%0 Journal Article
%T Estimating covariance matrices for two- and three-point correlation function moments in Arbitrary Survey Geometries
%A Philcox, Oliver H. E.
%A Eisenstein, Daniel J.
%+ AA(Center for Astrophysics | Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA; Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA), AB(Center for Astrophysics | Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 490
%D 2019
%8 December 01, 2019
%P 5931-5951
%K methods: numerical; methods: statistical; galaxies: statistics;
Cosmology: theory; large-scale structure of Universe; Astrophysics -
Cosmology and Nongalactic Astrophysics; Astrophysics - Instrumentation
and Methods for Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.5931P
%X We present configuration-space estimators for the auto- and cross-
covariance of two- and three-point correlation functions (2PCF and 3PCF)
in general survey geometries. These are derived in the Gaussian limit
(setting higher order correlation functions to zero), but for arbitrary
non-linear 2PCFs (which may be estimated from the survey itself), with a
shot-noise rescaling parameter included to capture non-Gaussianity. We
generalize previous approaches to include Legendre moments via a
geometry-correction function calibrated from measured pair and triple
counts. Making use of importance sampling and random particle
catalogues, we can estimate model covariances in fractions of the time
required to do so with mocks, obtaining estimates with negligible
sampling noise in ̃10 (̃100) CPU-hours for the 2PCF (3PCF)
autocovariance. We compare results to sample covariances from a suite of
BOSS DR12 mocks and find the matrices to be in good agreement, assuming
a shot-noise rescaling parameter of 1.03 (1.20) for the 2PCF (3PCF). To
obtain strongest constraints on cosmological parameters, we must use
multiple statistics in concert; having robust methods to measure their
covariances at low computational cost is thus of great relevance to
upcoming surveys.
%3 10.1093/mnras/stz2896
%= eprint: arXiv:1910.04764
%@ 0035-8711

%0 Journal Article
%T Revealing the galaxy-halo connection in IllustrisTNG
%A Bose, Sownak
%A Eisenstein, Daniel J.
%A Hernquist, Lars
%A Pillepich, Annalisa
%A Nelson, Dylan
%A Marinacci, Federico
%A Springel, Volker
%A Vogelsberger, Mark
%+ AA(Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA), AB(Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA), AC(Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA), AD(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany), AE(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany), AF(Department of Physics & Astronomy, University of Bologna, via Gobetti 93/2, I-40129 Bologna, Italy), AG(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany), AH(Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 490
%D 2019
%8 December 01, 2019
%P 5693-5711
%K methods: numerical; galaxies: haloes; cosmology: theory; large-scale
structure of Universe; Astrophysics - Cosmology and Nongalactic
Astrophysics; Astrophysics - Astrophysics of Galaxies
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.5693B
%X We use the IllustrisTNG (TNG) simulations to explore the galaxy-halo
connection as inferred from state-of-the-art cosmological,
magnetohydrodynamical simulations. With the high-mass resolution and
large volume achieved by combining the 100 Mpc (TNG100) and 300 Mpc
(TNG300) volumes, we establish the mean occupancy of central and
satellite galaxies and their dependence on the properties of the dark
matter haloes hosting them. We derive best-fitting HOD parameters from
TNG100 and TNG300 for target galaxy number densities of \bar{n}_g =
0.032 and \bar{n}_g = 0.016 h^3 Mpc<SUP>-3</SUP>, respectively,
corresponding to a minimum galaxy stellar mass of M_\star ̃ 1.9× 10^9
and M_\star ̃ 3.5× 10^9 M_☉, respectively, in hosts more massive than
10^{11} M_☉. Consistent with previous work, we find that haloes located
in dense environments, with low concentrations, later formation times,
and high angular momenta are richest in their satellite population. At
low mass, highly concentrated haloes and those located in overdense
regions are more likely to contain a central galaxy. The degree of
environmental dependence is sensitive to the definition adopted for the
physical boundary of the host halo. We examine the extent to which
correlations between galaxy occupancy and halo properties are
independent and demonstrate that HODs predicted by halo mass and
present-day concentration capture the qualitative dependence on the
remaining halo properties. At fixed halo mass, concentration is a strong
predictor of the stellar mass of the central galaxy, which may play a
defining role in the fate of the satellite population. The radial
distribution of satellite galaxies, which exhibits a universal form
across a wide range of host halo mass, is described accurately by the
best-fitting NFW density profile of their host haloes.
%3 10.1093/mnras/stz2546
%= eprint: arXiv:1905.08799
%@ 0035-8711

%0 Journal Article
%T Galaxy-Galaxy lensing in HSC: Validation tests and the impact of heterogeneous spectroscopic training sets
%A Speagle, Joshua S.
%A Leauthaud, Alexie
%A Huang, Song
%A Bradshaw, Christopher P.
%A Ardila, Felipe
%A Capak, Peter L.
%A Eisenstein, Daniel J.
%A Masters, Daniel C.
