%0 Journal Article
%T A Redshift-independent Efficiency Model: Star Formation and Stellar Masses in Dark Matter Halos at z ≳ 4
%A Tacchella, Sandro 
%A Bose, Sownak 
%A Conroy, Charlie 
%A Eisenstein, Daniel J. 
%A Johnson, Benjamin D.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-8224-4505</ID>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-0974-5266</ID>), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-1590-8551</ID>), AD(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AE(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-9280-7594</ID>)
%B The Astrophysical Journal
%V 868
%D 2018
%8 December 1, 2018
%K cosmology: theory;  galaxies: evolution;  galaxies: formation;  galaxies: high-redshift;  stars: formation 
%U http://adsabs.harvard.edu/abs/2018ApJ...868...92T
%X We explore the connection between the UV luminosity functions (LFs) of 
high-z galaxies and the distribution of stellar masses and star 
formation histories (SFHs) in their host dark matter halos. We provide a 
baseline for a redshift-independent star formation efficiency model to 
which observations and models can be compared. Our model assigns a star 
formation rate (SFR) to each dark matter halo based on the growth rate 
of the halo and a redshift-independent star formation efficiency. The 
dark matter halo accretion rate is obtained from a high-resolution 
N-body simulation in order to capture the stochasticity in accretion 
histories and to obtain spatial information for the distribution of 
galaxies. The halo mass dependence of the star formation efficiency is 
calibrated at z = 4 by requiring a match to the observed UV LF at this 
redshift. The model then correctly predicts the observed UV LF at z = 
5–10. We present predictions for the UV luminosity and stellar 
mass functions, JWST number counts, and SFHs. In particular, we find a 
stellar-to-halo mass relation at z = 4–10 that scales with halo 
mass at M <SUB>h</SUB> < 10<SUP>11</SUP> M <SUB>⊙</SUB> as M 
<SUB>⋆</SUB> ∝ M <SUB>h</SUB> <SUP>2</SUP>, with a 
normalization that is higher than the relation inferred at z = 0. The 
average SFRs increase as a function of time to z = 4, although there is 
significant scatter around the average: about 6% of the z = 4 galaxies 
show no significant mass growth. Using these SFHs, we present 
redshift-dependent UV-to-SFR conversion factors, mass return fractions, 
and mass-to-light ratios for different initial mass functions and 
metallicities, finding that current estimates of the cosmic SFR density 
at z ∼ 10 may be overestimated by ∼0.1–0.2 dex.
%3 10.3847/1538-4357/aae8e0
%= eprint: arXiv:1806.03299
%@ 0004-637X

%0 Electronic Article
%T A Deep Learning Approach to Galaxy Cluster X-ray Masses
%A Ntampaka, M. 
%A ZuHone, J. 
%A Eisenstein, D. 
%A Nagai, D. 
%A Vikhlinin, A. 
%A Hernquist, L. 
%A Marinacci, F. 
%A Nelson, D. 
%A Pakmor, R. 
%A Pillepich, A. 
%A Torrey, P. 
%A Vogelsberger, M.
%B arXiv e-prints
%V 1810
%D 2018
%8 October 1, 2018
%K Astrophysics - Cosmology and Nongalactic Astrophysics
%U http://adsabs.harvard.edu/abs/2018arXiv181007703N
%Z 10 pages, 6 figures, submitted to ApJ
%X We present a machine-learning approach for estimating galaxy cluster 
masses from Chandra mock images. We utilize a Convolutional Neural 
Network (CNN), a deep machine learning tool commonly used in image 
recognition tasks. The CNN is trained and tested on our sample of 7,896 
Chandra X-ray mock observations, which are based on 329 massive clusters 
from the IllustrisTNG simulation. Our CNN learns from a low resolution 
spatial distribution of photon counts and does not use spectral 
information. Despite our simplifying assumption to neglect spectral 
information, the resulting mass values estimated by the CNN exhibit 
small bias in comparison to the true masses of the simulated clusters 
(-0.02 dex) and reproduce the cluster masses with low intrinsic scatter, 
8% in our best fold and 12% averaging over all. In contrast, a more 
standard core-excised luminosity method achieves 15-18% scatter. We 
interpret the results with an approach inspired by Google DeepDream and 
find that the CNN ignores the central regions of clusters, which are 
known to have high scatter with mass.
%= eprint: arXiv:1810.07703

%0 Electronic Article
%T A High-Fidelity Realization of the Euclid Code Comparison $N$-body Simulation with Abacus
%A Garrison, Lehman H. 
%A Eisenstein, Daniel J. 
%A Pinto, Philip A.
%B arXiv e-prints
%V 1810
%D 2018
%8 October 1, 2018
%K Astrophysics - Cosmology and Nongalactic Astrophysics;  Astrophysics - Instrumentation and Methods for Astrophysics;  Physics - Computational Physics
%U http://adsabs.harvard.edu/abs/2018arXiv181002916G
%Z 13 pages, 8 figures. Submitted to MNRAS
%X We present a high-fidelity realization of the cosmological $N$-body 
simulation from the Schneider et al. (2016) code comparison project. The 
simulation was performed with our Abacus $N$-body code, which offers 
high force accuracy, high performance, and minimal particle integration 
errors. The simulation consists of $2048^3$ particles in a $500\ 
h^{-1}\mathrm{Mpc}$ box, for a particle mass of $1.2\times 10^9\ 
h^{-1}\mathrm{M}_\odot$ with $10\ h^{-1}\mathrm{kpc}$ spline softening. 
Abacus executed 1052 global time steps to $z=0$ in 107 hours on one 
dual-Xeon, dual-GPU node, for a mean rate of 23 million particles per 
second per step. We find Abacus is in good agreement with Ramses and 
PKDGrav and less so with Gadget-3. We validate our choice of time step 
by halving the step size and find sub-percent differences in the power 
spectrum and 2PCF at nearly all measured scales, with $<0.3\%$ errors 
at $k<10\ \mathrm{Mpc}^{-1}h$. Simulation snapshots are available at 
http://nbody.rc.fas.harvard.edu/public/S2016 .
%= eprint: arXiv:1810.02916

%0 Journal Article
%T Exploring the squeezed three-point galaxy correlation function with generalized halo occupation distribution models
%A Yuan, Sihan 
%A Eisenstein, Daniel J. 
%A Garrison, Lehman H.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-5992-7586</ID>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 478
%D 2018
%8 August 1, 2018
%P 2019-2033
%K methods: analytical;  galaxies: haloes;  (cosmology): dark matter;  (cosmology): large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2018MNRAS.478.2019Y
%X We present the GeneRalized ANd Differentiable Halo Occupation 
Distribution (GRAND-HOD) routine that generalizes the standard five 
parameter halo occupation distribution (HOD) model with various 
halo-scale physics and assembly bias. We describe the methodology of 
four different generalizations: satellite distribution generalization, 
velocity bias, closest approach distance generalization, and assembly 
bias. We showcase the signatures of these generalizations in the 2-point 
correlation function (2PCF) and the squeezed 3-point correlation 
function (squeezed 3PCF). We identify generalized HOD prescriptions that 
are nearly degenerate in the projected 2PCF and demonstrate that these 
degeneracies are broken in the redshift-space anisotropic 2PCF and the 
squeezed 3PCF. We also discuss the possibility of identifying 
degeneracies in the anisotropic 2PCF and further demonstrate the extra 
constraining power of the squeezed 3PCF on galaxy-halo connection 
models. We find that within our current HOD framework, the anisotropic 
2PCF can predict the squeezed 3PCF better than its statistical error. 
This implies that a discordant squeezed 3PCF measurement could falsify 
the particular HOD model space. Alternatively, it is possible that 
further generalizations of the HOD model would open opportunities for 
the squeezed 3PCF to provide novel parameter measurements. The GRAND-HOD 
PYTHON package is publicly available at 
https://github.com/SandyYuan/GRAND-HOD.
%3 10.1093/mnras/sty1089
%= eprint: arXiv:1802.10115
%@ 0035-8711

%0 Journal Article
%T An iterative reconstruction of cosmological initial density fields
%A Hada, Ryuichiro 
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA; Astronomical Institute, Tohoku University, Aoba-ku, Sendai 980-8578, Japan; Division for Interdisciplinary Advanced Research and Education, Tohoku University, Aoba-ku, Sendai 980-8578, Japan <ID system="ORCID">0000-0002-5959-9199</ID>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 478
%D 2018
%8 August 1, 2018
%P 1866-1874
%K dark matter;  distance scale;  large-scale structure of Universe;  cosmology:theory
%U http://adsabs.harvard.edu/abs/2018MNRAS.478.1866H
%X We present an iterative method to reconstruct the linear-theory initial 
conditions from the late-time cosmological matter density field, with 
the intent of improving the recovery of the cosmic distance scale from 
the baryon acoustic oscillations. We present tests using the dark matter 
density field in both real and redshift space generated from an N-body 
simulation. In redshift space at z = 0.5, we find that the reconstructed 
displacement field using our iterative method are more than 80 per cent 
correlated with the true displacement field of the dark matter particles 
on scales k < 0.10 h Mpc<SUP>-1</SUP>. Furthermore, we show that the 
two-point correlation function of our reconstructed density field 
matches that of the initial density field substantially better, 
especially on small scales (<40 h<SUP>-1</SUP> Mpc). Our 
redshift-space results are improved if we use an anisotropic smoothing 
so as to account for the reduced small-scale information along the line 
of sight in redshift space.
%3 10.1093/mnras/sty1203
%= eprint: arXiv:1804.04738
%@ 0035-8711

