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101. A Deep Learning Approach to Galaxy Cluster X-ray Masses

Author: Michelle Ntampaka, Ruediger Pakmor, Mark Vogelsberger, Daisuke Nagai, Annalisa Pillepich, Paul Torrey, Lars Hernquist, Federico Marinacci, Alexey Vikhlinin, Dylan Nelson, Daniel J. Eisenstein, J. ZuHone, Ntampaka M., Zuhone J., Eisenstein D., Nagai D., Vikhlinin A., Hernquist L., Marinacci F., Nelson D., Pakmor R., Pillepich A., Torrey P., and Vogelsberger M.
Subjects: Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Convolutional neural network, Luminosity, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Galaxy cluster, 0105 earth and related environmental sciences, Physics, methods: statistical, business.industry, Deep learning, Contrast (statistics), Astronomy and Astrophysics, Sample (graphics), galaxies: clusters: general, Space and Planetary Science, X-rays: galaxies: clusters, Artificial intelligence, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a machine-learning approach for estimating galaxy cluster masses from Chandra mock images. We utilize a Convolutional Neural Network (CNN), a deep machine learning tool commonly used in image recognition tasks. The CNN is trained and tested on our sample of 7,896 Chandra X-ray mock observations, which are based on 329 massive clusters from the IllustrisTNG simulation. Our CNN learns from a low resolution spatial distribution of photon counts and does not use spectral information. Despite our simplifying assumption to neglect spectral information, the resulting mass values estimated by the CNN exhibit small bias in comparison to the true masses of the simulated clusters (-0.02 dex) and reproduce the cluster masses with low intrinsic scatter, 8% in our best fold and 12% averaging over all. In contrast, a more standard core-excised luminosity method achieves 15-18% scatter. We interpret the results with an approach inspired by Google DeepDream and find that the CNN ignores the central regions of clusters, which are known to have high scatter with mass., Comment: 10 pages, 6 figures, accepted for publication in The Astrophysical Journal
Published: 2018
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102. Baryon acoustic oscillations from the complete SDSS-III Ly α -quasar cross-correlation function at z = 2.4

Author: Hélion du Mas des Bourboux, Jean-Marc Le Goff, Michael Blomqvist, Nicolás G. Busca, Julien Guy, James Rich, Christophe Yèche, Julian E. Bautista, Étienne Burtin, Kyle S. Dawson, Daniel J. Eisenstein, Andreu Font-Ribera, David Kirkby, Jordi Miralda-Escudé, Pasquier Noterdaeme, Nathalie Palanque-Delabrouille, Isabelle Pâris, Patrick Petitjean, Ignasi Pérez-Ràfols, Matthew M. Pieri, Nicholas P. Ross, David J. Schlegel, Donald P. Schneider, Anže Slosar, David H. Weinberg, Pauline Zarrouk, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Large-scale structure of Universe, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Cosmological parameters, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Measure (mathematics), 0103 physical sciences, Dark energy, cosmological parameters, Anisotropy, dark energy, 010303 astronomy & astrophysics, STFC, Physics, Cross-correlation, 010308 nuclear & particles physics, RCUK, Quasar, Astronomy and Astrophysics, Function (mathematics), Redshift, Space and Planetary Science, Baryon acoustic oscillations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a measurement of baryon acoustic oscillations (BAO) in the cross-correlation of quasars with the Ly$\alpha$-forest flux-transmission at a mean redshift $z=2.40$. The measurement uses the complete SDSS-III data sample: 168,889 forests and 234,367 quasars from the SDSS Data Release DR12. In addition to the statistical improvement on our previous study using DR11, we have implemented numerous improvements at the analysis level allowing a more accurate measurement of this cross-correlation. We also developed the first simulations of the cross-correlation allowing us to test different aspects of our data analysis and to search for potential systematic errors in the determination of the BAO peak position. We measure the two ratios $D_{H}(z=2.40)/r_{d} = 9.01 \pm 0.36$ and $D_{M}(z=2.40)/r_{d} = 35.7 \pm 1.7$, where the errors include marginalization over the non-linear velocity of quasars and the metal - quasar cross-correlation contribution, among other effects. These results are within $1.8\sigma$ of the prediction of the flat-$\Lambda$CDM model describing the observed CMB anisotropies. We combine this study with the Ly$\alpha$-forest auto-correlation function [2017A&A...603A..12B], yielding $D_{H}(z=2.40)/r_{d} = 8.94 \pm 0.22$ and $D_{M}(z=2.40)/r_{d} = 36.6 \pm 1.2$, within $2.3\sigma$ of the same flat-$\Lambda$CDM model., Comment: accepted by A&A
Published: 2017
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103. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample

Author: Nicholas P. Ross, Erin Sheldon, Anže Slosar, Mariana Vargas Magaña, Gong-Bo Zhao, Elena Malanushenko, Adam S. Bolton, Ashley J. Ross, Daniel J. Eisenstein, Daniel Thomas, Sergio Rodríguez-Torres, Salvador Salazar-Albornoz, Shun Saito, David H. Weinberg, Kyle S. Dawson, Christophe Yèche, Daniel Oravetz, Claudia Maraston, Francisco Prada, Beth Reid, Stephanie Escoffier, Shadab Alam, Jan Niklas Grieb, Ariel G. Sánchez, Florian Beutler, Claudia G. Scóccola, Nathalie Palanque-Delabrouille, Nikhil Padmanabhan, Matthew D. Olmstead, Jose Alberto Vazquez, David A. Wake, Viktor Malanushenko, Lado Samushia, Molly E. C. Swanson, Jonathan Blazek, Patrick Petitjean, Antonio J. Cuesta, Nick Hand, Graziano Rossi, Jeremy L. Tinker, Joel R. Brownstein, Licia Verde, Dmitry Bizyaev, Hee-Jong Seo, Kaike Pan, David J. Schlegel, Karen Kinemuchi, Donald P. Schneider, Rita Tojeiro, Will J. Percival, Yuting Wang, Héctor Gil-Marín, Michael A. Strauss, Adrian M. Price-Whelan, Robert C. Nichol, Audrey Simmons, Siddharth Satpathy, Natalie A. Roe, Cameron K. McBride, Angela Burden, Martin White, Marcos Pellejero-Ibanez, Metin Ata, Chia-Hsun Chuang, W. Michael Wood-Vasey, Francisco S. Kitaura, Shirley Ho, Johan Comparat, D. Kirkby, Stephen Bailey, Zhongxu Zhai, Jose Alberto Rubino-Martin, Idit Zehavi, Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, BOSS, Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), ANR-16-CE31-0021,eBOSS,Sondes cosmologiques de la gravitation et de l'énergie noire(2016), Vázquez, Jose Alberto, Universitat de Barcelona, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay
Subjects: Ciencias Astronómicas, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Ciencias Físicas, Cosmic microwave background, Astrophysics, distance scale, 01 natural sciences, purl.org/becyt/ford/1 [https], Redshift-space distortions, QB Astronomy, ST/M001709/1, 010303 astronomy & astrophysics, R2C, QC, QB, Physics, ST/N00180X/1, Clusters of galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ~DC~, Angular diameter distance, observations [cosmology], Cosmology, symbols, astro-ph.CO, Baryon acoustic oscillations, large-scale structure of Universe, BDC, CIENCIAS NATURALES Y EXACTAS, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Cúmuls de galàxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, symbols.namesake, 0103 physical sciences, STFC, Cosmologia, 010308 nuclear & particles physics, RCUK, DAS, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Galaxy, Redshift, Astronomía, QC Physics, Space and Planetary Science, cosmology: observations, Dark energy, ST/N000668/1, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract: We present cosmological results from the final galaxy clustering data set of the Baryon Oscillation Spectroscopic Survey, part of the Sloan Digital Sky Survey III. Our combined galaxy sample comprises 1.2 million massive galaxies over an effective area of 9329 deg2 and volume of 18.7 Gpc3, divided into three partially overlapping redshift slices centred at effective redshifts 0.38, 0.51 and 0.61. We measure the angular diameter distance DM and Hubble parameter H from the baryon acoustic oscillation (BAO) method, in combinationwith a cosmic microwave background prior on the sound horizon scale, after applying reconstruction to reduce non-linear effects on the BAO feature. Using the anisotropic clustering of the pre-reconstruction density field, we measure the product DMH from the Alcock-Paczynski (AP) effect and the growth of structure, quantified by fσ8(z), from redshift-space distortions (RSD). We combine individual measurements presented in seven companion papers into a set of consensus values and likelihoods, obtaining constraints that are tighter and more robust than those from any one method; in particular, the AP measurement from sub-BAO scales sharpens constraints from post-reconstruction BAOs by breaking degeneracy between DM and H. Combined with Planck 2016 cosmic microwave background measurements, our distance scale measurements simultaneously imply curvature ΩK = 0.0003 ± 0.0026 and a dark energy equation-of-state parameter ω =-1.01 ± 0.06, in strong affirmation of the spatially flat cold dark matter (CDM) model with a cosmological constant (ΛCDM). Our RSD measurements of fσ8, at 6 per cent precision, are similarly consistent with this model. When combined with supernova Ia data, we find H0 = 67.3 ± 1.0 kms-1 Mpc-1 even for our most general dark energy model, in tension with some direct measurements. Adding extra relativistic species as a degree of freedom loosens the constraint only slightly, to H0 = 67.8 ± 1.2 kms-1 Mpc-1. Assuming flat ΛCDM, we find Ωm = 0.310 ± 0.005 and H0 = 67.6 ± 0.5 kms-1 Mpc-1, and we find a 95 per cent upper limit of 0.16 eV c-2 on the neutrino mass sum., La lista completa de autores que integran el documento puede consultarse en el archivo., Facultad de Ciencias Astronómicas y Geofísicas
Published: 2017
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104. Emulating galaxy clustering and galaxy-galaxy lensing into the deeply nonlinear regime: methodology, information, and forecasts

Author: Marc Metchnik, B. Wibking, Philip A. Pinto, Andrés N. Salcedo, David H. Weinberg, Douglas Ferrer, Lehman H. Garrison, Daniel J. Eisenstein, and Jeremy L. Tinker
Subjects: Astroparticle physics, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Library science, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Galaxy, Graduate research, Space and Planetary Science, 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The combination of galaxy-galaxy lensing (GGL) with galaxy clustering is one of the most promising routes to determining the amplitude of matter clustering at low redshifts. We show that extending clustering+GGL analyses from the linear regime down to $\sim 0.5 \, h^{-1}$ Mpc scales increases their constraining power considerably, even after marginalizing over a flexible model of non-linear galaxy bias. Using a grid of cosmological N-body simulations, we construct a Taylor-expansion emulator that predicts the galaxy autocorrelation $\xi_{\text{gg}}(r)$ and galaxy-matter cross-correlation $\xi_{\text{gm}}(r)$ as a function of $\sigma_8$, $\Omega_m$, and halo occupation distribution (HOD) parameters, which are allowed to vary with large scale environment to represent possible effects of galaxy assembly bias. We present forecasts for a fiducial case that corresponds to BOSS LOWZ galaxy clustering and SDSS-depth weak lensing (effective source density $\sim 0.3$ arcmin$^{-2}$). Using tangential shear and projected correlation function measurements over $0.5 \leq r_p \leq 30 \, h^{-1}$ Mpc yields a 1.8% constraint on the parameter combination $\sigma_8\Omega_m^{0.58}$, a factor of two better than a constraint that excludes non-linear scales ($r_p > 2 \, h^{-1}$ Mpc, $4 \, h^{-1}$ Mpc for $\gamma_t,w_p$). Much of this improvement comes from the non-linear clustering information, which breaks degeneracies among HOD parameters that would otherwise degrade the inference of matter clustering from GGL. Increasing the effective source density to $3$ arcmin$^{-2}$ sharpens the constraint on $\sigma_8\Omega_m^{0.58}$ by a further factor of two. With robust modeling into the non-linear regime, low-redshift measurements of matter clustering at the 1-percent level with clustering+GGL alone are well within reach of current data sets such as those provided by the Dark Energy Survey., Comment: 23 pages, 7 figures
Published: 2017

105. The Apache Point Observatory Galactic Evolution Experiment (APOGEE)

Author: Steven R. Majewski, Ricardo P. Schiavon, Peter M. Frinchaboy, Carlos Allende Prieto, Robert Barkhouser, Dmitry Bizyaev, Basil Blank, Sophia Brunner, Adam Burton, Ricardo Carrera, S. Drew Chojnowski, Kátia Cunha, Courtney Epstein, Greg Fitzgerald, Ana E. García Pérez, Fred R. Hearty, Chuck Henderson, Jon A. Holtzman, Jennifer A. Johnson, Charles R. Lam, James E. Lawler, Paul Maseman, Szabolcs Mészáros, Matthew Nelson, Duy Coung Nguyen, David L. Nidever, Marc Pinsonneault, Matthew Shetrone, Stephen Smee, Verne V. Smith, Todd Stolberg, Michael F. Skrutskie, Eric Walker, John C. Wilson, Gail Zasowski, Friedrich Anders, Sarbani Basu, Stephane Beland, Michael R. Blanton, Jo Bovy, Joel R. Brownstein, Joleen Carlberg, William Chaplin, Cristina Chiappini, Daniel J. Eisenstein, Yvonne Elsworth, Diane Feuillet, Scott W. Fleming, Jessica Galbraith-Frew, Rafael A. García, D. Aníbal García-Hernández, Bruce A. Gillespie, Léo Girardi, James E. Gunn, Sten Hasselquist, Michael R. Hayden, Saskia Hekker, Inese Ivans, Karen Kinemuchi, Mark Klaene, Suvrath Mahadevan, Savita Mathur, Benoît Mosser, Demitri Muna, Jeffrey A. Munn, Robert C. Nichol, Robert W. O’Connell, John K. Parejko, A. C. Robin, Helio Rocha-Pinto, Matthias Schultheis, Aldo M. Serenelli, Neville Shane, Victor Silva Aguirre, Jennifer S. Sobeck, Benjamin Thompson, Nicholas W. Troup, David H. Weinberg, Olga Zamora, The University of Western Australia (UWA), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), National University of Singapore (NUS), Department of Psychology, St John's University, School of Physics and Astronomy [Birmingham], University of Birmingham [Birmingham], Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), School of Physics and Astronomy, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Department of Physics and Astronomy [Aarhus], and Aarhus University [Aarhus]
Subjects: RED-GIANT STARS, abundances [galaxy], kinematics and dynamics [galaxy], EXPLORING HALO SUBSTRUCTURE, Metallicity, Milky Way, FOS: Physical sciences, CHEMICAL EVOLUTION, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, STELLAR POPULATIONS, Observatory, GLOBULAR-CLUSTERS, structure [galaxy], 0103 physical sciences, EARLY-TYPE GALAXIES, AST-1616636, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, QB, SOLAR-TYPE STARS, 010308 nuclear & particles physics, RCUK, Astronomy, Astronomy and Astrophysics, formation [galaxy], Astrophysics - Astrophysics of Galaxies, Galaxy, RESOLUTION INFRARED-SPECTROSCOPY, stellar content [galaxy], Radial velocity, Interstellar medium, Stars, Star cluster, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), evolution [galaxy], DIGITAL SKY SURVEY, MILKY-WAY, AST-1109178, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology
Abstract: The Apache Point Observatory Galactic Evolution Experiment (APOGEE), one of the programs in the Sloan Digital Sky Survey III (SDSS-III), has now completed its systematic, homogeneous spectroscopic survey sampling all major populations of the Milky Way. After a three year observing campaign on the Sloan 2.5-m Telescope, APOGEE has collected a half million high resolution (R~22,500), high S/N (>100), infrared (1.51-1.70 microns) spectra for 146,000 stars, with time series information via repeat visits to most of these stars. This paper describes the motivations for the survey and its overall design---hardware, field placement, target selection, operations---and gives an overview of these aspects as well as the data reduction, analysis and products. An index is also given to the complement of technical papers that describe various critical survey components in detail. Finally, we discuss the achieved survey performance and illustrate the variety of potential uses of the data products by way of a number of science demonstrations, which span from time series analysis of stellar spectral variations and radial velocity variations from stellar companions, to spatial maps of kinematics, metallicity and abundance patterns across the Galaxy and as a function of age, to new views of the interstellar medium, the chemistry of star clusters, and the discovery of rare stellar species. As part of SDSS-III Data Release 12, all of the APOGEE data products are now publicly available., Submitted to The Astronomical Journal: 50 pages, including 38 figures, 4 tables, and 5 appendices
Published: 2017
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106. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey:On the measurement of growth rate using galaxy correlation functions