%A Mandelbaum, Rachel
%A More, Surhud
%A Simet, Melanie
%A Sifón, Cristóbal
%+ AA(Department of Astronomy, Harvard University, 60 Garden St., MS 46, Cambridge, MA 02138, USA;), AB(Department of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95064, USA), AC(Department of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95064, USA), AD(Department of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95064, USA), AE(Department of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA 95064, USA), AF(IPAC, California Institute of Technology, Pasadena, CA 91125, USA), AG(Department of Astronomy, Harvard University, 60 Garden St., MS 46, Cambridge, MA 02138, USA), AH(IPAC, California Institute of Technology, Pasadena, CA 91125, USA), AI(McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA 15213, USA), AJ(Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), University of Tokyo, Chiba 277-8582, Japan; The Inter-University Center for Astronomy and Astrophysics, Post bag 4, Ganeshkhind, Pune 411007, India), AK(Department of Physics &amp; Astronomy, University of California, Riverside, 900 University Avenue, Riverside, CA 92521, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA), AL(Department of Astrophysical Sciences, Princeton University, Peyton Hall, 4 Ivy Ln, Princeton, NJ 08544, USA; Instituto de Física, Pontificia Universidad Católica de Valparaíso, Casilla 4059, Valparaíso, Chile)
%B Monthly Notices of the Royal Astronomical Society
%V 490
%D 2019
%8 December 01, 2019
%P 5658-5677
%K gravitational lensing: weak; methods: statistical; techniques:
photometric; galaxies: distances and redshifts; cosmology: observations;
Astrophysics - Cosmology and Nongalactic Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.5658S
%X Although photometric redshifts (photo-z's) are crucial ingredients for
current and upcoming large-scale surveys, the high-quality spectroscopic
redshifts currently available to train, validate, and test them are
substantially non-representative in both magnitude and colour. We
investigate the nature and structure of this bias by tracking how
objects from a heterogeneous training sample contribute to photo-z
predictions as a function of magnitude and colour, and illustrate that
the underlying redshift distribution at fixed colour can evolve strongly
as a function of magnitude. We then test the robustness of the galaxy-
galaxy lensing signal in 120 deg<SUP>2</SUP> of HSC-SSP DR1 data to
spectroscopic completeness and photo-z biases, and find that their
impacts are sub-dominant to current statistical uncertainties. Our
methodology provides a framework to investigate how spectroscopic
incompleteness can impact photo-z-based weak lensing predictions in
future surveys such as LSST and WFIRST.
%3 10.1093/mnras/stz2968
%= eprint: arXiv:1906.05876
%@ 0035-8711

%0 Journal Article
%T Tests of acoustic scale shifts in halo-based mock galaxy catalogues
%A Duan, Yutong
%A Eisenstein, Daniel
%+ AA(Physics Department, Boston University, 590 Commonwealth Ave, Boston, MA 02215, USA), AB(Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 490
%D 2019
%8 December 01, 2019
%P 2718-2731
%K methods: data analysis; galaxies: haloes; dark energy; dark matter;
distance scale; large-scale structure of Universe; Astrophysics -
Cosmology and Nongalactic Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.2718D
%X We utilize mock catalogues from high-accuracy cosmological N-body
simulations to quantify shifts in the recovery of the acoustic scale
that could potentially result from galaxy clustering bias. The
relationship between galaxies and dark matter haloes presents a
complicated source of systematic errors in modern redshift surveys,
particularly when aiming to make cosmological measurements to sub-per
cent precision. Apart from a scalar, linear bias parameter accounting
for the density contrast ratio between matter tracers and the true
matter distribution, other types of galaxy bias, such as assembly and
velocity biases, may also significantly alter clustering signals from
small to large scales. We create mocks based on generalized halo
occupation populations of 36 periodic boxes from the ABACUS
COSMOSrelease, and test various biased models along with an unbiased
base case in a total volume of 48 h^{-3} Gpc<SUP>3</SUP>. Two
reconstruction methods are applied to galaxy samples and the apparent
acoustic scale is derived by fitting the two-point correlation function
multipoles. With respect to the baseline, we find a 0.3 per cent shift
in the line-of-sight acoustic scale for one variation in the satellite
galaxy population, and we find a 0.7 per cent shift for an extreme level
of velocity bias of the central galaxies. All other bias models are
consistent with zero shift at the 0.2 per cent level after
reconstruction. We note that the bias models explored are relatively
large variations, producing sizeable and likely distinguishable changes
in small-scale clustering, the modelling of which would further
calibrate the baryon acoustic oscillations standard ruler.
%3 10.1093/mnras/stz2578
%= eprint: arXiv:1906.04262
%@ 0035-8711

%0 Journal Article
%T Large covariance matrices: accurate models without mocks
%A O'Connell, Ross
%A Eisenstein, Daniel J.
%+ AA(McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 487
%D 2019
%8 August 01, 2019
%P 2701-2717
%K methods: statistical; large-scale structure of Universe; Astrophysics
- Cosmology and Nongalactic Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.2701O
%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.