%0 Journal Article
%T A practical computational method for the anisotropic redshift-space three-point correlation function
%A Slepian, Zachary 
%A Eisenstein, Daniel J.
%+ AA(Einstein Fellow, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Berkeley Center for Cosmological Physics, University of California, Berkeley, CA 94720, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 478
%D 2018
%8 August 1, 2018
%P 1468-1483
%K cosmology: observations;  distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2018MNRAS.478.1468S
%X We present an algorithm enabling computation of the anisotropic 
redshift-space galaxy three-point correlation function (3PCF) scaling as 
N<SUP>2</SUP>, with N the number of galaxies. Our previous work showed 
how to compute the isotropic 3PCF with this scaling by expanding the 
radially binned density field around each galaxy in the survey into 
spherical harmonics and combining these coefficients to form multipole 
moments. The N<SUP>2</SUP> scaling occurred because this approach never 
explicitly required the relative angle between a galaxy pair about the 
primary galaxy. Here, we generalize this work, demonstrating that in the 
presence of azimuthally symmetric anisotropy produced by redshift-space 
distortions (RSD), the 3PCF can be described by two triangle side 
lengths, two independent total angular momenta, and a spin. This basis 
for the anisotropic 3PCF allows its computation with negligible 
additional work over the isotropic 3PCF. We also present the covariance 
matrix of the anisotropic 3PCF measured in this basis. Our algorithm 
tracks the full 5D redshift-space 3PCF, uses an accurate line of sight 
to each triplet, is exact in angle, and easily handles edge correction. 
It will enable use of the anisotropic large-scale 3PCF as a probe of RSD 
in current and upcoming large-scale redshift surveys.
%3 10.1093/mnras/sty1063
%= eprint: arXiv:1709.10150
%@ 0035-8711

%0 Electronic Article
%T Large Covariance Matrices: Accurate Models Without Mocks
%A O'Connell, Ross 
%A Eisenstein, Daniel J.
%B arXiv e-prints
%V 1808
%D 2018
%8 August 1, 2018
%K Astrophysics - Cosmology and Nongalactic Astrophysics
%U http://adsabs.harvard.edu/abs/2018arXiv180805978O
%Z Submitted to MNRAS
%X Covariance matrix estimation is a persistent challenge for cosmology. We 
focus on a class of model covariance matrices that can be generated with 
high accuracy and precision, using a tiny fraction of the computational 
resources that would be required to achieve comparably precise 
covariance matrices using mock catalogues. In previous work, the free 
parameters in these models were determined using sample covariance 
matrices computed using a large number of mocks, but we demonstrate that 
those parameters can be estimated consistently and with good precision 
by applying jackknife methods to a single survey volume. This enables 
model covariance matrices that are calibrated from data alone, with no 
reference to mocks.
%= eprint: arXiv:1808.05978

%0 Conference Paper
%T Overview of the Dark Energy Spectroscopic Instrument
%A Martini, Paul 
%A Bailey, Stephen 
%A Besuner, Robert W. 
%A Brooks, David 
%A Doel, Peter 
%A Edelstein, Jerry 
%A Eisenstein, Daniel 
%A Flaugher, Brenna 
%A Gutierrez, Gaston 
%A Harris, Stewart E. 
%A Honscheid, Klaus 
%A Jelinsky, Patrick 
%A Joyce, Richard 
%A Kent, Stephen 
%A Levi, Michael 
%A Prada, Francisco 
%A Poppett, Claire 
%A Rabinowitz, David 
%A Rockosi, Constance 
%A Cardiel Sas, Laia 
%A Schlegel, David J. 
%A Schubnell, Michael 
%A Sharples, Ray 
%A Silber, Joseph H. 
%A Sprayberry, David 
%A Wechsler, Risa
%+ AA(The Ohio State Univ. (United States)), AB(Lawrence Berkeley National Lab. (United States)), AC(Lawrence Berkeley National Lab. (United States)), AD(Univ. College London (United Kingdom)), AE(University College London (United Kingdom)), AF(Lawrence Berkeley National Lab. (United States)), AG(Harvard-Smithsonian Center for Astrophysics (United States)), AH(Fermi National Accelerator Lab. (United States)), AI(Fermi National Accelerator Lab. (United States)), AJ(Lawrence Berkeley National Lab. (United States)), AK(The Ohio State Univ. (United States)), AL(Lawrence Berkeley National Lab. (United States)), AM(National Optical Astronomy Observatory (United States)), AN(Fermi National Accelerator Lab. (United States)), AO(Lawrence Berkeley National Lab. (United States)), AP(Instituto de Astrofisica de Andalucía (Spain)), AQ(Lawrence Berkeley National Lab. (United States)), AR(Yale Univ. (United States)), AS(Univ. of California, Santa Cruz (United States)), AT(Institut de Física d'Altes Energies (Spain)), AU(Lawrence Berkeley National Lab. (United States)), AV(Univ. of Michigan (United States)), AW(Durham Univ. (United Kingdom)), AX(Lawrence Berkeley National Lab. (United States)), AY(National Optical Astronomy Observatory (United States)), AZ(Kavli Institute for Particle Astrophysics and Cosmology (United States))
%B Ground-based and Airborne Instrumentation for Astronomy VII
%V 0702
%D 2018
%8 July 1, 2018
%U http://adsabs.harvard.edu/abs/2018SPIE10702E..1FM
%Z ISBN: <ISBN>9781510619579</ISBN>
%X The Dark Energy Spectroscopic Instrument (DESI) is under construction to 
measure the expansion history of the Universe using the Baryon Acoustic 
Oscillation technique. The spectra of 35 million galaxies and quasars 
over 14000 square degrees will be measured during the life of the 
experiment. A new prime focus corrector for the KPNO Mayall telescope 
will deliver light to 5000 fiber optic positioners. The fibers in turn 
feed ten broad-band spectrographs. We present an overview of the 
instrumentation, the main technical requirements and challenges, and the 
current status of the project.
%3 10.1117/12.2313063
%= eprint: arXiv:1807.09287
%@ 9781510619579

%0 Journal Article
%T Analysing baryon acoustic oscillations in sparse spectroscopic samples via cross-correlation with dense photometry
%A Patej, A. 
%A Eisenstein, D. J.
%+ AA(Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85719, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 477
%D 2018
%8 July 1, 2018
%P 5090-5103
%K distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2018MNRAS.477.5090P
%X We develop a formalism for measuring the cosmological distance scale 
from baryon acoustic oscillations (BAO) using the cross-correlation of a 
sparse redshift survey with a denser photometric sample. This reduces 
the shot noise that would otherwise affect the autocorrelation of the 
sparse spectroscopic map. As a proof of principle, we make the first 
on-sky application of this method to a sparse sample defined as the z 
> 0.6 tail of the Sloan Digital Sky Survey's (SDSS) BOSS/CMASS sample 
of galaxies and a dense photometric sample from SDSS DR9. We find a 
2.8σ preference for the BAO peak in the cross-correlation at an 
effective z = 0.64, from which we measure the angular diameter distance 
D<SUB>M</SUB>(z = 0.64) = (2418 ± 73 Mpc)(r<SUB>s</SUB>/r<SUB>s, 
fid</SUB>). Accordingly, we expect that using this method to combine 
sparse spectroscopy with the deep, high-quality imaging that is just now 
becoming available will enable higher precision BAO measurements than 
possible with the spectroscopy alone.
%3 10.1093/mnras/sty870
%= eprint: arXiv:1709.03514
%@ 0035-8711

