%0 Journal Article
%T Large covariance matrices: smooth models from the two-point correlation function
%A O'Connell, Ross 
%A Eisenstein, Daniel 
%A Vargas, Mariana 
%A Ho, Shirley 
%A Padmanabhan, Nikhil
%+ AA(McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA <EMAIL>rcoconne@andrew.cmu.edu</EMAIL>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AC(Instituto de Física, Universidad Nacional Autnoma de México, Apdo. Postal 20-364, México), AD(McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), AE(Department of Physics, Yale University, New Haven, CT 06511, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 462
%D 2016
%8 November 1, 2016
%P 2681-2694
%K large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.462.2681O
%X We introduce a new method for estimating the covariance matrix for the 
galaxy correlation function in surveys of large-scale structure. Our 
method combines simple theoretical results with a realistic 
characterization of the survey to dramatically reduce noise in the 
covariance matrix. For example, with an investment of only ≈1000 CPU 
hours we can produce a model covariance matrix with noise levels that 
would otherwise require ˜35 000 mocks. Non-Gaussian contributions 
to the model are calibrated against mock catalogues, after which the 
model covariance is found to be in impressive agreement with the mock 
covariance matrix. Since calibration of this method requires fewer mocks 
than brute force approaches, we believe that it could dramatically 
reduce the number of mocks required to analyse future surveys.
%3 10.1093/mnras/stw1821
%= eprint: arXiv:1510.01740
%@ 0035-8711

%0 Journal Article
%T Building a better understanding of the massive high-redshift BOSS CMASS galaxies as tools for cosmology
%A Favole, Ginevra 
%A McBride, Cameron K. 
%A Eisenstein, Daniel J. 
%A Prada, Francisco 
%A Swanson, Molly E. 
%A Chuang, Chia-Hsun 
%A Schneider, Donald P.
%+ AA(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 <EMAIL>g.favole@csic.es</EMAIL>), AB(Center for Astrophysics, Harvard University, 60 Garden Street, Cambridge, MA 02138, USA), AC(Center for Astrophysics, Harvard University, 60 Garden Street, Cambridge, MA 02138, USA), AD(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), Granada E-18008, Spain), AE(Center for Astrophysics, Harvard University, 60 Garden Street, Cambridge, MA 02138, USA), AF(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), AG(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)
%B Monthly Notices of the Royal Astronomical Society
%V 462
%D 2016
%8 October 1, 2016
%P 2218-2236
%K galaxies: distances and redshifts;  galaxies: haloes;  galaxies: statistics;  cosmology: observations;  cosmology: theory;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.462.2218F
%X We explore the massive bluer star-forming population of the Sloan 
Digital Sky Survey (SDSS) III/BOSS CMASS DR11 galaxies at z > 0.55 to 
quantify their differences, in terms of redshift-space distortions and 
large-scale bias, with respect to the luminous red galaxy sample. We 
perform a qualitative analysis to understand the significance of these 
differences and whether we can model and reproduce them in mock 
catalogues. Specifically, we measure galaxy clustering in CMASS on small 
and intermediate scales (0.1 ≲ r ≲ 50 h<SUP>-1</SUP> Mpc) by 
computing the two-point correlation function - both projected and 
redshift-space - of these galaxies, and a new statistic, Σ(π), 
able to separate the coherent and dispersed redshift-space distortion 
contributions and the large-scale bias. We interpret our clustering 
measurements by adopting a Halo Occupation Distribution (HOD) scheme 
that maps them on to high-resolution N-body cosmological simulations to 
produce suitable mock galaxy catalogues. The traditional HOD 
prescription can be applied to the red and the blue samples, 
independently, but this approach is unphysical since it allows the same 
mock galaxies to be either red or blue. To overcome this ambiguity, we 
modify the standard formulation and infer the red and the blue models by 
splitting the full mock catalogue into two complementary and 
non-overlapping submocks. This separation is performed by constraining 
the HOD with the observed CMASS red and blue galaxy fractions and 
produces reliable and accurate models.
%3 10.1093/mnras/stw1801
%= eprint: arXiv:1506.02044
%@ 0035-8711

%0 Journal Article
%T Improving initial conditions for cosmological N-body simulations
%A Garrison, Lehman H. 
%A Eisenstein, Daniel J. 
%A Ferrer, Douglas 
%A Metchnik, Marc V. 
%A Pinto, Philip A.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA <EMAIL>lgarrison@cfa.harvard.edu</EMAIL>), 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(Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85121, USA), AE(Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85121, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 461
%D 2016
%8 October 1, 2016
%P 4125-4145
%K methods: numerical;  galaxies: haloes;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.461.4125G
%X In cosmological N-body simulations, the representation of dark matter as 
discrete `macroparticles' suppresses the growth of structure, such that 
simulations no longer reproduce linear theory on small scales near 
k<SUB>Nyquist</SUB>. Marcos et al. demonstrate that this is due to 
sparse sampling of modes near k<SUB>Nyquist</SUB> and that the 
often-assumed continuum growing modes are not proper growing modes of 
the particle system. We develop initial conditions (ICs) that respect 
the particle linear theory growing modes and then rescale the mode 
amplitudes to account for growth suppression. These ICs also allow us to 
take advantage of our very accurate N-body code ABACUS to implement 
second-order Lagrangian perturbation theory (2LPT) in configuration 
space. The combination of 2LPT and rescaling improves the accuracy of 
the late-time power spectra, halo mass functions, and halo clustering. 
In particular, we achieve 1 per cent accuracy in the power spectrum down 
to k<SUB>Nyquist</SUB>, versus k<SUB>Nyquist</SUB>/4 without rescaling 
or k<SUB>Nyquist</SUB>/13 without 2LPT, relative to an oversampled 
reference simulation. We anticipate that our 2LPT will be useful for 
large simulations where fast Fourier transforms are expensive and that 
rescaling will be useful for suites of medium-resolution simulations 
used in cosmic emulators and galaxy survey mock catalogues. Code to 
generate ICs is available at https://github.com/lgarrison/zeldovich-PLT.
%3 10.1093/mnras/stw1594
%= eprint: arXiv:1605.02333
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering
%A Chuang, Chia-Hsun 
%A Prada, Francisco 
%A Pellejero-Ibanez, Marcos 
%A Beutler, Florian 
%A Cuesta, Antonio J. 
%A Eisenstein, Daniel J. 
%A Escoffier, Stephanie 
%A Ho, Shirley 
%A Kitaura, Francisco-Shu 
%A Kneib, Jean-Paul 
%A Manera, Marc 
%A Nuza, Sebastián E. 
%A Rodríguez-Torres, Sergio 
%A Ross, Ashley 
%A Rubiño-Martín, J. A. 
%A Samushia, Lado 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Wang, Yuting 
%A Weaver, Benjamin A. 
%A Zhao, Gongbo 
%A Brownstein, Joel R. 
%A Dawson, Kyle S. 
%A Maraston, Claudia 
%A Olmstead, Matthew D. 
%A Thomas, Daniel
%+ AA(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), AB(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), Glorieta de la Astronomía, E-18080 Granada, Spain), AC(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200 La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AD(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AE(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AF(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AG(CPPM, Aix-Marseille Université, CNRS/IN2P3, F-13288 Marseille, France), AH(Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), AI(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AJ(Laboratoire d'astrophysique, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland; Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, F-13388 Marseille, France), AK(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK), AL(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AM(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 Autonoma de Madrid (UAM), Cantoblanco, E-28049 Madrid, Spain), AN( Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA), AO(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200 La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AP(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Kansas State University, Manhattan, KS 66506, USA; National Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Ave., GE-1060 Tbilisi, Georgia), AQ(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AR(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), AS(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R.China), AT(Center for Cosmology and Particle Physics, New York University, New York, NY 10003, USA), AU(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R.China), AV(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AW(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AX(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AY(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AZ(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK)
%B Monthly Notices of the Royal Astronomical Society
%V 461
%D 2016
%8 October 1, 2016
%P 3781-3793
%K cosmological parameters;  cosmology: observations;  distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.461.3781C
%X With the largest spectroscopic galaxy survey volume drawn from the 
SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS), we can extract 
cosmological constraints from the measurements of redshift and geometric 
distortions at quasi-linear scales (e.g. above 50 h<SUP>-1</SUP> Mpc). 
We analyse the broad-range shape of the monopole and quadrupole 
correlation functions of the BOSS Data Release 12 (DR12) CMASS galaxy 
sample, at the effective redshift z = 0.59, to obtain constraints on the 
Hubble expansion rate H(z), the angular- diameter distance 
D<SUB>A</SUB>(z), the normalized growth rate f(z)σ<SUB>8</SUB>(z), 
and the physical matter density Ω<SUB>m</SUB> h<SUP>2</SUP>. We 
obtain robust measurements by including a polynomial as the model for 
the systematic errors, and find it works very well against the 
systematic effects, e.g. ones induced by stars and seeing. We provide 
accurate measurements 
{D<SUB>A</SUB>(0.59)r<SUB>s,fid</SUB>/r<SUB>s</SUB>, 
H(0.59)r<SUB>s</SUB>/r<SUB>s,fid</SUB>, 
f(0.59)σ<SUB>8</SUB>(0.59), Ω<SUB>m</SUB> h<SUP>2</SUP>} = 
{1427 ± 26 Mpc, 97.3 ± 3.3 km s<SUP>-1</SUP> 
Mpc<SUP>-1</SUP>, 0.488 ± 0.060, 0.135 ± 0.016}, where 
r<SUB>s</SUB> is the comoving sound horizon at the drag epoch and 
r<SUB>s,fid</SUB> = 147.66 Mpc is the sound scale of the fiducial 
cosmology used in this study. The parameters which are not well 
constrained by our galaxy clustering analysis are marginalized over with 
wide flat priors. Since no priors from other data sets, e.g. cosmic 
microwave background (CMB), are adopted and no dark energy models are 
assumed, our results from BOSS CMASS galaxy clustering alone may be 
combined with other data sets, i.e. CMB, SNe, lensing or other galaxy 
clustering data to constrain the parameters of a given cosmological 
model. The uncertainty on the dark energy equation of state parameter, 
w, from CMB+CMASS is about 8 per cent. The uncertainty on the curvature 
fraction, Ω<SUB>k</SUB>, is 0.3 per cent. We do not find deviation 
from flat ΛCDM.
%3 10.1093/mnras/stw1535
%= eprint: arXiv:1312.4889
%@ 0035-8711

%0 Journal Article
%T Exploring photometric redshifts as an optimization problem: an ensemble MCMC and simulated annealing-driven template-fitting approach
%A Speagle, Joshua S. 
%A Capak, Peter L. 
%A Eisenstein, Daniel J. 
%A Masters, Daniel C. 
%A Steinhardt, Charles L.
%+ AA(Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwanoha 5-1-5, Kashiwa, Chiba 277-8583, Japan; Harvard University Department of Astronomy, 60 Garden St, MS 46, Cambridge, MA 02138, USA; Infrared Processing and Analysis Center, California Institute of Technology, MC 100-22, 770 South Wilson Ave, Pasadena, CA 91125, USA <EMAIL>jspeagle@cfa.harvard.edu</EMAIL>), AB(Infrared Processing and Analysis Center, California Institute of Technology, MC 100-22, 770 South Wilson Ave, Pasadena, CA 91125, USA; Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA), AC(Harvard University Department of Astronomy, 60 Garden St, MS 46, Cambridge, MA 02138, USA), AD(Infrared Processing and Analysis Center, California Institute of Technology, MC 100-22, 770 South Wilson Ave, Pasadena, CA 91125, USA), AE(Infrared Processing and Analysis Center, California Institute of Technology, MC 100-22, 770 South Wilson Ave, Pasadena, CA 91125, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 461
%D 2016
%8 October 1, 2016
%P 3432-3442
%K methods: statistical;  techniques: photometric;  galaxies: distances and redshifts
%U http://adsabs.harvard.edu/abs/2016MNRAS.461.3432S
%X Using a 4D grid of ˜2 million model parameters (Δz = 0.005) 
adapted from Cosmological Origins Survey photometric redshift (photo-z) 
searches, we investigate the general properties of template-based 
photo-z likelihood surfaces. We find these surfaces are filled with 
numerous local minima and large degeneracies that generally confound 
simplistic gradient-descent optimization schemes. We combine ensemble 
Markov Chain Monte Carlo sampling with simulated annealing to robustly 
and efficiently explore these surfaces in approximately constant time. 
Using a mock catalogue of 384 662 objects, we show our approach samples 
˜40 times more efficiently compared to a `brute-force' counterpart 
while maintaining similar levels of accuracy. Our results represent 
first steps towards designing template-fitting photo-z approaches 
limited mainly by memory constraints rather than computation time.
%3 10.1093/mnras/stw1503
%= eprint: arXiv:1508.02484
%@ 0035-8711

%0 Journal Article
%T Clustering properties of g-selected galaxies at z ˜ 0.8
%A Favole, Ginevra 
%A Comparat, Johan 
%A Prada, Francisco 
%A Yepes, Gustavo 
%A Jullo, Eric 
%A Niemiec, Anna 
%A Kneib, Jean-Paul 
%A Rodríguez-Torres, Sergio A. 
%A Klypin, Anatoly 
%A Skibba, Ramin A. 
%A McBride, Cameron K. 
%A Eisenstein, Daniel J. 
%A Schlegel, David J. 
%A Nuza, Sebastián E. 
%A Chuang, Chia-Hsun 
%A Delubac, Timothée 
%A Yèche, Christophe 
%A Schneider, Donald P.
%+ AA(Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM/CSIC, Cantoblanco, E-28049 Madrid, Spain ), AB(Instituto de Física Teórica (IFT) 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 M-8, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; ), AC(Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM/CSIC, Cantoblanco, E-28049 Madrid, Spain; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Instituto de Astrofísica de Andalucía (CSIC), Granada E-18008, Spain), AD(Departamento de Física Teórica M-8, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AE(Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille and CNRS, UMR7326, F-13388 Marseille, France), AF(Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille and CNRS, UMR7326, F-13388 Marseille, France), AG(Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland; Laboratoire d'Astrophysique de Marseille - LAM, Université d'Aix-Marseille and CNRS, UMR7326, F-13388 Marseille, France), AH(Instituto de Física Teórica (IFT) 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 M-8, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AI(Astronomy Department, New Mexico State University, MSC 4500, PO Box 30001, Las Cruces, NM 880003-8001, USA), AJ(Center for Astrophysics and Space Sciences, University of California, 9500 Gilman Drive, San Diego, CA 92093, USA), AK(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AL(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AM(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AN(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AO(Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM/CSIC, Cantoblanco, E-28049 Madrid, Spain), AP(Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland), AQ(CEA, Centre de Saclay, IRFU, F-91191 Gif-sur-Yvette, France), AR(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)
%B Monthly Notices of the Royal Astronomical Society
%V 461
%D 2016
%8 October 1, 2016
%P 3421-3431
%K galaxies: distances and redshifts;  galaxies: haloes;  galaxies: statistics;  cosmology: observations;  cosmology: theory;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.461.3421F
%X Current and future large redshift surveys, as the Sloan Digital Sky 
Survey IV extended Baryon Oscillation Spectroscopic Survey 
(SDSS-IV/eBOSS) or the Dark Energy Spectroscopic Instrument (DESI), will 
use emission-line galaxies (ELGs) to probe cosmological models by 
mapping the large-scale structure of the Universe in the redshift range 
0.6 < z < 1.7. With current data, we explore the halo-galaxy 
connection by measuring three clustering properties of g-selected ELGs 
as matter tracers in the redshift range 0.6 < z < 1: (i) the 
redshift-space two-point correlation function using spectroscopic 
redshifts from the BOSS ELG sample and VIPERS; (ii) the angular 
two-point correlation function on the footprint of the CFHT-LS; (iii) 
the galaxy-galaxy lensing signal around the ELGs using the CFHTLenS. We 
interpret these observations by mapping them on to the latest 
high-resolution MultiDark Planck N-body simulation, using a novel 
(Sub)Halo-Abundance Matching technique that accounts for the ELG 
incompleteness. ELGs at z ˜ 0.8 live in haloes of (1 ± 0.5) 
× 10<SUP>12</SUP> h<SUP>-1</SUP>M<SUB>⊙</SUB> and 22.5 
± 2.5 per cent of them are satellites belonging to a larger halo. 
The halo occupation distribution of ELGs indicates that we are sampling 
the galaxies in which stars form in the most efficient way, according to 
their stellar-to-halo mass ratio.
%3 10.1093/mnras/stw1483
%= eprint: arXiv:1507.04356
%@ 0035-8711