%3 10.1093/mnras/stz1359
%= eprint: arXiv:1808.05978
%@ 0035-8711

%0 Journal Article
%T Decorrelating the errors of the galaxy correlation function with compact transformation matrices
%A Yuan, Sihan
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 486
%D 2019
%8 June 01, 2019
%P 708-724
%K methods: analytical; galaxies: haloes; dark matter; large-scale
structure of Universe; Astrophysics - Cosmology and Nongalactic
Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.486..708Y
%X Covariance matrix estimation is a persistent challenge for cosmology,
often requiring a large number of synthetic mock catalogues. The off-
diagonal components of the covariance matrix also make it difficult to
show representative error bars on the 2-point correlation function
(2PCF) since errors computed from the diagonal values of the covariance
matrix greatly underestimate the uncertainties. We develop a routine for
decorrelating the projected and anisotropic 2PCF with simple and scale-
compact transformations on the 2PCF. These transformation matrices are
modelled after the Cholesky decomposition and the symmetric square root
of the Fisher matrix. Using mock catalogues, we show that the
transformed projected and anisotropic 2PCF recover the same structure as
the original 2PCF while producing largely decorrelated error bars.
Specifically, we propose simple Cholesky-based transformation matrices
that suppress the off-diagonal covariances on the projected 2PCF by {̃ }
95{{ per cent}} and that on the anisotropic 2PCF by {̃ } 87{{ per
cent}}. These transformations also serve as highly regularized models of
the Fisher matrix, compressing the degrees of freedom so that one can
fit for the Fisher matrix with a much smaller number of mocks.
%3 10.1093/mnras/stz899
%= eprint: arXiv:1901.05019
%@ 0035-8711

%0 Journal Article
%T The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Spectrographs
%A Wilson, J. C.
%A Hearty, F. R.
%A Skrutskie, M. F.
%A Majewski, S. R.
%A Holtzman, J. A.
%A Eisenstein, D.
%A Gunn, J.
%A Blank, B.
%A Henderson, C.
%A Smee, S.
%A Nelson, M.
%A Nidever, D.
%A Arns, J.
%A Barkhouser, R.
%A Barr, J.
%A Beland, S.
%A Bershady, M. A.
%A Blanton, M. R.
%A Brunner, S.
%A Burton, A.
%A Carey, L.
%A Carr, M.
%A Colque, J. P.
%A Crane, J.
%A Damke, G. J.
%A Davidson, J. W., Jr.
%A Dean, J.
%A Di Mille, F.
%A Don, K. W.
%A Ebelke, G.
%A Evans, M.
%A Fitzgerald, G.
%A Gillespie, B.
%A Hall, M.
%A Harding, A.
%A Harding, P.
%A Hammond, R.
%A Hancock, D.
%A Harrison, C.
%A Hope, S.
%A Horne, T.
%A Karakla, J.
%A Lam, C.
%A Leger, F.
%A MacDonald, N.
%A Maseman, P.
%A Matsunari, J.
%A Melton, S.
%A Mitcheltree, T.
%A O'Brien, T.
%A O'Connell, R. W.
%A Patten, A.
%A Richardson, W.
%A Rieke, G.
%A Rieke, M.
%A Roman-Lopes, A.
%A Schiavon, R. P.
%A Sobeck, J. S.
%A Stolberg, T.
%A Stoll, R.
%A Tembe, M.
%A Trujillo, J. D.
%A Uomoto, A.
%A Vernieri, M.
%A Walker, E.
%A Weinberg, D. H.
%A Young, E.
%A Anthony-Brumfield, B.
%A Bizyaev, D.
%A Breslauer, B.
%A De Lee, N.
%A Downey, J.
%A Halverson, S.
%A Huehnerhoff, J.
%A Klaene, M.
%A Leon, E.
%A Long, D.
%A Mahadevan, S.
%A Malanushenko, E.
%A Nguyen, D. C.
%A Owen, R.
%A Sánchez-Gallego, J. R.
%A Sayres, C.
%A Shane, N.
%A Shectman, S. A.
%A Shetrone, M.
%A Skinner, D.
%A Stauffer, F.
%A Zhao, B.
%+ AA(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), AB(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA), AC(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), AD(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), AE(Dept of Astronomy, New Mexico State Univ, P.O. Box 30001, MSC 4500, Las Cruces, NM 88003, USA), AF(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 20, Cambridge, MA 02138, USA), AG(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA), AH(PulseRay, 4583 State Route 414, Beaver Dams, NY 14812, USA), AI(PulseRay, 4583 State Route 414, Beaver Dams, NY 14812, USA), AJ(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), AK(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), AL(National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA), AM(Kaiser Optical Systems, Inc., 371 Parkland Plaza, Ann Arbor, MI 48103, USA), AN(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), AO(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), AP(Laboratory for Atmospheric and Space Physics, University of Colorado, 3665 Discovery Dr., Boulder, CO 80303, USA), AQ(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter Street, Madison, WI 53726, USA ; South African Astronomical Observatory, P.O. Box 9, Observatory 7935, Cape Town, South Africa), AR(Center for Cosmology and Particle Physics, Department of Physics, New York University, 726 Broadway Rm. 1005, New York, NY 10003, USA), AS(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), AT(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), AU(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), AV(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA), AW(Centro de Astronomía (CITEVA), Universidad de Antofagasta, Avenida Angamos 601, Antofagasta, Chile), AX(Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA), AY(AURA Observatory in Chile, Cisternas 1500, La Serena, Chile ; Centro Multidisciplinario de Ciencia y Tecnología, Universidad de La Serena, Cisternas 1200, La Serena, Chile ; Departamento de Física, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile), AZ(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), BA(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), BB(Las Campanas Observatory, Colina El Pino Casilla 601 La Serena, Chile), BC(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), BD(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), BE(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), BF(New England Optical Systems, Inc., 237 Cedar Hill St., Marlborough, MA 01752, USA), BG(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), BH(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), BI(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), BJ(Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106, USA), BK(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), BL(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), BM(C