Author: Francisco-Shu Kitaura, Martin White, Rita Tojeiro, Chia-Hsun Chuang, Daniel Thomas, Shadab Alam, Jan Niklas Grieb, Florian Beutler, Hee-Jong Seo, Matthew D. Olmstead, Shirley Ho, Salvador Salazar-Albornoz, Ariel G. Sánchez, Joel R. Brownstein, Will J. Percival, Daniel J. Eisenstein, Siddharth Satpathy, Neta A. Bahcall, and Jeremy L. Tinker
Subjects: Cosmology and Gravitation, statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Redshift-space distortions, symbols.namesake, Theory of relativity, 0103 physical sciences, Planck, dark energy, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Sigma, Astronomy, Astronomy and Astrophysics, Galaxy, Redshift, Baryon, Space and Planetary Science, symbols, Dark energy, astro-ph.CO, large-scale structure of Universe, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a measurement of the linear growth rate of structure, \textit{f} from the Sloan Digital Sky Survey III (SDSS III) Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 12 (DR12) using Convolution Lagrangian Perturbation Theory (CLPT) with Gaussian Streaming Redshift-Space Distortions (GSRSD) to model the two point statistics of BOSS galaxies in DR12. The BOSS-DR12 dataset includes 1,198,006 massive galaxies spread over the redshift range $0.2 < z < 0.75$. These galaxy samples are categorized in three redshift bins. Using CLPT-GSRSD in our analysis of the combined sample of the three redshift bins, we report measurements of $f \sigma_8$ for the three redshift bins. We find $f \sigma_8 = 0.430 \pm 0.054$ at $z_{\rm eff} = 0.38$, $f \sigma_8 = 0.452 \pm 0.057$ at $z_{\rm eff} = 0.51$ and $f \sigma_8 = 0.457 \pm 0.052$ at $z_{\rm eff} = 0.61$. Our results are consistent with the predictions of Planck $\Lambda$CDM-GR. Our constraints on the growth rates of structure in the Universe at different redshifts serve as a useful probe, which can help distinguish between a model of the Universe based on dark energy and models based on modified theories of gravity. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS. The measurements and likelihoods presented here are combined with others in Alam et al. 2016 to produce the final cosmological constraints from BOSS., Comment: This is one of the companion papers of the SDSS DR12 final cosmological result. Submitted to MNRAS. 15 pages, 7 figures, 2 tables. The present draft is a reviewed version submitted to MNRAS after getting reviewer's comments
Published: 2017
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107. PRIMUS+DEEP2: The Dependence of Galaxy Clustering on Stellar Mass and Specific Star Formation Rate at 0.2 <z< 1.2

Author: Alison L. Coil, John Moustakas, Alexander J. Mendez, and Daniel J. Eisenstein
Subjects: Stellar mass, Population, Dark matter, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Atomic, Particle and Plasma Physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Nuclear, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], Physics, large-scale structure of universe, education.field_of_study, 010308 nuclear & particles physics, Star formation, Molecular, Astronomy and Astrophysics, Cosmic variance, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, halos [galaxies], Space and Planetary Science, Halo, high-redshift [galaxies], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract: We present results on the clustering properties of galaxies as a function of both stellar mass and specific star formation rate (sSFR) using data from the PRIMUS and DEEP2 galaxy redshift surveys spanning 0.2 < z < 1.2. We use spectroscopic redshifts of over 100,000 galaxies covering an area of 7.2 deg^2 over five separate fields on the sky, from which we calculate cosmic variance errors. We find that the galaxy clustering amplitude is as strong of a function of sSFR as of stellar mass, and that at a given sSFR, it does not significantly depend on stellar mass within the range probed here. We further find that within the star-forming population and at a given stellar mass, galaxies above the main sequence of star formation with higher sSFR are less clustered than galaxies below the main sequence with lower sSFR. We also find that within the quiescent population, galaxies with higher sSFR are less clustered than galaxies with lower sSFR, at a given stellar mass. We show that the galaxy clustering amplitude smoothly increases with both increasing stellar mass and decreasing sSFR, implying that galaxies likely evolve across the main sequence, not only along it, before galaxies eventually become quiescent. These results imply that the stellar mass to halo mass relation, which connects galaxies to dark matter halos, likely depends on sSFR., Comment: 17 pages, 7 figures, accepted to ApJ
Published: 2017
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108. New white dwarf stars in the Sloan Digital Sky Survey Data Release 10

Author: Detlev Koester, Ingrid Domingos Pelisoli, Atsuko Nitta, B. Külebi, Paolo Giommi, Patrick Dufour, Daniel J. Eisenstein, Souza Oliveira Kepler, J. E. S. Costa, S. J. Kleinman, Alejandra D. Romero, Gustavo Ourique, Stefan Jordan, and Alberto Rebassa-Mansergas
Subjects: media_common.quotation_subject, Subdwarfs, Brown dwarf, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Astrophysics::Solar and Stellar Astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, media_common, Physics, White dwarfs, Astronomy, White dwarf, Astronomy and Astrophysics, Catalogues, Planetary nebula, magnetic field [Stars], Astrophysics - Solar and Stellar Astrophysics, Anãs brancas, Space and Planetary Science, Sky, Catalogos astronomicos, Astrophysics::Earth and Planetary Astrophysics, Blue dwarf, Main sequence
Abstract: We report the discovery of 9 089 new spectroscopically confirmed white dwarfs and subdwarfs in the Sloan Digital Sky Survey Data Release 10. We obtain Teff, log g and mass for hydrogen atmosphere white dwarf stars (DAs) and helium atmosphere white dwarf stars (DBs), and estimate the calcium/helium abundances for the white dwarf stars with metallic lines (DZs) and carbon/helium for carbon dominated spectra DQs. We found 1 central star of a planetary nebula, 2 new oxygen spectra on helium atmosphere white dwarfs, 71 DQs, 42 hot DO/PG1159s, 171 white dwarf+main sequence star binaries, 206 magnetic DAHs, 327 continuum dominated DCs, 397 metal polluted white dwarfs, 450 helium dominated white dwarfs, 647 subdwarfs and 6888 new hydrogen dominated white dwarf stars., Comment: 11 pages, 10 figures, accepted for publication in the MNRAS
Published: 2014
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109. Testing the Detection Significance on the Large-scale Structure by a JWST Deep Field Survey

Author: Lehman H. Garrison, Douglas Ferrer, Daniel J. Eisenstein, and Hao Y. Zhang
Subjects: Physics, 010504 meteorology & atmospheric sciences, Hubble Deep Field, Dark matter, Order (ring theory), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Cosmology, Galaxy, symbols.namesake, Space and Planetary Science, 0103 physical sciences, symbols, Halo, Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: In preparation for deep extragalactic imaging with the James Webb Space Telescope, we explore the clustering of massive halos at $z=8$ and $10$ using a large N-body simulation. We find that halos with masses $10^9$ to $10^{11}$ $h^{-1}\;M_\odot$, which are those expected to host galaxies detectable with JWST, are highly clustered with bias factors ranging from 5 and 30 depending strongly on mass, as well as on redshift and scale. This results in correlation lengths of 5--10$h^{-1}\;{\rm Mpc}$, similar to that of today's galaxies. Our results are based on a simulation of 130 billion particles in a box of $250h^{-1}\;{\rm Mpc}$ size using our new high-accuracy ABACUS simulation code, the corrections to cosmological initial conditions of (Garrison et al. 2016, 2016MNRAS.461.4125G), and the Planck 2015 cosmology. We use variations between sub-volumes to estimate the detectability of the clustering. Because of the very strong inter-halo clustering, we find that surveys of order 25$h^{-1}\;{\rm Mpc}$ comoving transverse size may be able to detect the clustering of $z=8$--$10$ galaxies with only 500-1000 survey objects if the galaxies indeed occupy the most massive dark matter halos.
Published: 2019
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110. The clustering of galaxies in the SDSS-III DR10 Baryon Oscillation Spectroscopic Survey: no detectable colour dependence of distance scale or growth rate measurements

Author: Molly E. C. Swanson, Donald P. Schneider, Will J. Percival, Daniel J. Eisenstein, David A. Wake, Luiz N. da Costa, Jeremy L. Tinker, Demitri Muna, Flavia Sobreira, Marc Manera, Marcio A. G. Maia, Francesco Montesano, Hong Guo, Florian Beutler, Idit Zehavi, Alina Streblyanska, Joel R. Brownstein, A. Carnero, Lado Samushia, Daniel Thomas, Angela Burden, Ashley J. Ross, Gong-Bo Zhao, J. Brinkmann, Rita Tojeiro, Shirley Ho, Ariel G. Sánchez, Robert C. Nichol, Sebastián E. Nuza, Ramin A. Skibba, and University of St Andrews. School of Physics and Astronomy
Subjects: Length scale, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, Large-scale structure of Universe, Dark matter, FOS: Physical sciences, Astrophysics, Correlation function (astronomy), 01 natural sciences, 0103 physical sciences, QB Astronomy, observations [Cosmology], 010303 astronomy & astrophysics, QC, QB, Physics, Distance scale, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxy, Redshift, Baryon, QC Physics, Amplitude, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the clustering of galaxies, as a function of their colour, from Data Release Ten (DR10) of the SDSS-III Baryon Oscillation Spectroscopic Survey. We select 122,967 galaxies with 0.43 < z < 0.7 into a "Blue" sample and 131,969 into a "Red" sample based on k+e corrected (to z=0.55) r-i colours and i band magnitudes. The samples are chosen to each contain more than 100,000 galaxies, have similar redshift distributions, and maximize the difference in clustering amplitude. The Red sample has a 40% larger bias than the Blue (b_Red/b_Blue = 1.39+-0.04), implying the Red galaxies occupy dark matter halos with an average mass that is 0.5 log Mo greater. Spherically averaged measurements of the correlation function, \xi 0, and the power spectrum are used to locate the position of the baryon acoustic oscillation (BAO) feature of both samples. Using \xi 0, we obtain distance scales, relative to our reference LCDM cosmology, of 1.010+-0.027 for the Red sample and 1.005+-0.031 for the Blue. After applying reconstruction, these measurements improve to 1.013+/-0.020 for the Red sample and 1.008+-0.026 for the Blue. For each sample, measurements of \xi 0 and the second multipole moment, \xi 2, of the anisotropic correlation function are used to determine the rate of structure growth, parameterized by f\sigma 8. We find f\sigma 8,Red = 0.511+-0.083, f\sigma 8,Blue = 0.509+/-0.085, and f\sigma 8,Cross = 0.423+-0.061 (from the cross-correlation between the Red and Blue samples). We use the covariance between the bias and growth measurements obtained from each sample and their cross-correlation to produce an optimally-combined measurement of f\sigma 8,comb = 0.443+-0.055. In no instance do we detect significant differences in distance scale or structure growth measurements obtained from the Blue and Red samples., Comment: Accepted by MNRAS, typos fixed, references updated
Published: 2013
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111. Observational probes of cosmic acceleration

Author: Adam G. Riess, David H. Weinberg, Eduardo Rozo, Christopher M. Hirata, Michael J. Mortonson, and Daniel J. Eisenstein
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMIC cancer database, Equation of state (cosmology), Cosmic microwave background, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Metric expansion of space, Gravitation, Dark energy, Baryon acoustic oscillations, Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious experimental efforts to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski test, and direct measurements of H_0. We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from GR, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and CMB data. We also show the level of precision required for other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets with broad applications, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales., Comment: 289 pages, 55 figures. Accepted for publication in Physics Reports. Description of changes since original version --- fractionally small but significant in total --- is available at http://www.astronomy.ohio-state.edu/~dhw/Review
Published: 2013
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112. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements and the strong power of f(z) 8(z) on constraining dark energy

Author: Ariel G. Sánchez, David H. Weinberg, Nikhil Padmanabhan, Florian Beutler, Joel R. Brownstein, Chia-Hsun Chuang, Francisco Prada, Daniel Thomas, Jon Brinkmann, Xiaoying Xu, Daniel J. Eisenstein, Marc Manera, Eyal A. Kazin, David J. Schlegel, Antonio J. Cuesta, and Donald P. Schneider
Subjects: Physics, Cosmic microwave background, Shape of the universe, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, Baryon, Amplitude, Space and Planetary Science, Dark energy, Cluster analysis, Astrophysics::Galaxy Astrophysics
Abstract: We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyse the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift z = 0.57 of the sample, on the Hubble expansion rate H(z), the angular-diameter distance DA(z), the normalized growth rate f (z)σ8(z), the physical matter density Ωmh2, and the biased amplitude of matter fluctuation bσ8(z). We obtain {H(0.57), DA(0.57), f (0.57)σ8(0.57), Ωmh2, bσ8(0.57)} = {87.6+6.7−6.8 kms−1 Mpc−1, 1396 ± 73 Mpc, 0.428 ± 0.066, 0.126+0.008 -0.010 ,1.19 ± 0.14} and their covariance matrix as well. 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 [i.e. 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. We show that the major power on constraining dark energy from the anisotropic galaxy clustering signal, as compared to the angular-averaged one (monopole), arises from including the normalized growth rate f (z)σ8(z). In the case of the cosmological model assuming a constant dark energy equation of state and a flat universe (wCDM), our single-probe CMASS constraints, combined with CMB (WMAP9+SPT), yield a value for the dark energy equation-of-state parameter of w = −0.90 ± 0.11. Therefore, it is important to include f (z)σ8(z) while investigating the nature of dark energy with current and upcoming large-scale galaxy surveys.
Published: 2013
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113. Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe

Author: Michael R. Blanton, Matthew A. Bershady, Bela Abolfathi, Franco D. Albareti, Carlos Allende Prieto, Andres Almeida, Javier Alonso-García, Friedrich Anders, Scott F. Anderson, Brett Andrews, Erik Aquino-Ortíz, Alfonso Aragón-Salamanca, Maria Argudo-Fernández, Eric Armengaud, Eric Aubourg, Vladimir Avila-Reese, Carles Badenes, Stephen Bailey, Kathleen A. Barger, Jorge Barrera-Ballesteros, Curtis Bartosz, Dominic Bates, Falk Baumgarten, Julian Bautista, Rachael Beaton, Timothy C. Beers, Francesco Belfiore, Chad F. Bender, Andreas A. Berlind, Mariangela Bernardi, Florian Beutler, Jonathan C. Bird, Dmitry Bizyaev, Guillermo A. Blanc, Michael Blomqvist, Adam S. Bolton, Médéric Boquien, Jura Borissova, Remco van den Bosch, Jo Bovy, William N. Brandt, Jonathan Brinkmann, Joel R. Brownstein, Kevin Bundy, Adam J. Burgasser, Etienne Burtin, Nicolás G. Busca, Michele Cappellari, Maria Leticia Delgado Carigi, Joleen K. Carlberg, Aurelio Carnero Rosell, Ricardo Carrera, Nancy J. Chanover, Brian Cherinka, Edmond Cheung, Yilen Gómez Maqueo Chew, Cristina Chiappini, Peter Doohyun Choi, Drew Chojnowski, Chia-Hsun Chuang, Haeun Chung, Rafael Fernando Cirolini, Nicolas Clerc, Roger E. Cohen, Johan Comparat, Luiz da Costa, Marie-Claude Cousinou, Kevin Covey, Jeffrey D. Crane, Rupert A. C. Croft, Irene Cruz-Gonzalez, Daniel Garrido Cuadra, Katia Cunha, Guillermo J. Damke, Jeremy Darling, Roger Davies, Kyle Dawson, Axel de la Macorra, Flavia Dell’Agli, Nathan De Lee, Timothée Delubac, Francesco Di Mille, Aleks Diamond-Stanic, Mariana Cano-Díaz, John Donor, Juan José Downes, Niv Drory, Hélion du Mas des Bourboux, Christopher J. Duckworth, Tom Dwelly, Jamie Dyer, Garrett Ebelke, Arthur D. Eigenbrot, Daniel J. Eisenstein, Eric Emsellem, Mike Eracleous, Stephanie Escoffier, Michael L. Evans, Xiaohui Fan, Emma Fernández-Alvar, J. G. Fernandez-Trincado, Diane K. Feuillet, Alexis Finoguenov, Scott W. Fleming, Andreu Font-Ribera, Alexander Fredrickson, Gordon Freischlad, Peter M. Frinchaboy, Carla E. Fuentes, Lluís Galbany, R. Garcia-Dias, D. A. García-Hernández, Patrick Gaulme, Doug Geisler, Joseph D. Gelfand, Héctor Gil-Marín, Bruce A. Gillespie, Daniel Goddard, Violeta Gonzalez-Perez, Kathleen Grabowski, Paul J. Green, Catherine J. Grier, James E. Gunn, Hong Guo, Julien Guy, Alex Hagen, ChangHoon Hahn, Matthew Hall, Paul Harding, Sten Hasselquist, Suzanne L. Hawley, Fred Hearty, Jonay I. Gonzalez Hernández, Shirley Ho, David W. Hogg, Kelly Holley-Bockelmann, Jon A. Holtzman, Parker H. Holzer, Joseph Huehnerhoff, Timothy A. Hutchinson, Ho Seong Hwang, Héctor J. Ibarra-Medel, Gabriele da Silva Ilha, Inese I. Ivans, KeShawn Ivory, Kelly Jackson, Trey W. Jensen, Jennifer A. Johnson, Amy Jones, Henrik Jönsson, Eric Jullo, Vikrant Kamble, Karen Kinemuchi, David Kirkby, Francisco-Shu Kitaura, Mark Klaene, Gillian R. Knapp, Jean-Paul Kneib, Juna A. Kollmeier, Ivan Lacerna, Richard R. Lane, Dustin Lang, David R. Law, Daniel Lazarz, Youngbae Lee, Jean-Marc Le Goff, Fu-Heng Liang, Cheng Li, Hongyu Li, Jianhui Lian, Marcos Lima, Lihwai Lin, Yen-Ting Lin, Sara Bertran de Lis, Chao Liu, Miguel Angel C. de Icaza Lizaola, Dan Long, Sara Lucatello, Britt Lundgren, Nicholas K. MacDonald, Alice Deconto Machado, Chelsea L. MacLeod, Suvrath Mahadevan, Marcio Antonio Geimba Maia, Roberto Maiolino, Steven R. Majewski, Elena Malanushenko, Viktor Malanushenko, Arturo Manchado, Shude Mao, Claudia Maraston, Rui Marques-Chaves, Thomas Masseron, Karen L. Masters, Cameron K. McBride, Richard M. McDermid, Brianne McGrath, Ian D. McGreer, Nicolás Medina Peña, Matthew Melendez, Andrea Merloni, Michael R. Merrifield, Szabolcs Meszaros, Andres Meza, Ivan Minchev, Dante Minniti, Takamitsu Miyaji, Surhud More, John Mulchaey, Francisco Müller-Sánchez, Demitri Muna, Ricardo R. Munoz, Adam D. Myers, Preethi Nair, Kirpal Nandra, Janaina Correa do Nascimento, Alenka Negrete, Melissa Ness, Jeffrey A. Newman, Robert C. Nichol, David L. Nidever, Christian Nitschelm, Pierros Ntelis, Julia E. O’Connell, Ryan J. Oelkers, Audrey Oravetz, Daniel Oravetz, Zach Pace, Nelson Padilla, Nathalie Palanque-Delabrouille, Pedro Alonso Palicio, Kaike Pan, John K. Parejko, Taniya Parikh, Isabelle Pâris, Changbom Park, Alim Y. Patten, Sebastien Peirani, Marcos Pellejero-Ibanez, Samantha Penny, Will J. Percival, Ismael Perez-Fournon, Patrick Petitjean, Matthew M. Pieri, Marc Pinsonneault, Alice Pisani, Radosław Poleski, Francisco Prada, Abhishek Prakash, Anna Bárbara de Andrade Queiroz, M. Jordan Raddick, Anand Raichoor, Sandro Barboza Rembold, Hannah Richstein, Rogemar A. Riffel, Rogério Riffel, Hans-Walter Rix, Annie C. Robin, Constance M. Rockosi, Sergio Rodríguez-Torres, A. Roman-Lopes, Carlos Román-Zúñiga, Margarita Rosado, Ashley J. Ross, Graziano Rossi, John Ruan, Rossana Ruggeri, Eli S. Rykoff, Salvador Salazar-Albornoz, Mara Salvato, Ariel G. Sánchez, D. S. Aguado, José R. Sánchez-Gallego, Felipe A. Santana, Basílio Xavier Santiago, Conor Sayres, Ricardo P. Schiavon, Jaderson da Silva Schimoia, Edward F. Schlafly, David J. Schlegel, Donald P. Schneider, Mathias Schultheis, William J. Schuster, Axel Schwope, Hee-Jong Seo, Zhengyi Shao, Shiyin Shen, Matthew Shetrone, Michael Shull, Joshua D. Simon, Danielle Skinner, M. F. Skrutskie, Anže Slosar, Verne V. Smith, Jennifer S. Sobeck, Flavia Sobreira, Garrett Somers, Diogo Souto, David V. Stark, Keivan Stassun, Fritz Stauffer, Matthias Steinmetz, Thaisa Storchi-Bergmann, Alina Streblyanska, Guy S. Stringfellow, Genaro Suárez, Jing Sun, Nao Suzuki, Laszlo Szigeti, Manuchehr Taghizadeh-Popp, Baitian Tang, Charling Tao, Jamie Tayar, Mita Tembe, Johanna Teske, Aniruddha R. Thakar, Daniel Thomas, Benjamin A. Thompson, Jeremy L. Tinker, Patricia Tissera, Rita Tojeiro, Hector Hernandez Toledo, Sylvain de la Torre, Christy Tremonti, Nicholas W. Troup, Octavio Valenzuela, Inma Martinez Valpuesta, Jaime Vargas-González, Mariana Vargas-Magaña, Jose Alberto Vazquez, Sandro Villanova, M. Vivek, Nicole Vogt, David Wake, Rene Walterbos, Yuting Wang, Benjamin Alan Weaver, Anne-Marie Weijmans, David H. Weinberg, Kyle B. Westfall, David G. Whelan, Vivienne Wild, John Wilson, W. M. Wood-Vasey, Dominika Wylezalek, Ting Xiao, Renbin Yan, Meng Yang, Jason E. Ybarra, Christophe Yèche, Nadia Zakamska, Olga Zamora, Pauline Zarrouk, Gail Zasowski, Kai Zhang, Gong-Bo Zhao, Zheng Zheng, Xu Zhou, Zhi-Min Zhou, Guangtun B. Zhu, Manuela Zoccali, Hu Zou, The Leverhulme Trust, University of St Andrews. School of Physics and Astronomy, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon)
Subjects: Astrophysics and Astronomy, Milky Way, astro-ph.GA, FOS: Physical sciences, Espectros astronômicos, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, law.invention, Telescope, Redshift-space distortions, surveys, Observatory, law, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, spectrographs [Instrumentation], observations [Cosmology], Galaxy: general, stars: general, 010303 astronomy & astrophysics, general [Galaxy], QC, Astrophysics::Galaxy Astrophysics, instrumentation: spectrographs, QB, Mapeamentos astronômicos, Physics, general [Stars], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Quasar, general [Galaxies], DAS, galaxies: general, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, QC Physics, Space and Planetary Science, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), Catalogos astronomicos, Baryon acoustic oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We describe the Sloan Digital Sky Survey IV (SDSS-IV), a project encompassing three major spectroscopic programs. The Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2) is observing hundreds of thousands of Milky Way stars at high resolution and high signal-to-noise ratio in the near-infrared. The Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey is obtaining spatially-resolved spectroscopy for thousands of nearby galaxies (median redshift of z = 0.03). The extended Baryon Oscillation Spectroscopic Survey (eBOSS) is mapping the galaxy, quasar, and neutral gas distributions between redshifts z = 0.6 and 3.5 to constrain cosmology using baryon acoustic oscillations, redshift space distortions, and the shape of the power spectrum. Within eBOSS, we are conducting two major subprograms: the SPectroscopic IDentification of eROSITA Sources (SPIDERS), investigating X-ray AGN and galaxies in X-ray clusters, and the Time Domain Spectroscopic Survey (TDSS), obtaining spectra of variable sources. All programs use the 2.5-meter Sloan Foundation Telescope at Apache Point Observatory; observations there began in Summer 2014. APOGEE-2 also operates a second near-infrared spectrograph at the 2.5-meter du Pont Telescope at Las Campanas Observatory, with observations beginning in early 2017. Observations at both facilities are scheduled to continue through 2020. In keeping with previous SDSS policy, SDSS-IV provides regularly scheduled public data releases; the first one, Data Release 13, was made available in July 2016., Published in Astronomical Journal
Published: 2017
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114. Dynamical dark energy in light of the latest observations

Author: Robert Crittenden, Graziano Rossi, Matthew M. Pieri, Levon Pogosian, Marco Raveri, Florian Beutler, Hanyu Zhang, Daniel J. Eisenstein, Arman Shafieloo, Will J. Percival, Will Handley, Robert C. Nichol, Sergio Rodríguez-Torres, Benjamin L'Huillier, Ashley J. Ross, Kazuya Koyama, Antonio J. Cuesta, Jeremy L. Tinker, Gong-Bo Zhao, Chia-Hsun Chuang, Jose Alberto Vazquez, Jonathan Brinkmann, Rita Tojeiro, Francisco-Shu Kitaura, Yuting Wang, Ariel G. Sánchez, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, Laboratoire d'Astrophysique de Marseille ( LAM ), and Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Cosmological constant, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, STFC, media_common, ST/H002774/1, Physics, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, 3rd-DAS, Universe, astro-ph.CO, symbols, Dark energy, Baryon acoustic oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: A flat Friedman-Roberson-Walker universe dominated by a cosmological constant ($\Lambda$) and cold dark matter (CDM) has been the working model preferred by cosmologists since the discovery of cosmic acceleration. However, tensions of various degrees of significance are known to be present among existing datasets within the $\Lambda$CDM framework. In particular, the Lyman-$\alpha$ forest measurement of the Baryon Acoustic Oscillations (BAO) by the Baryon Oscillation Spectroscopic Survey (BOSS) prefers a smaller value of the matter density fraction $\Omega_{\rm M}$ compared to the value preferred by cosmic microwave background (CMB). Also, the recently measured value of the Hubble constant, $H_0=73.24\pm1.74 \ {\rm km}\ {\rm s}^{-1} \ {\rm Mpc}^{-1}$, is $3.4\sigma$ higher than $66.93\pm0.62 \ {\rm km}\ {\rm s}^{-1} \ {\rm Mpc}^{-1}$ inferred from the Planck CMB data. In this work, we investigate if these tensions can be interpreted as evidence for a non-constant dynamical dark energy (DE). Using the Kullback-Leibler (KL) divergence to quantify the tension between datasets, we find that the tensions are relieved by an evolving DE, with the dynamical DE model preferred at a $3.5\sigma$ significance level based on the improvement in the fit alone. While, at present, the Bayesian evidence for the dynamical DE is insufficient to favour it over $\Lambda$CDM, we show that, if the current best fit DE happened to be the true model, it would be decisively detected by the upcoming DESI survey., Comment: 27 pages, 3 figures and one table. A supplementary document is included. The BOSS DR12 BAO data used in the work can be downloaded from the SDSS website https://sdss3.org//science/boss_publications.php (check https://data.sdss.org/sas/dr12/boss/papers/clustering/Zhao_etal_2016_DR12COMBINED_tomoBAO_powspec.tar.gz for the tomographic BAO measurement presented in https://arxiv.org/abs/1607.03153)
Published: 2017
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115. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations in Fourier-space

Author: Chia-Hsun Chuang, Antonio J. Cuesta, Rita Tojeiro, Andreu Font-Ribera, Anze Slosar, Natalie A. Roe, Daniel J. Eisenstein, Nicholas P. Ross, Joel R. Brownstein, Adam S. Bolton, Ashley J. Ross, Shun Saito, Hee-Jong Seo, Florian Beutler, Chirag Modi, Patrick McDonald, Sergio Rodríguez-Torres, Jan Niklas Grieb, Nick Hand, Mariana Vargas-Magaña, Robert C. Nichol, Donald P. Schneider, Francisco-Shu Kitaura, Francisco Prada, Salvador Salazar-Albornoz, Ariel G. Sánchez, Jose Alberto Vazquez, Jeremy L. Tinker, Will J. Percival, University of St Andrews. School of Physics and Astronomy, and Universitat de Barcelona
Subjects: Cúmuls de galàxies, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, symbols.namesake, surveys, 0103 physical sciences, QB Astronomy, cosmological parameters, dark energy, 010303 astronomy & astrophysics, QC, STFC, Astrophysics::Galaxy Astrophysics, QB, Physics, ST/N00180X/1, Clusters of galaxies, 010308 nuclear & particles physics, Angular diameter distance, RCUK, DAS, Astronomy and Astrophysics, Espectroscòpia, Redshift survey, Galaxy, Redshift, observations [cosmology], Spectrum analysis, Baryon, QC Physics, Space and Planetary Science, gravitation, symbols, Dark energy, astro-ph.CO, Baryon acoustic oscillations, large-scale structure of Universe, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. We analyse the baryon acoustic oscillation (BAO) signal of the final Baryon Oscillation Spectroscopic Survey (BOSS) data release (DR12). Our analysis is performed in the Fourier space, using the power spectrum monopole and quadrupole. The data set includes 1198 006 galaxies over the redshift range 0.2 < z < 0.75.We divide this data set into three (overlapping) redshift bins with the effective redshifts zeff = 0.38, 0.51 and 0.61. We demonstrate the reliability of our analysis pipeline using N-body simulations as well as ~1000 MultiDark- Patchy mock catalogues that mimic the BOSS-DR12 target selection. We apply density field reconstruction to enhance the BAO signal-to-noise ratio. By including the power spectrum quadrupole we can separate the line of sight and angular modes, which allows us to constrain the angular diameter distance DA(z) and the Hubble parameter H(z) separately. We obtain two independent 1.6 and 1.5 per cent constraints on DA(z) and 2.9 and 2.3 per cent constraints on H(z) for the low (zeff = 0.38) and high (zeff = 0.61) redshift bin, respectively. We obtain two independent 1 and 0.9 per cent constraints on the angular averaged distance DV(z), when ignoring the Alcock-Paczynski effect. The detection significance of the BAO signal is of the order of 8σ (post-reconstruction) for each of the three redshift bins. Our results are in good agreement with the Planck prediction within Λ cold dark matter. This paper is part of a set that analyses the final galaxy clustering data set from BOSS. The measurements and likelihoods presented here are combined with others in Alam et al. to produce the final cosmological constraints from BOSS.
Published: 2017
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116. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey : cosmological implications of the configuration-space clustering wedges

Author: Joel R. Brownstein, Matthew D. Olmstead, Florian Beutler, Martin Crocce, Salvador Salazar-Albornoz, Rita Tojeiro, Sergio Rodríguez-Torres, Claudio Dalla Vecchia, Ariel G. Sánchez, Francisco Prada, Yuting Wang, Jeremy L. Tinker, Gong-Bo Zhao, Roman Scoccimarro, Jan Niklas Grieb, Lado Samushia, Will J. Percival, Daniel J. Eisenstein, Francisco-Shu Kitaura, Mariana Vargas-Magaña, Chia-Hsun Chuang, Hee-Jong Seo, Martha Lippich, Ashley J. Ross, and University of St Andrews. School of Physics and Astronomy
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmological parameters, FOS: Physical sciences, Large-scale structure of universe, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, QB Astronomy, Cluster analysis, 010303 astronomy & astrophysics, QC, QB, Physics, 010308 nuclear & particles physics, Oscillation, Astronomy, Spectral density, Astronomy and Astrophysics, DAS, Galaxy, Baryon, QC Physics, Space and Planetary Science, astro-ph.CO, Configuration space, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We explore the cosmological implications of anisotropic clustering measurements in configuration space of the final galaxy samples from Data Release 12 of the SDSS-III Baryon Oscillation Spectroscopic Survey. We implement a new detailed modelling of the effects of non-linearities, galaxy bias and redshift-space distortions that can be used to extract unbiased cosmological information from our measurements for scales $s \gtrsim 20\,h^{-1}{\rm Mpc}$. We combined the galaxy clustering information from BOSS with the latest cosmic microwave background (CMB) observations and Type Ia supernovae samples and found no significant evidence for a deviation from the $\Lambda$CDM cosmological model. In particular, these data sets can constrain the dark energy equation of state parameter to $w_{\rm DE}=-0.996\pm0.042$ when assumed time-independent, the curvature of the Universe to $\Omega_{k}=-0.0007\pm 0.0030$ and the sum of the neutrino masses to $\sum m_{\nu} < 0.25\,{\rm eV}$ at 95 per cent CL. We explore the constraints on the growth rate of cosmic structures assuming $f(z)=\Omega_{\rm m}(z)^\gamma$ and obtain $\gamma = 0.609\pm 0.079$, in good agreement with the predictions of general relativity of $\gamma=0.55$. We compress the information of our clustering measurements into constraints on the parameter combinations $D_{\rm V}(z)/r_{\rm d}$, $F_{\rm AP}(z)$ and $f\sigma_8(z)$ at the effective redshifts of $z=0.38$, $0.51$ and $0.61$ with their respective covariance matrices and find good agreement with the predictions for these parameters obtained from the best-fitting $\Lambda$CDM model to the CMB data from the Planck satellite. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS. The measurements and likelihoods presented here are combined with others in Alam et al. (2016) to produce the final cosmological constraints from BOSS., Comment: 20 pages, 16 figures
Published: 2017
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117. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from DR12 galaxy clustering – towards an accurate model