%0 Journal Article
%T The high-mass end of the red sequence at z ˜ 0.55 from SDSS-III/BOSS: completeness, bimodality and luminosity function
%A Montero-Dorta, Antonio D. 
%A Bolton, Adam S. 
%A Brownstein, Joel R. 
%A Swanson, Molly 
%A Dawson, Kyle 
%A Prada, Francisco 
%A Eisenstein, Daniel 
%A Maraston, Claudia 
%A Thomas, Daniel 
%A Comparat, Johan 
%A Chuang, Chia-Hsun 
%A McBride, Cameron K. 
%A Favole, Ginevra 
%A Guo, Hong 
%A Rodríguez-Torres, Sergio 
%A Schneider, Donald P.
%+ AA(Department of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USA <EMAIL>amontero@astro.utah.edu</EMAIL>), AB(Department of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USA; National Optical Astronomy Observatory, 950 N Cherry Ave, Tucson, AZ 85719, USA), AC(Department of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USA), AD(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AE(Department of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USA), AF(Instituto de Astrofísica de Andalucía (CSIC), E-18008 Granada, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AG(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AH(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AI(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AJ(Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AK(Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AL(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AM(Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AN(Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Shanghai 200030, China), AO(Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AP(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)
%B Monthly Notices of the Royal Astronomical Society
%V 461
%D 2016
%8 September 1, 2016
%P 1131-1153
%K methods: analytical;  methods: statistical;  surveys;  galaxies: evolution;  galaxies: luminosity function;  mass function;  galaxies: statistics
%U http://adsabs.harvard.edu/abs/2016MNRAS.461.1131M
%X We have developed an analytical method based on forward-modelling 
techniques to characterize the high-mass end of the red sequence (RS) 
galaxy population at redshift z ˜ 0.55, from the DR10 BOSS (Baryon 
Oscillation Spectroscopic Survey) CMASS spectroscopic sample, which 
comprises ˜600 000 galaxies. The method, which follows an unbinned 
maximum likelihood approach, allows the deconvolution of the intrinsic 
CMASS colour-colour-magnitude distributions from photometric errors and 
selection effects. This procedure requires modelling the covariance 
matrix for the i-band magnitude, g - r colour and r - i colour using 
Stripe 82 multi-epoch data. Our results indicate that the 
error-deconvolved intrinsic RS distribution is consistent, within the 
photometric uncertainties, with a single point (<0.05 mag) in the 
colour-colour plane at fixed magnitude, for a narrow redshift slice. We 
have computed the high-mass end (<SUP>0.55</SUP>M<SUB>i</SUB> ≲ 
-22) of the <SUP>0.55</SUP>i-band RS luminosity function (RS LF) in 
several redshift slices within the redshift range 0.52 < z < 0.63. 
In this narrow redshift range, the evolution of the RS LF is consistent, 
within the uncertainties in the modelling, with a passively evolving 
model with Φ<SUB>*</SUB> = (7.248 ± 0.204) × 10<SUP>- 
4</SUP> Mpc<SUP>-3</SUP> mag<SUP>-1</SUP>, fading at a rate of 1.5 
± 0.4 mag per unit redshift. We report RS completeness as a 
function of magnitude and redshift in the CMASS sample, which will 
facilitate a variety of galaxy-evolution and clustering studies using 
BOSS. Our forward-modelling method lays the foundations for future 
studies using other dark-energy surveys like the Extended Baryon 
Oscillation Spectroscopic Survey or the Dark Energy Spectroscopic 
Instrument, which are affected by the same type of photometric 
blurring/selection effects.
%3 10.1093/mnras/stw1352
%@ 0035-8711

%0 Journal Article
%T Quantifying the colour-dependent stochasticity of large-scale structure
%A Patej, Anna 
%A Eisenstein, Daniel
%+ AA(Department of Physics, Harvard University, 17 Oxford St, Cambridge, MA 02138, USA; <EMAIL>apatej@physics.harvard.edu</EMAIL>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 460
%D 2016
%8 August 1, 2016
%P 1310-1317
%K galaxies: statistics;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.460.1310P
%X We address the question of whether massive red and blue galaxies trace 
the same large-scale structure at z ˜ 0.6 using the CMASS sample 
of galaxies from Data Release 12 of the Sloan Digital Sky Survey III. 
After splitting the catalogue into subsamples of red and blue galaxies 
using a simple colour cut, we measure the clustering of both subsamples 
and construct the correlation coefficient, r, using two statistics. The 
correlation coefficient quantifies the stochasticity between the two 
subsamples, which we examine over intermediate scales (20 ≲ R 
≲ 100 h<SUP>-1</SUP> Mpc). We find that on these intermediate 
scales, the correlation coefficient is consistent with 1; in particular, 
we find r > 0.95 taking into account both statistics and r > 0.974 
using the favoured statistic.
%3 10.1093/mnras/stw635
%= eprint: arXiv:1510.01737
%@ 0035-8711

%0 Journal Article
%T ASPCAP: The APOGEE Stellar Parameter and Chemical Abundances Pipeline
%A García Pérez, Ana E. 
%A Allende Prieto, Carlos 
%A Holtzman, Jon A. 
%A Shetrone, Matthew 
%A Mészáros, Szabolcs 
%A Bizyaev, Dmitry 
%A Carrera, Ricardo 
%A Cunha, Katia 
%A García-Hernández, D. A. 
%A Johnson, Jennifer A. 
%A Majewski, Steven R. 
%A Nidever, David L. 
%A Schiavon, Ricardo P. 
%A Shane, Neville 
%A Smith, Verne V. 
%A Sobeck, Jennifer 
%A Troup, Nicholas 
%A Zamora, Olga 
%A Weinberg, David H. 
%A Bovy, Jo 
%A Eisenstein, Daniel J. 
%A Feuillet, Diane 
%A Frinchaboy, Peter M. 
%A Hayden, Michael R. 
%A Hearty, Fred R. 
%A Nguyen, Duy C. 
%A O'Connell, Robert W. 
%A Pinsonneault, Marc H. 
%A Wilson, John C. 
%A Zasowski, Gail
%+ AA(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA; Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain; <EMAIL>agp@iac.es</EMAIL>), AB(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain), AC(New Mexico State University, Las Cruces, NM 88003, USA), AD(University of Texas at Austin, McDonald Observatory, Fort Davis, TX 79734, USA), AE(ELTE Gothard Astrophysical Observatory, H-9704 Szombathely, Szent Imre Herceg St. 112, Hungary), AF(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349-0059, USA; Sternberg Astronomical Institute, Moscow State University, Moscow, Russia), AG(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain), AH(Observatório Nacional, São Cristóvão, Rio de Janeiro, Brazil; Steward Observatory, University of Arizona, Tucson, AZ 85719, USA), AI(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain), AJ(Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA), AK(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), AL(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA), AM(Astrophysics Research Institute, Liverpool John Moores University, Egerton Wharf, Birkenhead, Wirral CH41 1LD, UK), AN(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), AO(National Optical Astronomy Observatories, Tucson, AZ 85719, USA), AP(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), AQ(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), AR(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain), AS(Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA), AT(Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA), AU(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), AV(New Mexico State University, Las Cruces, NM 88003, USA), AW(Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA), AX(New Mexico State University, Las Cruces, NM 88003, USA), AY(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA), AZ(Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, ON, M5S 3H4, Canada), BA(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BB(Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA), BC(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BD(Johns Hopkins University, Department of Physics and Astronomy, Baltimore, MD 21218, USA)
%B The Astronomical Journal
%V 151
%D 2016
%8 June 1, 2016
%K Galaxy: center;  Galaxy: structure;  methods: data analysis;  stars: abundances;  stars: atmospheres
%U http://adsabs.harvard.edu/abs/2016AJ....151..144G
%X The Apache Point Observatory Galactic Evolution Experiment (APOGEE) has 
built the largest moderately high-resolution (R ≈ 22,500) 
spectroscopic map of the stars across the Milky Way, and including 
dust-obscured areas. The APOGEE Stellar Parameter and Chemical 
Abundances Pipeline (ASPCAP) is the software developed for the automated 
analysis of these spectra. ASPCAP determines atmospheric parameters and 
chemical abundances from observed spectra by comparing observed spectra 
to libraries of theoretical spectra, using χ<SUP>2</SUP> 
minimization in a multidimensional parameter space. The package consists 
of a fortran90 code that does the actual minimization and a wrapper IDL 
code for book-keeping and data handling. This paper explains in detail 
the ASPCAP components and functionality, and presents results from a 
number of tests designed to check its performance. ASPCAP provides 
stellar effective temperatures, surface gravities, and metallicities 
precise to 2%, 0.1 dex, and 0.05 dex, respectively, for most APOGEE 
stars, which are predominantly giants. It also provides abundances for 
up to 15 chemical elements with various levels of precision, typically 
under 0.1 dex. The final data release (DR12) of the Sloan Digital Sky 
Survey III contains an APOGEE database of more than 150,000 stars. 
ASPCAP development continues in the SDSS-IV APOGEE-2 survey.
%3 10.3847/0004-6256/151/6/144
%= eprint: arXiv:1510.07635
%@ 0004-6256

%0 Journal Article
%T Signatures of the Primordial Universe from Its Emptiness: Measurement of Baryon Acoustic Oscillations from Minima of the Density Field
%A Kitaura, Francisco-Shu 
%A Chuang, Chia-Hsun 
%A Liang, Yu 
%A Zhao, Cheng 
%A Tao, Charling 
%A Rodríguez-Torres, Sergio 
%A Eisenstein, Daniel J. 
%A Gil-Marín, Héctor 
%A Kneib, Jean-Paul 
%A McBride, Cameron 
%A Percival, Will J. 
%A Ross, Ashley J. 
%A Sánchez, Ariel G. 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Vargas-Magana, Mariana 
%A Zhao, Gong-Bo
%+ 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), AC(Tsinghua Center of Astrophysics and Department of Physics, Tsinghua University, Beijing 100084, China), AD(Tsinghua Center of Astrophysics and Department of Physics, Tsinghua University, Beijing 100084, China), AE(Tsinghua Center of Astrophysics and Department of Physics, Tsinghua University, Beijing 100084, China; Aix-Marseille Université, CNRS/IN2P3, CPPM UMR 7346, 13288 Marseille, France), AF(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 Fısica Teórica M8, Universidad Autonoma de Madrid (UAM), Cantoblanco, E-28049, Madrid, Spain), AG(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA), AH(Sorbonne Universits, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, 75014 Paris, France; Laboratoire de Physique Nuclaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, Tour 22, 1er tage, 75005 Paris, France), AI(Laboratoire dAstrophysique, Ecole Polytechnique Fedérale de Lausanne, CH-1015 Lausanne, Switzerland; Aix Marseille Université, CNRS, LAM (Laboratoire dAstrophysique de Marseille) UMR 7326, F-13388, Marseille, France), AJ(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA), AK(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, United Kingdom), AL(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, United Kingdom; Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, Ohio 43210, USA), AM(Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstraße, 85741 Garching, Germany), AN(Center for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, New York 10003, USA), AO(University of St. Andrews, North Haugh, St. Andrews Fife, KY16 9SS, United Kingdom), AP(Instituto de Física, Universidad Nacional Autónoma de México, Apartado Postal 20-364, México), AQ(National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, People's Republic of China; Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, United Kingdom)
%B Physical Review Letters
%V 116
%D 2016
%8 April 1, 2016
%U http://adsabs.harvard.edu/abs/2016PhRvL.116q1301K
%X Sound waves from the primordial fluctuations of the Universe imprinted 
in the large-scale structure, called baryon acoustic oscillations 
(BAOs), can be used as standard rulers to measure the scale of the 
Universe. These oscillations have already been detected in the 
distribution of galaxies. Here we propose to measure BAOs from the 
troughs (minima) of the density field. Based on two sets of accurate 
mock halo catalogues with and without BAOs in the seed initial 
conditions, we demonstrate that the BAO signal cannot be obtained from 
the clustering of classical disjoint voids, but it is clearly detected 
from overlapping voids. The latter represent an estimate of all troughs 
of the density field. We compute them from the empty circumsphere 
centers constrained by tetrahedra of galaxies using Delaunay 
triangulation. Our theoretical models based on an unprecedented large 
set of detailed simulated void catalogues are remarkably well confirmed 
by observational data. We use the largest recently publicly available 
sample of luminous red galaxies from SDSS-III BOSS DR11 to unveil for 
the first time a >3 σ BAO detection from voids in observations. 
Since voids are nearly isotropically expanding regions, their centers 
represent the most quiet places in the Universe, keeping in mind the 
cosmos origin and providing a new promising window in the analysis of 
the cosmological large-scale structure from galaxy surveys.
%3 10.1103/PhysRevLett.116.171301
%= eprint: arXiv:1511.04405
%@ 0031-9007

