Author: "Cameron K. McBride" - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Cameron K. McBride"' showing total 72 results

Start Over Author "Cameron K. McBride"

72 results on '"Cameron K. McBride"'

1. Towards accurate modelling of galaxy clustering on small scales: testing the standard ΛCDM + halo model

Author: Andreas A. Berlind, Roman Scoccimarro, Cameron K. McBride, Jennifer Piscionere, Manodeep Sinha, and B. Wibking
Subjects: Physics, 010308 nuclear & particles physics, Dark matter, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), Lambda, 01 natural sciences, Galaxy, Cosmology, symbols.namesake, Space and Planetary Science, 0103 physical sciences, symbols, Statistical physics, Halo, Planck, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Interpreting the small-scale clustering of galaxies with halo models can elucidate the connection between galaxies and dark matter halos. Unfortunately, the modelling is typically not sufficiently accurate for ruling out models statistically. It is thus difficult to use the information encoded in small scales to test cosmological models or probe subtle features of the galaxy-halo connection. In this paper, we attempt to push halo modelling into the "accurate" regime with a fully numerical mock-based methodology and careful treatment of statistical and systematic errors. With our forward-modelling approach, we can incorporate clustering statistics beyond the traditional two-point statistics. We use this modelling methodology to test the standard $\Lambda\mathrm{CDM}$ + halo model against the clustering of SDSS DR7 galaxies. Specifically, we use the projected correlation function, group multiplicity function and galaxy number density as constraints. We find that while the model fits each statistic separately, it struggles to fit them simultaneously. Adding group statistics leads to a more stringent test of the model and significantly tighter constraints on model parameters. We explore the impact of varying the adopted halo definition and cosmological model and find that changing the cosmology makes a significant difference. The most successful model we tried (Planck cosmology with Mvir halos) matches the clustering of low luminosity galaxies, but exhibits a 2.3$\sigma$ tension with the clustering of luminous galaxies, thus providing evidence that the "standard" halo model needs to be extended. This work opens the door to adding interesting freedom to the halo model and including additional clustering statistics as constraints.
Published: 2018
Full Text: View/download PDF

2. Galaxy morphology and star formation in the Illustris Simulation atz = 0

Author: Annalisa Pillepich, Debora Sijacki, Paul Torrey, Lars Hernquist, Gregory F. Snyder, Volker Springel, Mark Vogelsberger, Jennifer M. Lotz, Laura V. Sales, Shy Genel, Dylan Nelson, Cameron K. McBride, Sijacki, Debora [0000-0002-3459-0438], and Apollo - University of Cambridge Repository
Subjects: Stellar mass, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), Rotation, 01 natural sciences, methods: numerical, Bulge, 0103 physical sciences, galaxies: formation, education, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: structure, Astrophysics::Earth and Planetary Astrophysics, Halo
Abstract: We study how optical galaxy morphology depends on mass and star formation rate (SFR) in the Illustris Simulation. To do so, we measure automated galaxy structures in 10808 simulated galaxies at z=0 with stellar masses 10^9.7 < M_*/M_sun < 10^12.3. We add observational realism to idealized synthetic images and measure non-parametric statistics in rest-frame optical and near-IR images from four directions. We find that Illustris creates a morphologically diverse galaxy population, occupying the observed bulge strength locus and reproducing median morphology trends versus stellar mass, SFR, and compactness. Morphology correlates realistically with rotation, following classification schemes put forth by kinematic surveys. Type fractions as a function of environment agree roughly with data. These results imply that connections among mass, star formation, and galaxy structure arise naturally from models matching global star formation and halo occupation functions when simulated with accurate methods. This raises a question of how to construct experiments on galaxy surveys to better distinguish between models. We predict that at fixed halo mass near 10^12 M_sun, disc-dominated galaxies have higher stellar mass than bulge-dominated ones, a possible consequence of the Illustris feedback model. While Illustris galaxies at M_* ~ 10^11 M_sun have a reasonable size distribution, those at M_* ~ 10^10 M_sun have half-light radii larger than observed by a factor of two. Furthermore, at M_* ~ 10^10.5-10^11 M_sun, a relevant fraction of Illustris galaxies have distinct "ring-like" features, such that the bright pixels have an unusually wide spatial extent., 26 pages, 15 figures, MNRAS accepted version
Published: 2015
Full Text: View/download PDF

3. 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
Full Text: View/download PDF

4. Spatial Clustering of Dark Matter Halos: Secondary Bias, Neighbor Bias, and the Influence of Massive Neighbors on Halo Properties

Author: Andreas A. Berlind, Cameron K. McBride, Risa H. Wechsler, Manodeep Sinha, Ariyeh H. Maller, David H. Weinberg, Andrés N. Salcedo, and Peter Behroozi
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Space and Planetary Science, Excellence, Research council, Sky, 0103 physical sciences, Spatial clustering, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We explore the phenomenon commonly known as halo assembly bias, whereby dark matter halos of the same mass are found to be more or less clustered when a second halo property is considered, for halos in the mass range $3.7 \times 10^{11} \; h^{-1} \mathrm{M_{\odot}} - 5.0 \times 10^{13} \; h^{-1} \mathrm{M_{\odot}}$. Using the Large Suite of Dark Matter Simulations (LasDamas) we consider nine commonly used halo properties and find that a clustering bias exists if halos are binned by mass or by any other halo property. This secondary bias implies that no single halo property encompasses all the spatial clustering information of the halo population. The mean values of some halo properties depend on their halo's distance to a more massive neighbor. Halo samples selected by having high values of one of these properties therefore inherit a neighbor bias such that they are much more likely to be close to a much more massive neighbor. This neighbor bias largely accounts for the secondary bias seen in halos binned by mass and split by concentration or age. However, halos binned by other mass-like properties still show a secondary bias even when the neighbor bias is removed. The secondary bias of halos selected by their spin behaves differently than that for other halo properties, suggesting that the origin of the spin bias is different than of other secondary biases., 14 pages, LaTeX; minor revisions, and added references; results unchanged
Published: 2017

5. Constraining primordial non-Gaussianity with moments of the large-scale density field

Author: Andreas A. Berlind, Marc Manera, Robert J. Scherrer, Roman Scoccimarro, Cameron K. McBride, and Qingqing Mao
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Gaussian, Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, symbols.namesake, Space and Planetary Science, Skewness, Non-Gaussianity, 0103 physical sciences, Kurtosis, symbols, 010303 astronomy & astrophysics, Gaussian network model, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use cosmological N-body simulations to investigate whether measurements of the moments of large-scale structure can yield constraints on primordial non-Gaussianity. We measure the variance, skewness, and kurtosis of the evolved density field from simulations with Gaussian and three different non-Gaussian initial conditions: a local model with f_NL=100, an equilateral model with f_NL=-400, and an orthogonal model with f_NL=-400. We show that the moments of the dark matter density field differ significantly between Gaussian and non-Gaussian models. We also make the measurements on mock galaxy catalogs that contain galaxies with clustering properties similar to those of luminous red galaxies (LRGs). We find that, in the case of skewness and kurtosis, galaxy bias reduces the detectability of non-Gaussianity, though we can still clearly discriminate between different models in our simulation volume. However, in the case of the variance, galaxy bias greatly amplifies the detectability of non-Gaussianity. In all cases we find that redshift distortions do not significantly affect the detectability. When we restrict our measurements to volumes equivalent to the Sloan Digital Sky Survey II (SDSS-II) or Baryon Oscillation Spectroscopic Survey (BOSS) samples, the probability of detecting a departure from the Gaussian model is high by using measurements of the variance, but very low by using only skewness and kurtosis measurements. We find that skewness and kurtosis measurements are never likely to yield useful constraints on primordial non-Gaussianity, but future surveys should be large enough to place meaningful constraints using measurements of the galaxy variance.(Abridged)
Published: 2014
Full Text: View/download PDF

