chabanier, Solène %A Davis, Tamara M. %A Dawson, Kyle %A de laMacorra, Axel %A Dey, Arjun %A Dey, Biprateep %A Eftekharzadeh, Sarah %A Eisenstein, Daniel J. %A Fanning, Kevin %A Font-Ribera, Andreu %A Gaztañaga, Enrique %A A Gontcho, Satya Gontcho %A Gonzalez-Morales, Alma X. %A Guy, Julien %A Herrera-Alcantar, Hiram K. %A Honscheid, Klaus %A Ishak, Mustapha %A Jiang, Linhua %A Juneau, Stephanie %A Kehoe, Robert %A Kisner, Theodore %A Kovács, Andras %A Kremin, Anthony %A Lan, Ting-Wen %A Landriau, Martin %A Le Guillou, Laurent %A Levi, Michael E. %A Magneville, Christophe %A Martini, Paul %A Meisner, Aaron M. %A Moustakas, John %A Muñoz-Gutiérrez, Andrea %A Myers, Adam D. %A Newman, Jeffrey A. %A Nie, Jundan %A Percival, Will J. %A Poppett, Claire %A Prada, Francisco %A Raichoor, Anand %A Ravoux, Corentin %A Ross, Ashley J. %A Schlafly, Edward %A Schlegel, David %A Tan, Ting %A Tarlé, Gregory %A Zhou, Rongpu %A Zhou, Zhimin %A Zou, Hu %+ AA(Institut de Recherche sur les Lois Fondamentales de l'Universe), AB(Institut de Recherche sur les Lois Fondamentales de l'Universe), AC(Institut de Recherche sur les Lois Fondamentales de l'Universe; Lawrence Berkeley National Laboratory, California), AD(Durham University, Department of Physics; Durham University, Department of Physics), AE(University of Arizona, Department of Astronomy and Steward Observatory), AF(Boston University, Department of Physics), AG(Lawrence Berkeley National Laboratory, California), AH(University College London, Department of Physics and Astronomy), AI(Tsinghua University, China), AJ(Lawrence Berkeley National Laboratory, California), AK(University of Queensland, School of Mathematics and Physics), AL(University of Utah, Department of Physics and Astronomy), AM(UNAM, Institute of Physics), AN(National Optical Astronomy Observatory, Arizona), AO(University of Pittsburgh, Department of Physics and Astronomy), AP(NASA Ames Research Center), AQ(Harvard Smithsonian Center for Astrophysics), AR(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), AS(Institute for High Energy Physics, Barcelona), AT(Institute of Space Studies, Catalona; Institute of Space Studies, Catalona), AU(Lawrence Berkeley National Laboratory, California), AV(Consejo Nacional de Ciencia y Tecnología, Avenida Insurgentes Sur 1582. Colonia Crédito Constructor, Del. Benito Juárez C.P. 03940, México D.F. México; Departamento de Física, Universidad de Guanajuato-DCI, C.P. 37150, Leon, Guanajuato, México), AW(Lawrence Berkeley National Laboratory, California), AX(Departamento de Física, Universidad de Guanajuato-DCI, C.P. 37150, Leon, Guanajuato, México), AY(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Physics), AZ(University of Texas, Dallas, Department of Physics), BA(Kavli Institute for Astronomy and Astrophysics), BB(National Optical Astronomy Observatory, Arizona), BC(Southern Methodist University, Texas), BD(Lawrence Berkeley National Laboratory, California), BE(University of La Laguna, Department of Astrophysics; Astrophysical Institute of the Canaries), BF(Lawrence Berkeley National Laboratory, California), BG(Graduate Institute of Astrophysics and Department of Physics, National Taiwan University, No. 1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan), BH(Lawrence Berkeley National Laboratory, California), BI(Laboratoire de Physique Nucleaire et de Hautes Energies), BJ(Lawrence Berkeley National Laboratory, California), BK(Institut de Recherche sur les Lois Fondamentales de l'Universe), BL(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), BM(National Optical Astronomy Observatory, Arizona), BN(Siena College, New York), BO(UNAM, Institute of Physics), BP(University of Wyoming, Department of Physics and Astronomy), BQ(University of Pittsburgh, Department of Physics and Astronomy), BR(CAS, National Astronomical Observatories), BS(University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada; University of Waterloo, Canada), BT(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory; University of California, Berkeley), BU(Institute of Astrophysics of Andalusia), BV(Lawrence Berkeley National Laboratory, California), BW(Institut de Recherche sur les Lois Fondamentales de l'Universe), BX(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), BY(Lawrence Livermore National