%0 Journal Article
%T They Might Be Giants: An Efficient Color-based Selection of Red Giant Stars
%A Conroy, Charlie 
%A Bonaca, Ana 
%A Naidu, Rohan P. 
%A Eisenstein, Daniel J. 
%A Johnson, Benjamin D. 
%A Dotter, Aaron 
%A Finkbeiner, Douglas P.
%+ AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-1590-8551</ID>), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-7846-9787</ID>), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-4442-5700</ID>), AG(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA <ID system="ORCID">0000-0003-2808-275X</ID>)
%B The Astrophysical Journal Letters
%V 861
%D 2018
%8 July 1, 2018
%K Galaxy: halo;  Galaxy: kinematics and dynamics 
%U http://adsabs.harvard.edu/abs/2018ApJ...861L..16C
%X We present a color-based method for identifying red giants based on the 
Pan-STARRS grz and WISE W1 and W2 photometry. We utilize a subsample of 
bright stars with precise parallaxes from Gaia’s second data 
release (DR2) to verify that the color-based selection reliably 
separates dwarfs from giants. The selection is conservative in the sense 
that contamination is small (≈30%) but not all giants are included 
(the selection primarily identifies K giants). The color-based selection 
can be applied to stars brighter than W1 ≈ 16, more than two 
magnitudes fainter than techniques relying on shallower 2MASS 
photometry. Many streams and clouds are visible in the resulting sky 
maps, especially when binned by Gaia DR2 proper motions, including the 
Sagittarius stream, the Hercules–Aquila Cloud, the Eastern Banded 
Structure, Monoceros, and the Virgo Overdensity. In addition to the 
characterization of new and known stellar streams, we expect that this 
method for selecting red giants will enable detailed analysis of the 
diffuse stellar halo to distances exceeding 100 kpc.
%3 10.3847/2041-8213/aacdf1
%= eprint: arXiv:1805.05954
%@ 0004-637X

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: theoretical systematics and Baryon Acoustic Oscillations in the galaxy correlation function
%A Vargas-Magaña, Mariana 
%A Ho, Shirley 
%A Cuesta, Antonio J. 
%A O'Connell, Ross 
%A Ross, Ashley J. 
%A Eisenstein, Daniel J. 
%A Percival, Will J. 
%A Grieb, Jan Niklas 
%A Sánchez, Ariel G. 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Beutler, Florian 
%A Chuang, Chia-Hsun 
%A Kitaura, Francisco-Shu 
%A Prada, Francisco 
%A Rodríguez-Torres, Sergio A. 
%A Rossi, Graziano 
%A Seo, Hee-Jong 
%A Brownstein, Joel R. 
%A Olmstead, Matthew 
%A Thomas, Daniel
%+ AA(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México; Departments of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15217, USA; McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15217, USA), AB(Departments of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15217, USA; McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15217, USA; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AC(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain; Departamento de Física, Universidad de Córdoba, Campus de Rabanales, Edificio Albert Einstein, E-14071, Córdoba, Spain), AD(Departments of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15217, USA; McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15217, USA), AE(Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA <ID system="ORCID">0000-0002-7522-9083</ID>), AF(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AG(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), AH(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach,1312, Giessenbachstr., D-85741 Garching, Germany <ID system="ORCID">0000-0003-2178-0694</ID>), AI(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany), AJ(Center for Cosmology and Particle Physics, New York University, New York, NY 10003, USA), AK(School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS, UK <ID system="ORCID">0000-0001-5191-2286</ID>), AL(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK <ID system="ORCID">0000-0003-0467-5438</ID>), AM(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AN(Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AO(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autonóma de Madrid (UAM), Cantoblanco, E-28049, Madrid, Spain), AP(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autonóma de Madrid (UAM), Cantoblanco, E-28049, Madrid, Spain), AQ(Department of Physics and Astronomy, Sejong University, Seoul 143-747, Korea), AR(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), AS(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA <ID system="ORCID">0000-0002-8725-1069</ID>), AT(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AU(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK)
%B Monthly Notices of the Royal Astronomical Society
%V 477
%D 2018
%8 June 1, 2018
%P 1153-1188
%K surveys;  galaxies: distances and redshifts;  cosmology: observations
%U http://adsabs.harvard.edu/abs/2018MNRAS.477.1153V
%X We investigate the potential sources of theoretical systematics in the 
anisotropic Baryon Acoustic Oscillation (BAO) distance scale 
measurements from the clustering of galaxies in configuration space 
using the final Data Release (DR12) of the Baryon Oscillation 
Spectroscopic Survey (BOSS). We perform a detailed study of the impact 
on BAO measurements from choices in the methodology such as fiducial 
cosmology, clustering estimators, random catalogues, fitting templates, 
and covariance matrices. The theoretical systematic uncertainties in BAO 
parameters are found to be 0.002 in the isotropic dilation α and 
0.003 in the quadrupolar dilation ɛ. The leading source of 
systematic uncertainty is related to the reconstruction techniques. 
Theoretical uncertainties are sub-dominant compared with the statistical 
uncertainties for BOSS survey, accounting 0.2σ<SUB>stat</SUB> for 
α and 0.25σ<SUB>stat</SUB> for ɛ 
(σ<SUB>α, stat</SUB> ˜ 0.010 and 
σ<SUB>ɛ, stat</SUB> ˜ 0.012, respectively). We also 
present BAO-only distance scale constraints from the anisotropic 
analysis of the correlation function. Our constraints on the angular 
diameter distance D<SUB>A</SUB>(z) and the Hubble parameter H(z), 
including both statistical and theoretical systematic uncertainties, are 
1.5 per cent and 2.8 per cent at z<SUB>eff</SUB> = 0.38, 1.4 per cent 
and 2.4 per cent at z<SUB>eff</SUB> = 0.51, and 1.7 per cent and 2.6 per 
cent at z<SUB>eff</SUB> = 0.61. This paper is part of a set that 
analyses the final galaxy clustering data set from BOSS. The 
measurements and likelihoods presented here are cross-checked with other 
BAO analysis in Alam et al. The systematic error budget concerning the 
methodology on post-reconstruction BAO analysis presented here is used 
in Alam et al. to produce the final cosmological constraints from BOSS.
%3 10.1093/mnras/sty571
%= eprint: arXiv:1610.03506
%@ 0035-8711

%0 Journal Article
%T The Abacus Cosmos: A Suite of Cosmological N-body Simulations
%A Garrison, Lehman H. 
%A Eisenstein, Daniel J. 
%A Ferrer, Douglas 
%A Tinker, Jeremy L. 
%A Pinto, Philip A. 
%A Weinberg, David H.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-9853-5673</ID>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AD(Center for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AE(Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85121, USA), AF(Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA ;  Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA <ID system="ORCID">0000-0001-7775-7261</ID>)
%B The Astrophysical Journal Supplement Series
%V 236
%D 2018
%8 June 1, 2018
%K large-scale structure of universe;  methods: numerical
%U http://adsabs.harvard.edu/abs/2018ApJS..236...43G
%X We present a public data release of halo catalogs from a suite of 125 
cosmological N-body simulations from the ABACUS project. The simulations 
span 40 wCDM cosmologies centered on the Planck 2015 cosmology at two 
mass resolutions, 4 × 10<SUP>10</SUP> h <SUP>-1</SUP> M 
<SUB>⊙</SUB> and 1 × 10<SUP>10</SUP> h <SUP>-1</SUP> M 
<SUB>⊙</SUB>, in 1.1 h <SUP>-1</SUP> Gpc and 720 h 
<SUP>-1</SUP> Mpc boxes, respectively. The boxes are phase-matched 
to suppress sample variance and isolate cosmology dependence. Additional 
volume is available via 16 boxes of fixed cosmology and varied phase; a 
few boxes of single-parameter excursions from Planck 2015 are also 
provided. Catalogs spanning z = 1.5 to 0.1 are available for 
friends-of-friends and ROCKSTAR halo finders and include particle 
subsamples. All data products are available at <A href="https://lgarrison.github.io/AbacusCosmos">https://lgarrison.github.io/AbacusCosmos</A>.
%3 10.3847/1538-4365/aabfd3
%= eprint: arXiv:1712.05768
%@ 0067-0049