6. The WiggleZ Dark Energy Survey: constraining galaxy bias and cosmic growth with three-point correlation functions

Author: Cameron K. McBride, Rob Sharp, Felipe A. Marín, Ben Jelliffe, Michael D. Gladders, Karl Forster, H. K. C. Yee, Michael Pracy, Michael J. Drinkwater, David Woods, Sarah Brough, David Gilbank, D. Christopher Martin, Russell J. Jurek, Karl Glazebrook, Tamara M. Davis, I-hui Li, Ted K. Wyder, Scott M. Croom, Emily Wisnioski, Matthew Colless, Kevin A. Pimbblet, Chris Blake, Barry F. Madore, Carlos Contreras, Darren J. Croton, Gregory B. Poole, and Warrick J. Couch
Subjects: Physics, Cold dark matter, Dark matter, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift survey, Cosmology, Galaxy, Redshift, Space and Planetary Science, Dark energy, Baryon acoustic oscillations, Astrophysics::Galaxy Astrophysics
Abstract: Higher order statistics are a useful and complementary tool for measuring the clustering of galaxies, containing information on the non-Gaussian evolution and morphology of large-scale structure in the Universe. In this work we present measurements of the three-point correlation function (3PCF) for 187 000 galaxies in the WiggleZ spectroscopic galaxy survey. We explore the WiggleZ 3PCF scale and shape dependence at three different epochs z = 0.35, 0.55 and 0.68, the highest redshifts where these measurements have been made to date. Using N-body simulations to predict the clustering of dark matter, we constrain the linear and non-linear bias parameters of WiggleZ galaxies with respect to dark matter, and marginalize over them to obtain constraints on σ8(z), the variance of perturbations on a scale of 8 h^−1 Mpc and its evolution with redshift. These measurements of σ_8(z), which have 10–20 per cent accuracies, are consistent with the predictions of the Λ cold dark matter concordance cosmology and test this model in a new way.
Published: 2013
Full Text: View/download PDF

7. 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
Full Text: View/download PDF

8. 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
Full Text: View/download PDF

9. 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
Full Text: View/download PDF

10. 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
Full Text: View/download PDF

11. 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
Full Text: View/download PDF

12. The SDSS-IV extended Baryon Oscillation Spectroscopic Survey : Luminous Red Galaxy Target Selection

Author: Jeremy L. Tinker, Vivek Mariappan, Abhishek Prakash, Francisco Prada, Guangtun Zhu, Rita Tojeiro, A. C. Rosell, Stephen Bailey, Sandhya M. Rao, Cameron K. McBride, Kyle S. Dawson, Joel R. Brownstein, Jean-Paul Kneib, David J. Schlegel, Donald P. Schneider, Julian E. Bautista, Jeffrey A. Newman, Adam S. Bolton, Ashley J. Ross, Timothée Delubac, Shirley Ho, Dustin Lang, Johan Comparat, Michael R. Blanton, Hee-Jong Seo, Adam D. Myers, Timothy C. Licquia, Beth Reid, Will J. Percival, University of St Andrews. School of Physics and Astronomy, UAM. Departamento de Física Teórica, 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), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), McMaster University [Hamilton, Ontario], EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Universidad Autonoma de Madrid (UAM), and 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)
Subjects: Infrared, Astrophysics, 01 natural sciences, Atomic, Physical Chemistry, Spectral line, Particle and Plasma Physics, QB Astronomy, 010303 astronomy & astrophysics, media_common, QB, Physics, Oscillation, Cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, 3rd-DAS, observations [cosmology], astro-ph.CO, photometry [galaxies], Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Astrophysics - Cosmology and Nongalactic Astrophysics, Galaxies: general, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Galaxies: distances and redshifts, Methods: data analysis, 0103 physical sciences, data analysis [methods], Nuclear, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Homogeneity (statistics), Molecular, Física, Astronomy and Astrophysics, Galaxies: photometry, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Baryon, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), distances and redshifts [galaxies], Catalogs, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], uploaded-in-3-months-elsewhere, catalogs, general [galaxies]
Abstract: We describe the algorithm used to select the Luminous Red Galaxy (LRG) sample for the extended Baryon Oscillation Spectroscopic Survey (eBOSS) of the Sloan Digital Sky Survey IV (SDSS-IV) using photometric data from both the SDSS and the Wide-Field Infrared Survey Explorer (WISE). LRG targets are required to meet a set of color selection criteria and have z-band and i-band MODEL magnitudes z < 19.95 and 19.9 < i < 21.8, respectively. Our algorithm selects roughly 50 LRG targets per square degree, the great majority of which lie in the redshift range 0.6 < z < 1.0 (median redshift 0.71). We demonstrate that our methods are highly effective at eliminating stellar contamination and lower-redshift galaxies. We perform a number of tests using spectroscopic data from SDSS-III/BOSS to determine the redshift reliability of our target selection and its ability to meet the science requirements of eBOSS. The SDSS spectra are of high enough signal-to-noise ratio that at least 89% of the target sample yields secure redshift measurements. We also present tests of the uniformity and homogeneity of the sample, demonstrating that it should be clean enough for studies of the large-scale structure of the universe at higher redshifts than SDSS-III/BOSS LRGs reached., Submitted in ApJS, 15 pages, 10 figures
Published: 2016
Full Text: View/download PDF

13. 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
Full Text: View/download PDF