Author: Lado Samushia, Francisco Prada, Jose Alberto Vazquez, Anže Slosar, Yuting Wang, Will J. Percival, Joel R. Brownstein, Matthew D. Olmstead, Sergio Rodríguez-Torres, Robert C. Nichol, Chia-Hsun Chuang, Héctor Gil-Marín, Graziano Rossi, Siddharth Satpathy, Gong-Bo Zhao, Mariana Vargas-Magaña, Rita Tojeiro, Jose Alberto Rubino-Martin, Salvador Salazar-Albornoz, Antonio J. Cuesta, Ariel G. Sánchez, Florian Beutler, Daniel J. Eisenstein, Francisco-Shu Kitaura, Jeremy L. Tinker, Marcos Pellejero-Ibanez, Ashley J. Ross, Shadab Alam, Jan Niklas Grieb, Shirley Ho, Daniel Thomas, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), BOSS, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, Lambda, distance scale, 01 natural sciences, Omega, Cosmology, 0103 physical sciences, cosmological parameters, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Oscillation, Sigma, Astronomy and Astrophysics, Galaxy, Baryon, Space and Planetary Science, cosmology: observations, astro-ph.CO, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We analyse the broad-range shape of the monopole and quadrupole correlation functions of the BOSS Data Release 12 (DR12) CMASS and LOWZ galaxy sample to obtain constraints on the Hubble expansion rate $H(z)$, the angular-diameter distance $D_A(z)$, the normalised growth rate $f(z)\sigma_8(z)$, and the physical matter density $\Omega_mh^2$. We adopt wide and flat priors on all model parameters in order to ensure the results are those of a `single-probe' galaxy clustering analysis. We also marginalise over three nuisance terms that account for potential observational systematics affecting the measured monopole. However, such Monte Carlo Markov Chain analysis is computationally expensive for advanced theoretical models, thus we develop a new methodology to speed up our analysis. We obtain $\{D_A(z)r_{s,fid}/r_s$Mpc, $H(z)r_s/r_{s,fid}$kms$^{-1}$Mpc$^{-1}$, $f(z)\sigma_8(z)$, $\Omega_m h^2\}$ = $\{956\pm28$ , $75.0\pm4.0$ , $0.397 \pm 0.073$, $0.143\pm0.017\}$ at $z=0.32$ and $\{1421\pm23$, $96.7\pm2.7$ , $0.497 \pm 0.058$, $0.137\pm0.015\}$ at $z=0.59$ where $r_s$ is the comoving sound horizon at the drag epoch and $r_{s,fid}=147.66$Mpc for the fiducial cosmology in this study. In addition, we divide the galaxy sample into four redshift bins to increase the sensitivity of redshift evolution. However, we do not find improvements in terms of constraining dark energy model parameters. Combining our measurements with Planck data, we obtain $\Omega_m=0.306\pm0.009$, $H_0=67.9\pm0.7$kms$^{-1}$Mpc$^{-1}$, and $\sigma_8=0.815\pm0.009$ assuming $\Lambda$CDM; $\Omega_k=0.000\pm0.003$ assuming oCDM; $w=-1.01\pm0.06$ assuming $w$CDM; and $w_0=-0.95\pm0.22$ and $w_a=-0.22\pm0.63$ assuming $w_0w_a$CDM. Our results show no tension with the flat $\Lambda$CDM cosmological paradigm. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS., Comment: 22 pages, 11 figures
Published: 2017
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118. The Clustering of Galaxies in the Completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmic Flows and Cosmic Web from Luminous Red Galaxies

Author: Daniel J. Eisenstein, Matthew D. Olmstead, Falk Baumgarten, Volker Müller, Sergio Rodríguez-Torres, Alina Streblyanska, Graziano Rossi, Metin Ata, Mariana Vargas-Magaña, Gustavo Yepes, Nikhil Padmanabhan, Héctor Gil-Marín, Carlos Hernández Monteagudo, Hee-Jong Seo, Mathieu Autefage, Francisco Prada, Shirley Ho, Jeremy L. Tinker, Chia-Hsun Chuang, Cameron K. McBride, Angela Burden, Will J. Percival, Joel R. Brownstein, Simone Ferraro, Donald P. Schneider, Rita Tojeiro, Ariel G. Sánchez, Mark C. Neyrinck, Patrick McDonald, Raul E. Angulo, Francisco-Shu Kitaura, Hong Guo, Florian Beutler, David J. Schlegel, Institut Lagrange de Paris, Sorbonne Université (SU), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), BOSS, University of St Andrews. School of Physics and Astronomy, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Cosmology and Gravitation, statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Virial theorem, Cosmology, methods: numerical, Redshift-space distortions, cosmology: theory, 0103 physical sciences, Satellite galaxy, QB Astronomy, Large-scale structure of the Universe, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, catalogues, galaxies: statistics, QB, Physics, COSMIC cancer database, theory [cosmology], 010308 nuclear & particles physics, Astronomy, DAS, Astronomy and Astrophysics, numerical [methods], Galaxy, Baryon, QC Physics, Space and Planetary Science, astro-ph.CO, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a Bayesian phase-space reconstruction of the cosmic large-scale matter density and velocity fields from the SDSS-III Baryon Oscillations Spectroscopic Survey Data Release 12 (BOSS DR12) CMASS galaxy clustering catalogue. We rely on a given $\Lambda$CDM cosmology, a mesh resolution in the range of 6-10 $h^{-1}$ Mpc, and a lognormal-Poisson model with a redshift dependent nonlinear bias. The bias parameters are derived from the data and a general renormalised perturbation theory approach. We use combined Gibbs and Hamiltonian sampling, implemented in the \textsc{argo} code, to iteratively reconstruct the dark matter density field and the coherent peculiar velocities of individual galaxies, correcting hereby for coherent redshift space distortions (RSD). Our tests relying on accurate $N$-body based mock galaxy catalogues, show unbiased real space power spectra of the nonlinear density field up to $k\sim0.2\, h$ Mpc$^{-1}$, and vanishing quadrupoles down to $r\sim20\,h^{-1}$ Mpc. We also demonstrate that the nonlinear cosmic web can be obtained from the tidal field tensor based on the Gaussian component of the reconstructed density field. We find that the reconstructed velocities have a statistical correlation coefficient compared to the true velocities of each individual lightcone mock galaxy of $r\sim0.68$ including about 10% of satellite galaxies with virial motions (about $r=0.75$ without satellites). The power spectra of the velocity divergence agree well with theoretical predictions up to $k\sim0.2\,h\,{\rm Mpc}^{-1}$. This work will be especially useful to improve, e.g. BAO reconstructions, kinematic Sunyaev-Zeldovich (kSZ), integrated Sachs-Wolfe (ISW) measurements, or environmental studies., Comment: 21 pages, 17 figures submitted to MNRAS
Published: 2017
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119. The large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies

Author: Héctor Gil-Marín, Ashley J. Ross, Shirley Ho, Francisco-Shu Kitaura, Will J. Percival, Sergio Rodríguez-Torres, Zachary Slepian, Jeremy L. Tinker, Cameron K. McBride, Daniel J. Eisenstein, Antonio J. Cuesta, Florian Beutler, Roman Scoccimarro, Robert C. Nichol, Chia-Hsun Chuang, Hee-Jong Seo, Rita Tojeiro, Jian Ge, Mariana Vargas-Magaña, Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Physics, 010308 nuclear & particles physics, Covariance matrix, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Sigma, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), distance scale, 01 natural sciences, Cosmology, Galaxy, Baryon, Space and Planetary Science, cosmology: observations, 0103 physical sciences, large-scale structure of Universe, Multipole expansion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We report a measurement of the large-scale three-point correlation function of galaxies using the largest data set for this purpose to date, 777 202 luminous red galaxies in the Sloan Digital Sky Survey Baryon Acoustic Oscillation Spectroscopic Survey (SDSS BOSS) DR12 CMASS sample. This work exploits the novel algorithm of Slepian & Eisenstein to compute the multipole moments of the 3PCF in $$\mathcal {O}(N^2)$$ time, with N the number of galaxies. Leading-order perturbation theory models the data well in a compressed basis where one triangle side is integrated out. We also present an accurate and computationally efficient means of estimating the covariance matrix. With these techniques, the redshift-space linear and non-linear bias are measured, with 2.6 per cent precision on the former if σ_8 is fixed. The data also indicate a 2.8σ preference for the BAO, confirming the presence of BAO in the three-point function.
Published: 2017
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120. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the Fourier space wedges of the final sample

Author: Francesco Montesano, Claudio Dalla Vecchia, Chia-Hsun Chuang, Will J. Percival, Francisco Prada, Ashley J. Ross, Hee-Jong Seo, Matthew D. Olmstead, Mariana Vargas-Magaña, Sergio Rodríguez-Torres, Salvador Salazar-Albornoz, Rita Tojeiro, Ariel G. Sánchez, Robert C. Nichol, Martin Crocce, Daniel J. Eisenstein, Joel R. Brownstein, Gong-Bo Zhao, Alina Streblyanska, Roman Scoccimarro, Francisco-Shu Kitaura, Lado Samushia, Jeremy L. Tinker, Claudia Maraston, Florian Beutler, Héctor Gil-Marín, Antonio J. Cuesta, Jan Niklas Grieb, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Université (SU), BOSS, Sorbonne Universités, University of St Andrews. School of Physics and Astronomy, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Cosmological parameters, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, symbols.namesake, 0103 physical sciences, Dark energy, QB Astronomy, cosmological parameters, observations [Cosmology], dark energy, 010303 astronomy & astrophysics, QC, QB, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, DAS, Redshift, Galaxy, Baryon, QC Physics, Space and Planetary Science, cosmology: observations, symbols, astro-ph.CO, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: We extract cosmological information from the anisotropic power spectrum measurements from the recently completed Baryon Oscillation Spectroscopic Survey (BOSS), extending the concept of clustering wedges to Fourier space. Making use of new FFT-based estimators, we measure the power spectrum clustering wedges of the BOSS sample by filtering out the information of Legendre multipoles l > 4. Our modelling of these measurements is based on novel approaches to describe non-linear evolution, bias, and redshift-space distortions, which we test using synthetic catalogues based on large-volume N-body simulations. We are able to include smaller scales than in previous analyses, resulting in tighter cosmological constraints. Using three overlapping redshift bins, we measure the angular diameter distance, the Hubble parameter, and the cosmic growth rate, and explore the cosmological implications of our full shape clustering measurements in combination with CMB and SN Ia data. Assuming a {\Lambda}CDM cosmology, we constrain the matter density to {\Omega}_m = 0.311 -0.010 +0.009 and the Hubble parameter to H_0 = 67.6 -0.6 +0.7 km s^-1 Mpc^-1, at a confidence level (CL) of 68 per cent. We also allow for non-standard dark energy models and modifications of the growth rate, finding good agreement with the {\Lambda}CDM paradigm. For example, we constrain the equation-of-state parameter to w = -1.019 -0.039 +0.048. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS. The measurements and likelihoods presented here are combined with others in Alam et al. 2016 to produce the final cosmological constraints from BOSS., Comment: 23 pages, 16 figures in the main text, appendix of 6 pages and 5 figures; revision submitted to MNRAS. The data used in this analysis is publicly available at https://www.sdss3.org/science/boss_publications.php
Published: 2017
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121. The 13th Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-IV Survey Mapping Nearby Galaxies at Apache Point Observatory

Author: Franco D. Albareti, Carlos Allende Prieto, Andres Almeida, Friedrich Anders, Scott Anderson, Brett H. Andrews, Alfonso Aragón-Salamanca, Maria Argudo-Fernández, Eric Armengaud, Eric Aubourg, Vladimir Avila-Reese, Carles Badenes, Stephen Bailey, Beatriz Barbuy, Kat Barger, Jorge Barrera-Ballesteros, Curtis Bartosz, Sarbani Basu, Dominic Bates, Giuseppina Battaglia, Falk Baumgarten, Julien Baur, Julian Bautista, Timothy C. Beers, Francesco Belfiore, Matthew Bershady, Sara Bertran de Lis, Jonathan C. Bird, Dmitry Bizyaev, Guillermo A. Blanc, Michael Blanton, Michael Blomqvist, Adam S. Bolton, J. Borissova, Jo Bovy, William Nielsen Brandt, Jonathan Brinkmann, Joel R. Brownstein, Kevin Bundy, Etienne Burtin, Nicolás G. Busca, Hugo Orlando Camacho Chavez, M. Cano Díaz, Michele Cappellari, Ricardo Carrera, Yanping Chen, Brian Cherinka, Edmond Cheung, Cristina Chiappini, Drew Chojnowski, Chia-Hsun Chuang, Haeun Chung, Rafael Fernando Cirolini, Nicolas Clerc, Roger E. Cohen, Julia M. Comerford, Johan Comparat, Janaina Correa do Nascimento, Marie-Claude Cousinou, Kevin Covey, Jeffrey D. Crane, Rupert Croft, Katia Cunha, Jeremy Darling, James W. Davidson, Kyle Dawson, Luiz Da Costa, Gabriele Da Silva Ilha, Alice Deconto Machado, Timothée Delubac, Nathan De Lee, Axel De la Macorra, Sylvain De la Torre, Aleksandar M. Diamond-Stanic, John Donor, Juan Jose Downes, Niv Drory, Cheng Du, Hélion Du Mas des Bourboux, Tom Dwelly, Garrett Ebelke, Arthur Eigenbrot, Daniel J. Eisenstein, Yvonne P. Elsworth, Eric Emsellem, Michael Eracleous, Stephanie Escoffier, Michael L. Evans, Jesús Falcón-Barroso, Xiaohui Fan, Ginevra Favole, Emma Fernandez-Alvar, J. G. Fernandez-Trincado, Diane Feuillet, Scott W. Fleming, Andreu Font-Ribera, Gordon Freischlad, Peter Frinchaboy, Hai Fu, Yang Gao, Rafael A. Garcia, R. Garcia-Dias, D. A. Garcia-Hernández, Ana E. Garcia Pérez, Patrick Gaulme, Junqiang Ge, Douglas Geisler, Bruce Gillespie, Hector Gil Marin, Léo Girardi, Daniel Goddard, Yilen Gomez Maqueo Chew, Violeta Gonzalez-Perez, Kathleen Grabowski, Paul Green, Catherine J. Grier, Thomas Grier, Hong Guo, Julien Guy, Alex Hagen, Matt Hall, Paul Harding, R. E. Harley, Sten Hasselquist, Suzanne Hawley, Christian R. Hayes, Fred Hearty, Saskia Hekker, Hector Hernandez Toledo, Shirley Ho, David W. Hogg, Kelly Holley-Bockelmann, Jon A. Holtzman, Parker H. Holzer, Jian Hu, Daniel Huber, Timothy Alan Hutchinson, Ho Seong Hwang, Héctor J. Ibarra-Medel, Inese I. Ivans, KeShawn Ivory, Kurt Jaehnig, Trey W. Jensen, Jennifer A. Johnson, Amy Jones, Eric Jullo, T. Kallinger, Karen Kinemuchi, David Kirkby, Mark Klaene, Jean-Paul Kneib, Juna A. Kollmeier, Ivan Lacerna, Richard R. Lane, Dustin Lang, Pierre Laurent, David R. Law, Alexie Leauthaud, Jean-Marc Le Goff, Chen Li, Cheng Li, Niu Li, Ran Li, Fu-Heng Liang, Yu Liang, Marcos Lima, Lihwai Lin, Lin Lin, Yen-Ting Lin, Chao Liu, Dan Long, Sara Lucatello, Nicholas MacDonald, Chelsea L. MacLeod, J. Ted Mackereth, Suvrath Mahadevan, Marcio Antonio Geimba Maia, Roberto Maiolino, Steven R. Majewski, Olena Malanushenko, Viktor Malanushenko, Nícolas Dullius Mallmann, Arturo Manchado, Claudia Maraston, Rui Marques-Chaves, Inma Martinez Valpuesta, Karen L. Masters, Savita Mathur, Ian D. McGreer, Andrea Merloni, Michael R. Merrifield, Szabolcs Meszáros, Andres Meza, Andrea Miglio, Ivan Minchev, Karan Molaverdikhani, Antonio D. Montero-Dorta, Benoit Mosser, Demitri Muna, Adam Myers, Preethi Nair, Kirpal Nandra, Melissa Ness, Jeffrey A. Newman, Robert C. Nichol, David L. Nidever, Christian Nitschelm, Julia O’Connell, Audrey Oravetz, Daniel J. Oravetz, Zachary Pace, Nelson Padilla, Nathalie Palanque-Delabrouille, Kaike Pan, John Parejko, Isabelle Paris, Changbom Park, John A. Peacock, Sebastien Peirani, Marcos Pellejero-Ibanez, Samantha Penny, Will J. Percival, Jeffrey W. Percival, Ismael Perez-Fournon, Patrick Petitjean, Matthew Pieri, Marc H. Pinsonneault, Alice Pisani, Francisco Prada, Abhishek Prakash, Natalie Price-Jones, M. Jordan Raddick, Mubdi Rahman, Anand Raichoor, Sandro Barboza Rembold, A. M. Reyna, James Rich, Hannah Richstein, Jethro Ridl, Rogemar A. Riffel, Rogério Riffel, Hans-Walter Rix, Annie C. Robin, Constance M. Rockosi, Sergio Rodríguez-Torres, Thaíse S. Rodrigues, Natalie Roe, A. Roman Lopes, Carlos Román-Zúñiga, Ashley J. Ross, Graziano Rossi, John Ruan, Rossana Ruggeri, Jessie C. Runnoe, Salvador Salazar-Albornoz, Mara Salvato, Sebastian F. Sanchez, Ariel G. Sanchez, José R. Sanchez-Gallego, Basílio Xavier Santiago, Ricardo Schiavon, Jaderson S. Schimoia, Eddie Schlafly, David J. Schlegel, Donald P. Schneider, Ralph Schönrich, Mathias Schultheis, Axel Schwope, Hee-Jong Seo, Aldo Serenelli, Branimir Sesar, Zhengyi Shao, Matthew Shetrone, Michael Shull, Victor Silva Aguirre, M. F. Skrutskie, Anže Slosar, Michael Smith, Verne V. Smith, Jennifer Sobeck, Garrett Somers, Diogo Souto, David V. Stark, Keivan G. Stassun, Matthias Steinmetz, Dennis Stello, Thaisa Storchi Bergmann, Michael A. Strauss, Alina Streblyanska, Guy S. Stringfellow, Genaro Suarez, Jing Sun, Manuchehr Taghizadeh-Popp, Baitian Tang, Charling Tao, Jamie Tayar, Mita Tembe, Daniel Thomas, Jeremy Tinker, Rita Tojeiro, Christy Tremonti, Nicholas Troup, Jonathan R. Trump, Eduardo Unda-Sanzana, O. Valenzuela, Remco Van den Bosch, Mariana Vargas-Magaña, Jose Alberto Vazquez, Sandro Villanova, M. Vivek, Nicole Vogt, David Wake, Rene Walterbos, Yuting Wang, Enci Wang, Benjamin Alan Weaver, Anne-Marie Weijmans, David H. Weinberg, Kyle B. Westfall, David G. Whelan, Eric Wilcots, Vivienne Wild, Rob A. Williams, John Wilson, W. M. Wood-Vasey, Dominika Wylezalek, Ting Xiao, Renbin Yan, Meng Yang, Jason E. Ybarra, Christophe Yeche, Fang-Ting Yuan, Nadia Zakamska, Olga Zamora, Gail Zasowski, Kai Zhang, Cheng Zhao, Gong-Bo Zhao, Zheng Zheng, Zhi-Min Zhou, Guangtun Zhu, Joel C. Zinn, Hu Zou, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), SDSS, Maiolino, Roberto [0000-0002-4985-3819], Apollo - University of Cambridge Repository, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS Lyon ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, and Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], media_common.quotation_subject, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Set (abstract data type), surveys, Observatory, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, media_common, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Atlases, DAS, Astronomy and Astrophysics, Quasar, GALÁXIAS, Galaxy, Redshift, atlases, QC Physics, Data access, Space and Planetary Science, Sky, Catalogs, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs, Data reduction
Abstract: The fourth generation of the Sloan Digital Sky Survey (SDSS-IV) began observations in July 2014. It pursues three core programs: APOGEE-2,MaNGA, and eBOSS. In addition, eBOSS contains two major subprograms: TDSS and SPIDERS. This paper describes the first data release from SDSS-IV, Data Release 13 (DR13), which contains new data, reanalysis of existing data sets and, like all SDSS data releases, is inclusive of previously released data. DR13 makes publicly available 1390 spatially resolved integral field unit observations of nearby galaxies from MaNGA,the first data released from this survey. It includes new observations from eBOSS, completing SEQUELS. In addition to targeting galaxies and quasars, SEQUELS also targeted variability-selected objects from TDSS and X-ray selected objects from SPIDERS. DR13 includes new reductions ofthe SDSS-III BOSS data, improving the spectrophotometric calibration and redshift classification. DR13 releases new reductions of the APOGEE-1data from SDSS-III, with abundances of elements not previously included and improved stellar parameters for dwarf stars and cooler stars. For the SDSS imaging data, DR13 provides new, more robust and precise photometric calibrations. Several value-added catalogs are being released in tandem with DR13, in particular target catalogs relevant for eBOSS, TDSS, and SPIDERS, and an updated red-clump catalog for APOGEE.This paper describes the location and format of the data now publicly available, as well as providing references to the important technical papers that describe the targeting, observing, and data reduction. The SDSS website, http://www.sdss.org, provides links to the data, tutorials and examples of data access, and extensive documentation of the reduction and analysis procedures. DR13 is the first of a scheduled set that will contain new data and analyses from the planned ~6-year operations of SDSS-IV. Postprint
Published: 2017
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122. Detection of baryon acoustic oscillation features in the large-scale three-point correlation function of SDSS BOSS DR12 CMASS galaxies