Laboratory, California), BZ(Lawrence Berkeley National Laboratory, California), CA(Laboratoire de Physique Nucleaire et de Hautes Energies), CB(University of Michigan), CC(Lawrence Berkeley National Laboratory, California), CD(CAS, National Astronomical Observatories), CE(CAS, National Astronomical Observatories) %J The Astrophysical Journal %V 944 %D 2023 %8 February 01, 2023 %P 107 %K Quasars; Redshift surveys; Sky surveys; 1319; 1378; 1464; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023ApJ...944..107C %X The Dark Energy Spectroscopic Instrument (DESI) survey will measure large-scale structures using quasars as direct tracers of dark matter in the redshift range 0.9 < z < 2.1 and using Lyα forests in quasar spectra at z > 2.1. We present several methods to select candidate quasars for DESI, using input photometric imaging in three optical bands (g, r, z) from the DESI Legacy Imaging Surveys and two infrared bands (W1, W2) from the Wide-field Infrared Survey Explorer. These methods were extensively tested during the Survey Validation of DESI. In this paper, we report on the results obtained with the different methods and present the selection we optimized for the DESI main survey. The final quasar target selection is based on a random forest algorithm and selects quasars in the magnitude range of 16.5 < r < 23. Visual selection of ultra-deep observations indicates that the main selection consists of 71% quasars, 16% galaxies, 6% stars, and 7% inconclusive spectra. Using the spectra based on this selection, we build an automated quasar catalog that achieves a fraction of true QSOs higher than 99% for a nominal effective exposure time of ~1000 s. With a 310 deg-2 target density, the main selection allows DESI to select more than 200 deg-2 quasars (including 60 deg-2 quasars with z > 2.1), exceeding the project requirements by 20%. The redshift distribution of the selected quasars is in excellent agreement with quasar luminosity function predictions. %R 10.3847/1538-4357/acb3c2 %= eprint: arXiv:2208.08511 %@ 0004-637X %0 Journal Article %T Target Selection and Validation of DESI Luminous Red Galaxies %A Zhou, Rongpu %A Dey, Biprateep %A Newman, Jeffrey A. %A Eisenstein, Daniel J. %A Dawson, K. %A Bailey, S. %A Berti, A. %A Guy, J. %A Lan, Ting-Wen %A Zou, H. %A Aguilar, J. %A Ahlen, S. %A Alam, Shadab %A Brooks, D. %A de la Macorra, A. %A Dey, A. %A Dhungana, G. %A Fanning, K. %A Font-Ribera, A. %A Gontcho, S. Gontcho A. %A Honscheid, K. %A Ishak, Mustapha %A Kisner, T. %A Kovács, A. %A Kremin, A. %A Landriau, M. %A Levi, Michael E. %A Magneville, C. %A Manera, Marc %A Martini, P. %A Meisner, Aaron M. %A Miquel, R. %A Moustakas, J. %A Myers, Adam D. %A Nie, Jundan %A Palanque-Delabrouille, N. %A Percival, W. J. %A Poppett, C. %A Prada, F. %A Raichoor, A. %A Ross, A. J. %A Schlafly, E. %A Schlegel, D. %A Schubnell, M. %A Tarlé, Gregory %A Weaver, B. A. %A Wechsler, R. H. %A Yéche, Christophe %A Zhou, Zhimin %+ AA(Lawrence Berkeley National Laboratory, California), AB(University of Pittsburgh, Department of Physics and Astronomy), AC(University of Pittsburgh, Department of Physics and Astronomy), AD(Harvard Smithsonian Center for Astrophysics), AE(University of Utah, Department of Physics and Astronomy), AF(Lawrence Berkeley National Laboratory, California), AG(University of Utah, Department of Physics and Astronomy), AH(Lawrence Berkeley National Laboratory, California), AI(Graduate Institute of Astrophysics and Department of Physics, National Taiwan University, No. 1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan), AJ(CAS, National Astronomical Observatories), AK(Lawrence Berkeley National Laboratory, California), AL(Physics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, USA), AM(Royal Observatory Edinburgh), AN(University College London, Department of Physics and Astronomy), AO(UNAM, Institute of Physics), AP(National Optical Astronomy Observatory, Arizona), AQ(Southern Methodist University, Texas), AR(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), AS(Institute for High Energy Physics, Barcelona), AT(Lawrence Berkeley National Laboratory, California; University of Rochester, Department of Physics and Astronomy), AU(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), AV(University of Texas, Dallas, Department of