Technologies, 757 Route 202/206, Bridgewater, NJ 08807, USA), BN(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), BO(Meinel 733, College of Optical Sciences, Univ of Arizona, 1630 East Univ. Boulevard, Tucson, AZ 85721, USA), BP(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), BQ(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), BR(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), BS(University of California Observatories, UC Santa Cruz, 1156 High St., Santa Cruz, CA 95064, USA), BT(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), BU(THK America, Inc., 200 East Commerce Dr., Schaumburg, IL 60173, USA), BV(US Conec, Ltd., PO Box 2306, 1555 4th Avenue SE, Hickory, NC 28602, USA), BW(US Conec, Ltd., PO Box 2306, 1555 4th Avenue SE, Hickory, NC 28602, USA), BX(Department of Astronomy, Ohio State University, Columbus, OH 43210, USA), BY(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), BZ(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), CA(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), CB(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), CC(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), CD(Departamento de Física, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile), CE(Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool, L3 5RF, UK), CF(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), CG(New England Optical Systems, Inc., 237 Cedar Hill St., Marlborough, MA 01752, USA), CH(C Technologies, 757 Route 202/206, Bridgewater, NJ 08807, USA), CI(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), CJ(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), CK(Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA), CL(C Technologies, 757 Route 202/206, Bridgewater, NJ 08807, USA), CM(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), CN(Department of Astronomy, Ohio State University, Columbus, OH 43210, USA), CO(USRA, NASA Ames Research Center, Moffett Field, CA 94035, USA), CP(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), CQ(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA; Sternberg Astronomical Institute, Moscow State University, Moscow, Russia), CR(Astronomy Department, University of Virginia, Charlottesville, VA 22901, USA), CS(Department of Physics, Geology, and Engineering Tech, Northern Kentucky University, Highland Heights, KY 41099, USA ; Vanderbilt University, Department of Physics &amp; Astronomy, 6301 Stevenson Center Ln., Nashville, TN 37235, USA), CT(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), CU(MIT Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Avenue, 37-241, Cambridge, MA 02139, USA ;), CV(Hindsight Imaging, Inc., 1 Harvard St., Suite 302, Brookline, MA 02445, USA), CW(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), CX(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), CY(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), CZ(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA), DA(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), DB(Department of Computer Science, University of Illinois at Urbana-Champaign, Thomas M. Siebel Center for Computer Science, 201 North Goodwin Avenue, Urbana, IL 61801, USA), DC(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), DD(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), DE(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), DF(Lamont-Doherty Earth Observatory of Columbia University, 61 Route 9W, Palisades, NY 10960, USA), DG(Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA), DH(McDonald Observatory, University of Texas at Austin, Fort Davis, TX 79734, USA), DI(Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, 837 State Street, Atlanta, GA 30332, USA), DJ(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), DK(Dept of Astronomy, Univ of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA)
%B Publications of the Astronomical Society of the Pacific
%V 131
%D 2019
%8 May 01, 2019
%P 055001
%K Astrophysics - Instrumentation and Methods for Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019PASP..131e5001W
%X We describe the design and performance of the near-infrared (1.51-1.70
μm), fiber-fed, multi-object (300 fibers), high resolution (R = λ/∆λ ̃
22,500) spectrograph built for the Apache Point Observatory Galactic
Evolution Experiment (APOGEE). APOGEE is a survey of ̃10<SUP>5</SUP> red
giant stars that systematically sampled all Milky Way populations
(bulge, disk, and halo) to study the Galaxy’s chemical and kinematical
history. It was part of the Sloan Digital Sky Survey III (SDSS-III) from
2011 to 2014 using the 2.5 m Sloan Foundation Telescope at Apache Point
Observatory, New Mexico. The APOGEE-2 survey is now using the
spectrograph as part of SDSS-IV, as well as a second spectrograph, a
close copy of the first, operating at the 2.5 m du Pont Telescope at Las
Campanas Observatory in Chile. Although several fiber-fed, multi-object,
high resolution spectrographs have been built for visual wavelength
spectroscopy, the APOGEE spectrograph is one of the first such
instruments built for observations in the near-infrared. The
instrument’s successful development was enabled by several key
innovations, including a “gang connector” to allow simultaneous
connections of 300 fibers; hermetically sealed feedthroughs to allow
fibers to pass through the cryostat wall continuously; the first
cryogenically deployed mosaic volume phase holographic grating; and a
large refractive camera that includes mono-crystalline silicon and fused
silica elements with diameters as large as ̃400 mm. This paper contains
a comprehensive description of all aspects of the instrument including
the fiber system, optics and opto-mechanics, detector arrays, mechanics
and cryogenics, instrument control, calibration system, optical
performance and stability, lessons learned, and design changes for the
second instrument.