%0 Journal Article
%T Large-scale clustering of Lyman α emission intensity from SDSS/BOSS
%A Croft, Rupert A. C. 
%A Miralda-Escudé, Jordi 
%A Zheng, Zheng 
%A Bolton, Adam 
%A Dawson, Kyle S. 
%A Peterson, Jeffrey B. 
%A York, Donald G. 
%A Eisenstein, Daniel 
%A Brinkmann, Jon 
%A Brownstein, Joel 
%A Cen, Renyue 
%A Delubac, Timothée 
%A Font-Ribera, Andreu 
%A Hamilton, Jean-Christophe 
%A Lee, Khee-Gan 
%A Myers, Adam 
%A Palanque-Delabrouille, Nathalie 
%A Pâris, Isabelle 
%A Petitjean, Patrick 
%A Pieri, Matthew M. 
%A Ross, Nicholas P. 
%A Rossi, Graziano 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Slosar, Anže 
%A Vazquez, José 
%A Viel, Matteo 
%A Weinberg, David H. 
%A Yèche, Christophe
%+ AA(McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA 15213, USA; Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK <EMAIL>rcroft@cmu.edu</EMAIL>), AB(Institució Catalana de Recerca i Estudis Avançats, E-08001 Barcelona, Catalonia, Spain; Institut de Ciències del Cosmos, Universitat de Barcelona/IEEC, E-08028 Barcelona, Catalonia, Spain), AC(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AD(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AE(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AF(McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA 15213, USA), AG(Department of Astronomy and Astrophysics, The University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60615, USA), AH(Department of Astronomy, Harvard University, 60 Garden St, Cambridge MA 02138, USA), AI(Apache Point Observatory, PO Box 59, Sunspot, NM 88349, USA), AJ(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AK(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA), AL(CEA, Centre de Saclay, IRFU, F-91191 Gif-sur-Yvette, France), AM(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AN(APC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10, rueA. Domon & L. Duquet, F-75013 Paris, France), AO(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany), AP(Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA), AQ(CEA, Centre de Saclay, IRFU, F-91191 Gif-sur-Yvette, France), AR(INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34131 Trieste, Italy), AS(Université Paris 6 et CNRS, Institut d'Astrophysique de Paris, 98bis blvd. Arago, F-75014 Paris, France), AT(A*MIDEX, Aix Marseille Universit, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, F-13388 Marseille, France), AU(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AV(Department of Astronomy and Space Science, Sejong University, Seoul 143-747, Korea), AW(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AX(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), AY(Bldg 510 Brookhaven National Laboratory, Upton, NY 11973, USA), AZ(Bldg 510 Brookhaven National Laboratory, Upton, NY 11973, USA), BA(INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34131 Trieste, Italy; INFN/National Institute for Nuclear Physics, Via Valerio 2, I-34127 Trieste, Italy), BB(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), BC(CEA, Centre de Saclay, IRFU, F-91191 Gif-sur-Yvette, France)
%B Monthly Notices of the Royal Astronomical Society
%V 457
%D 2016
%8 April 1, 2016
%P 3541-3572
%K cosmology: observations
%U http://adsabs.harvard.edu/abs/2016MNRAS.457.3541C
%X We present a tentative detection of the large-scale structure of Ly 
α emission in the Universe at redshifts z = 2-3.5 by measuring the 
cross-correlation of Ly α surface brightness with quasars in Sloan 
Digital Sky Survey/Baryon Oscillation Spectroscopic Survey. We use a 
million spectra targeting luminous red galaxies at z < 0.8, after 
subtracting a best-fitting model galaxy spectrum from each one, as an 
estimate of the high-redshift Ly α surface brightness. The 
quasar-Ly α emission cross-correlation is detected on scales 1 
˜ 15 h<SUP>-1</SUP> Mpc, with shape consistent with a ΛCDM 
model with Ω _m =0.30^{+0.10}_{-0.07}. The predicted amplitude of 
this cross-correlation is proportional to the product of the mean Ly 
α surface brightness, <μ<SUB>α</SUB>>, the 
amplitude of mass fluctuations and the quasar and Ly α emission 
bias factors. We infer <μ<SUB>α</SUB>> 
(b<SUB>α</SUB>/3) = (3.9 ± 0.9) × 10<SUP>-21</SUP> 
erg s<SUP>-1</SUP> cm<SUP>-2</SUP> Å<SUP>-1</SUP> 
arcsec<SUP>-2</SUP>, where b<SUB>α</SUB> is the Ly α 
emission bias. If star-forming galaxies dominate this emission, we find 
ρ<SUB>SFR</SUB> = (0.28 ± 0.07)(3/b<SUB>α</SUB>) 
yr<SUP>-1</SUP> Mpc<SUP>-3</SUP>. For b<SUB>α</SUB> = 3, this 
value is ˜30 times larger than previous estimates from 
individually detected Ly α emitters, but consistent with the total 
ρ<SUB>SFR</SUB> derived from dust-corrected, continuum UV galaxy 
surveys, if most of the Ly α photons from these galaxies avoid 
dust absorption and are reemitted after diffusing in large gas haloes. 
Heating of intergalactic gas by He II photoionization from quasar 
radiation or jets may alternatively explain the detected correlation, 
and cooling radiation from gas in galactic haloes may also contribute. 
We also detect redshift space anisotropy of the quasar-Ly α 
emission cross-correlation, finding evidence at the 3.0σ level 
that it is radially elongated, which may be explained by 
radiative-transfer effects. Our measurements represent the first 
application of the intensity mapping technique to optical observations.
%3 10.1093/mnras/stw204
%= eprint: arXiv:1504.04088
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the correlation function of LOWZ and CMASS galaxies in Data Release 12
%A Cuesta, Antonio J. 
%A Vargas-Magaña, Mariana 
%A Beutler, Florian 
%A Bolton, Adam S. 
%A Brownstein, Joel R. 
%A Eisenstein, Daniel J. 
%A Gil-Marín, Héctor 
%A Ho, Shirley 
%A McBride, Cameron K. 
%A Maraston, Claudia 
%A Padmanabhan, Nikhil 
%A Percival, Will J. 
%A Reid, Beth A. 
%A Ross, Ashley J. 
%A Ross, Nicholas P. 
%A Sánchez, Ariel G. 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Thomas, Daniel 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Verde, Licia 
%A White, Martin
%+ AA(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain <EMAIL>ajcuesta@icc.ub.edu</EMAIL>), AB(Instituto de Física, UNAM, PO Box 20-364, 01000 México D.F., Mexico; Bruce and Astrid McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA; Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15217, USA), AC(Berkeley Center for Cosmological Physics, Department of Physics, University of California, Berkeley, CA 94720, USA; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AD(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AE(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AF(Harvard-Smithsonian Center for Astrophysics, Harvard University, 60 Garden St, Cambridge, MA 02138, USA), AG(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AH(Bruce and Astrid McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA; Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15217, USA), AI(Harvard-Smithsonian Center for Astrophysics, Harvard University, 60 Garden St, Cambridge, MA 02138, USA), AJ(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AK(Department of Physics, Yale University, 260 Whitney Avenue, New Haven, CT 06520, USA), AL(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AM(Berkeley Center for Cosmological Physics, Department of Physics, University of California, Berkeley, CA 94720, USA; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AN(Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA), AO(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill Edinburgh EH9 3HJ, UK; Department of Physics, Drexel University, 3141 Chestnut Street, Philadelphia, PA 19104, USA), AP(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany), AQ(Berkeley Center for Cosmological Physics, Department of Physics, University of California, Berkeley, CA 94720, USA; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AR(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), AS(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AT(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AU(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), AV(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain; ICREA (Institució Catalana de Recerca i Estudis Avançats), Passeig Lluís Companys, E-23 08010 Barcelona - Spain; Radcliffe Institute for Advanced Study, Harvard University, MA 02138, USA; Institute of Theoretical Astrophysics, University of Oslo, 0315 Oslo, Norway), AW(Berkeley Center for Cosmological Physics, Department of Physics, University of California, Berkeley, CA 94720, USA; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Department of Astronomy, University of California, Berkeley, CA 94720, USA; Department of Physics, University of California, Berkeley, CA 94720, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 457
%D 2016
%8 April 1, 2016
%P 1770-1785
%K cosmology: observations;  distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.457.1770C
%X We present distance scale measurements from the baryon acoustic 
oscillation signal in the constant stellar mass and low-redshift sample 
samples from the Data Release 12 of the Baryon Oscillation Spectroscopic 
Survey. The total volume probed is 14.5 Gpc<SUP>3</SUP>, a 10 per cent 
increment from Data Release 11. From an analysis of the spherically 
averaged correlation function, we infer a distance to z = 0.57 of 
D_V(z)r^fid_d/r_d = 2028± 21 Mpc and a distance to z = 0.32 of 
D_V(z)r^fid_d/r_d = 1264± 22 Mpc assuming a cosmology in which 
r^fid_d = 147.10 Mpc. From the anisotropic analysis, we find an angular 
diameter distance to z = 0.57 of D_A(z)r^fid_d/r_d = 1401± 21 Mpc 
and a distance to z = 0.32 of 981 ± 20 Mpc, a 1.5 and 2.0 per 
cent measurement, respectively. The Hubble parameter at z = 0.57 is 
H(z)r_d/r^fid_d = 100.3± 3.7 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> 
and its value at z = 0.32 is 79.2 ± 5.6 km s<SUP>-1</SUP> 
Mpc<SUP>-1</SUP>, a 3.7 and 7.1 per cent measurement, respectively. 
These cosmic distance scale constraints are in excellent agreement with 
a Λ cold dark matter model with cosmological parameters released 
by the recent Planck 2015 results.
%3 10.1093/mnras/stw066
%= eprint: arXiv:1509.06371
%@ 0035-8711

%0 Journal Article
%T PRIMUS + DEEP2: Clustering of X-Ray, Radio, and IR-AGNs at z~0.7
%A Mendez, Alexander J. 
%A Coil, Alison L. 
%A Aird, James 
%A Skibba, Ramin A. 
%A Diamond-Stanic, Aleksandar M. 
%A Moustakas, John 
%A Blanton, Michael R. 
%A Cool, Richard J. 
%A Eisenstein, Daniel J. 
%A Wong, Kenneth C. 
%A Zhu, Guangtun
%+ AA(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Drive, La Jolla, San Diego, CA 92093, USA; Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA; <EMAIL>ajmendez@jhu.edu</EMAIL> <ID system="ORCID">0000-0002-7726-1722</ID>), AB(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Drive, La Jolla, San Diego, CA 92093, USA <ID system="ORCID">0000-0002-2583-5894</ID>), AC(Department of Physics, Durham University, Durham DH1 3LE, UK <ID system="ORCID">0000-0003-1908-8463</ID>), AD(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Drive, La Jolla, San Diego, CA 92093, USA), AE(Department of Astronomy, University of Wisconsin-Madison, Madison, WI 53706-1582, USA), AF(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA), AG(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AH(MMT Observatory, 1540 East Second Street, University of Arizona, Tucson, AZ 85721, USA), AI(Harvard College Observatory, 60 Garden Street, Cambridge, MA 02138, USA), AJ(Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA <ID system="ORCID">0000-0002-8459-7793</ID>), AK(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA)
%B The Astrophysical Journal
%V 821
%D 2016
%8 April 1, 2016
%K galaxies: active;  galaxies: evolution;  infrared: galaxies;  radio continuum: galaxies;  X-rays: galaxies
%U http://adsabs.harvard.edu/abs/2016ApJ...821...55M
%X We measure the clustering of X-ray, radio, and mid-IR-selected active 
galactic nuclei (AGNs) at 0.2\lt z\lt 1.2 using multi-wavelength imaging 
and spectroscopic redshifts from the PRIMUS and DEEP2 redshift surveys, 
covering seven separate fields spanning ∼10 deg 2 . Using the 
cross-correlation of AGNs with dense galaxy samples, we measure the 
clustering scale length and slope, as well as the bias, of AGNs selected 
at different wavelengths. Similar to previous studies, we find that 
X-ray and radio AGNs are more clustered than mid-IR-selected AGNs. We 
further compare the clustering of each AGN sample with matched galaxy 
samples designed to have the same stellar mass, star-formation rate 
(SFR), and redshift distributions as the AGN host galaxies and find no 
significant differences between their clustering properties. The 
observed differences in the clustering of AGNs selected at different 
wavelengths can therefore be explained by the clustering differences of 
their host populations, which have different distributions in both 
stellar mass and SFR. Selection biases inherent in AGN selection 
therefore determine the clustering of observed AGN samples. We further 
find no significant difference between the clustering of obscured and 
unobscured AGNs, using IRAC or Wide-field Infrared Survey Explorer 
colors or X-ray hardness ratio.
%3 10.3847/0004-637X/821/1/55
%= eprint: arXiv:1504.06284
%@ 0004-637X

%0 Journal Article
%T A simple analytic treatment of linear growth of structure with baryon acoustic oscillations
%A Slepian, Zachary 
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA <EMAIL>zslepian@fas.harvard.edu</EMAIL>), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 457
%D 2016
%8 March 1, 2016
%P 24-37
%K cosmology: theory;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.457...24S
%X In linear perturbation theory, all information about the growth of 
structure is contained in the Green's function, or equivalently, 
transfer function. These functions are generally computed using 
numerical codes or by phenomenological fitting formula anchored in 
accurate analytic results in the limits of large and small scale. Here, 
we present a framework for analytically solving all scales, in 
particular the intermediate scales relevant for the baryon acoustic 
oscillations (BAO). We solve for the Green's function and transfer 
function using spherically averaged overdensities and the approximation 
that the density of the coupled baryon-photon fluid is constant interior 
to the sound horizon.
%3 10.1093/mnras/stv2889
%= eprint: arXiv:1509.08199
%@ 0035-8711

%0 Journal Article
%T New white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 12
%A Kepler, S. O. 
%A Pelisoli, I. 
%A Koester, D. 
%A Ourique, G. 
%A Romero, A. D. 
%A Reindl, N. 
%A Kleinman, S. J. 
%A Eisenstein, D. J. 
%A Valois, A. D. M. 
%A Amaral, L. A.
%+ AA(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-900 Porto-Alegre, RS, Brazil <EMAIL>kepler@if.ufrgs.br</EMAIL>), AB(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-900 Porto-Alegre, RS, Brazil), AC(Institut für Theoretische Physik und Astrophysik, Universität Kiel, D-24098 Kiel, Germany), AD(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-900 Porto-Alegre, RS, Brazil), AE(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-900 Porto-Alegre, RS, Brazil), AF(Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, D-72076 Tübingen, Germany), AG(Gemini Observatory, Hilo, HI 96720, USA), AH(Harvard Smithsonian Center for Astrophysics, 60 Garden St., MS #20, Cambridge, MA 02138, USA), AI(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-900 Porto-Alegre, RS, Brazil), AJ(Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-900 Porto-Alegre, RS, Brazil)
%B Monthly Notices of the Royal Astronomical Society
%V 455
%D 2016
%8 February 1, 2016
%P 3413-3423
%K catalogues;  stars: magnetic field;  subdwarfs;  white dwarfs
%U http://adsabs.harvard.edu/abs/2016MNRAS.455.3413K
%X We report the discovery of 6576 new spectroscopically confirmed white 
dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 
12. We obtain T<SUB>eff</SUB>, log g and mass for hydrogen atmosphere 
white dwarf stars (DAs) and helium atmosphere white dwarf stars (DBs), 
estimate the calcium/helium abundances for the white dwarf stars with 
metallic lines (DZs) and carbon/helium for carbon-dominated spectra 
(DQs). We found one central star of a planetary nebula, one ultracompact 
helium binary (AM CVn), one oxygen line-dominated white dwarf, 15 hot 
DO/PG1159s, 12 new cataclysmic variables, 36 magnetic white dwarf stars, 
54 DQs, 115 helium-dominated white dwarfs, 148 white dwarf + 
main-sequence star binaries, 236 metal-polluted white dwarfs, 300 
continuum spectra DCs, 230 hot subdwarfs, 2936 new hydrogen-dominated 
white dwarf stars, and 2675 cool hydrogen-dominated subdwarf stars. We 
calculate the mass distribution of all 5883 DAs with S/N ≥ 15 in 
DR12, including the ones in DR7 and DR10, with an average S/N = 26, 
corrected to the 3D convection scale, and also the distribution after 
correcting for the observed volume, using 1/V<SUB>max</SUB>.
%3 10.1093/mnras/stv2526
%= eprint: arXiv:1510.08409
%@ 0035-8711