Physics), AW(Lawrence Berkeley National Laboratory, California), AX(University of La Laguna, Department of Astrophysics; Astrophysical Institute of the Canaries), AY(Lawrence Berkeley National Laboratory, California), AZ(Lawrence Berkeley National Laboratory, California), BA(Lawrence Berkeley National Laboratory, California), BB(Institut de Recherche sur les Lois Fondamentales de l'Universe), BC(Institute for High Energy Physics, Barcelona; Autonomous University of Barcelona, Department of Physics), BD(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), BE(National Optical Astronomy Observatory, Arizona), BF(Institute for High Energy Physics, Barcelona; Institucio Catalona de Recerca i Estudis Avancats), BG(Siena College, New York), BH(University of Wyoming, Department of Physics and Astronomy), BI(CAS, National Astronomical Observatories), BJ(Lawrence Berkeley National Laboratory, California; Institut de Recherche sur les Lois Fondamentales de l'Universe), BK(University of Waterloo, Canada; University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada), BL(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory; University of California, Berkeley), BM(Institute of Astrophysics of Andalusia), BN(Lawrence Berkeley National Laboratory, California), BO(The Ohio State University, Department of Astronomy), BP(Space Telescope Science Institute, Baltimore, Maryland), BQ(Lawrence Berkeley National Laboratory, California), BR(University of Michigan, Department of Physics; University of Michigan), BS(University of Michigan), BT(National Optical Astronomy Observatory, Arizona), BU(Kavli Institute for Particle Astrophysics and Cosmology, California; Stanford University, Department of Physics; Stanford Linear Accelerator Center), BV(Institut de Recherche sur les Lois Fondamentales de l'Universe), BW(CAS, National Astronomical Observatories) %J The Astronomical Journal %V 165 %D 2023 %8 February 01, 2023 %P 58 %K Cosmology; Redshift surveys; 343; 1378; Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - Astrophysics of Galaxies %U https://ui.adsabs.harvard.edu/abs/2023AJ....165...58Z %X The Dark Energy Spectroscopic Instrument (DESI) is carrying out a five-year survey that aims to measure the redshifts of tens of millions of galaxies and quasars, including 8 million luminous red galaxies (LRGs) in the redshift range 0.4 < z ≲ 1.0. Here we present the selection of the DESI LRG sample and assess its spectroscopic performance using data from Survey Validation (SV) and the first two months of the Main Survey. The DESI LRG sample, selected using g, r, z, and W1 photometry from the DESI Legacy Imaging Surveys, is highly robust against imaging systematics. The sample has a target density of 605 deg-2 and a comoving number density of 5 × 10-4 h 3 Mpc-3 in 0.4 < z < 0.8; this is a significantly higher density than previous LRG surveys (such as SDSS, BOSS, and eBOSS) while also extending to z ~ 1. After applying a bright star veto mask developed for the sample, 98.9% of the observed LRG targets yield confident redshifts (with a catastrophic failure rate of 0.2% in the confident redshifts), and only 0.5% of the LRG targets are stellar contamination. The LRG redshift efficiency varies with source brightness and effective exposure time, and we present a simple model that accurately characterizes this dependence. In the appendices, we describe the extended LRG samples observed during SV. %R 10.3847/1538-3881/aca5fb %= eprint: arXiv:2208.08515 %@ 0004-6256 %0 Journal Article %T Morpheus Reveals Distant Disk Galaxy Morphologies with JWST: The First AI/ML Analysis of JWST Images %A Robertson, Brant E. %A Tacchella, Sandro %A Johnson, Benjamin D. %A Hausen, Ryan %A Alabi, Adebusola B. %A Boyett, Kristan %A Bunker, Andrew J. %A Carniani, Stefano %A Egami, Eiichi %A Eisenstein, Daniel J. %A Hainline, Kevin N. %A Helton, Jakob M. %A Ji, Zhiyuan %A Kumari, Nimisha %A Lyu, Jianwei %A Maiolino, Roberto %A Nelson, Erica J. %A Rieke, Marcia J. %A Shivaei, Irene %A Sun, Fengwu %A Übler, Hannah %A Williams, Christina C. %A Willmer, Christopher N. A. %A Witstok, Joris %+ AA(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AB(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AC(Harvard Smithsonian Center for Astrophysics), AD(Johns Hopkins University, Department of Physics