Author: Hee-Jong Seo, Anže Slosar, Daniel J. Eisenstein, Chia-Hsun Chuang, Graziano Rossi, Shirley Ho, Ashley J. Ross, Will J. Percival, Francisco-Shu Kitaura, Mariana Vargas-Magaña, Zachary Slepian, Héctor Gil-Marín, Joel R. Brownstein, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Correlation function (astronomy), distance scale, 01 natural sciences, Cosmology, distance sacle, 0103 physical sciences, ST/M001709/1, 010303 astronomy & astrophysics, STFC, Physics, 010308 nuclear & particles physics, Standard ruler, RCUK, Astronomy and Astrophysics, Galaxy, Redshift, observations [cosmology], Baryon, Space and Planetary Science, cosmology: observations, astro-ph.CO, ST/N000668/1, Baryon acoustic oscillations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Bispectrum, Astronomical and Space Sciences
Abstract: Author(s): Slepian, Z; Eisenstein, DJ; Brownstein, JR; Chuang, CH; Gil-Marin, H; Ho, S; Kitaura, FS; Percival, WJ; Ross, AJ; Rossi, G; Seo, HJ; Slosar, A; Vargas-Magana, M | Abstract: We present the large-scale three-point correlation function (3PCF) of the Sloan Digital Sky Survey DR12 Constant stellar Mass (CMASS) sample of 777 202 Luminous Red Galaxies, the largest-ever sample used for a 3PCF or bispectrum measurement. We make the first high-significance (4.5σ) detection of baryon acoustic oscillations (BAO) in the 3PCF. Using these acoustic features in the 3PCF as a standard ruler, we measure the distance to z = 0.57 to 1.7 per cent precision (statistical plus systematic). We find DV =2024±29 Mpc (stat)±20 Mpc (sys) for our fiducial cosmology (consistent with Planck 2015) and bias model. This measurement extends the use of the BAO technique from the twopoint correlation function (2PCF) and power spectrum to the 3PCF and opens an avenue for deriving additional cosmological distance information from future large-scale structure redshift surveys such as DESI. Our measured distance scale from the 3PCF is fairly independent from that derived from the pre-reconstruction 2PCF and is equivalent to increasing the length of BOSS by roughly 10 per cent; reconstruction appears to lower the independence of the distance measurements. Fitting a model including tidal tensor bias yields a moderatesignificance (2.6σ) detection of this bias with a value in agreement with the prediction from local Lagrangian biasing.
Published: 2017
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123. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: towards a computationally efficient analysis without informative priors

Author: Anže Slosar, Sergio Rodríguez-Torres, Antonio J. Cuesta, Gong-Bo Zhao, Jose Alberto Vazquez, Mariana Vargas-Magaña, Rita Tojeiro, Daniel J. Eisenstein, Marcos Pellejero-Ibanez, Jose Alberto Rubino-Martin, Siddharth Satpathy, Ashley J. Ross, Joel R. Brownstein, Shadab Alam, Jan Niklas Grieb, Francisco-Shu Kitaura, Will J. Percival, Robert C. Nichol, Jeremy L. Tinker, Shirley Ho, Chia-Hsun Chuang, Yuting Wang, Héctor Gil-Marín, Francisco Prada, Hee-Jong Seo, Matthew D. Olmstead, Graziano Rossi, Lado Samushia, Salvador Salazar-Albornoz, Ariel G. Sánchez, Florian Beutler, Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), BOSS, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Sorbonne Université (SU)
Subjects: Particle physics, Cold dark matter, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, 01 natural sciences, Omega, symbols.namesake, 0103 physical sciences, Planck, cosmological parameters, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, observations [observations], Astronomy and Astrophysics, Comoving distance, Redshift, Baryon, Space and Planetary Science, cosmology: observations, Dark energy, symbols, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We develop a new computationally efficient methodology called double-probe analysis with the aim of minimizing informative priors (those coming from extra probes) in the estimation of cosmological parameters. Using our new methodology, we extract the dark energy model-independent cosmological constraints from the joint data sets of the Baryon Oscillation Spectroscopic Survey (BOSS) galaxy sample and Planck cosmic microwave background (CMB) measurements. We measure the mean values and covariance matrix of {R, la, Ωbh2, ns, log(As), Ωk, H(z), DA(z), f(z)σ8(z)}, which give an efficient summary of the Planck data and two-point statistics from the BOSS galaxy sample. The CMB shift parameters are R=ΩmH20√r(z∗) and la = πr(z*)/rs(z*), where z* is the redshift at the last scattering surface, and r(z*) and rs(z*) denote our comoving distance to the z* and sound horizon at z*, respectively; Ωb is the baryon fraction at z = 0. This approximate methodology guarantees that we will not need to put informative priors on the cosmological parameters that galaxy clustering is unable to constrain, i.e. Ωbh2 and ns. The main advantage is that the computational time required for extracting these parameters is decreased by a factor of 60 with respect to exact full-likelihood analyses. The results obtained show no tension with the flat Λ cold dark matter (ΛCDM) cosmological paradigm. By comparing with the full-likelihood exact analysis with fixed dark energy models, on one hand we demonstrate that the double-probe method provides robust cosmological parameter constraints that can be conveniently used to study dark energy models, and on the other hand we provide a reliable set of measurements assuming dark energy models to be used, for example, in distance estimations. We extend our study to measure the sum of the neutrino mass using different methodologies, including double-probe analysis (introduced in this study), full-likelihood analysis and single-probe analysis. From full-likelihood analysis, we obtain Σmν mν wCDM. We also find that there is degeneracy between observational systematics and neutrino masses, which suggests that one should take great care when estimating these parameters in the case of not having control over the systematics of a given sample.
Published: 2017
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124. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in Fourier space

Author: Robert C. Nichol, Shun Saito, Jan Niklas Grieb, Gong-Bo Zhao, Joel R. Brownstein, Daniel J. Eisenstein, Sergio Rodríguez-Torres, Daniel Thomas, Chia-Hsun Chuang, Francisco Prada, Lado Samushia, David H. Weinberg, Ashley J. Ross, Matthew D. Olmstead, Fangzhou Zhu, Graziano Rossi, Antonio J. Cuesta, Florian Beutler, Jean-Paul Kneib, Dandan Wang, Salvador Salazar-Albornoz, Ariel G. Sánchez, Yuting Wang, Rita Tojeiro, Héctor Gil-Marín, Will J. Percival, Francisco-Shu Kitaura, Jeremy L. Tinker, Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), BOSS, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), University of St Andrews. School of Physics and Astronomy, and Sorbonne Université (SU)
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Nuclear Theory, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), distance scale, 01 natural sciences, scale structure of Universe, 0103 physical sciences, QB Astronomy, cosmological parameters, dark energy, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, large, Physics, 010308 nuclear & particles physics, Oscillation, Astrophysics::Instrumentation and Methods for Astrophysics, DAS, Astronomy and Astrophysics, Redshift survey, observations [cosmology], Galaxy, Redshift, Baryon, QC Physics, Space and Planetary Science, cosmology: observations, Dark energy, distances and redshifts [galaxies], High Energy Physics::Experiment, Baryon acoustic oscillations, large-scale structure of Universe, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a tomographic baryon acoustic oscillations (BAO) analysis using the monopole, quadrupole and hexadecapole of the redshift-space galaxy power spectrum measured from the pre-reconstructed combined galaxy sample of the completed Sloan Digital Sky Survey (SDSS-III) Baryon Oscillation Spectroscopic Survey (BOSS) Data Release (DR)12 covering the redshift range of $0.20, Comment: 20 pages, 22 figures; version accepted by MNRAS; This paper is part of a set that analyses the final galaxy clustering dataset from BOSS; The BAO measurements including the full covariance matrices presented in this work and a CosmoMC patch to use this measurement for cosmology is available at https://sdss3.org//science/boss_publications.php
Published: 2017
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125. Measuring DA and H at z=0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations

Author: Nikhil Padmanabhan, Xiaoying Xu, Antonio J. Cuesta, Cameron K. McBride, and Daniel J. Eisenstein
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Oscillation, Angular diameter distance, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Baryon, symbols.namesake, Space and Planetary Science, 0103 physical sciences, Dark energy, symbols, Baryon acoustic oscillations, Anisotropy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: We present measurements of the angular diameter distance D_A(z) and the Hubble parameter H(z) at z=0.35 using the anisotropy of the baryon acoustic oscillation (BAO) signal measured in the galaxy clustering distribution of the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) Luminous Red Galaxies (LRG) sample. Our work is the first to apply density-field reconstruction to an anisotropic analysis of the acoustic peak. Reconstruction partially removes the effects of non-linear evolution and redshift-space distortions in order to sharpen the acoustic signal. We present the theoretical framework behind the anisotropic BAO signal and give a detailed account of the fitting model we use to extract this signal from the data. Our method focuses only on the acoustic peak anisotropy, rather than the more model-dependent anisotropic information from the broadband power. We test the robustness of our analysis methods on 160 LasDamas DR7 mock catalogues and find that our models are unbiased at the ~0.2% level in measuring the BAO anisotropy. After reconstruction we measure D_A(z=0.35)=1050+/-38 Mpc and H(z=0.35)=84.4+/-7.0 km/s/Mpc assuming a sound horizon of r_s=152.76 Mpc. Note that these measurements are correlated with a correlation coefficient of 0.58. This represents a factor of 1.4 improvement in the error on D_A relative to the pre-reconstruction case; a factor of 1.2 improvement is seen for H., 30 pages, 21 figures, accepted by MNRAS, updated to version accepted by journal
Published: 2013
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126. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey:single-probe measurements from CMASS anisotropic galaxy clustering

Author: Chia-Hsun Chuang, Sebastián E. Nuza, Stephanie Escoffier, Yuting Wang, Florian Beutler, Kyle S. Dawson, Sergio Rodríguez-Torres, Marcos Pellejero-Ibanez, Donald P. Schneider, Francisco Prada, Daniel Thomas, David J. Schlegel, Matthew D. Olmstead, Benjamin A. Weaver, Claudia Maraston, Lado Samushia, Marc Manera, Antonio J. Cuesta, Gong-Bo Zhao, Francisco-Shu Kitaura, Joel R. Brownstein, Daniel J. Eisenstein, Jose Alberto Rubino-Martin, Shirley Ho, Jean-Paul Kneib, Ashley J. Ross, Universitat de Barcelona, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and ANR-16-CE31-0021,eBOSS,Sondes cosmologiques de la gravitation et de l'énergie noire(2016)
Subjects: Length scale, Cúmuls de galàxies, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Ciencias Físicas, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, distance scale, 01 natural sciences, purl.org/becyt/ford/1 [https], Universe, 0103 physical sciences, Single probe, cosmological parameters, Anisotropy, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Univers, largescale structure of Universe, Cosmologia, Clusters of galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Oscillation, Astronomy, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Galaxy, observations [cosmology], Cosmology, Astronomía, Baryon, Space and Planetary Science, cosmology: observations, astro-ph.CO, large-scale structure of Universe, LARGE-SCALE STRUCTURE OF UNIVERSE, CIENCIAS NATURALES Y EXACTAS, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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 $h^{-1}$Mpc). We analyze 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 $D_A(z)$, the normalized growth rate $f(z)\sigma_8(z)$, and the physical matter density $\Omega_mh^2$. 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 $\{D_A(0.59)r_{s,fid}/r_s$ $\rm Mpc$, $H(0.59)r_s/r_{s,fid}$ $km s^{-1} Mpc^{-1}$, $f(0.59)\sigma_8(0.59)$, $\Omega_m h^2\}$ = $\{1427\pm26$, $97.3\pm3.3$, $0.488 \pm 0.060$, $0.135\pm0.016\}$, where $r_s$ is the comoving sound horizon at the drag epoch and $r_{s,fid}=147.66$ 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, $\Omega_k$, is 0.3 per cent. We do not find deviation from flat $\Lambda$CDM., Comment: 15 pages, 11 figures. The latest version matches and the accepted version by MNRAS. A bug in the first version has been identified and fixed in the new version. We have redone the analysis with newest data (BOSS DR12)
Published: 2016
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127. The high-mass end of the red sequence at z ∼ 0.55 from SDSS-III/BOSS:completeness, bimodality and luminosity function

Author: Claudia Maraston, Chia-Hsun Chuang, Daniel Thomas, Johan Comparat, Ginevra Favole, Molly E. C. Swanson, Daniel J. Eisenstein, Donald P. Schneider, Sergio Rodríguez-Torres, Cameron K. McBride, Adam S. Bolton, Hong Guo, Francisco Prada, Joel R. Brownstein, Kyle S. Dawson, and Antonio D. Montero-Dorta
Subjects: statistics [galaxies], Cosmology and Gravitation, Population, statistical [methods], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Type (model theory), 01 natural sciences, analytical [methods], surveys, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], Luminosity function (astronomy), Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift survey, luminosity function, mass function [galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Distribution (mathematics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Magnitude (astronomy)
Abstract: We have developed an analytical method based on forward-modeling techniques to characterize the high-mass end of the red sequence (RS) galaxy population at redshift $z\sim0.55$, from the DR10 BOSS CMASS spectroscopic sample, which comprises $\sim600,000$ 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 modeling 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 ($, Comment: 27 pages, 20 figures, accepted for publication in MNRAS
Published: 2016
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128. PRIMUS: One- and Two-Halo Galactic Conformity at $0.2 < z < 1$