%0 Journal Article
%T The SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Overview and Early Data
%A Dawson, Kyle S. 
%A Kneib, Jean-Paul 
%A Percival, Will J. 
%A Alam, Shadab 
%A Albareti, Franco D. 
%A Anderson, Scott F. 
%A Armengaud, Eric 
%A Aubourg, Éric 
%A Bailey, Stephen 
%A Bautista, Julian E. 
%A Berlind, Andreas A. 
%A Bershady, Matthew A. 
%A Beutler, Florian 
%A Bizyaev, Dmitry 
%A Blanton, Michael R. 
%A Blomqvist, Michael 
%A Bolton, Adam S. 
%A Bovy, Jo 
%A Brandt, W. N. 
%A Brinkmann, Jon 
%A Brownstein, Joel R. 
%A Burtin, Etienne 
%A Busca, N. G. 
%A Cai, Zheng 
%A Chuang, Chia-Hsun 
%A Clerc, Nicolas 
%A Comparat, Johan 
%A Cope, Frances 
%A Croft, Rupert A. C. 
%A Cruz-Gonzalez, Irene 
%A da Costa, Luiz N. 
%A Cousinou, Marie-Claude 
%A Darling, Jeremy 
%A de la Macorra, Axel 
%A de la Torre, Sylvain 
%A Delubac, Timothée 
%A du Mas des Bourboux, Hélion 
%A Dwelly, Tom 
%A Ealet, Anne 
%A Eisenstein, Daniel J. 
%A Eracleous, Michael 
%A Escoffier, S. 
%A Fan, Xiaohui 
%A Finoguenov, Alexis 
%A Font-Ribera, Andreu 
%A Frinchaboy, Peter 
%A Gaulme, Patrick 
%A Georgakakis, Antonis 
%A Green, Paul 
%A Guo, Hong 
%A Guy, Julien 
%A Ho, Shirley 
%A Holder, Diana 
%A Huehnerhoff, Joe 
%A Hutchinson, Timothy 
%A Jing, Yipeng 
%A Jullo, Eric 
%A Kamble, Vikrant 
%A Kinemuchi, Karen 
%A Kirkby, David 
%A Kitaura, Francisco-Shu 
%A Klaene, Mark A. 
%A Laher, Russ R. 
%A Lang, Dustin 
%A Laurent, Pierre 
%A Le Goff, Jean-Marc 
%A Li, Cheng 
%A Liang, Yu 
%A Lima, Marcos 
%A Lin, Qiufan 
%A Lin, Weipeng 
%A Lin, Yen-Ting 
%A Long, Daniel C. 
%A Lundgren, Britt 
%A MacDonald, Nicholas 
%A Geimba Maia, Marcio Antonio 
%A Malanushenko, Elena 
%A Malanushenko, Viktor 
%A Mariappan, Vivek 
%A McBride, Cameron K. 
%A McGreer, Ian D. 
%A Ménard, Brice 
%A Merloni, Andrea 
%A Meza, Andres 
%A Montero-Dorta, Antonio D. 
%A Muna, Demitri 
%A Myers, Adam D. 
%A Nandra, Kirpal 
%A Naugle, Tracy 
%A Newman, Jeffrey A. 
%A Noterdaeme, Pasquier 
%A Nugent, Peter 
%A Ogando, Ricardo 
%A Olmstead, Matthew D. 
%A Oravetz, Audrey 
%A Oravetz, Daniel J. 
%A Padmanabhan, Nikhil 
%A Palanque-Delabrouille, Nathalie 
%A Pan, Kaike 
%A Parejko, John K. 
%A Pâris, Isabelle 
%A Peacock, John A. 
%A Petitjean, Patrick 
%A Pieri, Matthew M. 
%A Pisani, Alice 
%A Prada, Francisco 
%A Prakash, Abhishek 
%A Raichoor, Anand 
%A Reid, Beth 
%A Rich, James 
%A Ridl, Jethro 
%A Rodriguez-Torres, Sergio 
%A Carnero Rosell, Aurelio 
%A Ross, Ashley J. 
%A Rossi, Graziano 
%A Ruan, John 
%A Salvato, Mara 
%A Sayres, Conor 
%A Schneider, Donald P. 
%A Schlegel, David J. 
%A Seljak, Uros 
%A Seo, Hee-Jong 
%A Sesar, Branimir 
%A Shandera, Sarah 
%A Shu, Yiping 
%A Slosar, Anže 
%A Sobreira, Flavia 
%A Streblyanska, Alina 
%A Suzuki, Nao 
%A Taylor, Donna 
%A Tao, Charling 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana 
%A Wang, Yuting 
%A Weaver, Benjamin A. 
%A Weinberg, David H. 
%A White, Martin 
%A Wood-Vasey, W. M. 
%A Yeche, Christophe 
%A Zhai, Zhongxu 
%A Zhao, Cheng 
%A Zhao, Gong-bo 
%A Zheng, Zheng 
%A Ben Zhu, Guangtun 
%A Zou, Hu
%+ AA(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA <EMAIL>kdawson@astro.utah.edu</EMAIL>), AB(Laboratoire dástrophysique, Ecole Polytechnique Fédérale de Lausanne Observatoire de Sauverny, 1290 Versoix, Switzerland; Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, F-13388, Marseille, France), AC(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), AD(Bruce and Astrid McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), AE(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain;), AF(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), AG(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), AH(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cite, France), AI(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), AJ(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AK(Department of Physics and Astronomy, Vanderbilt University, PMB 401807, 2401 Vanderbilt Place, Nashville, TN 37240, USA), AL(University of Wisconsin-Madison, Department of Astronomy, 475 N. Charter St., Madison WI 53703, USA), AM(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), AN(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA; Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA; Sternberg Astronomical Institute, Moscow State University, Moscow, Russia), AO(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AP(Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA), AQ(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AR(Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON, M5S 3H4, Canada), AS(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA; Department of Physics, The Pennsylvania State University, University Park, PA 16802, USA), AT(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA), AU(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AV(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), AW(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cite, France), AX(Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA), AY(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AZ(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany), BA(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Departamento de Fisica Teorica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain;), BB(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA), BC(Bruce and Astrid McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), BD(Instituto de Astronomía, Universidad Nacional Autonoma de Mexico, A.P. 70-264, 04510, D.F., Mexico), BE(Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Laboratório Interinstitucional de e-Astronomia,—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), BF(Aix-Marseille Université, CNRS/IN2P3, CPPM UMR 7346, F-13288 Marseille, France), BG(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309, USA), BH(Instituto de Astronomía, Universidad Nacional Autonoma de Mexico, A.P. 70-264, 04510, D.F., Mexico), BI(Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, F-13388, Marseille, France), BJ(Laboratoire dástrophysique, Ecole Polytechnique Fédérale de Lausanne Observatoire de Sauverny, 1290 Versoix, Switzerland), BK(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), BL(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany), BM(Aix-Marseille Université, CNRS/IN2P3, CPPM UMR 7346, F-13288 Marseille, France), BN(Harvard-Smithsonian Center for Astrophysics, Harvard University, 60 Garden St., Cambridge MA 02138, USA), BO(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA; Department of Physics, The Pennsylvania State University, University Park, PA 16802, USA), BP(Aix-Marseille Université, CNRS/IN2P3, CPPM UMR 7346, F-13288 Marseille, France), BQ(Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA), BR(Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2a, FI-00014 Helsinki, Finland), BS(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), BT(Dept. of Physics & Astronomy, Texas Christian University, 2800 South University Dr., Fort Worth, TX 76129, USA), BU(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA), BV(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany), BW(Harvard-Smithsonian Center for Astrophysics, Harvard University, 60 Garden St., Cambridge MA 02138, USA), BX(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA; Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, China), BY(LPNHE, CNRS/IN2P3, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, 4 place Jussieu, F-75252 Paris CEDEX, France), BZ(Bruce and Astrid McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), CA(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA), CB(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA), CC(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), CD(IFSA Collaborative Innovation Center, Department of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, 200240, China), CE(Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, F-13388, Marseille, France), CF(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), CG(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA; Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), CH(Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA), CI(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), CJ(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA), CK(Spitzer Science Center, California Institute of Technology, M/S 314-6, Pasadena, CA 91125, USA), CL(Bruce and Astrid McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), CM(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), CN(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), CO(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, China), CP(Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China), CQ(Laboratório Interinstitucional de e-Astronomia,—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, CEP 05314-970, São Paulo, SP, Brazil), CR(Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China), CS(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, China; School of Astronomy and Space Science, Sun Yat-sen University, Guangzhou, 510275, China), CT(Institute of Astronomy and Astrophysics, Academia Sinica, Taipei 10617, Taiwan), CU(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA), CV(University of Wisconsin-Madison, Department of Astronomy, 475 N. Charter St., Madison WI 53703, USA;), CW(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), CX(Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Laboratório Interinstitucional de e-Astronomia,—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), CY(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA; Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), CZ(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA; Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), DA(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), DB(Harvard-Smithsonian Center for Astrophysics, Harvard University, 60 Garden St., Cambridge MA 02138, USA), DC(Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA), DD(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA; Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa, 277-8583, Japan), DE(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany), DF(Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 220, Santiago, Chile), DG(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), DH(Department of Physics and Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA), DI(Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA), DJ(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany), DK(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA), DL(Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA 15260, USA), DM(UPMC-CNRS, UMR7095, Institut dAstrophysique de Paris, 98bis Boulevard Arago, F-75014, Paris, France), DN(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA; Department of Astronomy, University of California, Berkeley, CA 94720, USA), DO(Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Laboratório Interinstitucional de e-Astronomia,—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), DP(Department of Chemistry and Physics, Kings College, Wilkes Barre, PA, 18711, USA), DQ(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA; Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), DR(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA; Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), DS(Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT, 06520, USA), DT(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), DU(Apache Point Observatory, P.O. Box 59, sunspot, NM 88349, USA; Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), DV(Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT, 06520, USA), DW(INAF—Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34131 Trieste, Italy), DX(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UK), DY(UPMC-CNRS, UMR7095, Institut dAstrophysique de Paris, 98bis Boulevard Arago, F-75014, Paris, France), DZ(Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, F-13388, Marseille, France), EA(Aix-Marseille Université, CNRS/IN2P3, CPPM UMR 7346, F-13288 Marseille, France; UPMC-CNRS, UMR7095, Institut dAstrophysique de Paris, 98bis Boulevard Arago, F-75014, Paris, France; Sorbonne Universités, UPMC (Paris 06), UMR7095, Institut d’Astrophysique de Paris, 98bis Bd. Arago, F-75014, Paris, France), EB(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), Glorieta de la Astronomía, E-18080 Granada, Spain), EC(Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA 15260, USA), ED(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), EE(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), EF(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), EG(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany), EH(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), EI(Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Laboratório Interinstitucional de e-Astronomia,—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), EJ(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), EK(Department of Astronomy and Space Science, Sejong University, Seoul, 143-747, Korea), EL(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), EM(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany), EN(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), EO(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), EP(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), EQ(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA; Department of Astronomy, University of California, Berkeley, CA 94720, USA; Department of Physics, University of California, Berkeley, CA 94720, USA; Berkeley Center for Cosmological Physics, LBL and Department of Physics, University of California, Berkeley, CA 94720, USA), ER(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701), ES(Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany), ET(Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), EU(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), EV(Bldg 510 Brookhaven National Laboratory Upton, NY 11973, USA), EW(Laboratório Interinstitucional de e-Astronomia,—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA), EX(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), EY(Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa, 277-8583, Japan), EZ(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), FA(Aix-Marseille Université, CNRS/IN2P3, CPPM UMR 7346, F-13288 Marseille, France; Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China), FB(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), FC(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), FD(Instituto de Fisíca, Universidad Nacional Autonoma de Mexico, Apdo. Postal 20-364, 01000, D.F, Mexico), FE(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, China), FF(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), FG(Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA; Department of Astronomy, Ohio State University, Columbus, OH 43210, USA), FH(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA; Department of Astronomy, University of California, Berkeley, CA 94720, USA; Department of Physics, University of California, Berkeley, CA 94720, USA), FI(Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA 15260, USA), FJ(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), FK(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), FL(Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China), FM(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, China), FN(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), FO(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA;), FP(National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, China)
%B The Astronomical Journal
%V 151
%D 2016
%8 February 1, 2016
%K cosmology: observations;  surveys
%U http://adsabs.harvard.edu/abs/2016AJ....151...44D
%X In a six-year program started in 2014 July, the Extended Baryon 
Oscillation Spectroscopic Survey (eBOSS) will conduct novel cosmological 
observations using the BOSS spectrograph at Apache Point Observatory. 
These observations will be conducted simultaneously with the Time Domain 
Spectroscopic Survey (TDSS) designed for variability studies and the 
Spectroscopic Identification of eROSITA Sources (SPIDERS) program 
designed for studies of X-ray sources. In particular, eBOSS will measure 
with percent-level precision the distance-redshift relation with baryon 
acoustic oscillations (BAO) in the clustering of matter. eBOSS will use 
four different tracers of the underlying matter density field to vastly 
expand the volume covered by BOSS and map the large-scale-structures 
over the relatively unconstrained redshift range 0.6 < z < 2.2. 
Using more than 250,000 new, spectroscopically confirmed luminous red 
galaxies at a median redshift z = 0.72, we project that eBOSS will yield 
measurements of the angular diameter distance d<SUB>A</SUB>(z) to an 
accuracy of 1.2% and measurements of H(z) to 2.1% when combined with the 
z > 0.6 sample of BOSS galaxies. With ∼195,000 new emission line 
galaxy redshifts, we expect BAO measurements of d<SUB>A</SUB>(z) to an 
accuracy of 3.1% and H(z) to 4.7% at an effective redshift of z = 0.87. 
A sample of more than 500,000 spectroscopically confirmed quasars will 
provide the first BAO distance measurements over the redshift range 0.9 
< z < 2.2, with expected precision of 2.8% and 4.2% on 
d<SUB>A</SUB>(z) and H(z), respectively. Finally, with 60,000 new 
quasars and re-observation of 60,000 BOSS quasars, we will obtain new 
Lyα forest measurements at redshifts z > 2.1 these new data 
will enhance the precision of d<SUB>A</SUB>(z) and H(z) at z > 2.1 by 
a factor of 1.44 relative to BOSS. Furthermore, eBOSS will provide 
improved tests of General Relativity on cosmological scales through 
redshift-space distortion measurements, improved tests for 
non-Gaussianity in the primordial density field, and new constraints on 
the summed mass of all neutrino species. Here, we provide an overview of 
the cosmological goals, spectroscopic target sample, demonstration of 
spectral quality from early data, and projected cosmological constraints 
from eBOSS.
%3 10.3847/0004-6256/151/2/44
%= eprint: arXiv:1508.04473
%@ 0004-6256

%0 Journal Article
%T Accelerating the two-point and three-point galaxy correlation functions using Fourier transforms
%A Slepian, Zachary 
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA <EMAIL>zslepian@cfa.harvard.edu</EMAIL>), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 455
%D 2016
%8 January 1, 2016
%P L31-L35
%K methods: data analysis;  methods: statistical;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.455L..31S
%X Though Fourier transforms (FTs) are a common technique for finding 
correlation functions, they are not typically used in computations of 
the anisotropy of the two-point correlation function (2PCF) about the 
line of sight in wide-angle surveys because the line-of-sight direction 
is not constant on the Cartesian grid. Here we show how FTs can be used 
to compute the multipole moments of the anisotropic 2PCF. We also show 
how FTs can be used to accelerate the 3PCF algorithm of Slepian & 
Eisenstein. In both cases, these FT methods allow one to avoid the 
computational cost of pair counting, which scales as the square of the 
number density of objects in the survey. With the upcoming large data 
sets of Dark Energy Spectroscopic Instrument, Euclid, and Large Synoptic 
Survey Telescope, FT techniques will therefore offer an important 
complement to simple pair or triplet counts.
%3 10.1093/mnrasl/slv133
%= eprint: arXiv:1506.04746
%@ 0035-8711