and Astronomy), AE(University of California, Santa Cruz, Department of Astronomy and Astrophysics), AF(University of Melbourne, Department of Physics; Centre of Excellence for All Sky Astrophysics), AG(University of Oxford, Department of Physics), AH(Scuola Normale Superiore, Pisa, Italy), AI(University of Arizona, Department of Astronomy and Steward Observatory), AJ(Harvard Smithsonian Center for Astrophysics), AK(University of Arizona, Department of Astronomy and Steward Observatory), AL(University of Arizona, Department of Astronomy and Steward Observatory), AM(UMass Amherst), AN(Space Telescope Science Institute, ESA Office, Baltimore, Maryland), AO(University of Arizona, Department of Astronomy and Steward Observatory), AP(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AQ(University of Colorado, Boulder, Department of Astrophysical and Planetary Sciences), AR(University of Arizona, Department of Astronomy and Steward Observatory), AS(University of Arizona, Department of Astronomy and Steward Observatory), AT(University of Arizona, Department of Astronomy and Steward Observatory), AU(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy), AV(University of Arizona, Department of Astronomy and Steward Observatory; National Optical Astronomy Observatory, Arizona), AW(University of Arizona, Department of Astronomy and Steward Observatory), AX(Kavli Institute for Cosmology, UK; University of Cambridge, Institute of Astronomy) %J The Astrophysical Journal %V 942 %D 2023 %8 January 01, 2023 %P L42 %K Galaxy classification systems; Neural networks; Disk galaxies; Galaxies; James Webb Space Telescope; 582; 1933; 391; 573; 2291; Astrophysics - Astrophysics of Galaxies; Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - Instrumentation and Methods for Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023ApJ...942L..42R %X The dramatic first images with JWST demonstrated its power to provide unprecedented spatial detail for galaxies in the high-redshift universe. Here, we leverage the resolution and depth of the JWST Cosmic Evolution Early Release Science Survey data in the Extended Groth Strip to perform pixel-level morphological classifications of galaxies in JWST F150W imaging using the Morpheus deep-learning framework for astronomical image analysis. By cross-referencing with existing photometric redshift catalogs from the Hubble Space Telescope (HST) CANDELS survey, we show that JWST images indicate the emergence of disk morphologies before z ~ 2 and with candidates appearing as early as z ~ 5. By modeling the light profile of each object and accounting for the JWST point-spread function, we find the high-redshift disk candidates have exponential surface brightness profiles with an average Sérsic index = 1.04 and >90% displaying "disky" profiles (n < 2). Comparing with prior Morpheus classifications in CANDELS we find that a plurality of JWST disk galaxy candidates were previously classified as compact based on the shallower HST imagery, indicating that the improved optical quality and depth of the JWST helps to reveal disk morphologies that were hiding in the noise. We discuss the implications of these early disk candidates on theories for cosmological disk galaxy formation. %R 10.3847/2041-8213/aca086 %= eprint: arXiv:2208.11456 %@ 0004-637X %0 Journal Article %T The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI) %A Silber, Joseph Harry %A Fagrelius, Parker %A Fanning, Kevin %A Schubnell, Michael %A Aguilar, Jessica Nicole %A Ahlen, Steven %A Ameel, Jon %A Ballester, Otger %A Baltay, Charles %A Bebek, Chris %A Benton Beard, Dominic %A Besuner, Robert %A Cardiel-Sas, Laia %A Casas, Ricard %A Castander, Francisco Javier %A Claybaugh, Todd %A Dobson, Carl %A Duan, Yutong %A Dunlop, Patrick %A Edelstein, Jerry %A Emmet, William T. %A Elliott, Ann %A Evatt, Matthew %A Gershkovich, Irena %A Guy, Julien %A Harris, Stu %A Heetderks, Henry %A Heetderks, Ian %A Honscheid, Klaus %A Illa, Jose Maria %A Jelinsky, Patrick %A Jelinsky, Sharon R. %A Jimenez, Jorge %A Karcher, Armin %A Kent, Stephen %A Kirkby, David %A Kneib, Jean-Paul %A Lambert, Andrew %A Lampton, Mike %A Leitner, Daniela %A Levi, Michael %A McCauley, Jeremy %A Meisner, Aaron %A Miller, Timothy N. %A Miquel, Ramon %A Mundet, Juliá %A Poppett, Claire %A Rabinowitz, David %A Reil, Kevin %A Roman, David %A Schlegel, David %A Serrano, Santiago %A Van Shourt, William %A Sprayberry, David %A Tarlé, Gregory %A Tie, Suk Sien %A Weaverdyck, Curtis %A Zhang, Kai %A Azzaro, Marco %A Bailey, Stephen %A Becerril, Santiago %A Blackwell, Tami %A Bouri, Mohamed %A Brooks, David %A Buckley-Geer, Elizabeth %A Castro, Jose Peñate %A Derwent, Mark %A Dey, Arjun %A Dhungana, Govinda %A Doel, Peter %A Eisenstein, Daniel J. %A Fahim, Nasib %A Garcia-Bellido, Juan %A Gaztañaga, Enrique %A A Gontcho, Satya Gontcho %A Gutierrez, Gaston %A Hörler, Philipp %A Kehoe, Robert %A Kisner, Theodore %A Kremin, Anthony %A Kronig, Luzius %A Landriau, Martin %A Le Guillou, Laurent %A Martini, Paul %A Moustakas, John %A Palanque-Delabrouille, Nathalie %A Peng, Xiyan %A Percival, Will %A Prada, Francisco %A Allende Prieto, Carlos %A de Rivera, Guillermo Gonzalez %A Sanchez, Eusebio %A Sanchez, Justo %A Sharples, Ray %A Soares-Santos, Marcelle %A Schlafly, Edward %A Weaver, Benjamin Alan %A Zhou, Zhimin %A Zhu, Yaling %A Zou, Hu %A DESI Collaboration %+ AA(Lawrence Berkeley National Laboratory, California), AB(National Optical Astronomy Observatory, Arizona; -), AC(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), AD(University of Michigan), AE(Lawrence Berkeley National Laboratory, California), AF(Boston University (BU), USA), AG(University of Michigan), AH(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), Spain), AI(Yale University, Connecticut), AJ(Lawrence Berkeley National Laboratory, California), AK(Lawrence Berkeley National Laboratory, California), AL(Lawrence Berkeley National Laboratory, California), AM(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), Spain), AN(Institut de Cìencies de l'Espai (ICE), IEEC-CSIC, Spain), AO(Institut de Cìencies de l'Espai (ICE), IEEC-CSIC, Spain), AP(Lawrence Berkeley National Laboratory, California), AQ(University of California, Berkeley, Space Sciences Laboratory), AR(Boston University (BU), USA), AS(National Optical Astronomy Observatory, Arizona; -), AT(University of California, Berkeley, Space Sciences Laboratory), AU(Yale University, Connecticut), AV(The Ohio State University, Department of Physics), AW(National Optical Astronomy Observatory, Arizona; -), AX(University of Michigan), AY(Lawrence Berkeley National Laboratory, California), AZ(University of California, Berkeley, Space Sciences Laboratory), BA(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory), BB(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory), BC(The Ohio State University, Department of Physics; The Ohio State University, Department of Astronomy), BD(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), Spain), BE(Lawrence Berkeley National Laboratory, California; University of California, Berkeley, Space Sciences Laboratory), BF(University of California, Berkeley, Space Sciences Laboratory), BG(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), Spain), BH(Lawrence Berkeley National Laboratory, California), BI(Fermi National Accelerator Laboratory, Illinois), BJ(University of California, Irvine), BK(Ecole Polytechnique Federale de Lausanne), BL(Lawrence Berkeley National Laboratory, California), BM(University of California, Berkeley, Space Sciences Laboratory), BN(Lawrence Berkeley National Laboratory, California), BO(Lawrence Berkeley National Laboratory, California), BP(University of California, Berkeley, Space Sciences Laboratory), BQ(National Optical Astronomy Observatory, Arizona; -), BR(University of California, Berkeley, Space Sciences Laboratory), BS(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), Spain; Institució Catalana de Recerca i Estudis Avançats (ICREA), Spain), BT(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), Spain), BU(University of California, Berkeley, Space Sciences Laboratory), BV(Yale University, Connecticut), BW(Kavli Institute for Particle Astrophysics and Cosmology, California; Stanford University, California), BX(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), Spain), BY(Lawrence Berkeley National Laboratory, California), BZ(Institut de Cìencies de l'Espai (ICE), IEEC-CSIC, Spain), CA(University of California, Berkeley, Space Sciences Laboratory), CB(National Optical Astronomy Observatory, Arizona; -), CC(University of Michigan), CD(The Ohio