%3 10.1088/1538-3873/ab0075
%= eprint: arXiv:1902.00928
%@ 0004-6280

%0 Journal 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.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AC(Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85121, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 485
%D 2019
%8 May 01, 2019
%P 3370-3377
%K methods: numerical; large-scale structure of universe; Astrophysics -
Cosmology and Nongalactic Astrophysics; Astrophysics - Instrumentation
and Methods for Astrophysics; Physics - Computational Physics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.485.3370G
%X We present a high-fidelity realization of the cosmological N-body
simulation from the Schneider et al. code comparison project. The
simulation was performed with our ABACUSN-body code, which offers high-
force accuracy, high performance, and minimal particle integration
errors. The simulation consists of 2048<SUP>3</SUP> particles in a 500
h^{-1} Mpc box for a particle mass of 1.2× 10^9 h^{-1} M_\odot with 10
h^{-1} kpc spline softening. ABACUS executed 1052 global time-steps to z
= 0 in 107 h 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 PKDGRAV3 and less so with GADGET3. 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 {\lt }0.3{{ per cent}} errors at k\lt 10 Mpc^{-1} h. On
large scales, ABACUS reproduces linear theory better than 0.01 per cent.
Simulation snapshots are available at
http://nbody.rc.fas.harvard.edu/public/S2016.
%3 10.1093/mnras/stz634
%= eprint: arXiv:1810.02916
%@ 0035-8711

%0 Journal Article
%T Generating approximate halo catalogues for blind challenges in precision cosmology
%A Garrison, Lehman H.
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 485
%D 2019
%8 May 01, 2019
%P 2407-2416
%K methods: numerical; large-scale structure of Universe; Astrophysics -
Cosmology and Nongalactic Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.485.2407G
%X We present a method for generating suites of dark matter halo catalogues
with only a few N-body simulations, focusing on making small changes to
the underlying cosmology of a simulation with high precision. In the
context of blind challenges, this allows us to re-use a simulation by
giving it a new cosmology after the original cosmology is revealed.
Starting with full N-body realizations of an original cosmology and a
target cosmology, we fit a transfer function that displaces haloes in
the original so that the galaxy/HOD power spectrum matches that of the
target cosmology. This measured transfer function can then be applied to
a new realization of the original cosmology to create a new realization
of the target cosmology. For a 1 per cent change in σ<SUB>8</SUB>, we
achieve 0.1 per cent accuracy to k = 1 h Mpc^{-1} in the real-space
power spectrum; this degrades to 0.3 per cent when the transfer function
is applied to a new realization. We achieve similar accuracy in the
redshift-space monopole and quadrupole. In all cases, the result is
better than the sample variance of our 1.1 h^{-1} Gpc simulation boxes.
%3 10.1093/mnras/stz600
%= eprint: arXiv:1902.09475
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: evolution of higher-order correlations demonstrated with Minkowski functionals
%A Sullivan, James M.
%A Wiegand, Alexander
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA; University of Texas at Austin, 110 Inner Campus Dr, Austin, TX 78705, USA; Department of Astronomy, University of California, Berkeley, CA 94720, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 485
%D 2019
%8 May 01, 2019
%P 1708-1719
%K methods: data analysis; methods: statistical; large-scale structure
of Universe; cosmology: observations
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.485.1708S
%X We probe the higher-order galaxy clustering in the final data release of
the Sloan Digital Sky Survey Baryon Oscillation Spectroscopic Survey
(BOSS) 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 z = 0.2-0.6. We extract the
higher-order part of the MFs, detecting the deviation from the purely
Gaussian case with χ ^2 ̃ O(10^3) on 24 degrees of freedom across the
entire data selection. We measure significant redshift evolution in the
higher-order functionals for the first time. We find 15-35{{ per cent}}
growth, depending on functional and scale, between our redshift bins
centred at z = 0.325 and z = 0.525. We show that the structure in
higher-order correlations grows faster than that in the two-point
correlations, especially on small scales where the excess approaches a
factor of 2. We demonstrate how this trend is generalizable by finding
good agreement of the data with a hierarchical model in which the higher
orders grow faster than the lower-order correlations. We find that the
non-Gaussianity of the underlying dark matter field grows even faster
than the one of the galaxies. Our method can be adapted to study the
redshift evolution of the three-point and higher functions individually.
%3 10.1093/mnras/stz498
%@ 0035-8711

%0 Journal 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.
%+ AA(Center for Astrophysics ∣ Harvard &amp; Smithsonian, Cambridge, MA 02138, USA ; Harvard Data Science Initiative, Harvard University, Cambridge, MA 02138, USA;), AB(Smithsonian Astrophysical Observatory, Cambridge, MA 02138, USA), AC(Center for Astrophysics ∣ Harvard &amp; Smithsonian, Cambridge, MA 02138, USA), AD(Department of Physics, Yale University, New Haven, CT 06520, USA), AE(Center for Astrophysics ∣ Harvard &amp; Smithsonian, Cambridge, MA 02138, USA; Space Research Institute (IKI), Profsoyuznaya 84/32, Moscow, Russia), AF(Center for Astrophysics ∣ Harvard &amp; Smithsonian, Cambridge, MA 02138, USA), AG(Center for Astrophysics ∣ Harvard &amp; Smithsonian, Cambridge, MA 02138, USA), AH(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85741, Garching bei München, Germany), AI(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85741, Garching bei München, Germany), AJ(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117, Heidelberg, Germany), AK(Department of Astronomy, University of Florida, 211 Bryant Space Sciences Center, Gainesville, FL 32611, USA), AL(Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA)
%B The Astrophysical Journal
%V 876
%D 2019
%8 May 01, 2019
%K galaxies: clusters: general; methods: statistical; X-rays: galaxies:
clusters; Astrophysics - Cosmology and Nongalactic Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019ApJ...876...82N
%X We present a machine-learning (ML) approach for estimating galaxy
cluster masses from Chandra mock images. We utilize a Convolutional
Neural Network (CNN), a deep ML tool commonly used in image recognition
tasks. The CNN is trained and tested on our sample of 7896 Chandra X-ray
mock observations, which are based on 329 massive clusters from the
{\text{}}{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.