Author: Angela M. Berti, Richard J. Cool, Alison L. Coil, Peter Behroozi, John Moustakas, Daniel J. Eisenstein, and Aaron D. Bray
Subjects: Physics, Stellar mass, 010308 nuclear & particles physics, Star formation, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics, Cosmic variance, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Stars, Space and Planetary Science, Sky, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Halo, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We test for galactic conformity at $0.23\sigma)$ one-halo conformity signal, or an excess of star-forming neighbors around star-forming central galaxies, of $\sim5$% on scales of 0-1 Mpc and a $2.5\sigma$ two-halo signal of $\sim1$% on scales of 1-3 Mpc. These signals are weaker than those detected in SDSS and are consistent with galactic conformity being the result of large-scale tidal fields and reflecting assembly bias. We also measure the star-forming fraction of central galaxies at fixed stellar mass as a function of large-scale environment and find that central galaxies are more likely to be quenched in overdense environments, independent of stellar mass. However, we find that environment does not affect the star formation efficiency of central galaxies, as long as they are forming stars. We test for redshift and stellar mass dependence of the conformity signal within our sample and show that large volumes and multiple fields are required at intermediate redshift to adequately account for cosmic variance., Comment: 19 pages, 12 figures
Published: 2016

129. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: combining correlated Gaussian posterior distributions

Author: Rita Tojeiro, Shadab Alam, Jan Niklas Grieb, Mariana Vargas-Magaña, Salvador Salazar-Albornoz, Ariel G. Sánchez, Gong-Bo Zhao, Jose Alberto Vazquez, Francisco-Shu Kitaura, Florian Beutler, Joel R. Brownstein, Daniel J. Eisenstein, Sergio Rodríguez-Torres, Jeremy L. Tinker, Antonio J. Cuesta, Will J. Percival, Hee-Jong Seo, Chia-Hsun Chuang, Ashley J. Ross, Francisco Prada, University of St Andrews. School of Physics and Astronomy, and Universitat de Barcelona
Subjects: Cúmuls de galàxies, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Gaussian, Posterior probability, Cosmological parameters, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, 01 natural sciences, symbols.namesake, 0103 physical sciences, QB Astronomy, Statistical physics, Cluster analysis, 010303 astronomy & astrophysics, QC, QB, Physics, Cosmologia, Clusters of galaxies, 010308 nuclear & particles physics, Astronomy and Astrophysics, DAS, Galaxy, Cosmology, Baryon, QC Physics, Boss, Space and Planetary Science, symbols, astro-ph.CO, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The cosmological information contained in anisotropic galaxy clustering measurements can often be compressed into a small number of parameters whose posterior distribution is well described by a Gaussian. We present a general methodology to combine these estimates into a single set of consensus constraints that encode the total information of the individual measurements, taking into account the full covariance between the different methods. We illustrate this technique by applying it to combine the results obtained from different clustering analyses, including measurements of the signature of baryon acoustic oscillations (BAO) and redshift-space distortions (RSD), based on a set of mock catalogues of the final SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). Our results show that the region of the parameter space allowed by the consensus constraints is smaller than that of the individual methods, highlighting the importance of performing multiple analyses on galaxy surveys even when the measurements are highly correlated. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS. The methodology presented here is used in Alam et al. (2016) to produce the final cosmological constraints from BOSS., 9 pages, 8 figures
Published: 2016
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130. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in configuration space

Author: Yuting Wang, Gong-Bo Zhao, Chia-Hsun Chuang, Ashley J. Ross, Will J. Percival, Héctor Gil-Marín, Antonio J. Cuesta, Francisco-Shu Kitaura, Sergio Rodriguez-Torres, Joel R. Brownstein, Daniel J. Eisenstein, Shirley Ho, Jean-Paul Kneib, Matthew D. Olmstead, Francisco Prada, Graziano Rossi, Ariel G. Sánchez, Salvador Salazar-Albornoz, Daniel Thomas, Jeremy Tinker, Rita Tojeiro, Mariana Vargas-Magaña, and Fangzhou Zhu
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, astro-ph.CO, dark energy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a tomographic baryon acoustic oscillations analysis using the two-point galaxy correlation function measured from the combined sample of BOSS DR12, which covers the redshift range of $0.2, Comment: 14 pages, 21 figures, 7 Tables. Submitted to MNRAS
Published: 2016
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131. Modeling the large-scale redshift-space 3-point correlation function of galaxies

Author: Zachary Slepian and Daniel J. Eisenstein
Subjects: Physics, Length scale, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Scale (ratio), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Function (mathematics), Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), 01 natural sciences, Redshift, Galaxy, Baryon, Renormalization, Space and Planetary Science, Quantum mechanics, 0103 physical sciences, Statistical physics, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a configuration-space model of the large-scale galaxy 3-point correlation function (3PCF) based on leading-order perturbation theory and including redshift space distortions (RSD). This model should be useful in extracting distance-scale information from the 3PCF via the Baryon Acoustic Oscillation (BAO) method. We include the first redshift-space treatment of biasing by the baryon-dark matter relative velocity. Overall, on large scales the effect of RSD is primarily a renormalization of the 3PCF that is roughly independent of both physical scale and triangle opening angle; for our adopted $\Omega_{\rm m}$ and bias values, the rescaling is a factor of $\sim 1.8$. We also present an efficient scheme for computing 3PCF predictions from our model, important for allowing fast exploration of the space of cosmological parameters in future analyses., Comment: 23 pages, 11 figures, submitted MNRAS
Published: 2016

132. Improving Initial Conditions for Cosmological $N$-Body Simulations

Author: Philip A. Pinto, Marc Metchnik, Lehman H. Garrison, Daniel J. Eisenstein, and Douglas Ferrer
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Group (mathematics), Foundation (engineering), FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Division (mathematics), 01 natural sciences, Space and Planetary Science, 0103 physical sciences, Calculus, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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 $k_{\rm Nyquist}$. Marcos et al. demonstrate that this is due to sparse sampling of modes near $k_{\rm Nyquist}$ and that the often-assumed continuum growing modes are not proper growing modes of the particle system. We develop initial conditions 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 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% accuracy in the power spectrum down to $k_{\rm Nyquist}$, versus $k_{\rm Nyquist}/4$ without rescaling or $k_{\rm Nyquist}/13$ without 2LPT, relative to an oversampled reference simulation. We anticipate that our 2LPT will be useful for large simulations where FFTs are expensive and that rescaling will be useful for suites of medium-resolution simulations used in cosmic emulators and galaxy survey mock catalogs. Code to generate initial conditions is available at https://github.com/lgarrison/zeldovich-PLT, 22 pages, 14 figures. Minor changes to match MNRAS published version. Code available at https://github.com/lgarrison/zeldovich-PLT
Published: 2016

133. 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

Author: Cameron K. McBride, David J. Schlegel, Beth Reid, Ariel G. Sánchez, Adam S. Bolton, Ashley J. Ross, Joel R. Brownstein, Daniel J. Eisenstein, Rita Tojeiro, Héctor Gil-Marín, Licia Verde, Antonio J. Cuesta, Donald P. Schneider, Martin White, Claudia Maraston, Shirley Ho, Daniel Thomas, Florian Beutler, Jeremy L. Tinker, Will J. Percival, Nikhil Padmanabhan, Mariana Vargas-Magaña, Nicholas P. Ross, University of St Andrews. School of Physics and Astronomy, and Universitat de Barcelona
Subjects: Cúmuls de galàxies, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), Astronomy & Astrophysics, Expanding universe, distance scale, 01 natural sciences, Cosmology, Expansió de l'univers, 0103 physical sciences, QB Astronomy, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, STFC, QB, Physics, Clusters of galaxies, 010308 nuclear & particles physics, Oscillation, ST/I001204/1, Astronomy, RCUK, Astronomy and Astrophysics, 3rd-DAS, Galaxy, observations [cosmology], Baryon, Space and Planetary Science, astro-ph.CO, High Energy Physics::Experiment, Baryon acoustic oscillations, Astrophysics::Earth and Planetary Astrophysics, large-scale structure of Universe, Data release, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present distance scale measurements from the baryon acoustic oscillation signal in the CMASS and LOWZ samples from the Data Release 12 of the Baryon Oscillation Spectroscopic Survey (BOSS). The total volume probed is 14.5 Gpc$^3$, 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 $D_V(z)r^{\rm fid}_{\rm d}/r_ {\rm d}=2028\pm21$ Mpc and a distance to $z=0.32$ of $D_V(z)r^{\rm fid}_{\rm d}/r_{\rm d}=1264\pm22$ Mpc assuming a cosmology in which $r^{\rm fid}_{\rm d}=147.10$ Mpc. From the anisotropic analysis, we find an angular diameter distance to $z=0.57$ of $D_{\rm A}(z)r^{\rm fid}_{\rm d}/r_{\rm d}=1401\pm21$ Mpc and a distance to $z=0.32$ of $981\pm20$ Mpc, a 1.5 per cent and 2.0 per cent measurement respectively. The Hubble parameter at $z=0.57$ is $H(z)r_{\rm d}/r^{\rm fid}_{\rm d}=100.3\pm3.7$ km s$^{-1}$ Mpc$^{-1}$ and its value at $z=0.32$ is $79.2\pm5.6$ km s$^{-1}$ Mpc$^{-1}$, a 3.7 per cent and 7.1 per cent measurement respectively. These cosmic distance scale constraints are in excellent agreement with a $\Lambda$CDM model with cosmological parameters released by the recent Planck 2015 results., Comment: 18 pages, 10 figures, 13 tables. Matches version accepted for publication in MNRAS. Here we account for a systematic error budget not included in the previous version of this manuscript
Published: 2016
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134. A 2 per cent distance toz= 0.35 by reconstructing baryon acoustic oscillations – III. Cosmological measurements and interpretation

Author: Xiaoying Xu, Nikhil Padmanabhan, Antonio J. Cuesta, Daniel J. Eisenstein, and Kushal T. Mehta
Subjects: Physics, 010308 nuclear & particles physics, Equation of state (cosmology), Cosmic microwave background, Shape of the universe, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmological constant, Astrophysics, 01 natural sciences, Galaxy, symbols.namesake, Space and Planetary Science, 0103 physical sciences, symbols, Dark energy, Baryon acoustic oscillations, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Hubble's law
Abstract: We use the 2% distance measurement from our reconstructed baryon acoustic oscillations (BAOs) signature using the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) Luminous Red Galaxies (LRGs) from Padmanabhan et al. (2012) and Xu et al. (2012) combined with cosmic microwave background (CMB) data from Wilkinson Microwave Anisotropy Probe (WMAP7) to measure parameters for various cosmological models. We find a 1.7% measurement of H_0 = 69.8 +/- 1.2 km/s/Mpc and a 5.0% measurement of Omega_m = 0.280 +/- 0.014 for a flat Universe with a cosmological constant. These measurements of H_0 and Omega_m are robust against a range of underlying models for the expansion history. We measure the dark energy equation of state parameter w = -0.97 +/- 0.17, which is consistent with a cosmological constant. If curvature is allowed to vary, we find that the Universe is consistent with a flat geometry (Omega_K = -0.004 +/- 0.005). We also use a combination of the 6 Degree Field Galaxy Survey BAO data, WiggleZ Dark Energy Survey data, Type Ia supernovae (SN) data, and a local measurement of the Hubble constant to explore cosmological models with more parameters. Finally, we explore the effect of varying the energy density of relativistic particles on the measurement of H_0.
Published: 2012
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135. A 2 per cent distance toz= 0.35 by reconstructing baryon acoustic oscillations – I. Methods and application to the Sloan Digital Sky Survey

Author: Nikhil Padmanabhan, Kushal T. Mehta, Daniel J. Eisenstein, Eyal A. Kazin, Antonio J. Cuesta, Xiaoying Xu, and Richard Scalzo
Subjects: Physics, 010308 nuclear & particles physics, Angular diameter distance, Astronomy and Astrophysics, Reconstruction algorithm, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Correlation function (astronomy), Redshift survey, 01 natural sciences, Galaxy, Baryon, Space and Planetary Science, 0103 physical sciences, Baryon acoustic oscillations, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Smoothing
Abstract: We apply the reconstruction technique to the clustering of galaxies from the SDSS DR7 LRG sample, sharpening the baryon acoustic oscillation (BAO) feature and achieving a 1.9% measurement of the distance to z=0.35. This is the first application of reconstruction of the BAO feature in a galaxy redshift survey. We update the reconstruction algorithm of Eisenstein et al, 2007 to account for the effects of survey geometry as well as redshift-space distortions and validate it on 160 LasDamas simulations. We demonstrate that reconstruction sharpens the BAO feature in the angle averaged galaxy correlation function, reducing the nonlinear smoothing scale \Sigma_nl from 8.1 Mpc/h to 4.4 Mpc/h. Reconstruction also significantly reduces the effects of redshift-space distortions at the BAO scale, isotropizing the correlation function. This sharpened BAO feature yields an unbiased distance estimate (< 0.2%) and reduces the scatter from 3.3% to 2.1%. We demonstrate the robustness of these results to the various reconstruction parameters, including the smoothing scale, the galaxy bias and the linear growth rate. Applying this reconstruction algorithm to the SDSS LRG DR7 sample improves the significance of the BAO feature in these data from 3.3 sigma for the unreconstructed correlation function, to 4.2 sigma after reconstruction. We estimate a relative distance scale D_V/r_s to z=0.35 of 8.88+/-0.17, where r_s is the sound horizon and D_V = (D_A^2/H)^{1/3} is a combination of the angular diameter distance D_A and Hubble parameter H. Assuming a sound horizon of 154.25 Mpc, this translates into a distance measurement D_V (z=0.35) = 1.356+/-0.025 Gpc. We find that reconstruction reduces the distance error in the DR7 sample from 3.5% to 1.9%, equivalent to a survey with three times the volume of SDSS.
Published: 2012
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136. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measurements of the growth of structure and expansion rate atz= 0.57 from anisotropic clustering

Author: Claudia Maraston, Hee-Jong Seo, Molly E. C. Swanson, Marc Manera, Gong-Bo Zhao, Elena Malanushenko, David J. Schlegel, Stephanie A. Snedden, Ashley J. Ross, Benjamin A. Weaver, Jon Brinkmann, Alaina Shelden, Nicholas P. Ross, K. Honscheid, Joel R. Brownstein, Licia Verde, Viktor Malanushenko, Erin S. Sheldon, Ariel G. Sánchez, Beth Reid, Demitri Muna, Martin White, Natalie A. Roe, Will J. Percival, Jeremy L. Tinker, Rita Tojeiro, James E. Gunn, Robert C. Nichol, Daniel Oravetz, Adam S. Bolton, Lado Samushia, Idit Zehavi, Nikhil Padmanabhan, Kaike Pan, Howard Brewington, David H. Weinberg, Ramin A. Skibba, Roland de Putter, David Wake, Dmitry Bizyaev, Antonio J. Cuesta, Audrey Simmons, Cameron K. McBride, Daniel J. Eisenstein, Stephen Bailey, Daniel Thomas, and Donald P. Schneider
Subjects: Physics, 010308 nuclear & particles physics, Oscillation, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Lambda, 01 natural sciences, Omega, Galaxy, Redshift, Baryon, Space and Planetary Science, Sky, 0103 physical sciences, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, 10. No inequality, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We analyze the anisotropic clustering of massive galaxies from the Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) sample, which consists of 264,283 galaxies in the redshift range 0.43 0.57, and when combined imply \Omega_{\Lambda} = 0.74 +/- 0.016, independent of the Universe's evolution at z
Published: 2012
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137. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large-scale two-point correlation function

Author: Daniel Thomas, K. Honscheid, Beth Reid, Kushal T. Mehta, David A. Wake, V. Malanushenko, David J. Schlegel, Kaike Pan, Daniel J. Eisenstein, Ashley J. Ross, Martin White, Robert C. Nichol, Shirley Ho, Joel R. Brownstein, A. Shelden, Gong-Bo Zhao, Jose Alberto Rubino-Martin, Eyal A. Kazin, Francesco Montesano, Antonio J. Cuesta, Howard Brewington, Rita Tojeiro, Will J. Percival, Cameron K. McBride, Natalie A. Roe, David H. Weinberg, A. Labatie, Éric Aubourg, Claudia Maraston, J. Richard Gott, Xiaoying Xu, Marc Manera, Francisco Prada, Stephen Bailey, Nicholas P. Ross, Donald P. Schneider, Demitri Muna, Neta A. Bahcall, Jeremy L. Tinker, Adam S. Bolton, Jean-Christophe Hamilton, Daniel Oravetz, Nikhil Padmanabhan, Ramin A. Skibba, Jon Brinkmann, Antonio D. Montero-Dorta, Benjamin A. Weaver, Claudia G. Scóccola, Stephanie A. Snedden, X. Mazzalay, Audrey Simmons, Elena Malanushenko, M. Vargas Magaña, Ariel G. Sánchez, Dmitry Bizyaev, and Idit Zehavi
Subjects: Physics, 010308 nuclear & particles physics, Oscillation, Cosmic microwave background, Astronomy and Astrophysics, Cosmological constant, Astrophysics, 01 natural sciences, Omega, Galaxy, Baryon, Correlation function, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Neutrino, 010303 astronomy & astrophysics
Abstract: We obtain constraints on cosmological parameters from the spherically averaged redshift-space correlation function of the CMASS Data Release 9 (DR9) sample of the Baryonic Oscillation Spectroscopic Survey (BOSS). We combine this information with additional data from recent CMB, SN and BAO measurements. Our results show no significant evidence of deviations from the standard flat-Lambda CDM model, whose basic parameters can be specified by Omega_m = 0.285 +- 0.009, 100 Omega_b = 4.59 +- 0.09, n_s = 0.96 +- 0.009, H_0 = 69.4 +- 0.8 km/s/Mpc and sigma_8 = 0.80 +- 0.02. The CMB+CMASS combination sets tight constraints on the curvature of the Universe, with Omega_k = -0.0043 +- 0.0049, and the tensor-to-scalar amplitude ratio, for which we find r < 0.16 at the 95 per cent confidence level (CL). These data show a clear signature of a deviation from scale-invariance also in the presence of tensor modes, with n_s
Published: 2012
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138. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: analysis of potential systematics