%0 Journal Article
%T The JWST Extragalactic Mock Catalog: Modeling Galaxy Populations from the UV through the Near-IR over 13 Billion Years of Cosmic History
%A Williams, Christina C. 
%A Curtis-Lake, Emma 
%A Hainline, Kevin N. 
%A Chevallard, Jacopo 
%A Robertson, Brant E. 
%A Charlot, Stephane 
%A Endsley, Ryan 
%A Stark, Daniel P. 
%A Willmer, Christopher N. A. 
%A Alberts, Stacey 
%A Amorin, Ricardo 
%A Arribas, Santiago 
%A Baum, Stefi 
%A Bunker, Andrew 
%A Carniani, Stefano 
%A Crandall, Sara 
%A Egami, Eiichi 
%A Eisenstein, Daniel J. 
%A Ferruit, Pierre 
%A Husemann, Bernd 
%A Maseda, Michael V. 
%A Maiolino, Roberto 
%A Rawle, Timothy D. 
%A Rieke, Marcia 
%A Smit, Renske 
%A Tacchella, Sandro 
%A Willott, Chris J.
%+ AA(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA ;; <EMAIL>ccwilliams@email.arizona.edu</EMAIL> <ID system="ORCID">0000-0003-2919-7495</ID>), AB(Sorbonne Universités, UPMC-CNRS, UMR7095, Institut d'Astrophysique de Paris, F-75014, Paris, France <EMAIL>curtis@iap.fr</EMAIL>), AC(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA <ID system="ORCID">0000-0003-4565-8239</ID>), AD(Sorbonne Universités, UPMC-CNRS, UMR7095, Institut d'Astrophysique de Paris, F-75014, Paris, France), AE(Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA <ID system="ORCID">0000-0002-4271-0364</ID>), AF(Sorbonne Universités, UPMC-CNRS, UMR7095, Institut d'Astrophysique de Paris, F-75014, Paris, France <ID system="ORCID">0000-0003-3458-2275</ID>), AG(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA), AH(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA), AI(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA <ID system="ORCID">0000-0001-9262-9997</ID>), AJ(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA), AK(Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Avenue, Cambridge CB3 0HE, UK ; Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK <ID system="ORCID">0000-0001-5758-1000</ID>), AL(Departamento de Astrofisica, Centro de Astrobiologia, CSIC-INTA, Cra. de Ajalvir, E-28850-Madrid, Spain), AM(University of Manitoba, Department of Physics and Astronomy, Winnipeg, MB R3T 2N2, Canada), AN(Department of Physics, University of Oxford, Oxford, UK), AO(Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Avenue, Cambridge CB3 0HE, UK ; Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK <ID system="ORCID">0000-0002-6719-380X</ID>), AP(Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA), AQ(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA), AR(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AS(Scientific Support Office, Directorate of Science, ESA/ESTEC, Keplerlaan 1, 2201AZ Noordwijk, The Netherlands), AT(Max Planck Institute for Astronomy, Konigstuhl 17, D-69117 Heidelberg, Germany <ID system="ORCID">0000-0003-2901-6842</ID>), AU(Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA, Leiden, The Netherlands <ID system="ORCID">0000-0003-0695-4414</ID>), AV(Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Avenue, Cambridge CB3 0HE, UK ; Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), AW(European Space Agency, c/o STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA), AX(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA), AY(Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Avenue, Cambridge CB3 0HE, UK ; Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK <ID system="ORCID">0000-0001-8034-7802</ID>), AZ(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-8224-4505</ID>), BA(NRC Herzberg, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada <ID system="ORCID">0000-0002-4201-7367</ID>)
%B The Astrophysical Journal Supplement Series
%V 236
%D 2018
%8 June 1, 2018
%K galaxies: evolution;  galaxies: high-redshift;  galaxies: photometry
%U http://adsabs.harvard.edu/abs/2018ApJS..236...33W
%X We present an original phenomenological model to describe the evolution 
of galaxy number counts, morphologies, and spectral energy distributions 
across a wide range of redshifts (0.2< z< 15) and stellar masses 
[{log}(M/{M}<SUB>⊙ </SUB>)≥slant 6]. Our model follows observed 
mass and luminosity functions of both star-forming and quiescent 
galaxies, and reproduces the redshift evolution of colors, sizes, star 
formation, and chemical properties of the observed galaxy population. 
Unlike other existing approaches, our model includes a self-consistent 
treatment of stellar and photoionized gas emission and dust attenuation 
based on the BEAGLE tool. The mock galaxy catalogs generated with our 
new model can be used to simulate and optimize extragalactic surveys 
with future facilities such as the James Webb Space Telescope (JWST), 
and to enable critical assessments of analysis procedures, 
interpretation tools, and measurement systematics for both photometric 
and spectroscopic data. As a first application of this work, we make 
predictions for the upcoming JWST Advanced Deep Extragalactic Survey 
(JADES), a joint program of the JWST/NIRCam and NIRSpec Guaranteed Time 
Observations teams. We show that JADES will detect, with NIRCam imaging, 
1000s of galaxies at z ≳ 6, and 10s at z ≳ 10 at 
{m}<SUB>{AB</SUB>}≲ 30 (5σ) within the 236 arcmin<SUP>2</SUP> 
of the survey. The JADES data will enable accurate constraints on the 
evolution of the UV luminosity function at z > 8, and resolve the 
current debate about the rate of evolution of galaxies at z ≳ 8. 
Ready-to-use mock catalogs and software to generate new realizations are 
publicly available as the JAdes extraGalactic Ultradeep Artificial 
Realizations (JAGUAR) package.
%3 10.3847/1538-4365/aabcbb
%= eprint: arXiv:1802.05272
%@ 0067-0049

%0 Electronic Article
%T Overview of the DESI Legacy Imaging Surveys
%A Dey, Arjun 
%A Schlegel, David J. 
%A Lang, Dustin 
%A Blum, Robert 
%A Burleigh, Kaylan 
%A Fan, Xiaohui 
%A Findlay, Joseph R. 
%A Finkbeiner, Doug 
%A Herrera, David 
%A Juneau, Stephanie 
%A Landriau, Martin 
%A Levi, Michael 
%A McGreer, Ian 
%A Meisner, Aaron 
%A Myers, Adam D. 
%A Moustakas, John 
%A Nugent, Peter 
%A Patej, Anna 
%A Schlafly, Edward F. 
%A Walker, Alistair R. 
%A Valdes, Francisco 
%A Weaver, Benjamin A. 
%A Zou, Christophe Yeche Hu 
%A Zhou, Xu 
%A Abareshi, Behzad 
%A Abbott, T. M. C. 
%A Abolfathi, Bela 
%A Aguilera, C. 
%A Alam, Shadab 
%A Allen, Lori 
%A Alvarez, A. 
%A Annis, James 
%A Ansarinejad, Behzad 
%A Aubert, Marie 
%A Beechert, Jacqueline 
%A Bell, Eric F. 
%A BenZvi, Segev Y. 
%A Beutler, Florian 
%A Bielby, Richard M. 
%A Bolton, Adam S. 
%A Buckley-Geer, Cesar Briceno Elizabeth J. 
%A Butler, Karen 
%A Calamida, Annalisa 
%A Carlberg, Raymond G. 
%A Carter, Paul 
%A Casas, Ricard 
%A Castander, Francisco J. 
%A Choi, Yumi 
%A Comparat, Johan 
%A Cukanovaite, Elena 
%A Delubac, Timothee 
%A DeVries, Kaitlin 
%A Dey, Sharmila 
%A Dhungana, Govinda 
%A Dickinson, Mark 
%A Ding, Zhejie 
%A Donaldson, John B. 
%A Duan, Yutong 
%A Duckworth, Christopher J. 
%A Eftekharzadeh, Sarah 
%A Eisenstein, Daniel J. 
%A Etourneau, Thomas 
%A Fagrelius, Parker A. 
%A Farihi, Jay 
%A Fitzpatrick, Mike 
%A Font-Ribera, Andreu 
%A Fulmer, Leah 
%A Gansicke, Boris T. 
%A Gaztanaga, Enrique 
%A George, Koshy 
%A Gerdes, David W. 
%A Gontcho, Satya Gontcho A 
%A Gorgoni, Claudio 
%A Green, Gregory 
%A Guy, Julien 
%A Harmer, Diane 
%A Hernandez, M. 
%A Honscheid, Klaus 
%A Lijuan 
%A Huang 
%A James, David 
%A Jannuzi, Buell T. 
%A Jiang, Linhua 
%A Joyce, Richard 
%A Karcher, Armin 
%A Karkar, Sonia 
%A Kehoe, Robert 
%A Kneib, Jean-Paul 
%A Kueter-Young, Andrea 
%A Lan, Ting-Wen 
%A Lauer, Tod 
%A Le Guillou, Laurent 
%A Le Van Suu, Auguste 
%A Lee, Jae Hyeon 
%A Lesser, Michael 
%A Perreault Levasseur, Laurence 
%A Li, Ting S. 
%A Mann, Justin L. 
%A Marshall, Bob 
%A Martinez-Vazquez, C. E. 
%A Martini, Paul 
%A du Mas des Bourboux, Helion 
%A McManus, Sean 
%A Meier, Tobias Gabriel 
%A Menard, Brice 
%A Metcalfe, Nigel 
%A Munoz-Gutierrez, Andrea 
%A Najita, Joan 
%A Napier, Kevin 
%A Narayan, Gautham 
%A Newman, Jeffrey A. 
%A Nie, Jundan 
%A Nord, Brian 
%A Norman, Dara J. 
%A Olsen, Knut A. G. 
%A Paat, Anthony 
%A Palanque-Delabrouille, Nathalie 
%A Peng, Xiyan 
%A Poppett, Claire L. 
%A Poremba, Megan R. 
%A Prakash, Abhishek 
%A Rabinowitz, David 
%A Raichoor, Anand 
%A Rezaie, Mehdi 
%A Robertson, A. N. 
%A Roe, Natalie A. 
%A Ross, Ashley J. 
%A Ross, Nicholas P. 
%A Rudnick, Gregory 
%A Safonova, Sasha 
%A Saha, Abhijit 
%A Sanchez, F. Javier 
%A Savary, Elodie 
%A Schweiker, Heidi 
%A Scott, Adam 
%A Seo, Hee-Jong 
%A Shan, Huanyuan 
%A Silva, David R. 
%A Slepian, Zachary 
%A Soto, Christian 
%A Sprayberry, David 
%A Staten, Ryan 
%A Stillman, Coley M. 
%A Stupak, Robert J. 
%A Summers, David L. 
%A Sien Tie, Suk 
%A Tirado, H. 
%A Vargas-Magana, Mariana 
%A Vivas, A. Katherina 
%A Wechsler, Risa H. 
%A Williams, Doug 
%A Yang, Jinyi 
%A Yang, Qian 
%A Yapici, Tolga 
%A Zaritsky, Dennis 
%A Zenteno, A. 
%A Zhang, Kai 
%A Zhang, Tianmeng 
%A Zhou, Rongpu 
%A Zhou, Zhimin
%B arXiv e-prints
%V 1804
%D 2018
%8 April 1, 2018
%K Astrophysics - Instrumentation and Methods for Astrophysics
%U http://adsabs.harvard.edu/abs/2018arXiv180408657D
%Z 47 pages, 18 figures; accepted for publication in the Astronomical Journal
%X The DESI Legacy Imaging Surveys are a combination of three public 
projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky 
Survey, and the Mayall z-band Legacy Survey) that will jointly image 
approximately 14,000 deg^2 of the extragalactic sky visible from the 
northern hemisphere in three optical bands (g, r, and z) using 
telescopes at the Kitt Peak National Observatory and the Cerro Tololo 
Inter-American Observatory. The combined survey footprint is split into 
two contiguous areas by the Galactic plane. The optical imaging is 
conducted using a unique strategy of dynamically adjusting the exposure 
times and pointing selection during observing that results in a survey 
of nearly uniform depth. In addition to calibrated images, the project 
is delivering a catalog, constructed by using a probabilistic 
inference-based approach to estimate source shapes and brightnesses. The 
catalog includes photometry from the grz optical bands and from four 
mid-infrared bands (at 3.4, 4.6, 12 and 22 micorons) observed by the 
Wide-field Infrared Survey Explorer (WISE) satellite during its full 
operational lifetime. The project plans two public data releases each 
year. All the software used to generate the catalogs is also released 
with the data. This paper provides an overview of the Legacy Surveys 
project.
%= eprint: arXiv:1804.08657