%3 10.3847/1538-4357/ab14eb
%= eprint: arXiv:1810.07703
%@ 0004-637X

%0 Journal 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, Stéphanie
%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 Yèche, Christophe
%A Zou, 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 Briceño, César
%A Buckley-Geer, 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, Timothée
%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 Gänsicke, 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 Huang, Lijuan Wendy
%A James, David J.
%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 R.
%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, Robert
%A Martínez-Vázquez, C. E.
%A Martini, Paul
%A du Mas des Bourboux, Hélion
%A McManus, Sean
%A Meier, Tobias Gabriel
%A Ménard, Brice
%A Metcalfe, Nigel
%A Muñoz-Gutiérrez, 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 Sánchez, 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-Magaña, 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
%+ AA(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), AB(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AC(Dunlap Institute, University of Toronto, Toronto, ON M5S 3H4, Canada ; Perimeter Institute for Theoretical Physics, Waterloo, ON N2L 2Y5, Canada ; Department of Astronomy &amp; Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada), AD(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA; LSST, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), AE(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AF(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), AG(Department of Physics &amp; Astronomy, University of Wyoming, 1000 E. University, Department 3905, Laramie, WY 8207, USA), AH(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AI(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), AJ(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), AK(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AL(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AM(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), AN(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AO(Department of Physics &amp; Astronomy, University of Wyoming, 1000 E. University, Department 3905, Laramie, WY 8207, USA), AP(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA), AQ(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AR(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), AS(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AT(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), AU(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), AV(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), AW(IRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), AX(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China), AY(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China), AZ(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), BA(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), BB(Department of Physics and Astronomy, University of California, Irvine, Irvine, CA 92697, USA), BC(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), BD(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK), BE(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), BF(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), BG(Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA), BH(Centre for Extragalactic Astronomy, Durham University, South Road, Durham, DH1 3LE, UK), BI(Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France), BJ(Department of Physics, University of California at Berkeley, Berkeley, CA 94720, USA), BK(Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI 48109, USA), BL(Department of Physics and Astronomy, University of Rochester, 500 Wilson Boulevard, Rochester, NY 14627, USA), BM(Institute of Cosmology &amp; Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UK), BN(Centre for Extragalactic Astronomy, Durham University, South Road, Durham, DH1 3LE, UK), BO(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), BP(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), BQ(Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA), BR(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), BS(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), BT(Department of Astronomy &amp; Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada), BU(Institute of Cosmology &amp; Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), BV(Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain ; Institut d'Estudis Espacials de Catalunya (IEEC), E-08193 Barcelona, Spain), BW(Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain ; Institut d'Estudis Espacials de Catalunya (IEEC), E-08193 Barcelona, Spain), BX(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA; Department of Physics, Montana State University, P.O. Box 173840, Bozeman, MT 59717-3840, USA), BY(Max-Planck Institut fur extraterrestrische Physik, Postfach 1312, D-85741 Garching bei Munchen, Germany), BZ(Department of Physics, University of Warwick, Coventry CV4 7AL, UK), CA(Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland), CB(Bentley School, 1000 Upper Happy Valley Road, Lafayette, CA 94549, USA), CC(University High School, 421 N Arcadia Avenue, Tucson, AZ 85711, USA), CD(Department of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75205, USA), CE(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), CF(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), CG(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), CH(Boston University Physics Department, 590 Commonwealth Avenue, Boston, MA 02215, USA), CI(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), CJ(Department of Physics &amp; Astronomy, University of Wyoming, 1000 E. University, Department 3905, Laramie, WY 8207, USA), CK(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), CL(IRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), CM(Department of Physics, University of California, Berkeley, Berkeley, CA 94720, USA), CN(Department of Physics and Astronomy, University College London, London WC1E 6BT, UK), CO(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), CP(Department of Physics and Astronomy, University College London, London WC1E 6BT, UK), CQ(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), CR(Department of Physics, University of Warwick, Coventry CV4 7AL, UK), CS(Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain ; Institut d'Estudis Espacials de Catalunya (IEEC), E-08193 Barcelona, Spain), CT(Indian Institute of Astrophysics, Koramangala II Block, Bangalore, India), CU(Department of Physics, University of Michigan, 450 Church Street, Ann Arbor, MI 48109, USA), CV(Department of Physics and Astronomy, University College London, London WC1E 6BT, UK), CW(Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland), CX(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), CY(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), CZ(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), DA(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), DB(Department of Physics, Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USA), DC(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), DD(Center for Astrophysics Harvard &amp; Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA ; Black Hole Initiative at Harvard University, 20 Garden Street, Cambridge, MA 02138, USA), DE(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), DF(Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People's Republic of China), DG(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), DH(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), DI(Sorbonne Université, Université Paris-Diderot, CNRS-IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies, LPNHE, F-75005 Paris, France), DJ(Department of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75205, USA), DK(Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland; Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, F-13388, Marseille, France), DL(Department of Physics &amp; Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019, USA), DM(Kavli