%0 Journal Article
%T SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: galaxy target selection and large-scale structure catalogues
%A Reid, Beth 
%A Ho, Shirley 
%A Padmanabhan, Nikhil 
%A Percival, Will J. 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A White, Martin 
%A Eisenstein, Daniel J. 
%A Maraston, Claudia 
%A Ross, Ashley J. 
%A Sánchez, Ariel G. 
%A Schlegel, David 
%A Sheldon, Erin 
%A Strauss, Michael A. 
%A Thomas, Daniel 
%A Wake, David 
%A Beutler, Florian 
%A Bizyaev, Dmitry 
%A Bolton, Adam S. 
%A Brownstein, Joel R. 
%A Chuang, Chia-Hsun 
%A Dawson, Kyle 
%A Harding, Paul 
%A Kitaura, Francisco-Shu 
%A Leauthaud, Alexie 
%A Masters, Karen 
%A McBride, Cameron K. 
%A More, Surhud 
%A Olmstead, Matthew D. 
%A Oravetz, Daniel 
%A Nuza, Sebastián E. 
%A Pan, Kaike 
%A Parejko, John 
%A Pforr, Janine 
%A Prada, Francisco 
%A Rodríguez-Torres, Sergio 
%A Salazar-Albornoz, Salvador 
%A Samushia, Lado 
%A Schneider, Donald P. 
%A Scóccola, Claudia G. 
%A Simmons, Audrey 
%A Vargas-Magana, Mariana
%+ AA(Department of Physics, Berkeley Center for Cosmological Physics, University of California, Berkeley, CA, 94720, USA; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA<EMAIL>will.percival@port.ac.uk</EMAIL>), AB(Department of Physics, Bruce and Astrid McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), AC(Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT 06520, USA), AD(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AE(Department of Physics, Center for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AF(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), AG(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AH(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AI(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AJ(Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA), AK(Max-Planck-Institut für extraterrestrische Physik, ch 1312, Giessenbachstr., D-85741 Garching, Germany), AL(Department of Physics, Berkeley Center for Cosmological Physics, University of California, Berkeley, CA, 94720, USA; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AM(Brookhaven National Laboratory, Bldg 510, Upton, New York, NY 11973, USA), AN(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA), AO(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AP(Department of Astronomy, University of Winsconsin-Madison, 475 N. Charter Street, Madison, WI 53706-1582, USA; Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK), AQ(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AR(Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349-0059, USA; Sternberg Astronomical Institute, Moscow State University, 119992 Moscow, Russia), AS(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AT(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AU(Instituto de Física Teórica, (UAM/CSIC), Universidad Autonoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AV(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AW(Department of Astronomy, Case Western Reserve University, 10900 Euclid Ave, Cleveland, OH 44106, USA), AX(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AY(Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan), AZ(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), BA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), BB(Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan), BC(Department of Chemistry and Physics, King's College, Wilkes Barre, PA 18711, USA; Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), BD(Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349-0059, USA), BE(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), BF(Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349-0059, USA), BG(Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT 06520, USA), BH(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Aix Marseille Universit, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, F-13388 Marseille, France), BI(Instituto de Física Teórica, (UAM/CSIC), Universidad Autonoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofisica de Andaluca (CSIC), Glorieta de la Astronoma, E-18080 Granada, Spain), BJ(Instituto de Física Teórica, (UAM/CSIC), Universidad Autonoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), BK(Max-Planck-Institut für extraterrestrische Physik, ch 1312, Giessenbachstr., D-85741 Garching, Germany; Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679 Munich, Germany), BL(Kansas State University, Manhattan, KS 66506, USA; National Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Ave, GE-1060 Tbilisi, Georgia; Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), BM(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), BN(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200 La Laguna, Spain; Facultad de Ciencias Astronómicas y Geofísicas -Universidad Nacional de La Plata, Paseo del Bosque, S/N (1900) La Plata, Argentina; CONICET, Rivadavia 1917, 1033 Buenos Aires, Argentina), BO(Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, NM 88349-0059, USA), BP(Instituto de Fisica, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, Mexico City, México)
%B Monthly Notices of the Royal Astronomical Society
%V 455
%D 2016
%8 January 1, 2016
%P 1553-1573
%K cosmology: observations;  (cosmology:) large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2016MNRAS.455.1553R
%X The Baryon Oscillation Spectroscopic Survey (BOSS), part of the Sloan 
Digital Sky Survey (SDSS) III project, has provided the largest survey 
of galaxy redshifts available to date, in terms of both the number of 
galaxy redshifts measured by a single survey, and the effective 
cosmological volume covered. Key to analysing the clustering of these 
data to provide cosmological measurements is understanding the detailed 
properties of this sample. Potential issues include variations in the 
target catalogue caused by changes either in the targeting algorithm or 
properties of the data used, the pattern of spectroscopic observations, 
the spatial distribution of targets for which redshifts were not 
obtained, and variations in the target sky density due to observational 
systematics. We document here the target selection algorithms used to 
create the galaxy samples that comprise BOSS. We also present the 
algorithms used to create large-scale structure catalogues for the final 
Data Release (DR12) samples and the associated random catalogues that 
quantify the survey mask. The algorithms are an evolution of those used 
by the BOSS team to construct catalogues from earlier data, and have 
been designed to accurately quantify the galaxy sample. The code used, 
designated MKSAMPLE, is released with this paper.
%3 10.1093/mnras/stv2382
%= eprint: arXiv:1509.06529
%@ 0035-8711

%0 Journal Article
%T Modelling galactic conformity with the colour-halo age relation in the Illustris simulation
%A Bray, Aaron D. 
%A Pillepich, Annalisa 
%A Sales, Laura V. 
%A Zhu, Emily 
%A Genel, Shy 
%A Rodriguez-Gomez, Vicente 
%A Torrey, Paul 
%A Nelson, Dylan 
%A Vogelsberger, Mark 
%A Springel, Volker 
%A Eisenstein, Daniel J. 
%A Hernquist, Lars
%+ 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(University of California Riverside, 900 University Avenue, Riverside, CA 92521, USA), AD(Phillips Academy, 180 Main Street, Andover, MA 01810, USA; Harvard College, Cambridge, MA 02138, USA), AE(Columbia University, 116th Street and Broadway, New York, NY 10027, USA), AF(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AG(Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA; TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA), AH(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AI(Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA), AJ(Heidelberg Institute for Theoretical Studies, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany; Zentrum fur Astronomie der Universitat Heidelberg, ARI, Monchhofstr. 12-14, D-69120 Heidelberg, Germany), AK(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AL(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 455
%D 2016
%8 January 1, 2016
%P 185-198
%K galaxies: formation;  galaxies: haloes;  cosmology: theory;  dark matter
%U http://adsabs.harvard.edu/abs/2016MNRAS.455..185B
%X Comparisons between observational surveys and galaxy formation models 
find that dark matter haloes' mass can largely explain their galaxies' 
stellar mass. However, it remains uncertain whether additional 
environmental variables, known as assembly bias, are necessary to 
explain other galaxy properties. We use the Illustris simulation to 
investigate the role of assembly bias in producing galactic conformity 
by considering 18 000 galaxies with M<SUB>stellar</SUB> > 2 × 
10<SUP>9</SUP> M<SUB>⊙</SUB>. We find a significant signal of 
galactic conformity: out to distances of about 10 Mpc, the mean red 
fraction of galaxies around redder galaxies is higher than around bluer 
galaxies at fixed stellar mass. Dark matter haloes exhibit an analogous 
conformity signal, in which the fraction of haloes formed at earlier 
times (old haloes) is higher around old haloes than around younger ones 
at fixed halo mass. A plausible interpretation of galactic conformity is 
the combination of the halo conformity signal with the galaxy 
colour-halo age relation: at fixed stellar mass, particularly towards 
the low-mass end, Illustris' galaxy colours correlate with halo age, 
with the reddest galaxies (often satellites) preferentially found in the 
oldest haloes. We explain the galactic conformity effect with a simple 
semi-empirical model, assigning stellar mass via halo mass (abundance 
matching) and galaxy colour via halo age (age matching). Regarding 
comparison to observations, we conclude that the adopted 
selection/isolation criteria, projection effects, and stacking 
techniques can have a significant impact on the measured amplitude of 
the conformity signal.
%3 10.1093/mnras/stv2316
%= eprint: arXiv:1508.05393
%@ 0035-8711

%0 Journal Article
%T Cosmological implications of baryon acoustic oscillation measurements
%A Aubourg, Éric 
%A Bailey, Stephen 
%A Bautista, Julian E. 
%A Beutler, Florian 
%A Bhardwaj, Vaishali 
%A Bizyaev, Dmitry 
%A Blanton, Michael 
%A Blomqvist, Michael 
%A Bolton, Adam S. 
%A Bovy, Jo 
%A Brewington, Howard 
%A Brinkmann, J. 
%A Brownstein, Joel R. 
%A Burden, Angela 
%A Busca, Nicolás G. 
%A Carithers, William 
%A Chuang, Chia-Hsun 
%A Comparat, Johan 
%A Croft, Rupert A. C. 
%A Cuesta, Antonio J. 
%A Dawson, Kyle S. 
%A Delubac, Timothée 
%A Eisenstein, Daniel J. 
%A Font-Ribera, Andreu 
%A Ge, Jian 
%A Le Goff, J.-M. 
%A Gontcho, Satya Gontcho A. 
%A Gott, J. Richard 
%A Gunn, James E. 
%A Guo, Hong 
%A Guy, Julien 
%A Hamilton, Jean-Christophe 
%A Ho, Shirley 
%A Honscheid, Klaus 
%A Howlett, Cullan 
%A Kirkby, David 
%A Kitaura, Francisco S. 
%A Kneib, Jean-Paul 
%A Lee, Khee-Gan 
%A Long, Dan 
%A Lupton, Robert H. 
%A Magaña, Mariana Vargas 
%A Malanushenko, Viktor 
%A Malanushenko, Elena 
%A Manera, Marc 
%A Maraston, Claudia 
%A Margala, Daniel 
%A McBride, Cameron K. 
%A Miralda-Escudé, Jordi 
%A Myers, Adam D. 
%A Nichol, Robert C. 
%A Noterdaeme, Pasquier 
%A Nuza, Sebastián E. 
%A Olmstead, Matthew D. 
%A Oravetz, Daniel 
%A Pâris, Isabelle 
%A Padmanabhan, Nikhil 
%A Palanque-Delabrouille, Nathalie 
%A Pan, Kaike 
%A Pellejero-Ibanez, Marcos 
%A Percival, Will J. 
%A Petitjean, Patrick 
%A Pieri, Matthew M. 
%A Prada, Francisco 
%A Reid, Beth 
%A Rich, James 
%A Roe, Natalie A. 
%A Ross, Ashley J. 
%A Ross, Nicholas P. 
%A Rossi, Graziano 
%A Rubiño-Martín, Jose Alberto 
%A Sánchez, Ariel G. 
%A Samushia, Lado 
%A Génova-Santos, Ricardo Tanausú 
%A Scóccola, Claudia G. 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Seo, Hee-Jong 
%A Sheldon, Erin 
%A Simmons, Audrey 
%A Skibba, Ramin A. 
%A Slosar, Anže 
%A Strauss, Michael A. 
%A Thomas, Daniel 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Vazquez, Jose Alberto 
%A Viel, Matteo 
%A Wake, David A. 
%A Weaver, Benjamin A. 
%A Weinberg, David H. 
%A Wood-Vasey, W. M. 
%A Yèche, Christophe 
%A Zehavi, Idit 
%A Zhao, Gong-Bo 
%A BOSS Collaboration
%+ AA(APC, Astroparticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon & Léonie Duquet, 75205 Paris Cedex 13, France), AB(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA), AC(APC, Astroparticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon & Léonie Duquet, 75205 Paris Cedex 13, France), AD(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA), AE(Department of Astronomy, University of Washington, Box 351580, Seattle, Washington 98195, USA; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA), AF(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), AG(Center for Cosmology and Particle Physics, New York University, New York, New York 10003, USA), AH(Department of Physics and Astronomy, UC Irvine, 4129 Frederick Reines Hall, Irvine, California 92697, USA), AI(Department Physics and Astronomy, University of Utah, Utah 84112, USA), AJ(Institute for Advanced Study, Einstein Drive, Princeton, New Jersey 08540, USA), AK(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), AL(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), AM(Department Physics and Astronomy, University of Utah, Utah 84112, USA), AN(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom), AO(APC, Astroparticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon & Léonie Duquet, 75205 Paris Cedex 13, France; Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil; Laboratório Interinstitucional de e-Astronomia, - LIneA, Rua Gal.José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil), AP(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA), AQ(Instituto de Fisica Teorica (UAM/CSIC), Universidad Autonoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AR(Instituto de Fisica Teorica (UAM/CSIC), Universidad Autonoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AS(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, Pennsylvania 15213, USA; Astrophysics, University of Oxford, Keble Road, Oxford OX13RH, United Kingdom), AT(Department of Physics, Yale University, 260 Whitney Ave, New Haven, Connecticut 06520, USA; Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Martí i Franquès 1, E08028 Barcelona, Spain), AU(Department Physics and Astronomy, University of Utah, Utah 84112, USA), AV(Laboratoire d'astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny,CH-1290 Versoix, Switzerland), AW(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, Massachusetts 02138, USA), AX(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA), AY(Department of Astronomy, University of Florida, Gainesville, Florida 32611, USA), AZ(CEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, France), BA(Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Martí i Franquès 1, E08028 Barcelona, Spain), BB(Department of Astrophysical Sciences, Princeton University, Ivy Lane, Princeton, New Jersey 08544, USA), BC(Department of Astrophysical Sciences, Princeton University, Ivy Lane, Princeton, New Jersey 08544, USA), BD(Key Laboratory for Research in Galaxies and Cosmology of Chinese Academy of Sciences, Shanghai Astronomical Observatory, Shanghai 200030, China; Department Physics and Astronomy, University of Utah, Utah 84112, USA), BE(LPNHE, CNRS/IN2P3, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, 4 place Jussieu, 75252 Paris CEDEX, France; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA), BF(APC, Astroparticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon & Léonie Duquet, 75205 Paris Cedex 13, France), BG(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, Pennsylvania 15213, USA), BH(Department of Physics, The Ohio State University, Columbus, Ohio 43210, USA; Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, Ohio 43210, USA), BI(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom), BJ(Department of Physics and Astronomy, UC Irvine, 4129 Frederick Reines Hall, Irvine, California 92697, USA), BK(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany), BL(Laboratoire d'astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny,CH-1290 Versoix, Switzerland; CPPM, Aix-Marseille Université, CNRS/IN2P3, Marseille, France), BM(Max-Planck-Institut für Astronomie, Königstuhl 17, D69117 Heidelberg, Germany), BN(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), BO(Department of Astrophysical Sciences, Princeton University, Ivy Lane, Princeton, New Jersey 08544, USA), BP(APC, Astroparticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon & Léonie Duquet, 75205 Paris Cedex 13, France), BQ(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), BR(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), BS(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom; University College London, Gower Street, London WC1E 6BT, United Kingdom), BT(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom), BU(Department of Physics and Astronomy, UC Irvine, 4129 Frederick Reines Hall, Irvine, California 92697, USA), BV(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, Massachusetts 02138, USA), BW(Institució Catalana de Recerca i Estudis Avançats, Barcelona, Spain; Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Martí i Franquès 1, E08028 Barcelona, Spain), BX(Department of Physics and Astronomy, University of Wyoming, Laramie, Wyoming 82071, USA), BY(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom), BZ(Institut d'Astrophysique de Paris, UPMC-CNRS, UMR7095, 98bis boulevard Arago, 75014 Paris, France), CA(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany), CB(Department Physics and Astronomy, University of Utah, Utah 84112, USA), CC(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), CD(INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34131 Trieste, Italy), CE(Department of Physics, Yale University, 260 Whitney Ave, New Haven, Connecticut 06520, USA), CF(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA; CEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, France), CG(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), CH(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), CI(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom), CJ(Institut d'Astrophysique de Paris, UPMC-CNRS, UMR7095, 98bis boulevard Arago, 75014 Paris, France), CK(A*MIDEX, Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, Marseille, France), CL(Instituto de Fisica Teorica (UAM/CSIC), Universidad Autonoma 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), CM(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA; Department of Physics, University of California, 366 LeConte Hall, Berkeley, California 94720, USA), CN(CEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, France), CO(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA), CP(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom; Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, Ohio 43210, USA), CQ(Department of Physics, Drexel University, 3141 Chestnut Street, Philadelphia, Pennsylvania 19104, USA), CR(Department of Astronomy and Space Science, Sejong University, Seoul, 143-747, Korea; CEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, France), CS(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), CT(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstrasse, 85748 Garching, Germany), CU(Department of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, Kansas 666506, USA; National Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Avenue GE-1060 Tbilisi, Georgia), CV(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain), CW(Instituto de Fisica Teorica (UAM/CSIC), Universidad Autonoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049 Cantoblanco, Madrid, Spain), CX(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA), CY(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, Pennsylvania 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, Pennsylvania 16802, USA), CZ(Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, Ohio 43210, USA; Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, Ohio 45701), DA(Brookhaven National Laboratory, 2 Center Road, Upton, New York 11973, USA), DB(Apache Point Observatory, P.O. Box 59, Sunspot, New Mexico 88349-0059, USA), DC(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Dr., San Diego, California 92093 USA), DD(Brookhaven National Laboratory, 2 Center Road, Upton, New York 11973, USA), DE(Department of Astrophysical Sciences, Princeton University, Ivy Lane, Princeton, New Jersey 08544, USA), DF(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom), DG(Center for Cosmology and Particle Physics, New York University, New York, New York 10003, USA), DH(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom), DI(Brookhaven National Laboratory, 2 Center Road, Upton, New York 11973, USA), DJ(INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34131 Trieste, Italy; INFN/National Institute for Nuclear Physics, Via Valerio 2, 34127 Trieste, Italy), DK(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter Street, Madison, Wisconsin, 53706, USA; Department of Physical Sciences, The Open University, Milton Keynes, MK7 6AA, United Kingdom), DL(Center for Cosmology and Particle Physics, New York University, New York, New York 10003, USA), DM(Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, Ohio 43210, USA; Department of Astronomy, Ohio State University, Columbus, Ohio 43210, USA), DN(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, Pennsylvania 15260, USA), DO(CEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, France), DP(Department of Astronomy, Case Western Reserve University, Cleveland, Ohio 44106, USA), DQ(National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, Peoples Republic of China; Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom)
%B Physical Review D
%V 92
%D 2015
%8 December 1, 2015
%K Cosmology;  Dark energy
%U http://adsabs.harvard.edu/abs/2015PhRvD..92l3516A
%X We derive constraints on cosmological parameters and tests of dark 
energy models from the combination of baryon acoustic oscillation (BAO) 
measurements with cosmic microwave background (CMB) data and a recent 
reanalysis of Type Ia supernova (SN) data. In particular, we take 
advantage of high-precision BAO measurements from galaxy clustering and 
the Lyman-α forest (LyaF) in the SDSS-III Baryon Oscillation 
Spectroscopic Survey (BOSS). Treating the BAO scale as an uncalibrated 
standard ruler, BAO data alone yield a high confidence detection of dark 
energy; in combination with the CMB angular acoustic scale they further 
imply a nearly flat universe. Adding the CMB-calibrated physical scale 
of the sound horizon, the combination of BAO and SN data into an 
"inverse distance ladder" yields a measurement of H<SUB>0</SUB>=67.3 
±1.1 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> , with 1.7% precision. 
This measurement assumes standard prerecombination physics but is 
insensitive to assumptions about dark energy or space curvature, so 
agreement with CMB-based estimates that assume a flat Λ CDM 
cosmology is an important corroboration of this minimal cosmological 
model. For constant dark energy (Λ ), our BAO +SN +CMB 
combination yields matter density Ω<SUB>m</SUB>=0.301 
±0.008 and curvature Ω<SUB>k</SUB>=-0.003 ±0.003 . 
When we allow more general forms of evolving dark energy, the BAO +SN 
+CMB parameter constraints are always consistent with flat Λ CDM 
values at ≈1 σ . While the overall χ<SUP>2</SUP> of model 
fits is satisfactory, the LyaF BAO measurements are in moderate (2 - 2.5 
σ ) tension with model predictions. Models with early dark energy 
that tracks the dominant energy component at high redshift remain 
consistent with our expansion history constraints, and they yield a 
higher H<SUB>0</SUB> and lower matter clustering amplitude, improving 
agreement with some low redshift observations. Expansion history alone 
yields an upper limit on the summed mass of neutrino species, 
∑m<SUB>ν</SUB><0.56 eV (95% confidence), improving to 
∑m<SUB>ν</SUB><0.25 eV if we include the lensing signal in the 
Planck CMB power spectrum. In a flat Λ CDM model that allows 
extra relativistic species, our data combination yields 
N<SUB>eff</SUB>=3.43 ±0.26 ; while the LyaF BAO data prefer 
higher N<SUB>eff</SUB> when excluding galaxy BAO, the galaxy BAO alone 
favor N<SUB>eff</SUB>≈3 . When structure growth is extrapolated 
forward from the CMB to low redshift, standard dark energy models 
constrained by our data predict a level of matter clustering that is 
high compared to most, but not all, observational estimates.
%3 10.1103/PhysRevD.92.123516
%= eprint: arXiv:1411.1074
%@ 0556-2821