Author: Ashley J. Ross, Will J. Percival, Ariel G. Sánchez, Lado Samushia, Shirley Ho, Eyal Kazin, Marc Manera, Beth Reid, Martin White, Rita Tojeiro, Cameron K. McBride, Xiaoying Xu, David A. Wake, Michael A. Strauss, Francesco Montesano, Molly E. C. Swanson, Stephen Bailey, Adam S. Bolton, Antonio Montero Dorta, Daniel J. Eisenstein, Hong Guo, Jean-Christophe Hamilton, Robert C. Nichol, Nikhil Padmanabhan, Francisco Prada, David J. Schlegel, Mariana Vargas Magaña, Idit Zehavi, Michael Blanton, Dmitry Bizyaev, Howard Brewington, Antonio J. Cuesta, Elena Malanushenko, Viktor Malanushenko, Daniel Oravetz, John Parejko, Kaike Pan, Donald P. Schneider, Alaina Shelden, Audrey Simmons, Stephanie Snedden, and Gong-bo Zhao
Subjects: Physics, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Correlation function (astronomy), 01 natural sciences, Galaxy, Redshift, Baryon, Stars, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Surface brightness, 010303 astronomy & astrophysics, Stellar density, Astrophysics::Galaxy Astrophysics
Abstract: We analyze the density field of galaxies observed by the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS) included in the SDSS Data Release Nine (DR9). DR9 includes spectroscopic redshifts for over 400,000 galaxies spread over a footprint of 3,275 deg^2. We identify, characterize, and mitigate the impact of sources of systematic uncertainty on large-scale clustering measurements, both for angular moments of the redshift-space correlation function and the spherically averaged power spectrum, P(k), in order to ensure that robust cosmological constraints will be obtained from these data. A correlation between the projected density of stars and the higher redshift (0.43 120h^-1Mpc or k < 0.01hMpc^-1. We find that these errors can be ameliorated by weighting galaxies based on their surface brightness and the local stellar density. We use mock galaxy catalogs that simulate the CMASS selection function to determine that randomly selecting galaxy redshifts in order to simulate the radial selection function of a random sample imparts the least systematic error on correlation function measurements and that this systematic error is negligible for the spherically averaged correlation function. The methods we recommend for the calculation of clustering measurements using the CMASS sample are adopted in companion papers that locate the position of the baryon acoustic oscillation feature (Anderson et al. 2012), constrain cosmological models using the full shape of the correlation function (Sanchez et al. 2012), and measure the rate of structure growth (Reid et al. 2012). (abridged)
Published: 2012
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139. STRONG FIELD-TO-FIELD VARIATION OF Lyα NEBULAE POPULATIONS ATz≃ 2.3

Author: Romeel Davé, Yujin Yang, Daniel J. Eisenstein, and Ann I. Zabludoff
Subjects: Physics, Space and Planetary Science, Hubble Deep Field, Dark matter, Chandra Deep Field South, Astronomy and Astrophysics, Astrophysics, Halo, Galaxy cluster, Luminosity function, Galaxy, Luminosity
Abstract: Understanding the nature of distant Lyα nebulae, aka blobs, and connecting them to their present-day descendants requires constraining their number density, clustering, and large-scale environment. To measure these basic quantities, we conduct a deep narrowband imaging survey in four different fields, Chandra Deep Field South (CDFS), Chandra Deep Field North (CDFN), and two COSMOS subfields, for a total survey area of 1.2 deg2. We discover 25 blobs at z = 2.3 with Lyα luminosities of L Lyα= (0.7-8) × 1043 erg s–1 and isophotal areas of A iso = 10-60 . The transition from compact Lyα emitters (LAEs; A iso ~ a few ) to extended Lyα blobs (A iso > 10 ) is continuous, suggesting a single family perhaps governed by similar emission mechanisms. Surprisingly, most blobs (16/25) are in one survey field, the CDFS. The six brightest, largest blobs with L Lyα 1.5×1043 erg s–1 and A iso > 16 lie only in the CDFS. These large, bright blobs have a field-to-field variance of σ v 1.5 (150%) about their number density n ~1.0+1.8 –0.6× 10–5 Mpc–3. This variance is large, significantly higher than that of unresolved LAEs (σ v ~ 0.3 or 30%), and can adversely affect comparisons of blob number densities and luminosity functions (LFs) among different surveys. Our deep, blind survey allows us to construct a reliable blob LF. We compare the statistics of our blobs with dark matter halos in a 1 h –1 Gpc cosmological N-body simulation. At z = 2.3, n implies that each bright, large blob could occupy a halo of M halo 1013 M ☉ if most halos have detectable blobs. The predicted variance in n is consistent with that observed and corresponds to a bias of ~7. Blob halos lie at the high end of the halo mass distribution at z = 2.3 and are likely to evolve into the ~1014 M ☉ halos typical of galaxy clusters today. On larger scales of ~10 comoving Mpc, blobs cluster where compact LAEs cluster, indicating that blobs lie in coherent, highly overdense structures.
Published: 2010
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140. THE EVOLUTION OF THE STAR FORMATION RATE OF GALAXIES AT 0.0 ⩽z⩽ 1.2

Author: S. S. Murray, George H. Rieke, John Moustakas, Emeric Le Floc'h, Richard J. Cool, Wiphu Rujopakarn, Christopher S. Kochanek, Peter Eisenhardt, Daniel J. Eisenstein, Arjun Dey, Casey Papovich, Michael J. I. Brown, Buell T. Januzzi, and Marcia J. Rieke
Subjects: Physics, Active galactic nucleus, 010504 meteorology & atmospheric sciences, Star formation, Extinction (astronomy), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, Luminosity, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, 0105 earth and related environmental sciences, Luminosity function (astronomy)
Abstract: We present the 24 micron rest-frame luminosity function (LF) of star-forming galaxies in the redshift range 0.0 < z < 0.6 constructed from 4047 spectroscopic redshifts from the AGN and Galaxy Evolution Survey of 24 micron selected sources in the Bootes field of the NOAO Deep Wide-Field Survey. This sample provides the best available combination of large area (9 deg^2), depth, and statistically complete spectroscopic observations, allowing us to probe the evolution of the 24 micron LF of galaxies at low and intermediate redshifts while minimizing the effects of cosmic variance. In order to use the observed 24 micron luminosity as a tracer for star formation, active galactic nuclei (AGNs) that could contribute significantly at 24 micron are identified and excluded from our star-forming galaxy sample based on their mid-IR spectral energy distributions or the detection of X-ray emission. The evolution of the 24 micron LF of star-forming galaxies for redshifts of z < 0.65 is consistent with a pure luminosity evolution where the characteristic 24 micron luminosity evolves as (1+z)^(3.8+/-0.3). We extend our evolutionary study to encompass 0.0 < z < 1.2 by combining our data with that of the Far-Infrared Deep Extragalactic Legacy Survey. Over this entire redshift range the evolution of the characteristic 24 micron luminosity is described by a slightly shallower power law of (1+z)^(3.4+/-0.2). We find a local star formation rate density of (1.09+/-0.21) x 10^-2 Msun/yr/Mpc^-3, and that it evolves as (1+z)^(3.5+/-0.2) over 0.0 < z < 1.2. These estimates are in good agreement with the rates using optical and UV fluxes corrected for the effects of intrinsic extinction in the observed sources. This agreement confirms that star formation at z, Comment: ApJ, in press, 16 pages 9 figures
Published: 2010
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141. THE SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY

Author: Kevork N. Abazajian, Jennifer K. Adelman-McCarthy, Marcel A. Agüeros, Sahar S. Allam, Carlos Allende Prieto, Deokkeun An, Kurt S. J. Anderson, Scott F. Anderson, James Annis, Neta A. Bahcall, C. A. L. Bailer-Jones, J. C. Barentine, Bruce A. Bassett, Andrew C. Becker, Timothy C. Beers, Eric F. Bell, Vasily Belokurov, Andreas A. Berlind, Eileen F. Berman, Mariangela Bernardi, Steven J. Bickerton, Dmitry Bizyaev, John P. Blakeslee, Michael R. Blanton, John J. Bochanski, William N. Boroski, Howard J. Brewington, Jarle Brinchmann, J. Brinkmann, Robert J. Brunner, Tamás Budavári, Larry N. Carey, Samuel Carliles, Michael A. Carr, Francisco J. Castander, David Cinabro, A. J. Connolly, István Csabai, Carlos E. Cunha, Paul C. Czarapata, James R. A. Davenport, Ernst de Haas, Ben Dilday, Mamoru Doi, Daniel J. Eisenstein, Michael L. Evans, N. W. Evans, Xiaohui Fan, Scott D. Friedman, Joshua A. Frieman, Masataka Fukugita, Boris T. Gänsicke, Evalyn Gates, Bruce Gillespie, G. Gilmore, Belinda Gonzalez, Carlos F. Gonzalez, Eva K. Grebel, James E. Gunn, Zsuzsanna Györy, Patrick B. Hall, Paul Harding, Frederick H. Harris, Michael Harvanek, Suzanne L. Hawley, Jeffrey J. E. Hayes, Timothy M. Heckman, John S. Hendry, Gregory S. Hennessy, Robert B. Hindsley, J. Hoblitt, Craig J. Hogan, David W. Hogg, Jon A. Holtzman, Joseph B. Hyde, Shin-ichi Ichikawa, Takashi Ichikawa, Myungshin Im, Željko Ivezić, Sebastian Jester, Linhua Jiang, Jennifer A. Johnson, Anders M. Jorgensen, Mario Jurić, Stephen M. Kent, R. Kessler, S. J. Kleinman, G. R. Knapp, Kohki Konishi, Richard G. Kron, Jurek Krzesinski, Nikolay Kuropatkin, Hubert Lampeitl, Svetlana Lebedeva, Myung Gyoon Lee, Young Sun Lee, R. French Leger, Sébastien Lépine, Nolan Li, Marcos Lima, Huan Lin, Daniel C. Long, Craig P. Loomis, Jon Loveday, Robert H. Lupton, Eugene Magnier, Olena Malanushenko, Viktor Malanushenko, Rachel Mandelbaum, Bruce Margon, John P. Marriner, David Martínez-Delgado, Takahiko Matsubara, Peregrine M. McGehee, Timothy A. McKay, Avery Meiksin, Heather L. Morrison, Fergal Mullally, Jeffrey A. Munn, Tara Murphy, Thomas Nash, Ada Nebot, Eric H. Neilsen, Heidi Jo Newberg, Peter R. Newman, Robert C. Nichol, Tom Nicinski, Maria Nieto-Santisteban, Atsuko Nitta, Sadanori Okamura, Daniel J. Oravetz, Jeremiah P. Ostriker, Russell Owen, Nikhil Padmanabhan, Kaike Pan, Changbom Park, George Pauls, John Peoples, Will J. Percival, Jeffrey R. Pier, Adrian C. Pope, Dimitri Pourbaix, Paul A. Price, Norbert Purger, Thomas Quinn, M. Jordan Raddick, Paola Re Fiorentin, Gordon T. Richards, Michael W. Richmond, Adam G. Riess, Hans-Walter Rix, Constance M. Rockosi, Masao Sako, David J. Schlegel, Donald P. Schneider, Ralf-Dieter Scholz, Matthias R. Schreiber, Axel D. Schwope, Uroš Seljak, Branimir Sesar, Erin Sheldon, Kazu Shimasaku, Valena C. Sibley, A. E. Simmons, Thirupathi Sivarani, J. Allyn Smith, Martin C. Smith, Vernesa Smolčić, Stephanie A. Snedden, Albert Stebbins, Matthias Steinmetz, Chris Stoughton, Michael A. Strauss, Mark SubbaRao, Yasushi Suto, Alexander S. Szalay, István Szapudi, Paula Szkody, Masayuki Tanaka, Max Tegmark, Luis F. A. Teodoro, Aniruddha R. Thakar, Christy A. Tremonti, Douglas L. Tucker, Alan Uomoto, Daniel E. Vanden Berk, Jan Vandenberg, S. Vidrih, Michael S. Vogeley, Wolfgang Voges, Nicole P. Vogt, Yogesh Wadadekar, Shannon Watters, David H. Weinberg, Andrew A. West, Simon D. M. White, Brian C. Wilhite, Alainna C. Wonders, Brian Yanny, D. R. Yocum, Donald G. York, Idit Zehavi, Stefano Zibetti, and Daniel B. Zucker
Subjects: Cosmology and Gravitation, Astronomy, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, atlases, catalogs, surveys, law.invention, Photometry (optics), law, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Imaging systems in astronomy, Stars--Observations, Celestial equator, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Quasar, Astrometry, Astrograph, Galaxy, Stars, Space and Planetary Science, Sky
Abstract: This paper describes the Seventh Data Release of the Sloan Digital Sky Survey (SDSS), marking the completion of the original goals of the SDSS and the end of the phase known as SDSS-II. It includes 11663 deg^2 of imaging data, with most of the roughly 2000 deg^2 increment over the previous data release lying in regions of low Galactic latitude. The catalog contains five-band photometry for 357 million distinct objects. The survey also includes repeat photometry over 250 deg^2 along the Celestial Equator in the Southern Galactic Cap. A coaddition of these data goes roughly two magnitudes fainter than the main survey. The spectroscopy is now complete over a contiguous area of 7500 deg^2 in the Northern Galactic Cap, closing the gap that was present in previous data releases. There are over 1.6 million spectra in total, including 930,000 galaxies, 120,000 quasars, and 460,000 stars. The data release includes improved stellar photometry at low Galactic latitude. The astrometry has all been recalibrated with the second version of the USNO CCD Astrograph Catalog (UCAC-2), reducing the rms statistical errors at the bright end to 45 milli-arcseconds per coordinate. A systematic error in bright galaxy photometr is less severe than previously reported for the majority of galaxies. Finally, we describe a series of improvements to the spectroscopic reductions, including better flat-fielding and improved wavelength calibration at the blue end, better processing of objects with extremely strong narrow emission lines, and an improved determination of stellar metallicities. (Abridged), Comment: 20 pages, 10 embedded figures. Accepted to ApJS after minor corrections
Published: 2009
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142. EXTENDED Lyα NEBULAE ATz≃ 2.3: AN EXTREMELY RARE AND STRONGLY CLUSTERED POPULATION?