IPMU, The University of Tokyo (WPI), Kashiwa 277-8583, Japan), DN(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), DO(Sorbonne Université, Université Paris-Diderot, CNRS-IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies, LPNHE, F-75005 Paris, France), DP(Aix Marseille University, CNRS, Institut Pytheas-Observatoire Haute Provence, F-04870 St-Michel-l'Observatoire, France), DQ(Physics Department, Harvard University, Cambridge, MA 02138, USA), DR(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), DS(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA, USA), DT(Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA), DU(Department of Physics and Astronomy, University of Kansas, 1251 Wescoe Hall Drive, Room 1082, Lawrence, KS 66045, USA), DV(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), DW(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), DX(Department of Astronomy and Center for Cosmology and Astroparticle Physics, The Ohio State University, Columbus, OH 43210, USA), DY(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA), DZ(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), EA(Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland), EB(Johns Hopkins University, Department of Physics &amp; Astronomy, 3400 N. Charles Street, Baltimore, MD 21218, USA), EC(Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France), ED(Instituto de Física, Universidad Nacional Autónoma de México, A.P. 20-364, 04510 Ciudad de México, México), EE(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), EF(Department of Physics, University of Michigan, 450 Church Street, Ann Arbor, MI 48109, USA), EG(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), EH(Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USA), EI(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China), EJ(Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA; Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA), EK(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), EL(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), EM(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), EN(IRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France), EO(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China), EP(Space Sciences Lab, UC Berkeley, Berkeley, CA 94720, USA), EQ(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA), ER(Infrared Processing and Analysis Center (IPAC), California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA), ES(Yale University Physics Department, P.O. Box 2018120, New Haven, CT 06520-8120, USA), ET(Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland), EU(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), EV(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), EW(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), EX(Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA), EY(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK), EZ(Department of Physics and Astronomy, University of Kansas, 1251 Wescoe Hall Drive, Room 1082, Lawrence, KS 66045, USA), FA(Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94550, USA), FB(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FC(Department of Physics and Astronomy, University of California, Irvine, Irvine, CA 92697, USA), FD(Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland), FE(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FF(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FG(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), FH(Shanghai Astronomical Observatory (SHAO), Nandan Road 80, Shanghai 200030, People's Republic of China ; Argelander-Institut für Astronomie, Auf dem Hügel 71, D-53121 Bonn, Germany), FI(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FJ(Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611-2055, USA), FK(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FL(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FM(Department of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75205, USA), FN(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA), FO(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FP(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FQ(Department of Astronomy and Center for Cosmology and Astroparticle Physics, The Ohio State University, Columbus, OH 43210, USA), FR(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), FS(Instituto de Física, Universidad Nacional Autónoma de México, A.P. 20-364, 04510 Ciudad de México, México), FT(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), FU(Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, Stanford, CA 94305, USA ; Department of Particle Physics and Astrophysics, SLAC National Accelerator Laboratory, Stanford, CA 94305, USA), FV(National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719, USA), FW(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), FX(Department of Astronomy, School of Physics, Peking University, Beijing 100871, People's Republic of China), FY(Department of Physics and Astronomy, University of Rochester, 500 Wilson Boulevard, Rochester, NY 14627, USA), FZ(Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA), GA(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), GB(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), GC(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China), GD(Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USA), GE(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China)
%B The Astronomical Journal
%V 157
%D 2019
%8 May 01, 2019
%K catalogs; surveys; Astrophysics - Instrumentation and Methods for
Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019AJ....157..168D
%X The DESI Legacy Imaging Surveys (<A
href="http://legacysurvey.org/">http://legacysurvey.org/</A>) 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 ≈14,000 deg<SUP>2</SUP> 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 μm) observed by the Wide-field Infrared Survey Explorer
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.
%3 10.3847/1538-3881/ab089d
%= eprint: arXiv:1804.08657
%@ 0004-6256

%0 Journal Article
%T Testing the Detection Significance on the Large-scale Structure by a JWST Deep Field Survey
%A Zhang, Hao
%A Eisenstein, Daniel J.
%A Garrison, Lehman H.
%A Ferrer, Douglas W.
%+ AA(Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 02138, USA ; School of Physics, Peking University, Beijing 100871, People's Republic of China), AB(Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 02138, USA), AC(Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 02138, USA), AD(Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 02138, USA)
%B The Astrophysical Journal
%V 875
%D 2019
%8 April 01, 2019
%K cosmology: theory; galaxies: high-redshift; galaxies: statistics;
large-scale structure of universe
%U https://ui.adsabs.harvard.edu/abs/2019ApJ...875..132Z
%X In preparation for deep extragalactic imaging with the James Webb Space
Telescope, we explore the clustering of massive halos at z = 8 and 10
using a large N-body simulation. We find that halos with masses of
10<SUP>9</SUP>-10<SUP>11</SUP> h <SUP>-1</SUP> M <SUB>☉</SUB>, which are
those expected to host galaxies detectable with JWST, are highly
clustered with bias factors ranging from 5 to 30 depending strongly on
mass, as well as on redshift and scale. This results in correlation
lengths of 5-10 h <SUP>-1</SUP> Mpc, similar to those of today’s
galaxies. Our results are based on a simulation of 130 billion particles
in a box of size 250 h <SUP>-1</SUP> Mpc using our new high-accuracy
ABACUS simulation code, the corrections to cosmological initial
conditions of Garrison et al., and the Planck 2015 cosmology. We use
variations between sub-volumes to estimate the detectability of the
clustering. Because of the very strong interhalo clustering, we find
that a medium-sized survey with a transverse size of the order of 25 h
<SUP>-1</SUP> comoving Mpc (about 13′) may be able to detect the
clustering of z = 8-10 galaxies with only 500-1000 survey objects if the
galaxies indeed occupy the most massive dark matter halos.