14. The extended Baryon Oscillation Spectroscopic Survey: a cosmological forecast

Author: Gong-Bo Zhao, Sarah Shandera, Donald P. Schneider, Francisco Prada, Jean-Paul Kneib, Yuting Wang, Timothée Delubac, Christophe Yèche, Xu Zhou, Kyle S. Dawson, H. Y. Zhang, Andres Meza, Dandan Wang, Nathalie Palanque-Delabrouille, Graziano Rossi, Ashley J. Ross, Alireza Hojjati, Hee-Jong Seo, Yuecheng Zhang, Levon Pogosian, Cameron K. McBride, Hu Zou, Adam D. Myers, Johan Comparat, Kazuya Koyama, Pengyuan Gao, Will J. Percival, Charling Tao, Jeffrey A. Newman, Fangzhou Zhu, Joel R. Brownstein, Key Laboratory for Liquid-Solid Structural Evolution and Processing of Materials, Shandong University, Department of Electrical and Computer Engineering [Minneapolis] (ECE), University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, 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), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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 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), and Universidad Autonoma de Madrid (UAM)
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, NEUTRINO MASS, 01 natural sciences, ACOUSTIC-OSCILLATIONS, symbols.namesake, ST/K00090/1, 0103 physical sciences, Planck, dark energy, 010303 astronomy & astrophysics, Weak gravitational lensing, STFC, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Oscillation, RCUK, CONSTRAINTS, Astronomy and Astrophysics, Quasar, FOREST, Galaxy, Baryon, large scale structure of Universe, GALAXIES, QUASARS, DATA SETS, Space and Planetary Science, SDSS-III, NON-GAUSSIANITY, symbols, Dark energy, astro-ph.CO, DIGITAL SKY SURVEY, DARK ENERGY, large-scale structure of Universe, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a science forecast for the eBOSS survey, part of the SDSS-IV project, which is a spectroscopic survey using multiple tracers of large-scale structure, including luminous red galaxies (LRGs), emission line galaxies (ELGs) and quasars (both as a direct probe of structure and through the Ly-$\alpha$ forest). Focusing on discrete tracers, we forecast the expected accuracy of the baryonic acoustic oscillation (BAO), the redshift-space distortion (RSD) measurements, the $f_{\rm NL}$ parameter quantifying the primordial non-Gaussianity, the dark energy and modified gravity parameters. We also use the line-of-sight clustering in the Ly-$\alpha$ forest to constrain the total neutrino mass. We find that eBOSS LRGs ($0.60.6$), ELGs ($0.6, Comment: 15 pages, 9 figures, 6 tables; matches the published version on MNRAS
Published: 2016
Full Text: View/download PDF

15. 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
Full Text: View/download PDF

16. 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
Full Text: View/download PDF

17. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring structure growth using passive galaxies

Author: Lado Samushia, Claudia Maraston, Jon Brinkmann, Joel R. Brownstein, Marc Manera, Demitri Duna, Licia Verde, Nicholas P. Ross, Beth Reid, David A. Wake, Molly E. C. Swanson, Rita Tojeiro, Danniel J. Eisenstein, Donald P. Schneider, Ashley J. Ross, Gong-Bo Zhao, Ariel G. Sánchez, Jeremy L. Tinker, Daniel Thomas, Cameron K. McBride, Nikhil Padmanabhan, Ramin A. Skibba, Benjamin A. Weaver, and Will J. Percival
Subjects: Physics, Normalization (statistics), education.field_of_study, Cold dark matter, 010308 nuclear & particles physics, General relativity, Population, Sigma, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Lambda, 01 natural sciences, Galaxy, Baryon, Space and Planetary Science, 0103 physical sciences, education, 010303 astronomy & astrophysics
Abstract: We explore the benefits of using a passively evolving population of galaxies to measure the evolution of the rate of structure growth between z=0.25 and z=0.65 by combining data from the SDSS-I/II and SDSS-III surveys. The large-scale linear bias of a population of dynamically passive galaxies, which we select from both surveys, is easily modeled. Knowing the bias evolution breaks degeneracies inherent to other methodologies, and decreases the uncertainty in measurements of the rate of structure growth and the normalization of the galaxy power-spectrum by up to a factor of two. If we translate our measurements into a constraint on sigma_8(z=0) assuming a concordance cosmological model and General Relativity (GR), we find that using a bias model improves our uncertainty by a factor of nearly 1.5. Our results are consistent with a flat Lambda Cold Dark Matter model and with GR.
Published: 2012
Full Text: View/download PDF

18. 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
Full Text: View/download PDF

19. Haloes gone MAD★: The Halo-Finder Comparison Project

Author: Anatoly Klypin, V. Turchaninov, Stefan Gottloeber, Yann Rasera, Daniel Ceverino, Frazer R. Pearce, Joachim Stadel, Fabrice Roy, Peter Behroozi, Paul M. Sutter, Chung-Hsing Hsu, Dylan Tweed, Juerg Diemand, Paul M. Ricker, Marcel Zemp, Mark C. Neyrinck, Gustavo Yepes, Patricia Fasel, Doug Potter, Michal Maciejewski, Greg Stinson, Steffen R. Knollmann, Volker Springel, Miguel A. Aragon-Calvo, Alexander Knebe, Susana Planelles, Francesca Iannuzzi, Yago Ascasibar, Stuart I. Muldrew, Zarija Lukić, Vicent Quilis, Jeffrey P. Gardner, Klaus Dolag, Justin I. Read, Cameron K. McBride, Stephane Colombi, and Bridget Falck
Subjects: Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Dark matter halo, Circular motion, Space and Planetary Science, Position (vector), Phase space, 0103 physical sciences, Substructure, Configuration space, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy rotation curve
Abstract: [abridged] We present a detailed comparison of fundamental dark matter halo properties retrieved by a substantial number of different halo finders. These codes span a wide range of techniques including friends-of-friends (FOF), spherical-overdensity (SO) and phase-space based algorithms. We further introduce a robust (and publicly available) suite of test scenarios that allows halo finder developers to compare the performance of their codes against those presented here. This set includes mock haloes containing various levels and distributions of substructure at a range of resolutions as well as a cosmological simulation of the large-scale structure of the universe. All the halo finding codes tested could successfully recover the spatial location of our mock haloes. They further returned lists of particles (potentially) belonging to the object that led to coinciding values for the maximum of the circular velocity profile and the radius where it is reached. All the finders based in configuration space struggled to recover substructure that was located close to the centre of the host halo and the radial dependence of the mass recovered varies from finder to finder. Those finders based in phase space could resolve central substructure although they found difficulties in accurately recovering its properties. Via a resolution study we found that most of the finders could not reliably recover substructure containing fewer than 30-40 particles. However, also here the phase space finders excelled by resolving substructure down to 10-20 particles. By comparing the halo finders using a high resolution cosmological volume we found that they agree remarkably well on fundamental properties of astrophysical significance (e.g. mass, position, velocity, and peak of the rotation curve).
Published: 2011
Full Text: View/download PDF

20. THE BARYONIC ACOUSTIC FEATURE AND LARGE-SCALE CLUSTERING IN THE SLOAN DIGITAL SKY SURVEY LUMINOUS RED GALAXY SAMPLE

Author: Alexander S. Szalay, Andreas A. Berlind, Michael R. Blanton, Paul C. Czarapata, Roman Scoccimarro, Neta A. Bahcall, Cameron K. McBride, Donald P. Schneider, Stephan M. Kent, Jon Brinkmann, Joshua A. Frieman, and Eyal A. Kazin
Subjects: Baryon, Physics, Space and Planetary Science, Spectral density, Sigma, Astronomy and Astrophysics, Sample variance, Astrophysics, Correlation function (astronomy), Galaxy, Redshift, Cosmology
Abstract: We examine the correlation function \xi of the Sloan Digital Sky Survey (SDSS) Luminous Red Galaxy sample (LRG) at large scales (60
Published: 2010
Full Text: View/download PDF

21. 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
Full Text: View/download PDF