%0 Journal Article
%T The Fourteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the Extended Baryon Oscillation Spectroscopic Survey and from the Second Phase of the Apache Point Observatory Galactic Evolution Experiment
%A Abolfathi, Bela 
%A Aguado, D. S. 
%A Aguilar, Gabriela 
%A Allende Prieto, Carlos 
%A Almeida, Andres 
%A Ananna, Tonima Tasnim 
%A Anders, Friedrich 
%A Anderson, Scott F. 
%A Andrews, Brett H. 
%A Anguiano, Borja 
%A Aragón-Salamanca, Alfonso 
%A Argudo-Fernández, Maria 
%A Armengaud, Eric 
%A Ata, Metin 
%A Aubourg, Eric 
%A Avila-Reese, Vladimir 
%A Badenes, Carles 
%A Bailey, Stephen 
%A Balland, Christophe 
%A Barger, Kathleen A. 
%A Barrera-Ballesteros, Jorge 
%A Bartosz, Curtis 
%A Bastien, Fabienne 
%A Bates, Dominic 
%A Baumgarten, Falk 
%A Bautista, Julian 
%A Beaton, Rachael 
%A Beers, Timothy C. 
%A Belfiore, Francesco 
%A Bender, Chad F. 
%A Bernardi, Mariangela 
%A Bershady, Matthew A. 
%A Beutler, Florian 
%A Bird, Jonathan C. 
%A Bizyaev, Dmitry 
%A Blanc, Guillermo A. 
%A Blanton, Michael R. 
%A Blomqvist, Michael 
%A Bolton, Adam S. 
%A Boquien, Médéric 
%A Borissova, Jura 
%A Bovy, Jo 
%A Andres Bradna Diaz, Christian 
%A Brandt, William Nielsen 
%A Brinkmann, Jonathan 
%A Brownstein, Joel R. 
%A Bundy, Kevin 
%A Burgasser, Adam J. 
%A Burtin, Etienne 
%A Busca, Nicolás G. 
%A Cañas, Caleb I. 
%A Cano-Díaz, Mariana 
%A Cappellari, Michele 
%A Carrera, Ricardo 
%A Casey, Andrew R. 
%A Cervantes Sodi, Bernardo 
%A Chen, Yanping 
%A Cherinka, Brian 
%A Chiappini, Cristina 
%A Doohyun Choi, Peter 
%A Chojnowski, Drew 
%A Chuang, Chia-Hsun 
%A Chung, Haeun 
%A Clerc, Nicolas 
%A Cohen, Roger E. 
%A Comerford, Julia M. 
%A Comparat, Johan 
%A Correa do Nascimento, Janaina 
%A da Costa, Luiz 
%A Cousinou, Marie-Claude 
%A Covey, Kevin 
%A Crane, Jeffrey D. 
%A Cruz-Gonzalez, Irene 
%A Cunha, Katia 
%A da Silva Ilha, Gabriele 
%A Damke, Guillermo J. 
%A Darling, Jeremy 
%A Davidson, James W., Jr. 
%A Dawson, Kyle 
%A de Icaza Lizaola, Miguel Angel C. 
%A de la Macorra, Axel 
%A de la Torre, Sylvain 
%A De Lee, Nathan 
%A de Sainte Agathe, Victoria 
%A Deconto Machado, Alice 
%A Dell'Agli, Flavia 
%A Delubac, Timothée 
%A Diamond-Stanic, Aleksandar M. 
%A Donor, John 
%A Downes, Juan José 
%A Drory, Niv 
%A du Mas des Bourboux, Hélion 
%A Duckworth, Christopher J. 
%A Dwelly, Tom 
%A Dyer, Jamie 
%A Ebelke, Garrett 
%A Davis Eigenbrot, Arthur 
%A Eisenstein, Daniel J. 
%A Elsworth, Yvonne P. 
%A Emsellem, Eric 
%A Eracleous, Michael 
%A Erfanianfar, Ghazaleh 
%A Escoffier, Stephanie 
%A Fan, Xiaohui 
%A Fernández Alvar, Emma 
%A Fernandez-Trincado, J. G. 
%A Fernando Cirolini, Rafael 
%A Feuillet, Diane 
%A Finoguenov, Alexis 
%A Fleming, Scott W. 
%A Font-Ribera, Andreu 
%A Freischlad, Gordon 
%A Frinchaboy, Peter 
%A Fu, Hai 
%A Gómez Maqueo Chew, Yilen 
%A Galbany, Lluís 
%A García Pérez, Ana E. 
%A Garcia-Dias, R. 
%A García-Hernández, D. A. 
%A Garma Oehmichen, Luis Alberto 
%A Gaulme, Patrick 
%A Gelfand, Joseph 
%A Gil-Marín, Héctor 
%A Gillespie, Bruce A. 
%A Goddard, Daniel 
%A González Hernández, Jonay I. 
%A Gonzalez-Perez, Violeta 
%A Grabowski, Kathleen 
%A Green, Paul J. 
%A Grier, Catherine J. 
%A Gueguen, Alain 
%A Guo, Hong 
%A Guy, Julien 
%A Hagen, Alex 
%A Hall, Patrick 
%A Harding, Paul 
%A Hasselquist, Sten 
%A Hawley, Suzanne 
%A Hayes, Christian R. 
%A Hearty, Fred 
%A Hekker, Saskia 
%A Hernandez, Jesus 
%A Hernandez Toledo, Hector 
%A Hogg, David W. 
%A Holley-Bockelmann, Kelly 
%A Holtzman, Jon A. 
%A Hou, Jiamin 
%A Hsieh, Bau-Ching 
%A Hunt, Jason A. S. 
%A Hutchinson, Timothy A. 
%A Hwang, Ho Seong 
%A Jimenez Angel, Camilo Eduardo 
%A Johnson, Jennifer A. 
%A Jones, Amy 
%A Jönsson, Henrik 
%A Jullo, Eric 
%A Khan, Fahim Sakil 
%A Kinemuchi, Karen 
%A Kirkby, David 
%A Kirkpatrick, Charles C., IV 
%A Kitaura, Francisco-Shu 
%A Knapp, Gillian R. 
%A Kneib, Jean-Paul 
%A Kollmeier, Juna A. 
%A Lacerna, Ivan 
%A Lane, Richard R. 
%A Lang, Dustin 
%A Law, David R. 
%A Le Goff, Jean-Marc 
%A Lee, Young-Bae 
%A Li, Hongyu 
%A Li, Cheng 
%A Lian, Jianhui 
%A Liang, Yu 
%A Lima, Marcos 
%A Lin, Lihwai 
%A Long, Dan 
%A Lucatello, Sara 
%A Lundgren, Britt 
%A Mackereth, J. Ted 
%A MacLeod, Chelsea L. 
%A Mahadevan, Suvrath 
%A Maia, Marcio Antonio Geimba 
%A Majewski, Steven 
%A Manchado, Arturo 
%A Maraston, Claudia 
%A Mariappan, Vivek 
%A Marques-Chaves, Rui 
%A Masseron, Thomas 
%A Masters, Karen L. 
%A McDermid, Richard M. 
%A McGreer, Ian D. 
%A Melendez, Matthew 
%A Meneses-Goytia, Sofia 
%A Merloni, Andrea 
%A Merrifield, Michael R. 
%A Meszaros, Szabolcs 
%A Meza, Andres 
%A Minchev, Ivan 
%A Minniti, Dante 
%A Mueller, Eva-Maria 
%A Muller-Sanchez, Francisco 
%A Muna, Demitri 
%A Muñoz, Ricardo R. 
%A Myers, Adam D. 
%A Nair, Preethi 
%A Nandra, Kirpal 
%A Ness, Melissa 
%A Newman, Jeffrey A. 
%A Nichol, Robert C. 
%A Nidever, David L. 
%A Nitschelm, Christian 
%A Noterdaeme, Pasquier 
%A O'Connell, Julia 
%A Oelkers, Ryan James 
%A Oravetz, Audrey 
%A Oravetz, Daniel 
%A Ortíz, Erik Aquino 
%A Osorio, Yeisson 
%A Pace, Zach 
%A Padilla, Nelson 
%A Palanque-Delabrouille, Nathalie 
%A Palicio, Pedro Alonso 
%A Pan, Hsi-An 
%A Pan, Kaike 
%A Parikh, Taniya 
%A Pâris, Isabelle 
%A Park, Changbom 
%A Peirani, Sebastien 
%A Pellejero-Ibanez, Marcos 
%A Penny, Samantha 
%A Percival, Will J. 
%A Perez-Fournon, Ismael 
%A Petitjean, Patrick 
%A Pieri, Matthew M. 
%A Pinsonneault, Marc 
%A Pisani, Alice 
%A Prada, Francisco 
%A Prakash, Abhishek 
%A Queiroz, Anna Bárbara de Andrade 
%A Raddick, M. Jordan 
%A Raichoor, Anand 
%A Barboza Rembold, Sandro 
%A Richstein, Hannah 
%A Riffel, Rogemar A. 
%A Riffel, Rogério 
%A Rix, Hans-Walter 
%A Robin, Annie C. 
%A Rodríguez Torres, Sergio 
%A Román-Zúñiga, Carlos 
%A Ross, Ashley J. 
%A Rossi, Graziano 
%A Ruan, John 
%A Ruggeri, Rossana 
%A Ruiz, Jose 
%A Salvato, Mara 
%A Sánchez, Ariel G. 
%A Sánchez, Sebastián F. 
%A Sanchez Almeida, Jorge 
%A Sánchez-Gallego, José R. 
%A Santana Rojas, Felipe Antonio 
%A Santiago, Basílio Xavier 
%A Schiavon, Ricardo P. 
%A Schimoia, Jaderson S. 
%A Schlafly, Edward 
%A Schlegel, David 
%A Schneider, Donald P. 
%A Schuster, William J. 
%A Schwope, Axel 
%A Seo, Hee-Jong 
%A Serenelli, Aldo 
%A Shen, Shiyin 
%A Shen, Yue 
%A Shetrone, Matthew 
%A Shull, Michael 
%A Silva Aguirre, Víctor 
%A Simon, Joshua D. 
%A Skrutskie, Mike 
%A Slosar, Anže 
%A Smethurst, Rebecca 
%A Smith, Verne 
%A Sobeck, Jennifer 
%A Somers, Garrett 
%A Souter, Barbara J. 
%A Souto, Diogo 
%A Spindler, Ashley 
%A Stark, David V. 
%A Stassun, Keivan 
%A Steinmetz, Matthias 
%A Stello, Dennis 
%A Storchi-Bergmann, Thaisa 
%A Streblyanska, Alina 
%A Stringfellow, Guy S. 
%A Suárez, Genaro 
%A Sun, Jing 
%A Szigeti, Laszlo 
%A Taghizadeh-Popp, Manuchehr 
%A Talbot, Michael S. 
%A Tang, Baitian 
%A Tao, Charling 
%A Tayar, Jamie 
%A Tembe, Mita 
%A Teske, Johanna 
%A Thakar, Aniruddha R. 
%A Thomas, Daniel 
%A Tissera, Patricia 
%A Tojeiro, Rita 
%A Tremonti, Christy 
%A Troup, Nicholas W. 
%A Urry, Meg 
%A Valenzuela, O. 
%A van den Bosch, Remco 
%A Vargas-González, Jaime 
%A Vargas-Magaña, Mariana 
%A Vazquez, Jose Alberto 
%A Villanova, Sandro 
%A Vogt, Nicole 
%A Wake, David 
%A Wang, Yuting 
%A Weaver, Benjamin Alan 
%A Weijmans, Anne-Marie 
%A Weinberg, David H. 
%A Westfall, Kyle B. 
%A Whelan, David G. 
%A Wilcots, Eric 
%A Wild, Vivienne 
%A Williams, Rob A. 
%A Wilson, John 
%A Wood-Vasey, W. M. 
%A Wylezalek, Dominika 
%A Xiao, Ting 
%A Yan, Renbin 
%A Yang, Meng 
%A Ybarra, Jason E. 
%A Yèche, Christophe 
%A Zakamska, Nadia 
%A Zamora, Olga 
%A Zarrouk, Pauline 
%A Zasowski, Gail 
%A Zhang, Kai 
%A Zhao, Cheng 
%A Zhao, Gong-Bo 
%A Zheng, Zheng 
%A Zheng, Zheng 
%A Zhou, Zhi-Min 
%A Zhu, Guangtun 
%A Zinn, Joel C. 
%A Zou, Hu
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Vicuña Mackenna 4860, Macul, Santiago, Chile ; Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuna Mackenna 4860, 782-0436 Macul, Santiago, Chile ; Astrophysical Research Consortium, Physics/Astronomy Building, Rm C319, 3910 15th Avenue NE, Seattle, WA 98195, USA <ID system="ORCID">0000-0002-7802-7356</ID>), GJ(Instituto Milenio de Astrofísica, Av. Vicuña Mackenna 4860, Macul, Santiago, Chile ; Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. 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Libertador Bernardo O‘Higgins 1058, Santiago de Chile, Chile), HW(Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA), HX(The University of Alabama, Tuscaloosa, AL 35487, USA), HY(Max-Planck-Institut für extraterrestrische Physik, Gießenbachstr. 1, D-85748 Garching, Germany <ID system="ORCID">0000-0002-7150-9192</ID>), HZ(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany), IA(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0001-8684-2222</ID>), IB(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), IC(National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA <ID system="ORCID">0000-0002-1793-3689</ID>), ID(Unidad de Astronomía, Fac. Cs. Básicas, Universidad de Antofagasta, Avda. 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Charter St., Madison, WI 53726, USA <ID system="ORCID">0000-0003-4843-4185</ID>), IM(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuna Mackenna 4860, 782-0436 Macul, Santiago, Chile <ID system="ORCID">0000-0001-9850-9419</ID>), IN(CEA/Irfu, Universit e Paris-Saclay, F-91191 Gif-sur-Yvette, France), IO(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), IP(Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan <ID system="ORCID">0000-0002-1370-6964</ID>), IQ(Apache Point Observatory, P.O. 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Libertador Bernardo O‘Higgins 1058, Santiago de Chile, Chile), KB(Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brasil ; Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil), KC(Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK), KD(Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brasil ; Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil <ID system="ORCID">0000-0002-5640-6697</ID>), KE(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA <ID system="ORCID">0000-0002-3569-7421</ID>), KF(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA <ID system="ORCID">0000-0002-5042-5088</ID>), KG(Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA; Department of Astronomy and Astrophysics, Eberly College of Science, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA), KH(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, México <ID system="ORCID">0000-0002-0988-7491</ID>), KI(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), KJ(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), KK(Institute of Space Sciences (CSIC-IEEC), Carrer de Can Magrans S/N, Campus UAB, Barcelona, E-08193, Spain ; Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capita, 2-4, E-08034, Barcelona, Spain <ID system="ORCID">0000-0001-6359-2769</ID>), KL(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, People's Republic of China <ID system="ORCID">0000-0002-3073-5871</ID>), KM(Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA ; National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA <ID system="ORCID">0000-0003-1659-7035</ID>), KN(McDonald Observatory, The University of Texas at Austin, 1 University Station, Austin, TX 78712, USA <ID system="ORCID">0000-0003-0509-2656</ID>), KO(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309-0389, USA <ID system="ORCID">0000-0002-4594-9936</ID>), KP(Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark <ID system="ORCID">0000-0002-6137-903X</ID>), KQ(The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA), KR(Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA), KS(Brookhaven National Laboratory, Upton, NY 11973, USA), KT(School of Physics & Astronomy, University of Nottingham, Nottingham, NG7 2RD, UK), KU(National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA), KV(Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA), KW(Vanderbilt University, Department of Physics & Astronomy, 6301 Stevenson Center Ln., Nashville, TN 37235, USA <ID system="ORCID">0000-0002-9322-0314</ID>), KX(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218, USA), KY(Observatório Nacional, Rio de Janeiro, Brasil), KZ(Department of Physical Sciences, The Open University, Milton Keynes, MK7 6AA, UK), LA(Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa 277-8583, Japan <ID system="ORCID">0000-0002-3746-2853</ID>), LB(Vanderbilt University, Department of Physics & Astronomy, 6301 Stevenson Center Ln., Nashville, TN 37235, USA <ID system="ORCID">0000-0002-3481-9052</ID>), LC(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany <ID system="ORCID">0000-0001-6516-7459</ID>), LD(Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark; Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia ; School of Physics, University of New South Wales, NSW 2052, Australia <ID system="ORCID">0000-0002-4879-3519</ID>), LE(Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brasil ; Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil <ID system="ORCID">0000-0003-1772-0023</ID>), LF(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), LG(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309-0389, USA <ID system="ORCID">0000-0003-1479-3059</ID>), LH(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, México <ID system="ORCID">0000-0002-2011-4924</ID>), LI(Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA), LJ(ELTE Eötvös Loránd University, Gothard Astrophysical Observatory, Szombathely, Hungary), LK(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. 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Postal 20-364, México), MC(Brookhaven National Laboratory, Upton, NY 11973, USA), MD(Departamento de Astronomia, Casilla 160-C, Universidad de Concepcion, Concepcion, Chile), ME(Department of Astronomy, New Mexico State University, Box 30001, MSC 4500, Las Cruces NM 88003, USA), MF(Department of Physics, University of North Carolina Asheville, One University Heights, Asheville, NC 28804, USA; Department of Physical Sciences, The Open University, Milton Keynes, MK7 6AA, UK <ID system="ORCID">0000-0002-6047-1010</ID>), MG(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China), MH(National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA), MI(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, UK), MJ(Department of Astronomy, Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA; Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA), MK(University of California Observatories, University of California, Santa Cruz, Santa Cruz, CA 95064, USA <ID system="ORCID">0000-0003-1809-6920</ID>), ML(Department of Physics, Austin College, Sherman, TX 75090, USA), MM(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI 53726, USA), MN(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, UK), MO(Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK), MP(Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA), MQ(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0001-7113-1233</ID>), MR(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0003-2212-6045</ID>), MS(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, People's Republic of China), MT(Department of Physics and Astronomy, University of Kentucky, 505 Rose St., Lexington, KY, 40506-0055, USA <ID system="ORCID">0000-0003-1025-1711</ID>), MU(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, UK), MV(Department of Physics, Bridgewater College, 402 E. College St., Bridgewater, VA 22812 USA <ID system="ORCID">0000-0002-3576-4508</ID>), MW(CEA/Irfu, Universit e Paris-Saclay, F-91191 Gif-sur-Yvette, France), MX(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218, USA <ID system="ORCID">0000-0001-6100-6869</ID>), MY(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), MZ(CEA/Irfu, Universit e Paris-Saclay, F-91191 Gif-sur-Yvette, France), NA(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), NB(Department of Physics and Astronomy, University of Kentucky, 505 Rose St., Lexington, KY, 40506-0055, USA <ID system="ORCID">0000-0002-9808-3646</ID>), NC(Tsinghua Center for Astrophysics & Department of Physics, Tsinghua University, Beijing 100084, People's Republic of China), ND(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK; National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China), NE(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA), NF(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China), NG(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China <ID system="ORCID">0000-0002-4135-0977</ID>), NH(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA;), NI(Department of Astronomy, Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA <ID system="ORCID">0000-0002-7550-7151</ID>), NJ(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China <ID system="ORCID">0000-0002-6684-3997</ID>)
%B The Astrophysical Journal Supplement Series
%V 235
%D 2018
%8 April 1, 2018
%K atlases;  catalogs;  surveys
%U http://adsabs.harvard.edu/abs/2018ApJS..235...42A
%X The fourth generation of the Sloan Digital Sky Survey (SDSS-IV) has been 
in operation since 2014 July. This paper describes the second data 
release from this phase, and the 14th from SDSS overall (making this 
Data Release Fourteen or DR14). This release makes the data taken by 
SDSS-IV in its first two years of operation (2014-2016 July) 
public. Like all previous SDSS releases, DR14 is cumulative, including 
the most recent reductions and calibrations of all data taken by SDSS 
since the first phase began operations in 2000. New in DR14 is the first 
public release of data from the extended Baryon Oscillation 
Spectroscopic Survey; the first data from the second phase of the Apache 
Point Observatory (APO) Galactic Evolution Experiment (APOGEE-2), 
including stellar parameter estimates from an innovative data-driven 
machine-learning algorithm known as “The Cannon” and almost 
twice as many data cubes from the Mapping Nearby Galaxies at APO (MaNGA) 
survey as were in the previous release (N = 2812 in total). This paper 
describes the location and format of the publicly available data from 
the SDSS-IV surveys. We provide references to the important technical 
papers describing how these data have been taken (both targeting and 
observation details) and processed for scientific use. The SDSS web site 
(<A href="http://www.sdss.org">www.sdss.org</A>) has been updated for 
this release and provides links to data downloads, as well as tutorials 
and examples of data use. SDSS-IV is planning to continue to collect 
astronomical data until 2020 and will be followed by SDSS-V.
%3 10.3847/1538-4365/aa9e8a
%= eprint: arXiv:1707.09322
%@ 0067-0049