%0 Journal Article
%T Computing the three-point correlation function of galaxies in O(N^2) time
%A Slepian, Zachary 
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA <EMAIL>zslepian@cfa.harvard.edu</EMAIL>), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 454
%D 2015
%8 December 1, 2015
%P 4142-4158
%K methods: data analysis;  cosmology: large-scale structure of Universe;  methods: data analysis
%U http://adsabs.harvard.edu/abs/2015MNRAS.454.4142S
%X We present an algorithm that computes the multipole coefficients of the 
galaxy three-point correlation function (3PCF) without explicitly 
considering triplets of galaxies. Rather, centring on each galaxy in the 
survey, it expands the radially binned density field in spherical 
harmonics and combines these to form the multipoles without ever 
requiring the relative angle between a pair about the central. This 
approach scales with number and number density in the same way as the 
two-point correlation function, allowing run-times that are comparable, 
and 500 times faster than a naive triplet count. It is exact in angle 
and easily handles edge correction. We demonstrate the algorithm on the 
LasDamas SDSS-DR7 mock catalogues, computing an edge corrected 3PCF out 
to 90 Mpc h<SUP>-1</SUP> in under an hour on modest computing resources. 
We expect this algorithm will render it possible to obtain the 
large-scale 3PCF for upcoming surveys such as Euclid, Large Synoptic 
Survey Telescope (LSST), and Dark Energy Spectroscopic Instrument.
%3 10.1093/mnras/stv2119
%= eprint: arXiv:1506.02040
%@ 0035-8711

%0 Journal Article
%T Abundances, Stellar Parameters, and Spectra from the SDSS-III/APOGEE Survey
%A Holtzman, Jon A. 
%A Shetrone, Matthew 
%A Johnson, Jennifer A. 
%A Allende Prieto, Carlos 
%A Anders, Friedrich 
%A Andrews, Brett 
%A Beers, Timothy C. 
%A Bizyaev, Dmitry 
%A Blanton, Michael R. 
%A Bovy, Jo 
%A Carrera, Ricardo 
%A Chojnowski, S. Drew 
%A Cunha, Katia 
%A Eisenstein, Daniel J. 
%A Feuillet, Diane 
%A Frinchaboy, Peter M. 
%A Galbraith-Frew, Jessica 
%A García Pérez, Ana E. 
%A García-Hernández, D. A. 
%A Hasselquist, Sten 
%A Hayden, Michael R. 
%A Hearty, Fred R. 
%A Ivans, Inese 
%A Majewski, Steven R. 
%A Martell, Sarah 
%A Meszaros, Szabolcs 
%A Muna, Demitri 
%A Nidever, David 
%A Nguyen, Duy Cuong 
%A O'Connell, Robert W. 
%A Pan, Kaike 
%A Pinsonneault, Marc 
%A Robin, Annie C. 
%A Schiavon, Ricardo P. 
%A Shane, Neville 
%A Sobeck, Jennifer 
%A Smith, Verne V. 
%A Troup, Nicholas 
%A Weinberg, David H. 
%A Wilson, John C. 
%A Wood-Vasey, W. M. 
%A Zamora, Olga 
%A Zasowski, Gail
%+ AA(New Mexico State University, Las Cruces, NM 88003, USA <EMAIL>holtz@nmsu.edu,mrhayden@nmsu.edu,feuilldk@nmsu.edu</EMAIL> <ID system="ORCID">0000-0002-9771-9622</ID>), AB(University of Texas at Austin, McDonald Observatory, Fort Davis, TX 79734, USA <EMAIL>shetrone@astro.as.utexas.edu</EMAIL> <ID system="ORCID">0000-0003-0509-2656</ID>), AC(Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA <EMAIL>jaj@astronomy.ohio-state.edu,muna@astronomy.ohio-state.edu</EMAIL> <ID system="ORCID">0000-0001-7258-1834</ID>), AD(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain; <EMAIL>callende@iac.es,agp@iac.es</EMAIL>), AE(Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482, Potsdam, Germany; Laboratório Interinstitucional de e-Astronomía (LIneA), Rua Gal. José Cristino 77, Rio de Janeíro, RJ-20921400, Brasil; <EMAIL>wmwv@pitt.edu</EMAIL>), AF(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <EMAIL>dmbiz@apo.nmsu.edu</EMAIL>), AG(Dept. of Physics and JINA Center for Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556, USA <EMAIL>michael.blanton@gmail.com</EMAIL>), AH(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349-0059, USA <EMAIL>bovy@ias.edu</EMAIL> <ID system="ORCID">0000-0002-3601-133X</ID>), AI(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA <EMAIL>cunha@email.noao.edu</EMAIL>), AJ(Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA;; <EMAIL>p.frinchaboy@tcu.edu</EMAIL> <ID system="ORCID">0000-0001-6855-442X</ID>), AK(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain; <EMAIL>deisenstein@cfa.harvard.edu</EMAIL> <ID system="ORCID">0000-0001-6143-8151</ID>), AL(New Mexico State University, Las Cruces, NM 88003, USA <EMAIL>iii@physics.utah.edu</EMAIL> <ID system="ORCID">0000-0001-9984-0891</ID>), AM(Observatório Nacional, São Cristóvão, Rio de Janeiro, Brazil; University of Arizona, Tucson, AZ 85719, USA; <EMAIL>frh10@psu.edu</EMAIL>), AN(Texas Christian University, Fort Worth, TX 76129, USA; Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA; <EMAIL>srm4n@virginia.edu,aeg4x@virginia.edu,rwo@virginia.edu</EMAIL>), AO(New Mexico State University, Las Cruces, NM 88003, USA <EMAIL>dnidever@umich.edu</EMAIL>), AP(Texas Christian University, Fort Worth, TX 76129, USA <EMAIL>annie@obs-besancon.fr</EMAIL> <ID system="ORCID">0000-0002-0740-8346</ID>), AQ(Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA <EMAIL>rpschiavon@gmail.com</EMAIL>), AR(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain; <EMAIL>vsmith@email.noao.edu</EMAIL>), AS(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain; <EMAIL>gail.zasowski@gmail.com</EMAIL>), AT(New Mexico State University, Las Cruces, NM 88003, USA), AU(New Mexico State University, Las Cruces, NM 88003, USA <ID system="ORCID">0000-0001-7294-9766</ID>), AV(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), AW(Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AX(Dept. of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA <ID system="ORCID">0000-0003-2025-3147</ID>), AY(School of Physics, University of New South Wales, Sydney NSW 2 052, Australia <ID system="ORCID">0000-0002-3430-4163</ID>), AZ(ELTE Gothard Astrophysical Observatory, H-9704 Szombathely, Szent Imre herceg st. 112, Hungary), BA(Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA), BB(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA <ID system="ORCID">0000-0002-1793-3689</ID>), BC(Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, Ontario, Canada), BD(Dept. of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BE(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349-0059, USA), BF(Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA <ID system="ORCID">0000-0002-7549-7766</ID>), BG(Institut UTINAM, OSU THETA, University of Franche-Comté, Besançon, France), BH(Gemini Observatory, 670 N A’Ohoku Place, Hilo, HI 96720, USA; Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, UK), BI(Dept. of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BJ(Dept. of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BK(National Optical Astronomy Observatories, Tucson, AZ 85719, USA), BL(Dept. of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BM(Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA <ID system="ORCID">0000-0001-7775-7261</ID>), BN(Dept. of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BO(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA), BP(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain), BQ(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA)
%B The Astronomical Journal
%V 150
%D 2015
%8 November 1, 2015
%K astronomical databases: miscellaneous;  Galaxy: abundances;  stars: abundances;  surveys
%U http://adsabs.harvard.edu/abs/2015AJ....150..148H
%X The SDSS-III/Apache Point Observatory Galactic Evolution Experiment 
(APOGEE) survey operated from 2011-2014 using the APOGEE 
spectrograph, which collects high-resolution (R ˜ 22,500), near-IR 
(1.51-1.70 μm) spectra with a multiplexing (300 fiber-fed 
objects) capability. We describe the survey data products that are 
publicly available, which include catalogs with radial velocity, stellar 
parameters, and 15 elemental abundances for over 150,000 stars, as well 
as the more than 500,000 spectra from which these quantities are 
derived. Calibration relations for the stellar parameters 
({T}<SUB>{eff</SUB>}, {log} g, [M/H], [α/M]) and abundances (C, N, 
O, Na, Mg, Al, Si, S, K, Ca, Ti, V, Mn, Fe, Ni) are presented and 
discussed. The internal scatter of the abundances within clusters 
indicates that abundance precision is generally between 0.05 and 0.09 
dex across a broad temperature range; it is smaller for some elemental 
abundances within more limited ranges and at high signal-to-noise ratio. 
We assess the accuracy of the abundances using comparison of mean 
cluster metallicities with literature values, APOGEE observations of the 
solar spectrum and of Arcturus, comparison of individual star abundances 
with other measurements, and consideration of the locus of derived 
parameters and abundances of the entire sample, and find that it is 
challenging to determine the absolute abundance scale; external accuracy 
may be good to 0.1-0.2 dex. Uncertainties may be larger at cooler 
temperatures ({T}<SUB>{eff</SUB>}  \lt  4000 {{K}}). Access to the 
public data release and data products is described, and some guidance 
for using the data products is provided.
%3 10.1088/0004-6256/150/5/148
%= eprint: arXiv:1501.04110
%@ 0004-6256

%0 Journal Article
%T PRIMUS: The Effect of Physical Scale on the Luminosity Dependence of Galaxy Clustering via Cross-correlations
%A Bray, Aaron D. 
%A Eisenstein, Daniel J. 
%A Skibba, Ramin A. 
%A Blanton, Michael R. 
%A Coil, Alison L. 
%A Cool, Richard J. 
%A Mendez, Alexander J. 
%A Moustakas, John 
%A Zhu, Guangtun
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA <EMAIL>abray@cfa.harvard.edu</EMAIL>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AC(Department of Physics, Center for Astrophysics and Space Sciences, University of California, 9500 Gilman Dr., La Jolla, San Diego, CA 92093, USA), AD(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AE(Department of Physics, Center for Astrophysics and Space Sciences, University of California, 9500 Gilman Dr., La Jolla, San Diego, CA 92093, USA <ID system="ORCID">0000-0002-2583-5894</ID>), AF(MMT Observatory, 1540 E Second Street, University of Arizona, Tucson, AZ 85721, USA), AG(Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0002-7726-1722</ID>), AH(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA), AI(Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA;)
%B The Astrophysical Journal
%V 811
%D 2015
%8 October 1, 2015
%K cosmology: observations;  galaxies: statistics;  galaxies: evolution;  galaxies: high-redshift;  cosmology: large-scale structure of universe;  surveys
%U http://adsabs.harvard.edu/abs/2015ApJ...811...90B
%X We report small-scale clustering measurements from the PRIsm 
MUlti-object Survey (PRIMUS) spectroscopic redshift survey as a function 
of color and luminosity. We measure the real-space cross-correlations 
between 62,106 primary galaxies with PRIMUS redshifts and a tracer 
population of ∼545,000 photometric galaxies over redshifts from z = 
0.2 to z = 1. We separately fit a power-law model in redshift and 
luminosity to each of three independent color-selected samples of 
galaxies. We report clustering amplitudes at fiducial values of z = 0.5 
and L=1.5{L}<SUP>*</SUP>. The clustering of the red galaxies is ∼ 3 
times as strong as that of the blue galaxies and ∼ 1.5 as strong as 
that of the green galaxies. We also find that the luminosity dependence 
of the clustering is strongly dependent on physical scale, with greater 
luminosity dependence being found between r=0.0625 {h}<SUP>-1</SUP> 
{Mpc} and r=0.25 {h}<SUP>-1</SUP> {Mpc}, compared to the r=0.5 
{h}<SUP>-1</SUP> {Mpc} to r=2 {h}<SUP>-1</SUP> {Mpc} range. Moreover, 
over a range of two orders of magnitude in luminosity, a single 
power-law fit to the luminosity dependence is not sufficient to explain 
the increase in clustering at both the bright and faint ends at the 
smaller scales. We argue that luminosity-dependent clustering at small 
scales is a necessary component of galaxy-halo occupation models for 
blue, star-forming galaxies as well as for red, quenched galaxies.
%3 10.1088/0004-637X/811/2/90
%= eprint: arXiv:1502.01348
%@ 0004-637X