Author: Romeel Davé, Daniel J. Eisenstein, Yujin Yang, Ann I. Zabludoff, and Christy A. Tremonti
Subjects: Physics, education.field_of_study, Radio galaxy, Population, Astronomy and Astrophysics, BOOTES, Astrophysics, Redshift, Galaxy, Space and Planetary Science, Halo, education, Galaxy cluster, Line (formation)
Abstract: To obtain an unbiased sample of bright LyA blobs [L(LyA) > 10^43 ergs/s], we have undertaken a blind, wide-field, narrow-band imaging survey in the NOAO Deep Wide Field Survey Bootes field with the Steward Bok-2.3m telescope. After searching over 4.82 sq. degrees at z=2.3, we discover four LyA blobs with L(LyA) = 1.6-5.3 x 10^43 ergs/s, isophotal areas of 28-57 sq. arcsec, and broad LyA line profiles (FWHM = 900-1250 km/s). In contrast with the extended Lyman alpha halos associated with high-z radio galaxies, none of our four blobs are radio-loud. The X-ray luminosities and optical spectra of these blobs are diverse. Two blobs (3 and 4) are X-ray-detected with L_X(2-7 keV) = 2-4 x 10^44 ergs/s and have broad optical emission lines (C IV) characteristic of AGN, implying that 50% of our sample blobs are associated with strong AGN. The other 50% of blobs (1 and 2) are not X-ray or optically-detected as AGN down to similar limits. The number density of the four blobs is ~3 x 10^{-6} Mpc^{-3}, comparable to that of galaxy clusters at similar redshifts and 3x lower than that found in the SSA22 proto-cluster at z=3.1, even after accounting for the over-density of that region. The two X-ray undetected blobs are separated by only 70" (550 kpc) and have almost identical redshifts (< 360 kpc along the line-of-sight), suggesting that they are part of the same system. Given the rarity of the blobs and our discovery of a close pair, we speculate that blobs occupy the highest density regions and thus may be precursors of today's rich cluster galaxies.
Published: 2009
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143. The Radial Velocity Experiment (RAVE)

Author: A. Siebert, Ivan Minchev, M. Fiorucci, Randy D. Campbell, Gerry Gilmore, J. P. Fulbright, M. C. Smith, U. Munari, Quentin A. Parker, D. Burton, M. Hartley, George M. Seabroke, U. Jauregi, Gregory R. Ruchti, B. J. Boyle, Olivier Bienaymé, Ortwin Gerhard, Nick Evans, Matthias Steinmetz, Alessandro Siviero, Tomaz Zwitter, Harry Enke, R. von Berlepsch, James Binney, Daniel J. Eisenstein, Rosanna Sordo, Genevieve Parmentier, Eva K. Grebel, Will Saunders, Alice C. Quillen, Siegfried Roeser, Joss Bland-Hawthorn, F. G. Watson, Kenneth C. Freeman, A. Kelz, S. Vidrih, L. Mijovic, J. Penarrubia, J. A. Dawe, Ralf-Dieter Scholz, K. S. Russell, Rosemary F. G. Wyse, Kristin Fiegert, Jeremy Bailin, C. J. P. Cass, M. Williams, Corrado Boeche, W. Dehnen, Julio F. Navarro, Mike Read, Amina Helmi, Brad K. Gibson, Elena Schilbach, L. Veltz, Astronomy, and Kapteyn Astronomical Institute
Subjects: Cold dark matter, 010504 meteorology & atmospheric sciences, RESOLUTION GALACTIC SPECTRA, STELLAR CONTENT, Milky Way, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Kinematics, Astrophysics, 01 natural sciences, ABUNDANCES, surveys, stars : fundamental parameters, 0103 physical sciences, Galaxy formation and evolution, Maximum a posteriori estimation, Astrophysics::Solar and Stellar Astrophysics, KINEMATICS, Disc, MAXIMUM A-POSTERIORI, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, OPEN CLUSTER M67, Radial velocity, Red-giant branch, BAADES WINDOW GIANTS, 13. Climate action, Space and Planetary Science, MILKY-WAY, Astrophysics::Earth and Planetary Astrophysics, KECK HIRES SPECTRA, SKY SURVEY, catalogs
Abstract: We present the second data release of the Radial Velocity Experiment (RAVE), an ambitious spectroscopic survey to measure radial velocities (RVs) and stellar atmosphere parameters of up to one million stars using the 6dF multi-object spectrograph on the 1.2-m UK Schmidt Telescope of the Anglo-Australian Observatory (AAO). It is obtaining medium resolution spectra (median R=7,500) in the Ca-triplet region (8,410--8,795 \AA) for southern hemisphere stars in the magnitude range 9, Comment: 85 pages, 23 figures, 14 tables, accepted for publication in the Astronomical Journal
Published: 2008
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144. On the Stellar Populations in Faint Red Galaxies in theHubbleUltra Deep Field1

Author: Daniel J. Eisenstein, Casey Papovich, and Amelia M. Stutz
Subjects: Physics, Stellar population, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Large range, Astrophysics, Hubble Ultra-Deep Field, Redshift, Galaxy, Photometry (optics), Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We study the nature of faint, red-selected galaxies at z ~ 2-3 using the Hubble Ultra Deep Field (HUDF) and Spitzer IRAC photometry. We detect candidate galaxies to H 1.0 mag color selection, 16 of which have unblended [3.6um] and [4.5um] IRAC photometry. We derive photometric redshifts, masses, and stellar population parameters for these objects. We find that the selected objects span a diverse range of properties over a large range of redshifts, 1 2.5 objects that are dominated by evolved stellar populations have a space density at most one-third that of z ~ 0 red, early-type galaxies. Therefore, at least two-thirds of present-day early-type galaxies assemble or evolve into their current configuration at redshifts below 2.5. We find a dearth of candidates for low-mass galaxies at 1.5 < z < 3 that are dominated by passively evolving stellar populations even though the data should be sensitive to them; thus, at these redshifts, galaxies whose light is dominated by evolved stellar populations are restricted to only those galaxies that have assembled high stellar mass.[Abridged]
Published: 2008
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145. Cosmic sound waves rule

Author: Daniel J. Eisenstein and Charles L. Bennett
Subjects: Physics, Physics::General Physics, Physics::Popular Physics, COSMIC cancer database, Distribution (number theory), Cosmic microwave background, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics, Physics::History of Physics, Sound wave, Galaxy
Abstract: In the microwave background and the distribution of galaxies, relic imprints of primordial sound waves have contributed to an extraordinarily detailed history of the cosmos. And they provide yardsticks for resolving a great mystery.
Published: 2008
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146. Low‐Resolution Spectral Templates for Galaxies from 0.2 to 10 μm

Author: Roberto J. Assef, D. Stern, Christopher S. Kochanek, Peter Eisenhardt, M. Brodwin, Daniel J. Eisenstein, R. Cool, C. Jones, Michael J. I. Brown, Nelson Caldwell, E. McKenzie, Anthony H. Gonzalez, S. S. Murray, and Buell T. Jannuzi
Subjects: Physics, Field (physics), Sigma, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), Redshift, Galaxy, Luminosity, Photometry (optics), Space and Planetary Science, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We built an optimal basis of low resolution templates for galaxies over the wavelength range from 0.2 to 10 $\mu$m using a variant of the algorithm presented by Budavari et al. (2000). We derived them using eleven bands of photometry from the NDWFS, FLAMEX, zBo\"otes and IRAC Shallow surveys for 16033 galaxies in the NDWFS Bo\"otes field with spectroscopic redshifts measured by the AGN and Galaxy Evolution Survey. We also developed algorithms to accurately determine photometric redshifts, K corrections and bolometric luminosities using these templates. Our photometric redshifts have an accuracy of $\sigma_z/(1+z) = 0.04$ when clipped to the best 95%. We used these templates to study the spectral type distribution in the field and to estimate luminosity functions of galaxies as a function of redshift and spectral type. In particular, we note that the 5-8$\mu$m color distribution of galaxies is bimodal, much like the optical g--r colors.
Published: 2008
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147. THE SLOAN DIGITAL SKY SURVEY QUASAR LENS SEARCH. II. STATISTICAL LENS SAMPLE FROM THE THIRD DATA RELEASE

Author: Michael D. Gregg, Masamune Oguri, Patrick B. Hall, Alejandro Clocchiatti, Bartosz Pindor, Hans-Walter Rix, David Johnston, Tomoki Morokuma, Neta A. Bahcall, Scott F. Anderson, Min-Su Shin, Michael A. Strauss, Robert H. Lupton, Daniel J. Eisenstein, Issha Kayo, Joshua A. Frieman, Scott Burles, Charles R. Keeton, Ryan Scranton, Yozo Kawano, Edwin L. Turner, Christopher S. Kochanek, Robert J. Brunner, Richard L. White, Robert H. Becker, Erin S. Sheldon, Gordon T. Richards, Joseph F. Hennawi, Donald G. York, Francisco J. Castander, Kuenley Chiu, Naohisa Inada, Donald P. Schneider, and Masataka Fukugita
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, law.invention, Lens (optics), Space and Planetary Science, Sky, law, Magnitude (astronomy), Astrophysics::Solar and Stellar Astrophysics, Data release, Astrophysics::Galaxy Astrophysics, Galaxy cluster, media_common
Abstract: We report the first results of our systematic search for strongly lensed quasars using the spectroscopically confirmed quasars in the Sloan Digital Sky Survey (SDSS). Among 46,420 quasars from the SDSS Data Release 3 (~4188 deg^2), we select a subsample of 22,683 quasars that are located at redshifts between 0.6 and 2.2 and are brighter than the Galactic extinction corrected i-band magnitude of 19.1. We identify 220 lens candidates from the quasar subsample, for which we conduct extensive and systematic follow-up observations in optical and near-infrared wavebands, in order to construct a complete lensed quasar sample at image separations between 1'' and 20'' and flux ratios of faint to bright lensed images larger than 10^{-0.5}. We construct a statistical sample of 11 lensed quasars. Ten of these are galaxy-scale lenses with small image separations (~1''-2'') and one is a large separation (15'') system which is produced by a massive cluster of galaxies, representing the first statistical sample of lensed quasars including both galaxy- and cluster-scale lenses. The Data Release 3 spectroscopic quasars contain an additional 11 lensed quasars outside the statistical sample., Comment: 15 pages, 4 figures, 5 tables, accepted for publication in AJ; see http://www-utap.phys.s.u-tokyo.ac.jp/~sdss/sqls/ for supplemental information
Published: 2008
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148. The SDSS-IV Extended Baryon Oscillation Spectroscopic Survey : overview and early data

Author: Joe Huehnerhoff, Jo Bovy, Jean-Marc Le Goff, Nicolás G. Busca, Matthew A. Bershady, Will J. Percival, Yipeng Jing, Marcio A. G. Maia, Conor Sayres, Diana Holder, Xiaohui Fan, Eric Jullo, Flavia Sobreira, Sergio Rodríguez-Torres, Vikrant Kamble, Antonio D. Montero-Dorta, Yu Liang, Andreas A. Berlind, Patrick Gaulme, Beth Reid, Stephen Bailey, Peter Nugent, Andrea Merloni, Peter M. Frinchaboy, Dmitry Bizyaev, A. C. Rosell, Gong-Bo Zhao, Tracy Naugle, Yen-Ting Lin, Vivek Mariappan, Zhongxu Zhai, Julien Guy, Hélion du Mas des Bourboux, Shirley Ho, Martin White, Éric Aubourg, Abhishek Prakash, Pasquier Noterdaeme, Yuting Wang, Audrey Oravetz, Dustin Lang, Uroš Seljak, W. N. Brandt, Demitri Muna, Patrick Petitjean, Sylvain de la Torre, M. C. Cousinou, Ian D. McGreer, Pierre Laurent, Adam D. Myers, Isabelle Paris, Andres Meza, John J. Ruan, Franco D. Albareti, Etienne Burtin, Kyle S. Dawson, Adam S. Bolton, Alina Streblyanska, Nikhil Padmanabhan, Marcos Lima, Chia-Hsun Chuang, Kaike Pan, Benjamin A. Weaver, Daniel J. Eisenstein, Branimir Sesar, Mariana Vargas-Magaña, Ashley J. Ross, Alice Pisani, Axel de la Macorra, Mark A. Klaene, Nathalie Palanque-Delabrouille, Karen Kinemuchi, Nicholas R. MacDonald, Rita Tojeiro, Nicolas Clerc, Nao Suzuki, Scott F. Anderson, Dan Long, John A. Peacock, Kirpal Nandra, Johan Comparat, D. Kirkby, Anze Slosar, Timothy A. Hutchinson, Michael Blomqvist, Donald P. Schneider, Stephanie Escoffier, Jeremy L. Tinker, Charling Tao, Irene Cruz-González, Jon Brinkmann, Michael Eracleous, Francisco-Shu Kitaura, Hu Zou, Elena Malanushenko, Yiping Shu, Anand Raichoor, W. M. Wood-Vasey, Andreu Font-Ribera, Tom Dwelly, J. Ridl, Graziano Rossi, Hee-Jong Seo, Britt Lundgren, Sarah Shandera, Brice Ménard, Luiz N. da Costa, Shadab Alam, Ricardo L. C. Ogando, Christophe Yèche, Daniel Oravetz, Matthew M. Pieri, Jean-Paul Kneib, Julian E. Bautista, Weipeng Lin, Mara Salvato, Antonis Georgakakis, Alexis Finoguenov, Hong Guo, Florian Beutler, Guangtun Zhu, Jeremy Darling, Zheng Zheng, Frances Cope, Donna Taylor, Francisco Prada, David H. Weinberg, Cheng Li, Rupert A. C. Croft, Joel R. Brownstein, Viktor Malanushenko, Paul J. Green, Jeffrey A. Newman, John K. Parejko, David J. Schlegel, Matthew D. Olmstead, Russ R. Laher, Cameron K. McBride, Cheng Zhao, Timothée Delubac, James Rich, Michael R. Blanton, Eric Armengaud, Anne Ealet, Zheng Cai, Qiufan Lin, University of St Andrews. School of Physics and Astronomy, AVL, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Research Institute of Forest Resource Information Techniques, Chinese Academy of Forestry, Centre Hospitalier Universitaire de Dijon - Hôpital François Mitterrand (CHU Dijon), McMaster University [Hamilton, Ontario], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Shanghai Astronomical Observatory [Shanghai] (SHAO), Chinese Academy of Sciences [Beijing] (CAS), Departamento de Fisica Matematica, Universidade de São Paulo = University of São Paulo (USP), Max-Planck-Institut für Astrophysik (MPA), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Universidad de Chile = University of Chile [Santiago] (UCHILE), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Department of Electrical and Computer Engineering [Minneapolis] (ECE), University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, China National Research Center of Intelligent Equipment for Agriculture [Beijing] (NRCIEA), Key Laboratory for Liquid-Solid Structural Evolution and Processing of Materials, Shandong University, Laboratoire de Chimie - UMR5182 (LC), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Universidad Autonoma de Madrid (UAM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of California [Irvine] (UCI), University of California-University of California, Département de Physique des Particules (ex SPP) (DPP), Universidade de São Paulo (USP), Universidad Santiago de Chile, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, University of Minnesota [Twin Cities], École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), UAM. Departamento de Física Teórica, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon)-Institut de Chimie du CNRS (INC), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, surveys, Tests of general relativity, 0103 physical sciences, ST/K0090X/1, QB Astronomy, Emission spectrum, observations [Cosmology], 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, QC, QB, Physics, 010308 nuclear & particles physics, Física, RCUK, Astronomy and Astrophysics, Quasar, 3rd-DAS, Redshift, Galaxy, Baryon, QC Physics, Space and Planetary Science, cosmology: observations, astro-ph.CO, Baryon acoustic oscillations, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Astrophysical Journal 151.2 (2016): 44 reproduced by permission of the AAS, 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 dA(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 dA(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 dA(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 dA(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, K.D. acknowledges support from the U.S. Department of Energy under Grant DE-SC000995. J.P.K. and T.D. acknowledge support from the ERC advanced grant LIDA. W.J.P. acknowledges support from the UK STFC through the consolidated grant ST/K0090X/1, and from the European Research Council through grant Darksurvey
Published: 2016
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149. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: higher-order correlations revealed by germ-grain Minkowski Functionals

Author: Daniel J. Eisenstein and Alexander Wiegand
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Oscillation, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), 01 natural sciences, Redshift, Galaxy, Baryon, Amplitude, Space and Planetary Science, 0103 physical sciences, Minkowski space, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We probe the higher-order clustering of the galaxies in the final data release (DR12) of the Sloan Digital Sky Survey Baryon Oscillation Spectroscopic Survey (BOSS) using the method of germ-grain Minkowski Functionals (MFs). Our sample consists of 410,615 BOSS galaxies from the northern Galactic cap in the redshift range 0.450--0.595. We show the MFs to be sensitive to contributions up to the six-point correlation function for this data set. We ensure with a custom angular mask that the results are more independent of boundary effects than in previous analyses of this type. We extract the higher-order part of the MFs and quantify the difference to the case without higher-order correlations. The resulting $\chi^{2}$ value of over 10,000 for a modest number of degrees of freedom, O(200), indicates a 100-sigma deviation and demonstrates that we have a highly significant signal of the non-Gaussian contributions to the galaxy distribution. This statistical power can be useful in testing models with differing higher-order correlations. Comparing the galaxy data to the QPM and MultiDark-Patchy mocks, we find that the latter better describes the observed structure. From an order-by-order decomposition we expect that, for example, already a reduction of the amplitude of the MD-Patchy mock power spectrum by 5% would remove the remaining tension., Comment: 18 pages, 18 figures
Published: 2016
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150. Modelling galactic conformity with the colour–halo age relation in the Illustris simulation

Author: Mark Vogelsberger, Laura V. Sales, Volker Springel, Shy Genel, Vicente Rodriguez-Gomez, Paul Torrey, Emily Chengxi Zhu, Aaron D. Bray, Lars Hernquist, Daniel J. Eisenstein, Annalisa Pillepich, Dylan Nelson, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Vogelsberger, Mark, and Torrey, Paul A.
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, 010308 nuclear & particles physics, Dark matter, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Type-cD galaxy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Dark matter halo, Galactic halo, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Galaxy formation and evolution, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Comparisons between observational surveys and galaxy formation models find that the mass of dark matter haloes can largely explain galaxies' stellar mass. However, it remains uncertain whether additional environmental variables, generally referred to 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 $M_{stellar}$ > $2 \times 10^9$ $M_{\odot}$. 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 can be given as a combination of the halo conformity signal with the galaxy color-halo age relation: at fixed stellar mass, particularly toward the low-mass end, Illustris' galaxy colors correlate with halo age, with the reddest galaxies (often satellites) being preferentially found in the oldest haloes. In fact, we can explain the galactic conformity effect with a simple semi-empirical model, by assigning stellar mass based on halo mass (abundance matching) and by assigning galaxy color based on halo age (age matching). We investigate other interpretations for the galactic conformity, particularly its dependence on the isolation criterion and on the central-satellite information. 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., 15 pages, 8 figures; accepted for publication in MNRAS (minor revisions to match accepted version)
Published: 2016

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