%0 Journal Article
%T Constraining the baryon-dark matter relative velocity with the large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies
%A Slepian, Zachary 
%A Eisenstein, Daniel J. 
%A Blazek, Jonathan A. 
%A Brownstein, Joel R. 
%A Chuang, Chia-Hsun 
%A Gil-Marín, Héctor 
%A Ho, Shirley 
%A Kitaura, Francisco-Shu 
%A McEwen, Joseph E. 
%A Percival, Will J. 
%A Ross, Ashley J. 
%A Rossi, Graziano 
%A Seo, Hee-Jong 
%A Slosar, Anže 
%A Vargas-Magaña, Mariana
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AC(Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA), AD(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AE(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AF(Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France), AG(Lawrence Berkeley National Lab, 1 Cyclotron Road, Berkeley, CA 94720, USA; McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; Department of Physics, University of California, Berkeley, CA 94720, USA), AH(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AI(Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA), AJ(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AK(Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA), AL(Department of Physics and Astronomy, Sejong University, Seoul 143-747, Korea), AM(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), AN(Brookhaven National Laboratory, Upton, NY 11973, USA), AO(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, Mexico 04510, Mexico)
%B Monthly Notices of the Royal Astronomical Society
%V 474
%D 2018
%8 February 1, 2018
%P 2109-2115
%K cosmological parameters;  cosmology: observations
%U http://adsabs.harvard.edu/abs/2018MNRAS.474.2109S
%X We search for a galaxy clustering bias due to a modulation of galaxy 
number with the baryon-dark matter relative velocity resulting from 
recombination-era physics. We find no detected signal and place the 
constraint b<SUB>v</SUB> < 0.01 on the relative velocity bias for the 
CMASS galaxies. This bias is an important potential systematic of baryon 
acoustic oscillation (BAO) method measurements of the cosmic distance 
scale using the two-point clustering. Our limit on the relative velocity 
bias indicates a systematic shift of no more than 0.3 per cent rms in 
the distance scale inferred from the BAO feature in the BOSS two-point 
clustering, well below the 1 per cent statistical error of this 
measurement. This constraint is the most stringent currently available 
and has important implications for the ability of upcoming large-scale 
structure surveys such as the Dark Energy Spectroscopic Instrument 
(DESI) to self-protect against the relative velocity as a possible 
systematic.
%3 10.1093/mnras/stx2723
%@ 0035-8711