%0 Journal Article
%T The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III
%A Alam, Shadab 
%A Albareti, Franco D. 
%A Allende Prieto, Carlos 
%A Anders, F. 
%A Anderson, Scott F. 
%A Anderton, Timothy 
%A Andrews, Brett H. 
%A Armengaud, Eric 
%A Aubourg, Éric 
%A Bailey, Stephen 
%A Basu, Sarbani 
%A Bautista, Julian E. 
%A Beaton, Rachael L. 
%A Beers, Timothy C. 
%A Bender, Chad F. 
%A Berlind, Andreas A. 
%A Beutler, Florian 
%A Bhardwaj, Vaishali 
%A Bird, Jonathan C. 
%A Bizyaev, Dmitry 
%A Blake, Cullen H. 
%A Blanton, Michael R. 
%A Blomqvist, Michael 
%A Bochanski, John J. 
%A Bolton, Adam S. 
%A Bovy, Jo 
%A Shelden Bradley, A. 
%A Brandt, W. N. 
%A Brauer, D. E. 
%A Brinkmann, J. 
%A Brown, Peter J. 
%A Brownstein, Joel R. 
%A Burden, Angela 
%A Burtin, Etienne 
%A Busca, Nicolás G. 
%A Cai, Zheng 
%A Capozzi, Diego 
%A Carnero Rosell, Aurelio 
%A Carr, Michael A. 
%A Carrera, Ricardo 
%A Chambers, K. C. 
%A Chaplin, William James 
%A Chen, Yen-Chi 
%A Chiappini, Cristina 
%A Chojnowski, S. Drew 
%A Chuang, Chia-Hsun 
%A Clerc, Nicolas 
%A Comparat, Johan 
%A Covey, Kevin 
%A Croft, Rupert A. C. 
%A Cuesta, Antonio J. 
%A Cunha, Katia 
%A da Costa, Luiz N. 
%A Da Rio, Nicola 
%A Davenport, James R. A. 
%A Dawson, Kyle S. 
%A De Lee, Nathan 
%A Delubac, Timothée 
%A Deshpande, Rohit 
%A Dhital, Saurav 
%A Dutra-Ferreira, Letícia 
%A Dwelly, Tom 
%A Ealet, Anne 
%A Ebelke, Garrett L. 
%A Edmondson, Edward M. 
%A Eisenstein, Daniel J. 
%A Ellsworth, Tristan 
%A Elsworth, Yvonne 
%A Epstein, Courtney R. 
%A Eracleous, Michael 
%A Escoffier, Stephanie 
%A Esposito, Massimiliano 
%A Evans, Michael L. 
%A Fan, Xiaohui 
%A Fernández-Alvar, Emma 
%A Feuillet, Diane 
%A Filiz Ak, Nurten 
%A Finley, Hayley 
%A Finoguenov, Alexis 
%A Flaherty, Kevin 
%A Fleming, Scott W. 
%A Font-Ribera, Andreu 
%A Foster, Jonathan 
%A Frinchaboy, Peter M. 
%A Galbraith-Frew, J. G. 
%A García, Rafael A. 
%A García-Hernández, D. A. 
%A García Pérez, Ana E. 
%A Gaulme, Patrick 
%A Ge, Jian 
%A Génova-Santos, R. 
%A Georgakakis, A. 
%A Ghezzi, Luan 
%A Gillespie, Bruce A. 
%A Girardi, Léo 
%A Goddard, Daniel 
%A Gontcho, Satya Gontcho A. 
%A González Hernández, Jonay I. 
%A Grebel, Eva K. 
%A Green, Paul J. 
%A Grieb, Jan Niklas 
%A Grieves, Nolan 
%A Gunn, James E. 
%A Guo, Hong 
%A Harding, Paul 
%A Hasselquist, Sten 
%A Hawley, Suzanne L. 
%A Hayden, Michael 
%A Hearty, Fred R. 
%A Hekker, Saskia 
%A Ho, Shirley 
%A Hogg, David W. 
%A Holley-Bockelmann, Kelly 
%A Holtzman, Jon A. 
%A Honscheid, Klaus 
%A Huber, Daniel 
%A Huehnerhoff, Joseph 
%A Ivans, Inese I. 
%A Jiang, Linhua 
%A Johnson, Jennifer A. 
%A Kinemuchi, Karen 
%A Kirkby, David 
%A Kitaura, Francisco 
%A Klaene, Mark A. 
%A Knapp, Gillian R. 
%A Kneib, Jean-Paul 
%A Koenig, Xavier P. 
%A Lam, Charles R. 
%A Lan, Ting-Wen 
%A Lang, Dustin 
%A Laurent, Pierre 
%A Le Goff, Jean-Marc 
%A Leauthaud, Alexie 
%A Lee, Khee-Gan 
%A Lee, Young Sun 
%A Licquia, Timothy C. 
%A Liu, Jian 
%A Long, Daniel C. 
%A López-Corredoira, Martín 
%A Lorenzo-Oliveira, Diego 
%A Lucatello, Sara 
%A Lundgren, Britt 
%A Lupton, Robert H. 
%A Mack, Claude E., III 
%A Mahadevan, Suvrath 
%A Maia, Marcio A. G. 
%A Majewski, Steven R. 
%A Malanushenko, Elena 
%A Malanushenko, Viktor 
%A Manchado, A. 
%A Manera, Marc 
%A Mao, Qingqing 
%A Maraston, Claudia 
%A Marchwinski, Robert C. 
%A Margala, Daniel 
%A Martell, Sarah L. 
%A Martig, Marie 
%A Masters, Karen L. 
%A Mathur, Savita 
%A McBride, Cameron K. 
%A McGehee, Peregrine M. 
%A McGreer, Ian D. 
%A McMahon, Richard G. 
%A Ménard, Brice 
%A Menzel, Marie-Luise 
%A Merloni, Andrea 
%A Mészáros, Szabolcs 
%A Miller, Adam A. 
%A Miralda-Escudé, Jordi 
%A Miyatake, Hironao 
%A Montero-Dorta, Antonio D. 
%A More, Surhud 
%A Morganson, Eric 
%A Morice-Atkinson, Xan 
%A Morrison, Heather L. 
%A Mosser, Benôit 
%A Muna, Demitri 
%A Myers, Adam D. 
%A Nandra, Kirpal 
%A Newman, Jeffrey A. 
%A Neyrinck, Mark 
%A Nguyen, Duy Cuong 
%A Nichol, Robert C. 
%A Nidever, David L. 
%A Noterdaeme, Pasquier 
%A Nuza, Sebastián E. 
%A O'Connell, Julia E. 
%A O'Connell, Robert W. 
%A O'Connell, Ross 
%A Ogando, Ricardo L. C. 
%A Olmstead, Matthew D. 
%A Oravetz, Audrey E. 
%A Oravetz, Daniel J. 
%A Osumi, Keisuke 
%A Owen, Russell 
%A Padgett, Deborah L. 
%A Padmanabhan, Nikhil 
%A Paegert, Martin 
%A Palanque-Delabrouille, Nathalie 
%A Pan, Kaike 
%A Parejko, John K. 
%A Pâris, Isabelle 
%A Park, Changbom 
%A Pattarakijwanich, Petchara 
%A Pellejero-Ibanez, M. 
%A Pepper, Joshua 
%A Percival, Will J. 
%A Pérez-Fournon, Ismael 
%A P´rez-Ra`fols, Ignasi 
%A Petitjean, Patrick 
%A Pieri, Matthew M. 
%A Pinsonneault, Marc H. 
%A Porto de Mello, Gustavo F. 
%A Prada, Francisco 
%A Prakash, Abhishek 
%A Price-Whelan, Adrian M. 
%A Protopapas, Pavlos 
%A Raddick, M. Jordan 
%A Rahman, Mubdi 
%A Reid, Beth A. 
%A Rich, James 
%A Rix, Hans-Walter 
%A Robin, Annie C. 
%A Rockosi, Constance M. 
%A Rodrigues, Thaíse S. 
%A Rodríguez-Torres, Sergio 
%A Roe, Natalie A. 
%A Ross, Ashley J. 
%A Ross, Nicholas P. 
%A Rossi, Graziano 
%A Ruan, John J. 
%A Rubiño-Martín, J. A. 
%A Rykoff, Eli S. 
%A Salazar-Albornoz, Salvador 
%A Salvato, Mara 
%A Samushia, Lado 
%A Sánchez, Ariel G. 
%A Santiago, Basílio 
%A Sayres, Conor 
%A Schiavon, Ricardo P. 
%A Schlegel, David J. 
%A Schmidt, Sarah J. 
%A Schneider, Donald P. 
%A Schultheis, Mathias 
%A Schwope, Axel D. 
%A Scóccola, C. G. 
%A Scott, Caroline 
%A Sellgren, Kris 
%A Seo, Hee-Jong 
%A Serenelli, Aldo 
%A Shane, Neville 
%A Shen, Yue 
%A Shetrone, Matthew 
%A Shu, Yiping 
%A Silva Aguirre, V. 
%A Sivarani, Thirupathi 
%A Skrutskie, M. F. 
%A Slosar, Anže 
%A Smith, Verne V. 
%A Sobreira, Flávia 
%A Souto, Diogo 
%A Stassun, Keivan G. 
%A Steinmetz, Matthias 
%A Stello, Dennis 
%A Strauss, Michael A. 
%A Streblyanska, Alina 
%A Suzuki, Nao 
%A Swanson, Molly E. C. 
%A Tan, Jonathan C. 
%A Tayar, Jamie 
%A Terrien, Ryan C. 
%A Thakar, Aniruddha R. 
%A Thomas, Daniel 
%A Thomas, Neil 
%A Thompson, Benjamin A. 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Troup, Nicholas W. 
%A Vargas-Magaña, Mariana 
%A Vazquez, Jose A. 
%A Verde, Licia 
%A Viel, Matteo 
%A Vogt, Nicole P. 
%A Wake, David A. 
%A Wang, Ji 
%A Weaver, Benjamin A. 
%A Weinberg, David H. 
%A Weiner, Benjamin J. 
%A White, Martin 
%A Wilson, John C. 
%A Wisniewski, John P. 
%A Wood-Vasey, W. M. 
%A Ye`che, Christophe 
%A York, Donald G. 
%A Zakamska, Nadia L. 
%A Zamora, O. 
%A Zasowski, Gail 
%A Zehavi, Idit 
%A Zhao, Gong-Bo 
%A Zheng, Zheng 
%A Zhou, Xu 
%A Zhou, Zhimin 
%A Zou, Hu 
%A Zhu, Guangtun
%+ AA(McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), AB(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AC(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), AD(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AE(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), AF(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AG(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA; PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA), AH(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), AI(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris, France), AJ(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), AK(Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101, USA), AL(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris, France), AM(Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA; Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA), AN(Department of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556, USA), AO(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802, USA), AP(Department of Physics and Astronomy, Vanderbilt University, VU Station 1807, Nashville, TN 37235, USA), AQ(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), AR(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA; Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), AS(Department of Physics and Astronomy, Vanderbilt University, VU Station 1807, Nashville, TN 37235, USA), AT(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA; Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA; Sternberg Astronomical Institute, Moscow State University, Universitetskij Prosp. 13, Moscow 119992, Russia), AU(University of Pennsylvania, Department of Physics and Astronomy, 219 South 33rd Street, Philadelphia, PA 19104, USA), AV(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AW(Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA), AX(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA; Rider University, 2083 Lawrenceville Road, Lawrenceville, NJ 08648, USA), AY(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AZ(Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA;), BA(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), BB(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA; Department of Physics, The Pennsylvania State University, University Park, PA 16802, USA), BC(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), BD(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), BE(George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A. and M. University, Department of Physics and Astronomy, 4242 TAMU, College Station, TX 77843, USA), BF(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), BG(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), BH(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), BI(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris, France; Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Laboratório Interinstitucional de e-Astronomia, - LIneA, Rua Gal.José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), BJ(Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA), BK(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), BL(Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Laboratório Interinstitucional de e-Astronomia, - LIneA, Rua Gal.José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), BM(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA), BN(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), BO(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA), BP(School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK; Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark), BQ(Department of Statistics, Bruce and Astrid McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA), BR(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Laboratório Interinstitucional de e-Astronomia, - LIneA, Rua Gal.José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), BS(Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), BT(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), BU(Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstrasse D-85741 Garching, Germany), BV(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), BW(Lowell Observatory, 1400 W. Mars Hill Road, Flagstaff AZ 86001, USA; Western Washington University, Department of Physics & Astronomy, 516 High Street, Bellingham WA 98225, USA), BX(McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), BY(Institut de Ciències del Cosmos, Universitat de Barcelona/IEEC, Barcelona E-08028, Spain; Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT, 06520, USA), BZ(Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA), CA(Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Laboratório Interinstitucional de e-Astronomia, - LIneA, Rua Gal.José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), CB(Department of Astronomy, University of Florida, Bryant Space Science Center, Gainesville, FL 32611-2055, USA), CC(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), CD(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), CE(Department of Physics and Geology, Northern Kentucky University, Highland Heights, KY 41099, USA), CF(Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290, Versoix, Switzerland), CG(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802, USA), CH(Department of Physical Sciences, Embry-Riddle Aeronautical University, 600 South Clyde Morris Boulevard, Daytona Beach, FL 32114, USA), CI(Laboratório Interinstitucional de e-Astronomia, - LIneA, Rua Gal.José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Universidade Federal do Rio de Janeiro, Observatório do Valongo, Ladeira do Pedro Antônio 43, 20080-090 Rio de Janeiro, Brazil; Departamento de Física, Universidade Federal do Rio Grande do Norte, 59072-970, Natal, RN, Brazil), CJ(Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstrasse D-85741 Garching, Germany), CK(Centre de Physique des Particules de Marseille, Aix-Marseille Université, CNRS/IN2P3, F-13288 Marseille, France), CL(Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA), CM(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK), CN(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, USA), CO(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), CP(School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK; Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark), CQ(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), CR(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA; Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA; Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA 30332, USA), CS(Centre de Physique des Particules de Marseille, Aix-Marseille Université, CNRS/IN2P3, F-13288 Marseille, France), CT(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), CU(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), CV(Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA), CW(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), CX(Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), CY(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA; Faculty of Sciences, Department of Astronomy and Space Sciences, Erciyes University, 38039 Kayseri, Turkey), CZ(Institut d’Astrophysique de Paris, UPMC-CNRS, UMR7095, 98 bis Boulevard Arago, F-75014, Paris, France), DA(Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2, Helsinki FI-00140, Finland), DB(Department of Astronomy, Van Vleck Observatory, Wesleyan University, Middletown, CT 06459, USA), DC(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; Computer Sciences Corporation, 3700 San Martin Drive, Baltimore, MD 21218, USA), DD(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), DE(Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT, 06520, USA), DF(Department of Physics and Astronomy, Texas Christian University, 2800 South University Drive, Fort Worth, TX 76129, USA), DG(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), DH(Laboratoire AIM, CEA/DSM—CNRS—Univ. Paris Diderot—IRFU/SAp, Centre de Saclay, F-91191 Gif-sur-Yvette Cedex, France), DI(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), DJ(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain; Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA), DK(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), DL(Department of Astronomy, University of Florida, Bryant Space Science Center, Gainesville, FL 32611-2055, USA), DM(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), DN(Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstrasse D-85741 Garching, Germany), DO(Observatório Nacional, Rua Gal. 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A’Ohoku Place, Hilo, HI 96720, USA; Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK), JG(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA), JH(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), JI(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), JJ(Université de Nice Sophia-Antipolis, CNRS, Observatoire de Côte d’Azur, Laboratoire Lagrange, BP 4229, F-06304 Nice Cedex 4, France), JK(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), JL(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), JM(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, USA), JN(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), JO(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), JP(Instituto de Ciencias del Espacio (CSIC-IEEC), Facultad de Ciencias, Campus UAB, E-08193, Bellaterra, Spain), JQ(Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA), JR(Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA; Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China), JS(University of Texas at Austin, Hobby-Eberly Telescope, 32 Fowlkes Road, McDonald Observatory, TX 79734-3005, USA), JT(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), JU(Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark), JV(Indian Institute of Astrophysics, II Block, Koramangala, Bangalore 560 034, India), JW(Department of Astronomy, University of Virginia, P.O. 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José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), KB(Department of Physics and Astronomy, Vanderbilt University, VU Station 1807, Nashville, TN 37235, USA; Department of Physics, Fisk University, 1000 17th Avenue North, Nashville, TN 37208, USA), KC(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), KD(Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark; Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, NSW 2006, Australia), KE(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA;), KF(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), KG(Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa, 277-8583, Japan), KH(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, USA), KI(Department of Astronomy, University of Florida, Bryant Space Science Center, Gainesville, FL 32611-2055, USA), KJ(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), KK(Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA; Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802, USA; The Penn State Astrobiology Research Center, Pennsylvania State University, University Park, PA 16802, USA), KL(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), KM(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK; SEPnet, South East Physics Network, UK), KN(Department of Astronomy, University of Florida, Bryant Space Science Center, Gainesville, FL 32611-2055, USA), KO(Department of Physics and Astronomy, Texas Christian University, 2800 South University Drive, Fort Worth, TX 76129, USA), KP(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), KQ(School of Physics and Astronomy, University of St Andrews, St Andrews, Fife, KY16 9SS, UK), KR(Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA), KS(McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), KT(Brookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA), KU(Institut de Ciències del Cosmos, Universitat de Barcelona/IEEC, Barcelona E-08028, Spain; Institució Catalana de Recerca i Estudis Avançats, Barcelona E-08010, Spain; Institute of Theoretical Astrophysics, University of Oslo, NO-0315 Oslo, Norway), KV(INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34131 Trieste, Italy; INFN/National Institute for Nuclear Physics, Via Valerio 2, I-34127 Trieste, Italy), KW(Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA), KX(Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison WI 53703, USA; Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK), KY(Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101, USA), KZ(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), LA(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), LB(Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA), LC(Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA; Department of Physics, University of California, Berkeley, CA 94720, USA), LD(Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA), LE(H.L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA), LF(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA;), LG(CEA, Centre de Saclay, Irfu/SPP, F-91191 Gif-sur-Yvette, France), LH(Department of Astronomy and Astrophysics and the Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA), LI(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), LJ(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain), LK(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), LL(Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106, USA), LM(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK; National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China), LN(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), LO(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China), LP(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China), LQ(Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China), LR(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA;)
%B The Astrophysical Journal Supplement Series
%V 219
%D 2015
%8 July 1, 2015
%K atlases;  catalogs;  surveys
%U http://adsabs.harvard.edu/abs/2015ApJS..219...12A
%X The third generation of the Sloan Digital Sky Survey (SDSS-III) took 
data from 2008 to 2014 using the original SDSS wide-field imager, the 
original and an upgraded multi-object fiber-fed optical spectrograph, a 
new near-infrared high-resolution spectrograph, and a novel optical 
interferometer. All of the data from SDSS-III are now made public. In 
particular, this paper describes Data Release 11 (DR11) including all 
data acquired through 2013 July, and Data Release 12 (DR12) adding data 
acquired through 2014 July (including all data included in previous data 
releases), marking the end of SDSS-III observing. Relative to our 
previous public release (DR10), DR12 adds one million new spectra of 
galaxies and quasars from the Baryon Oscillation Spectroscopic Survey 
(BOSS) over an additional 3000 deg<SUP>2</SUP> of sky, more than triples 
the number of H-band spectra of stars as part of the Apache Point 
Observatory (APO) Galactic Evolution Experiment (APOGEE), and includes 
repeated accurate radial velocity measurements of 5500 stars from the 
Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS). 
The APOGEE outputs now include the measured abundances of 15 different 
elements for each star. In total, SDSS-III added 5200 deg<SUP>2</SUP> of 
ugriz imaging; 155,520 spectra of 138,099 stars as part of the Sloan 
Exploration of Galactic Understanding and Evolution 2 (SEGUE-2) survey; 
2,497,484 BOSS spectra of 1,372,737 galaxies, 294,512 quasars, and 
247,216 stars over 9376 deg<SUP>2</SUP>; 618,080 APOGEE spectra of 
156,593 stars; and 197,040 MARVELS spectra of 5513 stars. Since its 
first light in 1998, SDSS has imaged over 1/3 of the Celestial sphere in 
five bands and obtained over five million astronomical spectra.
%3 10.1088/0067-0049/219/1/12
%= eprint: arXiv:1501.00963
%@ 0067-0049