22. A Cosmic Void Catalog of SDSS DR12 BOSS Galaxies

Author: Cameron K. McBride, Andreas A. Berlind, Mark C. Neyrinck, Kaike Pan, Roman Scoccimarro, Dmitry Bizyaev, Robert J. Scherrer, Qingqing Mao, Viktor Malanushenko, Elena Malanushenko, Jeremy L. Tinker, and Donald P. Schneider
Subjects: Physics, Void (astronomy), COSMIC cancer database, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, 010308 nuclear & particles physics, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Redshift, Baryon, Boss, Space and Planetary Science, Sky, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a cosmic void catalog using the large-scale structure galaxy catalog from the Baryon Oscillation Spectroscopic Survey (BOSS). This galaxy catalog is part of the Sloan Digital Sky Survey (SDSS) Data Release 12 and is the final catalog of SDSS-III. We take into account the survey boundaries, masks, and angular and radial selection functions, and apply the ZOBOV void finding algorithm to the galaxy catalog. We identify a total of 10,643 voids. After making quality cuts to ensure that the voids represent real underdense regions, we obtain 1,228 voids with effective radii spanning the range 20-100Mpc/h and with central densities that are, on average, 30% of the mean sample density. We release versions of the catalogs both with and without quality cuts. We discuss the basic statistics of voids, such as their size and redshift distributions, and measure the radial density profile of the voids via a stacking technique. In addition, we construct mock void catalogs from 1000 mock galaxy catalogs, and find that the properties of BOSS voids are in good agreement with those in the mock catalogs. We compare the stellar mass distribution of galaxies living inside and outside of the voids, and find no significant difference. These BOSS and mock void catalogs are useful for a number of cosmological and galaxy environment studies., Comment: 7 pages, 7 figures, submitted to the ApJ
Published: 2016
Full Text: View/download PDF

23. Building a better understanding of the massive high-redshift BOSS CMASS galaxies as tools for cosmology

Author: Francisco Prada, Chia-Hsun Chuang, Ginevra Favole, Molly E. C. Swanson, Cameron K. McBride, Donald P. Schneider, Daniel J. Eisenstein, Ministerio de Educación y Ciencia (España), Ministerio de Ciencia e Innovación (España), Department of Energy (US), Ministerio de Economía y Competitividad (España), Alfred P. Sloan Foundation, and National Science Foundation (US)
Subjects: Galaxies: statistics, haloes [Galaxies], Large-scale structure of Universe, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxies: distances and redshifts, statistics [Galaxies], Hospitality, theory [Cosmology], 0103 physical sciences, distances and redshifts [Galaxies], Astrophysics::Solar and Stellar Astrophysics, Galaxies: haloes, observations [Cosmology], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, business.industry, Cosmology: observations, Astronomy, Astronomy and Astrophysics, Boss, Space and Planetary Science, Cosmology: theory, business
Abstract: We explore the massive bluer star-forming population of the Sloan Digital Sky Survey (SDSS) III/BOSS CMASS DR11 galaxies at z > 0.55 to quantify their differences, in terms of redshiftspace distortions and large-scale bias, with respect to the luminous red galaxy sample. We perform a qualitative analysis to understand the significance of these differences and whether we can model and reproduce them in mock catalogues. Specifically, we measure galaxy clustering in CMASS on small and intermediate scales (0.1 ≲ r ≲ 50 h Mpc) by computing the two-point correlation function - both projected and redshift-space - of these galaxies, and a new statistic, Σ(π), able to separate the coherent and dispersed redshift-space distortion contributions and the large-scale bias. We interpret our clustering measurements by adopting a Halo Occupation Distribution (HOD) scheme that maps them on to high-resolution N-body cosmological simulations to produce suitable mock galaxy catalogues. The traditional HOD prescription can be applied to the red and the blue samples, independently, but this approach is unphysical since it allows the same mock galaxies to be either red or blue. To overcome this ambiguity, we modify the standard formulation and infer the red and the blue models by splitting the full mock catalogue into two complementary and non-overlapping submocks. This separation is performed by constraining the HOD with the observed CMASS red and blue galaxy fractions and produces reliable and accurate models. © 2016 The Authors., GF is supported by the Ministerio de Educacion y Ciencia of the Spanish Government through FPI grant AYA2010-2131-C02-01 and wishes to thank the Smithsonian Center for Astrophysics and the Harvard University, Astronomy Department, for the hospitality during the creation of this work. GF acknowledges support from the Spanish Government through EEBB-I-13-07167 and EEBB-I-12-05220 grants. GF, FP, and CC acknowledge support from the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, MINECO Centro de Excelencia Severo Ochoa Programme under grant SEV-2012-0249, and MINECO grant AYA2014-60641-C2-1-P. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the U.S. Department of Energy.
Published: 2016

24. Clustering properties of g-selected galaxies at z ~ 0.8

Author: Eric Jullo, Francisco Prada, Anna Niemiec, Anatoly Klypin, Sebastín E. Nuza, Ginevra Favole, Sergio Rodríguez-Torres, Timothée Delubac, Chia-Hsun Chuang, Christophe Yèche, Johan Comparat, Jean-Paul Kneib, Ramin A. Skibba, Daniel J. Eisenstein, Gustavo Yepes, David J. Schlegel, Cameron K. McBride, Donald P. Schneider, German Research Foundation, Centre National de la Recherche Scientifique (France), Ministerio de Economía y Competitividad (España), Ministerio de Educación y Ciencia (España), and Ministerio de Ciencia e Innovación (España)
Subjects: haloes [Galaxies], Galaxies: statistics, Ciencias Físicas, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), 01 natural sciences, Halo occupation distribution, Cosmology: observations - cosmology, purl.org/becyt/ford/1 [https], statistics [Galaxies], Galaxies: distances and redshifts, 0103 physical sciences, distances and redshifts [Galaxies], Galaxies: haloes, 010303 astronomy & astrophysics, observations - cosmology [Cosmology], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Mass ratio, Galaxy, Redshift, Astronomía, Stars, Theory - large-scale structure of Universe, 13. Climate action, Space and Planetary Science, Dark energy, Halo, CIENCIAS NATURALES Y EXACTAS
Abstract: Current and future large redshift surveys, as the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey (SDSS-IV/eBOSS) or the Dark Energy Spectroscopic Instrument (DESI), will use emission-line galaxies (ELGs) to probe cosmological models by mapping the large-scale structure of the Universe in the redshift range 0.6 < z < 1.7. With current data, we explore the halo-galaxy connection by measuring three clustering properties of g-selected ELGs as matter tracers in the redshift range 0.6 < z < 1: (i) the redshift-space two-point correlation function using spectroscopic redshifts from the BOSS ELG sample and VIPERS; (ii) the angular two-point correlation function on the footprint of the CFHT-LS; (iii) the galaxy-galaxy lensing signal around the ELGs using the CFHTLenS. We interpret these observations by mapping them on to the latest high-resolution MultiDark Planck N-body simulation, using a novel (Sub)Halo-Abundance Matching technique that accounts for the ELG incompleteness. ELGs at z ~ 0.8 live in haloes of (1 ± 0.5) × 10 hM⊙ and 22.5 ± 2.5 per cent of them are satellites belonging to a larger halo. The halo occupation distribution of ELGs indicates that we are sampling the galaxies in which stars form in the most efficient way, according to their stellar-to-halo mass ratio. © 2016 The Authors., GF is supported by the Ministerio de Educacion y Ciencia of the Spanish Government through FPI grant AYA2010-2131-C02-01. JC acknowledges financial support from MINECO (Spain) under project number AYA2012-31101. GY acknowledges financial support from MINECO (Spain) under project number AYA2012-31101 and grant FPA2012-34694. EJ acknowledges the support of CNRS, and the Labex OCEVU. SEN acknowledges support by the Deutsche Forschungsgemeinschaft under the grant NU 332/21. GF, FP, SART, AK, SN and CC acknowledge financial support from the Spanish MICINN Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, MINECO Centro de Excelencia Severo Ochoa Programme under grant SEV-2012-0249, and MINECO grant AYA2014-60641-C2-1-P. GF, JC and FP wish to thank the Lawrence Berkeley National Laboratory for the hospitality during the creation of this work. FP acknowledges the spanish MEC 'Salvador de Madariaga' program, Ref. PRX14/00444.
Published: 2016

25. SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: Galaxy target selection and large-scale structure catalogues

Author: Michael A. Strauss, Sergio Rodríguez-Torres, Kyle S. Dawson, Daniel Thomas, Shirley Ho, Claudia Maraston, Beth Reid, Daniel Oravetz, Salvador Salazar-Albornoz, Francisco Prada, Chia-Hsun Chuang, Cameron K. McBride, Nikhil Padmanabhan, Ariel G. Sánchez, Will J. Percival, David A. Wake, Mariana Vargas-Magaña, Matthew D. Olmstead, Kaike Pan, Lado Samushia, Daniel J. Eisenstein, Erin S. Sheldon, Dmitry Bizyaev, Florian Beutler, Sebastián E. Nuza, Paul Harding, Donald P. Schneider, Martin White, Adam S. Bolton, Surhud More, Claudia G. Scóccola, Karen L. Masters, Ashley J. Ross, Francisco-Shu Kitaura, Audrey Simmons, Alexie Leauthaud, Rita Tojeiro, Joel R. Brownstein, Jeremy L. Tinker, Janine Pforr, John K. Parejko, David J. Schlegel, McMaster University [Hamilton, Ontario], Institut de cardiologie [CHU Pitié-Salpêtrière], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Pitié-Salpêtrière [AP-HP], Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), California Institute of Technology (CALTECH), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), 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), University of St Andrews. School of Physics and Astronomy, Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-CHU Pitié-Salpêtrière [APHP], 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), CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), 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, and 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)
Subjects: ) LARGE-SCALE STRUCTURE OF UNIVERSE [OBSERVATIONS - (COSMOLOGY], Ciencias Físicas, Astrophysics, 01 natural sciences, Cosmology, purl.org/becyt/ford/1 [https], QB Astronomy, observations [Cosmology], 010303 astronomy & astrophysics, QC, QB, media_common, Physics, ) large-scale structure of Universe [(Cosmology], Astrophysics::Instrumentation and Methods for Astrophysics, astro-ph.CO, large-scale structure of Universe, Astronomical and Space Sciences, CIENCIAS NATURALES Y EXACTAS, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, media_common.quotation_subject, FOS: Physical sciences, Sample (statistics), Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Observations - (cosmology:) large-scale structure of Universe, 0103 physical sciences, Ciencias Agrarias, Cluster analysis, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy, DAS, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Astronomía, Baryon, QC Physics, Boss, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), COSMOLOGY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Baryon Oscillation Spectroscopic Survey (BOSS), part of the Sloan Digital Sky Survey (SDSS) III project, has provided the largest survey of galaxy redshifts available to date, in terms of both the number of galaxy redshifts measured by a single survey, and the effective cosmological volume covered. Key to analysing the clustering of these data to provide cosmological measurements is understanding the detailed properties of this sample. Potential issues include variations in the target catalogue caused by changes either in the targeting algorithm or properties of the data used, the pattern of spectroscopic observations, the spatial distribution of targets for which redshifts were not obtained, and variations in the target sky density due to observational systematics. We document here the target selection algorithms used to create the galaxy samples that comprise BOSS. We also present the algorithms used to create large scale structure catalogues for the final Data Release (DR12) samples and the associated random catalogues that quantify the survey mask. The algorithms are an evolution of those used by the BOSS team to construct catalogues from earlier data, and have been designed to accurately quantify the galaxy sample. The code used, designated MKSAMPLE, is released with this paper., 21 pages, 12 figures, version accepted for publication in MNRAS
Published: 2016
Full Text: View/download PDF

26. The SDSS-IV extended Baryon Oscillation Spectroscopic Survey:quasar target selection

Author: Jeffrey A. Newman, Eran O. Ofek, Jeremy L. Tinker, Jo Bovy, Ian D. McGreer, Cameron K. McBride, Peter Nugent, Abhishek Prakash, Mansi M. Kasliwal, Donald P. Schneider, Alina Streblyanska, Dustin Lang, Adam A. Miller, Russ R. Laher, Jean-Paul Kneib, David Levitan, Zheng Cai, Pierre Laurent, Will J. Percival, Kyle S. Dawson, Branimir Sesar, Jason Surace, Graziano Rossi, Hee-Jong Seo, Joel R. Brownstein, Nathalie Palanque-Delabrouille, Isabelle Pâris, eBOSS, Johan Comparat, David J. Schlegel, Ashley J. Ross, Etienne Burtin, Patrick Petitjean, Shrinivas R. Kulkarni, Eric Armengaud, John J. Ruan, Adam D. Myers, Christophe Yèche, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Universidad de Chile = University of Chile [Santiago] (UCHILE), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Ecole Polytechnique Fédérale de Lausanne (EPFL), Département de Physique des Particules (ex SPP) (DPP), 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, AVL List GmbH, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), UAM. Departamento de Física Teórica, 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) (DPhP), and Universidad Autónoma de Madrid (UAM)
Subjects: Astrophysics, Physical Chemistry, 01 natural sciences, Atomic, Spectral line, Particle and Plasma Physics, 010303 astronomy & astrophysics, media_common, Physics, Oscillation, Astrophysics::Instrumentation and Methods for Astrophysics, observations [cosmology], astro-ph.CO, photometry [galaxies], galaxies: distances and redshifts, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Physical Chemistry (incl. Structural), Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, quasars: general, 0103 physical sciences, data analysis [methods], Nuclear, Selection (genetic algorithm), Astrophysics::Galaxy Astrophysics, STFC, general [quasars], 010308 nuclear & particles physics, Física, Molecular, RCUK, Astronomy and Astrophysics, Quasar, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Baryon, galaxies: photometry, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, distances and redshifts [galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract: The Astrophysical Journal 221.2 (2015): 27 reproduced by permission of the AAS, As part of the Sloan Digital Sky Survey (SDSS) IV the extended Baryon Oscillation Spectroscopic Survey (eBOSS) will improve measurements of the cosmological distance scale by applying the Baryon Acoustic Oscillation (BAO) method to quasar samples. eBOSS will adopt two approaches to target quasars over 7500 deg2. First, a "CORE" quasar sample will combine the optical selection in ugriz using a likelihood-based routine called XDQSOz, with a mid-IR-optical color cut. eBOSS CORE selection (to g < 22 or r < 22) should return ∼70 deg-2 quasars at redshifts 0.9 < z < 2.2 and ∼7 deg-2z > 2.1 quasars. Second, a selection based on variability in multi-epoch imaging from the Palomar Transient Factory should recover an additional ∼3-4 deg-2z > 2.1 quasars to g < 22.5. A linear model of how imaging systematics affect target density recovers the angular distribution of eBOSS CORE quasars over 96.7% (76.7%) of the SDSS north (south) Galactic Cap area. The eBOSS CORE quasar sample should thus be sufficiently dense and homogeneous over 0.9 < z < 2.2 to yield the first few-percent-level BAO constraint near eBOSS quasars at z > 2.1 will be used to improve BAO measurements in the Lyα Forest. Beyond its key cosmological goals, eBOSS should be the next-generation quasar survey, comprising >500,000 new quasars and >500,000 uniformly selected spectroscopically confirmed 0.9 < z < 2.2 quasars. At the conclusion of eBOSS, the SDSS will have provided unique spectra for more than 800,000 quasars, We are grateful for insightful discussions about quasar selection statistics with Joe Hennawi, David Hogg, and Gordon Richards. A.D.M. acknowledges a generous research fellowship from the Alexander von Humboldt Foundation at the MaxPlanck-Institut für Astronomie and was supported in part by NASA-ADAP awards NNX12AI49G and NNX12AE38G and by NSF awards 1211112 and 1515404. J.P.K. acknowledges support from the ERC advanced grant LIDA. This paper includes targets derived from the images of the Wide-Field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the JetPropulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This paper represents an effort by both the SDSS-III and SDSS-IV collaborations. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for HighPerformance Computing at the University of Utah. The SDSS web site is www.sdss.org.
Published: 2015
Full Text: View/download PDF