%0 Journal Article
%T The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: first measurement of baryon acoustic oscillations between redshift 0.8 and 2.2
%A Ata, Metin 
%A Baumgarten, Falk 
%A Bautista, Julian 
%A Beutler, Florian 
%A Bizyaev, Dmitry 
%A Blanton, Michael R. 
%A Blazek, Jonathan A. 
%A Bolton, Adam S. 
%A Brinkmann, Jonathan 
%A Brownstein, Joel R. 
%A Burtin, Etienne 
%A Chuang, Chia-Hsun 
%A Comparat, Johan 
%A Dawson, Kyle S. 
%A de la Macorra, Axel 
%A Du, Wei 
%A du Mas des Bourboux, Hélion 
%A Eisenstein, Daniel J. 
%A Gil-Marín, Héctor 
%A Grabowski, Katie 
%A Guy, Julien 
%A Hand, Nick 
%A Ho, Shirley 
%A Hutchinson, Timothy A. 
%A Ivanov, Mikhail M. 
%A Kitaura, Francisco-Shu 
%A Kneib, Jean-Paul 
%A Laurent, Pierre 
%A Le Goff, Jean-Marc 
%A McEwen, Joseph E. 
%A Mueller, Eva-Maria 
%A Myers, Adam D. 
%A Newman, Jeffrey A. 
%A Palanque-Delabrouille, Nathalie 
%A Pan, Kaike 
%A Pâris, Isabelle 
%A Pellejero-Ibanez, Marcos 
%A Percival, Will J. 
%A Petitjean, Patrick 
%A Prada, Francisco 
%A Prakash, Abhishek 
%A Rodríguez-Torres, Sergio A. 
%A Ross, Ashley J. 
%A Rossi, Graziano 
%A Ruggeri, Rossana 
%A Sánchez, Ariel G. 
%A Satpathy, Siddharth 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Seo, Hee-Jong 
%A Slosar, Anže 
%A Streblyanska, Alina 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Vargas Magaña, Mariana 
%A Vivek, M. 
%A Wang, Yuting 
%A Yèche, Christophe 
%A Yu, Liang 
%A Zarrouk, Pauline 
%A Zhao, Cheng 
%A Zhao, Gong-Bo 
%A Zhu, Fangzhou
%+ AA(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AB(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Humboldt-Universität zu Berlin, Institut für Physik, Newtonstrasse 15, D-12589, Berlin, Germany), AC(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AD(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK <ID system="ORCID">0000-0003-0467-5438</ID>), AE(Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349, USA; Sternberg Astronomical Institute, Moscow State University, Universitetski pr. 13, 119992, Moscow, Russia), AF(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA), AG(Institute of Physics, Laboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland), AH(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA; National Optical Astronomy Observatory, 950 N Cherry Ave, Tucson, AZ 85719, USA), AI(Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), AJ(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AK(IRFU,CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), AL(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AM(Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstr., 85748 Garching bei München, Germany), AN(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AO(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México), AP(National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P. R. China), AQ(IRFU,CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), AR(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS #20, Cambridge, MA 02138, USA), AS(Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, 75014, Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, 75005, Paris, France), AT(Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), AU(LPNHE, CNRS/IN2P3, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris, 4 place Jussieu, 75252 Paris CEDEX, France), AV(Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720, USA), AW(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA; Berkeley Center for Cosmological Physics, LBL and Department of Physics, University of California, Berkeley, CA 94720, USA), AX(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AY(Institute of Physics, LPPC, École Polytechnique Fédérale de Lausanne (EPFL), CH-1015, Lausanne, Switzerland; Institute for Nuclear Research of the Russian Academy of Sciences, 60th October Anniversary Prospect, 7a, 117312, Moscow, Russia), AZ(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Dpto. Astrofísica, Universidad de La Laguna (ULL), E-38206, La Laguna, Tenerife, Spain), BA(Institute of Physics, Laboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland; Aix-Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), 38 rue F. Joliot-Curie 13388 Marseille Cedex 13, France), BB(IRFU,CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), BC(IRFU,CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), BD(Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA), BE(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), BF(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), BG(Department of Physics and Astronomy and the Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USA), BH(IRFU,CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), BI(Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), BJ(Aix-Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), 38 rue F. Joliot-Curie 13388 Marseille Cedex 13, France), BK(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Dpto. Astrofísica, Universidad de La Laguna (ULL), E-38206, La Laguna, Tenerife, Spain), BL(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), BM(Institut d'Astrophysique de Paris, Université Paris 6 et CNRS, 98bis Boulevard Arago, 75014, Paris, France), BN(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049, Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049, Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), E-18080, Granada, Spain), BO(Department of Physics and Astronomy and the Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USA), BP(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049, Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049, Madrid, Spain; Departamento de Física Teórica M8, Universidad Autónoma de Madrid, E-28049 Cantoblanco, Madrid, Spain), BQ(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK; Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA <ID system="ORCID">0000-0002-7522-9083</ID>), BR(Department of Physics and Astronomy, Sejong University, Seoul 143-747, Korea), BS(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), BT(Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstr., 85748 Garching bei München, Germany), BU(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), BV(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), BW(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), BX(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), BY(Brookhaven National Laboratory, Bldg 510, Upton, New York 11973, USA), BZ(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Dpto. Astrofísica, Universidad de La Laguna (ULL), E-38206, La Laguna, Tenerife, Spain), CA(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA), CB(School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS, UK <ID system="ORCID">0000-0001-5191-2286</ID>), CC(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México), CD(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), CE(National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P. R. China; Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), CF(IRFU,CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), CG(Tsinghua Center for Astrophysics and Department of Physics, Tsinghua University, Beijing 100084, China), CH(IRFU,CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), CI(Tsinghua Center for Astrophysics and Department of Physics, Tsinghua University, Beijing 100084, China), CJ(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P. R. China), CK(Department of Physics, Yale University, 260 Whitney Ave, New Haven, CT 06520, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 473
%D 2018
%8 February 1, 2018
%P 4773-4794
%K cosmology: observations;  dark energy;  distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2018MNRAS.473.4773A
%X We present measurements of the Baryon Acoustic Oscillation (BAO) scale 
in redshift-space using the clustering of quasars. We consider a sample 
of 147 000 quasars from the extended Baryon Oscillation Spectroscopic 
Survey (eBOSS) distributed over 2044 square degrees with redshifts 0.8 
< z < 2.2 and measure their spherically averaged clustering in 
both configuration and Fourier space. Our observational data set and the 
1400 simulated realizations of the data set allow us to detect a 
preference for BAO that is greater than 2.8σ. We determine the 
spherically averaged BAO distance to z = 1.52 to 3.8 per cent precision: 
D<SUB>V</SUB>(z = 1.52) = 3843 ± 147(r<SUB>d</SUB>/r<SUB>d, 
fid</SUB>)Mpc. This is the first time the location of the BAO feature 
has been measured between redshifts 1 and 2. Our result is fully 
consistent with the prediction obtained by extrapolating the Planck flat 
ΛCDM best-fitting cosmology. All of our results are consistent 
with basic large-scale structure (LSS) theory, confirming quasars to be 
a reliable tracer of LSS, and provide a starting point for numerous 
cosmological tests to be performed with eBOSS quasar samples. We combine 
our result with previous, independent, BAO distance measurements to 
construct an updated BAO distance-ladder. Using these BAO data alone and 
marginalizing over the length of the standard ruler, we find 
Ω<SUB>Λ</SUB> > 0 at 6.6σ significance when 
testing a ΛCDM model with free curvature.
%3 10.1093/mnras/stx2630
%= eprint: arXiv:1705.06373
%@ 0035-8711