%0 Journal Article
%T Dark Matter Halo Models of Stellar Mass-dependent Galaxy Clustering in PRIMUS+DEEP2 at 0.2>z>1.2
%A Skibba, Ramin A. 
%A Coil, Alison L. 
%A Mendez, Alexander J. 
%A Blanton, Michael R. 
%A Bray, Aaron D. 
%A Cool, Richard J. 
%A Eisenstein, Daniel J. 
%A Guo, Hong 
%A Miyaji, Takamitsu 
%A Moustakas, John 
%A Zhu, Guangtun
%+ AA(Department of Physics, Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USA <EMAIL>raminskibba@gmail.com</EMAIL>), AB(Department of Physics, Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USA <ID system="ORCID">0000-0002-2583-5894</ID>), AC(Department of Physics, Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USA; Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0002-7726-1722</ID>), AD(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AE(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AF(MMT Observatory, University of Arizona, 1540 E Second Street, Tucson, AZ 85721, USA), AG(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AH(Key Laboratory for Research in Galaxies and Cosmology of Chinese Academy of Sciences, Shanghai Astronomical Observatory, Shanghai 200030, China <ID system="ORCID">0000-0003-4936-8247</ID>), AI(Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, Baja California, Mexico; Visiting Scholar, University of California, San Diego <ID system="ORCID">0000-0002-7562-485X</ID>), AJ(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA), AK(Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA;)
%B The Astrophysical Journal
%V 807
%D 2015
%8 July 1, 2015
%K dark matter;  galaxies: evolution;  galaxies: halos;  large-scale structure of universe;  methods: analytical;  methods: statistical
%U http://adsabs.harvard.edu/abs/2015ApJ...807..152S
%X We utilize ΛCDM halo occupation models of galaxy clustering to 
investigate the evolving stellar mass dependent clustering of galaxies 
in the PRIsm MUlti-object Survey (PRIMUS) and DEEP2 Redshift Survey over 
the past eight billion years of cosmic time, between 0.2\lt z\lt 1.2. 
These clustering measurements provide new constraints on the connections 
between dark matter halo properties and galaxy properties in the context 
of the evolving large-scale structure of the universe. Using both an 
analytic model and a set of mock galaxy catalogs, we find a strong 
correlation between central galaxy stellar mass and dark matter halo 
mass over the range {M}<SUB>{halo</SUB>}˜ 
{10}<SUP>11</SUP>-{10}<SUP>13</SUP> {h}<SUP>-1</SUP> 
{M}<SUB>⊙ </SUB>, approximately consistent with previous 
observations and theoretical predictions. However, the stellar-to-halo 
mass relation and the mass scale where star formation efficiency reaches 
a maximum appear to evolve more strongly than predicted by other models, 
including models based primarily on abundance-matching constraints. We 
find that the fraction of satellite galaxies in halos of a given mass 
decreases significantly from z˜ 0.5 to z˜ 0.9, partly due to the 
fact that halos at fixed mass are rarer at higher redshift and have 
lower abundances. We also find that the 
{M}<SUB>1</SUB>/{M}<SUB>{min</SUB>} ratio, a model parameter that 
quantifies the critical mass above which halos host at least one 
satellite, decreases from ≈ 20 at z˜ 0 to ≈ 13 at z˜ 0.9. 
Considering the evolution of the subhalo mass function vis-à-vis 
satellite abundances, this trend has implications for relations between 
satellite galaxies and halo substructures and for intracluster mass, 
which we argue has grown due to stripped and disrupted satellites 
between z˜ 0.9 and z˜ 0.5.
%3 10.1088/0004-637X/807/2/152
%= eprint: arXiv:1503.00731
%@ 0004-637X

%0 Journal Article
%T PRIMUS: The Relationship between Star Formation and AGN Accretion
%A Azadi, Mojegan 
%A Aird, James 
%A Coil, Alison L. 
%A Moustakas, John 
%A Mendez, Alexander J. 
%A Blanton, Michael R. 
%A Cool, Richard J. 
%A Eisenstein, Daniel J. 
%A Wong, Kenneth C. 
%A Zhu, Guangtun
%+ AA(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Dr., La Jolla, San Diego, CA 92093, USA <ID system="ORCID">0000-0001-6004-9728</ID>), AB(Department of Physics, Durham University, Durham DH1 3LE, UK;  Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), AC(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Dr., La Jolla, San Diego, CA 92093, USA <ID system="ORCID">0000-0002-2583-5894</ID>), AD(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA), AE(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Dr., La Jolla, San Diego, CA 92093, USA <ID system="ORCID">0000-0002-7726-1722</ID>), AF(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AG(MMT Observatory, 1540 E Second Street, University of Arizona, Tucson, AZ 85721, USA), AH(Harvard College Observatory, 60 Garden St., Cambridge, MA 02138, USA), AI(Institute of Astronomy and Astrophysics, Academia Sinica, No.1, Section 4, Roosevelt Rd., Taipei 10617, Taiwan <ID system="ORCID">0000-0002-8459-7793</ID>), AJ(Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA)
%B The Astrophysical Journal
%V 806
%D 2015
%8 June 1, 2015
%K galaxies: active;  galaxies: evolution;  X-rays: galaxies
%U http://adsabs.harvard.edu/abs/2015ApJ...806..187A
%X We study the evidence for a connection between active galactic nuclei 
(AGNs) fueling and star formation by investigating the relationship 
between the X-ray luminosities of AGNs and the star formation rates 
(SFRs) of their host galaxies. We identify a sample of 309 AGNs with 
{10}<SUP>41</SUP>\lt {L}<SUB>X</SUB>\lt {10}<SUP>44</SUP> erg 
s<SUP>-1</SUP> at 0.2\lt z\lt 1.2 in the PRIMUS redshift survey. 
We find AGNs in galaxies with a wide range of SFR at a given 
L<SUB>X</SUB>. We do not find a significant correlation between SFR and 
the observed instantaneous L<SUB>X</SUB> for star-forming AGN host 
galaxies. However, there is a weak but significant correlation between 
the mean L<SUB>X</SUB> and SFR of detected AGNs in star-forming 
galaxies, which likely reflects that L<SUB>X</SUB> varies on shorter 
timescales than SFR. We find no correlation between stellar mass and 
L<SUB>X</SUB> within the AGN population. Within both populations of 
star-forming and quiescent galaxies, we find a similar power-law 
distribution in the probability of hosting an AGN as a function of 
specific accretion rate. Furthermore, at a given stellar mass, we find a 
star-forming galaxy ˜2-3 more likely than a quiescent galaxy 
to host an AGN of a given specific accretion rate. The probability of a 
galaxy hosting an AGN is constant across the main sequence of star 
formation. These results indicate that there is an underlying connection 
between star formation and the presence of AGNs, but AGNs are often 
hosted by quiescent galaxies.
%3 10.1088/0004-637X/806/2/187
%= eprint: arXiv:1407.1975
%@ 0004-637X

%0 Journal Article
%T PRIMUS: Effects of Galaxy Environment on the Quiescent Fraction Evolution at z < 0.8
%A Hahn, ChangHoon 
%A Blanton, Michael R. 
%A Moustakas, John 
%A Coil, Alison L. 
%A Cool, Richard J. 
%A Eisenstein, Daniel J. 
%A Skibba, Ramin A. 
%A Wong, Kenneth C. 
%A Zhu, Guangtun
%+ AA(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA <EMAIL>chh327@nyu.edu</EMAIL> <ID system="ORCID">0000-0003-1197-0902</ID>), AB(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AC(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA), AD(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Dr., La Jolla, CA 92093, USA <ID system="ORCID">0000-0002-2583-5894</ID>), AE(MMT Observatory, University of Arizona, 1540 E Second Street, Tucson AZ 85721, USA), AF(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AG(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Dr., La Jolla, CA 92093, USA), AH(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA), AI(Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA;)
%B The Astrophysical Journal
%V 806
%D 2015
%8 June 1, 2015
%K cosmology: observations;  galaxies: evolution;  galaxies: groups: general;  galaxies: star formation;  galaxies: statistics
%U http://adsabs.harvard.edu/abs/2015ApJ...806..162H
%X We investigate the effects of galaxy environment on the evolution of the 
quiescent fraction ({{f}<SUB>Q</SUB>}) from z=0.8 to 0.0 using 
spectroscopic redshifts and multi-wavelength imaging data from the PRIsm 
MUlti-object Survey (PRIMUS) and the Sloan Digital Sky Survey (SDSS). 
Our stellar mass limited galaxy sample consists of ˜14,000 PRIMUS 
galaxies within z = 0.2-0.8 and ˜64,000 SDSS galaxies within z 
= 0.05-0.12. We classify the galaxies as quiescent or star-forming 
(SF) based on an evolving specific star formation cut, and as low or 
high density environments based on fixed cylindrical aperture 
environment measurements on a volume-limited environment defining 
population. For quiescent and SF galaxies in low or high density 
environments, we examine the evolution of their stellar mass function 
(SMF). Then using the SMFs we compute 
{{f}<SUB>Q</SUB>}({{M}<SUB>*</SUB>}) and quantify its evolution within 
our redshift range. We find that the quiescent fraction is higher at 
higher masses and in denser environments. The quiescent fraction rises 
with cosmic time for all masses and environments. At a fiducial mass of 
{{10}<SUP>10.5</SUP>} {{M}<SUB>⊙ </SUB>}, from z˜ 0.7 to 0.1, 
the quiescent fraction rises by 15% at the lowest environments and by 
25% at the highest environments we measure. These results suggest that 
for a minority of galaxies their cessation of star formation is due to 
external influences on them. In other words, in the recent universe a 
substantial fraction of the galaxies that cease forming stars do so due 
to internal processes.
%3 10.1088/0004-637X/806/2/162
%= eprint: arXiv:1412.7162
%@ 0004-637X

%0 Journal Article
%T Measuring the Luminosity and Virial Black Hole Mass Dependence of Quasar-Galaxy Clustering At z ˜ 0.8
%A Krolewski, Alex G. 
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA <ID system="ORCID">0000-0003-2183-7021</ID>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA)
%B The Astrophysical Journal
%V 803
%D 2015
%8 April 1, 2015
%K galaxies: active;  large-scale structure of universe;  quasars: general
%U http://adsabs.harvard.edu/abs/2015ApJ...803....4K
%X We study the dependence of quasar clustering on quasar luminosity and 
black hole mass by measuring the angular overdensity of photometrically 
selected galaxies imaged by the Wide-field Infrared Survey Explorer 
(WISE) about z ˜ 0.8 quasars from SDSS. By measuring the 
quasar-galaxy cross-correlation function and using photometrically 
selected galaxies, we achieve a higher density of tracer objects and a 
more sensitive detection of clustering than measurements of the quasar 
autocorrelation function. We test models of quasar formation and 
evolution by measuring the luminosity dependence of clustering 
amplitude. We find a significant overdensity of WISE galaxies about z 
˜ 0.8 quasars at 0.2-6.4 h<SUP>-1</SUP> Mpc in projected 
comoving separation. We find no appreciable increase in clustering 
amplitude with quasar luminosity across a decade in luminosity, and a 
power-law fit between luminosity and clustering amplitude gives an 
exponent of -0.01 ± 0.06 (1 σ error). We also fail to 
find a significant relationship between clustering amplitude and black 
hole mass, although our dynamic range in true mass is suppressed due to 
the large uncertainties in virial black hole mass estimates. Our results 
indicate that a small range in host dark matter halo mass maps to a 
large range in quasar luminosity.
%3 10.1088/0004-637X/803/1/4
%= eprint: arXiv:1501.03898
%@ 0004-637X