27. Tests of redshift-space distortions models in configuration space for the analysis of the BOSS final data release

Author: Francisco Prada, Chia-Hsun Chuang, Beth Reid, Jeremy L. Tinker, Martin White, Lado Samushia, and Cameron K. McBride
Subjects: statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Galaxies: statistics, Large-scale structure of Universe, Cosmological parameters, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Redshift-space distortions, Gravitation, Galaxies: haloes, cosmological parameters, Tinker, Astrophysics::Galaxy Astrophysics, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Física, Astronomy, Astronomy and Astrophysics, haloes [galaxies], Boss, Space and Planetary Science, gravitation, astro-ph.CO, Configuration space, large-scale structure of Universe, Data release, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved, Observations of redshift-space distortions in spectroscopic galaxy surveys offer an attractive method for observing the build-up of cosmological structure, which depends both on the expansion rate of the Universe and our theory of gravity. In preparation for analysis of redshiftspace distortions from the Baryon Oscillation Spectroscopic Survey (BOSS) final data release, we compare a number of analytic and phenomenological models, specified in configuration space, to mock catalogues derived in different ways from several N-body simulations. The galaxies in each mock catalogue have properties similar to those of the higher redshift galaxies measured by BOSS but differ in the details of how small-scale velocities and halo occupancy are determined. We find that all of the analytic models fit the simulations over a limited range of scales while failing at small scales.We discuss which models are most robust and on which scales they return reliable estimates of the rate of growth of structure: we find that models based on some form of resummation can fit our N_body data for BOSS-like galaxies above 30 h-1 Mpc well enough to return unbiased parameter estimates, The MultiDark Database used in this paper and the web application providing online access to it were constructed as part of the activities of the German Astrophysical Virtua lObservatory as result of a collaboration between the Leibniz-Institute forAstrophysics Potsdam (AIP) and the Spanish MultiDark Consolider Project CSD2009-00064
Published: 2015
Full Text: View/download PDF

28. Signatures of the Primordial Universe from Its Emptiness: Measurement of Baryon Acoustic Oscillations from Minima of the Density Field

Author: Will J. Percival, Ashley J. Ross, Gong-Bo Zhao, Yu Liang, Héctor Gil-Marín, Mariana Vargas-Magaña, Chia-Hsun Chuang, Cheng Zhao, Cameron K. McBride, Charling Tao, Jean-Paul Kneib, Rita Tojeiro, Jeremy L. Tinker, Francisco-Shu Kitaura, Daniel J. Eisenstein, Ariel G. Sánchez, Sergio Rodríguez-Torres, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, Leibniz-Institut für Astrophysik Potsdam (AIP), Tsinghua University [Beijing] (THU), 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), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad Autónoma de Madrid (UAM), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Institut Lagrange de Paris, 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'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), Ecole Polytechnique Fédérale de Lausanne (EPFL), University of Portsmouth, Center for Cosmology & AstroParticle Physics, Ohio State University [Columbus] (OSU), Max-Planck-Institut für Extraterrestrische Physik (MPE), New York University [New York] (NYU), NYU System (NYU), University of St Andrews [Scotland], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Chinese Academy of Sciences [Beijing] (CAS), ANR-11-IDEX-0004,SUPER,Sorbonne Universités à Paris pour l'Enseignement et la Recherche(2011), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad Autonoma de Madrid (UAM), Harvard University [Cambridge]-Smithsonian Institution, Sorbonne Université (SU), 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), Universidad Nacional Autónoma de México (UNAM), and UAM. Departamento de Física Teórica
Subjects: Void (astronomy), Cosmology and Gravitation, Density fields, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Observational data, Primordial fluctuations, media_common.quotation_subject, General Physics and Astronomy, FOS: Physical sciences, Disjoint sets, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Acoustic oscillation, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010303 astronomy & astrophysics, STFC, QC, Astrophysics::Galaxy Astrophysics, media_common, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Delaunay triangulation, Astronomy, RCUK, Física, Large scale structures, 3rd-DAS, Galaxy, Universe, QC Physics, astro-ph.CO, Halo, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Sound waves from the primordial fluctuations of the Universe imprinted in the large-scale structure, called baryon acoustic oscillations (BAOs), can be used as standard rulers to measure the scale of the Universe. These oscillations have already been detected in the distribution of galaxies. Here we propose to measure BAOs from the troughs (minima) of the density field. Based on two sets of accurate mock halo catalogues with and without BAOs in the seed initial conditions, we demonstrate that the BAO signal cannot be obtained from the clustering of classical disjoint voids, but it is clearly detected from overlapping voids. The latter represent an estimate of all troughs of the density field. We compute them from the empty circumsphere centers constrained by tetrahedra of galaxies using Delaunay triangulation. Our theoretical models based on an unprecedented large set of detailed simulated void catalogues are remarkably well confirmed by observational data. We use the largest recently publicly available sample of luminous red galaxies from SDSS-III BOSS DR11 to unveil for the first time a > 3σ BAO detection from voids in observations. Since voids are nearly isotropically expanding regions, their centers represent the most quiet places in the Universe, keeping in mind the cosmos origin and providing a new promising window in the analysis of the cosmological large-scale structure from galaxy surveys, Y. L., C. T., and C. Z. acknowledge support from Tsinghua University through a 985 grant, 973 programme 2013CB834906, NSFC Grants No. 11033003 and No. 11173017, Sino French CNRS-CAS International Laboratories LIA Origins, and FCPPL. R. T. thanks the STFC for support. H. G. M. thanks the Labex ILP (Reference No. ANR-10-LABX-63), part of the Idex SUPER, for support, receiving financial state aid managed by the Agence Nationale de la Recherche, as part of the programme Investissements d’avenir under Reference No. ANR-11-IDEX-0004-02. G. Z. is supported by the Strategic Priority Research Program of the Chinese Academy of Sciences Grant No. XDB09000000. The authors are also thankful for the access to computing facilities at Barcelona (MareNostrum), LRZ (Supermuc), AIP (erebos), CCIN2P3 (Quentin Le Boulc’h), and Tsinghua University. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/ Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University
Published: 2015
Full Text: View/download PDF