%3 10.3847/1538-4357/ab1268
%@ 0004-637X

%0 Journal Article
%T Emulating galaxy clustering and galaxy-galaxy lensing into the deeply non-linear regime: methodology, information, and forecasts
%A Wibking, Benjamin D.
%A Salcedo, Andrés N.
%A Weinberg, David H.
%A Garrison, Lehman H.
%A Ferrer, Douglas
%A Tinker, Jeremy
%A Eisenstein, Daniel
%A Metchnik, Marc
%A Pinto, Philip
%+ AA(Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, 140 W 18th Ave, Columbus, OH, USA 43210), AB(Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, 140 W 18th Ave, Columbus, OH, USA 43210), AC(Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, 140 W 18th Ave, Columbus, OH, USA 43210), AD(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS-10, Cambridge, MA 02138, USA), AE(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS-10, Cambridge, MA 02138, USA), AF(Center for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AG(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS-10, Cambridge, MA 02138, USA), AH(Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85121, USA), AI(Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85121, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 484
%D 2019
%8 March 01, 2019
%P 989-1006
%K gravitational lensing: weak; cosmological parameters; arge-scale
structure of Universe; Astrophysics - Cosmology and Nongalactic
Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.484..989W
%X The combination of galaxy-galaxy lensing (GGL) with galaxy clustering is
one of the most promising routes to determining the amplitude of matter
clustering at low redshifts. We show that extending clustering+GGL
analyses from the linear regime down to {̃ } 0.5 h^{-1} Mpc scales
increases their constraining power considerably, even after
marginalizing over a flexible model of non-linear galaxy bias. Using a
grid of cosmological N-body simulations, we construct a Taylor-expansion
emulator that predicts the galaxy autocorrelation ξ<SUB>gg</SUB>(r) and
galaxy-matter cross-correlation ξ<SUB>gm</SUB>(r) as a function of
σ<SUB>8</SUB>, Ω<SUB>m</SUB>, and halo occupation distribution (HOD)
parameters, which are allowed to vary with large-scale environment to
represent possible effects of galaxy assembly bias. We present forecasts
for a fiducial case that corresponds to BOSS LOWZ galaxy clustering and
SDSS-depth weak lensing (effective source density ̃0.3
arcmin<SUP>-2</SUP>). Using tangential shear and projected correlation
function measurements over 0.5 ≤ r_ p ≤ 30 h^{-1} Mpc yields a 2 per
cent constraint on the parameter combination σ _8Ω _ m^{0.6}, a factor
of two better than a constraint that excludes non-linear scales (r_ p
&gt; 2 h^{-1} Mpc, 4 h^{-1} Mpc for γ<SUB>t</SUB>, w<SUB>p</SUB>). Much
of this improvement comes from the non-linear clustering information,
which breaks degeneracies among HOD parameters. Increasing the effective
source density to 3 arcmin<SUP>-2</SUP> sharpens the constraint on σ _8Ω
_ m^{0.6} by a further factor of two. With robust modelling into the
non-linear regime, low-redshift measurements of matter clustering at the
1-per cent level with clustering+GGL alone are well within reach of
current data sets such as those provided by the Dark Energy Survey.
%3 10.1093/mnras/sty2258
%= eprint: arXiv:1709.07099
%@ 0035-8711

%0 Journal Article
%T Application of the iterative reconstruction to simulated galaxy 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), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 482
%D 2019
%8 February 01, 2019
%P 5685-5693
%K galaxies: haloes; dark matter; distance scale; large-scale structure
of Universe; Astrophysics - Cosmology and Nongalactic Astrophysics
%U https://ui.adsabs.harvard.edu/abs/2019MNRAS.482.5685H
%X We apply an iterative reconstruction method to galaxy mocks in redshift
space obtained from N-body simulations. Comparing the two-point
correlation functions for the reconstructed density field, we find that
although the performance is limited by shot noise and galaxy bias
compared to the matter field, the iterative method can still reconstruct
the initial linear density field from the galaxy field better than the
standard method both in real and in redshift space. Furthermore, the
iterative method is able to reconstruct both the monopole and quadrupole
more precisely, unlike the standard method. We see that as the number
density of galaxies gets smaller, the performance of reconstruction gets
worse due to the sparseness. However, the precision in the determination
of bias ({̃ }20{{ per cent}}) hardly impacts on the reconstruction
processes.
%3 10.1093/mnras/sty3137
%= eprint: arXiv:1810.05026
%@ 0035-8711