%0 Conference Paper
%T Redshift Evolution of Non-Gaussianity in Cosmic Large-Scale Structure
%A Sullivan, James 
%A Wiegand, Alexander 
%A Eisenstein, Daniel
%+ AA(Harvard-Smithsonian Center for Astrophysics), AB(Harvard-Smithsonian Center for Astrophysics), AC(Harvard-Smithsonian Center for Astrophysics)
%B American Astronomical Society Meeting Abstracts #231
%V 231
%D 2018
%8 January 1, 2018
%U http://adsabs.harvard.edu/abs/2018AAS...23135101S
%X We probe the higher-order galaxy clustering in the final data release 
(DR12) of the Sloan Digital Sky Survey using germ-grain Minkowski 
Functionals (MFs). Our data selection contains 979,430 BOSS galaxies 
from both the northern and southern galactic caps over the redshift 
range 0.2 - 0.6. We extract the higher-order parts of the MFs and find 
deviations from the case without higher order MFs with chi-squared 
values of order 1000 for 24 degrees of freedom across the entire data 
selection. We show the MFs to be sensitive to contributions up to the 
five-point correlation function across the entire data selection. We 
measure significant redshift evolution in the higher-order functionals 
for the first time, with a percentage growth between redshift bins of 
approximately 20 % in both galactic caps. This is a nearly a factor of 2 
greater than similar growth in the two-point correlation function and 
will allow for tests of non-linear structure growth by comparing the 
three-point and higher-order parts to their expected theoretical values. 
The SAO REU program is funded by the National Science Foundation REU and 
Department of Defense ASSURE programs under NSF Grant AST-1659473, and 
by the Smithsonian Institution.