29. The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III

Author: Shadab Alam, Franco D. Albareti, Carlos Allende Prieto, F. Anders, Scott F. Anderson, Timothy Anderton, Brett H. Andrews, Eric Armengaud, Éric Aubourg, Stephen Bailey, Sarbani Basu, Julian E. Bautista, Rachael L. Beaton, Timothy C. Beers, Chad F. Bender, Andreas A. Berlind, Florian Beutler, Vaishali Bhardwaj, Jonathan C. Bird, Dmitry Bizyaev, Cullen H. Blake, Michael R. Blanton, Michael Blomqvist, John J. Bochanski, Adam S. Bolton, Jo Bovy, A. Shelden Bradley, W. N. Brandt, D. E. Brauer, J. Brinkmann, Peter J. Brown, Joel R. Brownstein, Angela Burden, Etienne Burtin, Nicolás G. Busca, Zheng Cai, Diego Capozzi, Aurelio Carnero Rosell, Michael A. Carr, Ricardo Carrera, K. C. Chambers, William James Chaplin, Yen-Chi Chen, Cristina Chiappini, S. Drew Chojnowski, Chia-Hsun Chuang, Nicolas Clerc, Johan Comparat, Kevin Covey, Rupert A. C. Croft, Antonio J. Cuesta, Katia Cunha, Luiz N. da Costa, Nicola Da Rio, James R. A. Davenport, Kyle S. Dawson, Nathan De Lee, Timothée Delubac, Rohit Deshpande, Saurav Dhital, Letícia Dutra-Ferreira, Tom Dwelly, Anne Ealet, Garrett L. Ebelke, Edward M. Edmondson, Daniel J. Eisenstein, Tristan Ellsworth, Yvonne Elsworth, Courtney R. Epstein, Michael Eracleous, Stephanie Escoffier, Massimiliano Esposito, Michael L. Evans, Xiaohui Fan, Emma Fernández-Alvar, Diane Feuillet, Nurten Filiz Ak, Hayley Finley, Alexis Finoguenov, Kevin Flaherty, Scott W. Fleming, Andreu Font-Ribera, Jonathan Foster, Peter M. Frinchaboy, J. G. Galbraith-Frew, Rafael A. García, D. A. García-Hernández, Ana E. García Pérez, Patrick Gaulme, Jian Ge, R. Génova-Santos, A. Georgakakis, Luan Ghezzi, Bruce A. Gillespie, Léo Girardi, Daniel Goddard, Satya Gontcho A Gontcho, Jonay I. González Hernández, Eva K. Grebel, Paul J. Green, Jan Niklas Grieb, Nolan Grieves, James E. Gunn, Hong Guo, Paul Harding, Sten Hasselquist, Suzanne L. Hawley, Michael Hayden, Fred R. Hearty, Saskia Hekker, Shirley Ho, David W. Hogg, Kelly Holley-Bockelmann, Jon A. Holtzman, Klaus Honscheid, Daniel Huber, Joseph Huehnerhoff, Inese I. Ivans, Linhua Jiang, Jennifer A. Johnson, Karen Kinemuchi, David Kirkby, Francisco Kitaura, Mark A. Klaene, Gillian R. Knapp, Jean-Paul Kneib, Xavier P. Koenig, Charles R. Lam, Ting-Wen Lan, Dustin Lang, Pierre Laurent, Jean-Marc Le Goff, Alexie Leauthaud, Khee-Gan Lee, Young Sun Lee, Timothy C. Licquia, Jian Liu, Daniel C. Long, Martín López-Corredoira, Diego Lorenzo-Oliveira, Sara Lucatello, Britt Lundgren, Robert H. Lupton, Claude E. Mack III, Suvrath Mahadevan, Marcio A. G. Maia, Steven R. Majewski, Elena Malanushenko, Viktor Malanushenko, A. Manchado, Marc Manera, Qingqing Mao, Claudia Maraston, Robert C. Marchwinski, Daniel Margala, Sarah L. Martell, Marie Martig, Karen L. Masters, Savita Mathur, Cameron K. McBride, Peregrine M. McGehee, Ian D. McGreer, Richard G. McMahon, Brice Ménard, Marie-Luise Menzel, Andrea Merloni, Szabolcs Mészáros, Adam A. Miller, Jordi Miralda-Escudé, Hironao Miyatake, Antonio D. Montero-Dorta, Surhud More, Eric Morganson, Xan Morice-Atkinson, Heather L. Morrison, Benôit Mosser, Demitri Muna, Adam D. Myers, Kirpal Nandra, Jeffrey A. Newman, Mark Neyrinck, Duy Cuong Nguyen, Robert C. Nichol, David L. Nidever, Pasquier Noterdaeme, Sebastián E. Nuza, Julia E. O’Connell, Robert W. O’Connell, Ross O’Connell, Ricardo L. C. Ogando, Matthew D. Olmstead, Audrey E. Oravetz, Daniel J. Oravetz, Keisuke Osumi, Russell Owen, Deborah L. Padgett, Nikhil Padmanabhan, Martin Paegert, Nathalie Palanque-Delabrouille, Kaike Pan, John K. Parejko, Isabelle Pâris, Changbom Park, Petchara Pattarakijwanich, M. Pellejero-Ibanez, Joshua Pepper, Will J. Percival, Ismael Pérez-Fournon, Ignasi Pe´rez-Ra`fols, Patrick Petitjean, Matthew M. Pieri, Marc H. Pinsonneault, Gustavo F. Porto de Mello, Francisco Prada, Abhishek Prakash, Adrian M. Price-Whelan, Pavlos Protopapas, M. Jordan Raddick, Mubdi Rahman, Beth A. Reid, James Rich, Hans-Walter Rix, Annie C. Robin, Constance M. Rockosi, Thaíse S. Rodrigues, Sergio Rodríguez-Torres, Natalie A. Roe, Ashley J. Ross, Nicholas P. Ross, Graziano Rossi, John J. Ruan, J. A. Rubiño-Martín, Eli S. Rykoff, Salvador Salazar-Albornoz, Mara Salvato, Lado Samushia, Ariel G. Sánchez, Basílio Santiago, Conor Sayres, Ricardo P. Schiavon, David J. Schlegel, Sarah J. Schmidt, Donald P. Schneider, Mathias Schultheis, Axel D. Schwope, C. G. Scóccola, Caroline Scott, Kris Sellgren, Hee-Jong Seo, Aldo Serenelli, Neville Shane, Yue Shen, Matthew Shetrone, Yiping Shu, V. Silva Aguirre, Thirupathi Sivarani, M. F. Skrutskie, Anže Slosar, Verne V. Smith, Flávia Sobreira, Diogo Souto, Keivan G. Stassun, Matthias Steinmetz, Dennis Stello, Michael A. Strauss, Alina Streblyanska, Nao Suzuki, Molly E. C. Swanson, Jonathan C. Tan, Jamie Tayar, Ryan C. Terrien, Aniruddha R. Thakar, Daniel Thomas, Neil Thomas, Benjamin A. Thompson, Jeremy L. Tinker, Rita Tojeiro, Nicholas W. Troup, Mariana Vargas-Magaña, Jose A. Vazquez, Licia Verde, Matteo Viel, Nicole P. Vogt, David A. Wake, Ji Wang, Benjamin A. Weaver, David H. Weinberg, Benjamin J. Weiner, Martin White, John C. Wilson, John P. Wisniewski, W. M. Wood-Vasey, Christophe Ye`che, Donald G. York, Nadia L. Zakamska, O. Zamora, Gail Zasowski, Idit Zehavi, Gong-Bo Zhao, Zheng Zheng, Xu Zhou (周旭), Zhimin Zhou (周志民), Hu Zou (邹虎), Guangtun Zhu, UAM. Departamento de Física Teórica, University of St Andrews. School of Physics and Astronomy, 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), SDSS Collaboration, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), ITA, USA, GBR, FRA, DEU, ESP, CHN, and Department of Physics
Subjects: 10TH DATA RELEASE, OSCILLATION SPECTROSCOPIC SURVEY, purl.org/becyt/ford/1 [https], SOLAR-LIKE STARS, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, ComputingMilieux_MISCELLANEOUS, QC, QB, media_common, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Celestial sphere, Composicao estelar, Exoplanet, Radial velocity, atlases, Astrophysics - Solar and Stellar Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, MAIN-SEQUENCE STARS, FIXED-DELAY INTERFEROMETRY, Cosmology and Gravitation, astro-ph.SR, GALACTIC EVOLUTION EXPERIMENT, astro-ph.GA, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, catalogs, surveys, Movimento estelar, Settore FIS/05 - Astronomia e Astrofisica, BROWN DWARF CANDIDATE, LOW-MASS STELLAR, ST/J500665/1, Galáxias, Instrumentation and Methods for Astrophysics (astro-ph.IM), Quasars, Spectrograph, STFC, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], RCUK, Astronomy, Física, DAS, Astronomy and Astrophysics, Quasar, purl.org/becyt/ford/1.3 [https], 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Espectros estelares, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 1ST DATA RELEASE, Stars, QC Physics, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Catalogos astronomicos, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BARYON ACOUSTIC-OSCILLATIONS, astro-ph.IM
Abstract: The third generation of the Sloan Digital Sky Survey (SDSS-III) took data from 2008 to 2014 using the original SDSS wide-field imager, the original and an upgraded multi-object fiber-fed optical spectrograph, a new near-infrared high-resolution spectrograph, and a novel optical interferometer. All the data from SDSS-III are now made public. In particular, this paper describes Data Release 11 (DR11) including all data acquired through 2013 July, and Data Release 12 (DR12) adding data acquired through 2014 July (including all data included in previous data releases), marking the end of SDSS-III observing. Relative to our previous public release (DR10), DR12 adds one million new spectra of galaxies and quasars from the Baryon Oscillation Spectroscopic Survey (BOSS) over an additional 3000 sq. deg of sky, more than triples the number of H-band spectra of stars as part of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE), and includes repeated accurate radial velocity measurements of 5500 stars from the Multi-Object APO Radial Velocity Exoplanet Large-area Survey (MARVELS). The APOGEE outputs now include measured abundances of 15 different elements for each star. In total, SDSS-III added 2350 sq. deg of ugriz imaging; 155,520 spectra of 138,099 stars as part of the Sloan Exploration of Galactic Understanding and Evolution 2 (SEGUE-2) survey; 2,497,484 BOSS spectra of 1,372,737 galaxies, 294,512 quasars, and 247,216 stars over 9376 sq. deg; 618,080 APOGEE spectra of 156,593 stars; and 197,040 MARVELS spectra of 5,513 stars. Since its first light in 1998, SDSS has imaged over 1/3 of the Celestial sphere in five bands and obtained over five million astronomical spectra., Comment: DR12 data are available at http://www.sdss3.org/dr12. 30 pages. 11 figures. Accepted to ApJS
Published: 2015
Full Text: View/download PDF