State University, Department of Astronomy), CE(University of Michigan), CF(Lawrence Berkeley National Laboratory, California), CG(Institute of Astrophysics of Andalusia), CH(Lawrence Berkeley National Laboratory, California), CI(Institute of Astrophysics of Andalusia), CJ(Lawrence Berkeley National Laboratory, California), CK(Ecole Polytechnique Federale de Lausanne), CL(University College London (UCL), USA), CM(Fermi National Accelerator Laboratory, Illinois), CN(Astrophysical Institute of the Canaries), CO(The Ohio State University, Department of Astronomy), CP(National Optical Astronomy Observatory, Arizona; -), CQ(Southern Methodist University (SMU), USA), CR(University College London (UCL), USA), CS(Harvard Smithsonian Center for Astrophysics), CT(Grupo de Investigación HCTLab, Escuela Politécnica Superior, Universidad Autónoma de Madrid, Spain), CU(Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Spain), CV(Institut de Cìencies de l'Espai (ICE), IEEC-CSIC, Spain), CW(Lawrence Berkeley National Laboratory, California), CX(Fermi National Accelerator Laboratory, Illinois), CY(Ecole Polytechnique Federale de Lausanne), CZ(Southern Methodist University (SMU), USA), DA(Lawrence Berkeley National Laboratory, California), DB(Lawrence Berkeley National Laboratory, California; University of Michigan), DC(Ecole Polytechnique Federale de Lausanne), DD(Lawrence Berkeley National Laboratory, California), DE(Laboratoire de Physique Nucleaire et de Hautes Energies), DF(The Ohio State University, Department of Astronomy; The Ohio State University, Department of Astronomy), DG(Siena College, New York), DH(Lawrence Berkeley National Laboratory, California; Institut de Recherche sur les Lois Fondamentales de l'Universe), DI(National Astronomical Observatories, Chinese Academy of Sciences, Canada), DJ(University of Waterloo, Department of Physics and Astronomy; Perimeter Institute for Theoretical Physics, Canada), DK(Institute of Astrophysics of Andalusia), DL(Astrophysical Institute of the Canaries), DM(Grupo de Investigación HCTLab, Escuela Politécnica Superior, Universidad Autónoma de Madrid, Spain), DN(Centro de Investigaciones Energeticas Medioambientales y Tecnologicas, Spain), DO(Institute of Astrophysics of Andalusia), DP(Durham University, Department of Physics; Durham University, Department of Physics), DQ(University of Michigan), DR(Lawrence Livermore National Laboratory (LLNL), USA), DS(National Optical Astronomy Observatory, Arizona; -), DT(National Astronomical Observatories, Chinese Academy of Sciences, Canada), DU(University of California, Berkeley, Space Sciences Laboratory), DV(National Astronomical Observatories, Chinese Academy of Sciences, Canada) %J The Astronomical Journal %V 165 %D 2023 %8 January 01, 2023 %P 9 %K Dark energy; Astronomical instrumentation; Spectrometers; Galaxy spectroscopy; 351; 799; 1554; 2171; Astrophysics - Instrumentation and Methods for Astrophysics; Astrophysics - Cosmology and Nongalactic Astrophysics %U https://ui.adsabs.harvard.edu/abs/2023AJ....165....9S %X A system of 5020 robotic fiber positioners was installed in 2019 on the Mayall Telescope, at Kitt Peak National Observatory. The robots automatically retarget their optical fibers every 10-20 minutes, each to a precision of several microns, with a reconfiguration time of fewer than 2 minutes. Over the next 5 yr, they will enable the newly constructed Dark Energy Spectroscopic Instrument (DESI) to measure the spectra of 35 million galaxies and quasars. DESI will produce the largest 3D map of the universe to date and measure the expansion history of the cosmos. In addition to the 5020 robotic positioners and optical fibers, DESI's Focal Plane System includes six guide cameras, four wave front cameras, 123 fiducial point sources, and a metrology camera mounted at the primary mirror. The system also includes associated structural, thermal, and electrical systems. In all, it contains over 675,000 individual parts. We discuss the design, construction, quality control, and integration of all these components. We include a summary of the key requirements, the review and acceptance process, on-sky validations of requirements, and lessons learned for future multiobject, fiber-fed spectrographs. %R 10.3847/1538-3881/ac9ab1 %= eprint: arXiv:2205.09014 %@ 0004-6256