30. Synthetic galaxy images and spectra from the Illustris simulation

Author: Mariska Kriek, Lars Hernquist, Gregory F. Snyder, Cameron K. McBride, Laura V. Sales, Annalisa Pillepich, Shy Genel, Dylan Nelson, Mark Vogelsberger, Christopher C. Hayward, Volker Springel, Debora Sijacki, Paul Torrey, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Torrey, Paul, and Vogelsberger, Mark
Subjects: Physics, Stellar mass, Stellar population, 010308 nuclear & particles physics, Star formation, Metallicity, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Type-cD galaxy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Interacting galaxy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present our methods for generating a catalog of 7,000 synthetic images and 40,000 integrated spectra of redshift z = 0 galaxies from the Illustris Simulation. The mock data products are produced by using stellar population synthesis models to assign spectral energy distributions (SED) to each star particle in the galaxies. The resulting synthetic images and integrated SEDs therefore properly reflect the spatial distribution, stellar metallicity distribution, and star formation history of the galaxies. From the synthetic data products it is possible to produce monochromatic or color-composite images, perform SED fitting, classify morphology, determine galaxy structural properties, and evaluate the impacts of galaxy viewing angle. The main contribution of this paper is to describe the production, format, and composition of the image catalog that makes up the Illustris Simulation Obsevatory. As a demonstration of this resource, we derive galactic stellar mass estimates by applying the SED fitting code FAST to the synthetic galaxy products, and compare the derived stellar masses against the true stellar masses from the simulation. We find from this idealized experiment that systematic biases exist in the photometrically derived stellar mass values that can be reduced by using a fixed metallicity in conjunction with a minimum galaxy age restriction., Comment: 21 pages, 17 figures, submitted to MNRAS. Comments welcome
Published: 2015

31. The Formation and Evolution of Intracluster Light

Author: Craig S. Rudick, Cameron K. McBride, and J. Christopher Mihos
Subjects: Physics, Brightness, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Statistics::Computation, Luminosity, High surface, Space and Planetary Science, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Envelope (waves)
Abstract: Using N-body simulations, we have modeled the production and evolution of diffuse, low surface brightness intracluster light (ICL) in three simulated galaxy clusters. Using an observational definition of ICL to be luminosity at a surface brightness mu_V>26.5 mag/sq.arcsec, we have found that the fraction of cluster luminosity contained in ICL generally increases as clusters evolve, although there are large deviations from this trend over short timescales, including sustained periods of decreasing ICL luminosity. Most ICL luminosity increases come in short, discrete events which are highly correlated with group accretion events within the cluster. In evolved clusters we find that ~10-15% of the clusters' luminosity is at ICL surface brightness. The morphological structure of the ICL changes with time, evolving from a complex of filaments and small-scale, relatively high surface brightness features early in a cluster's history, to a more diffuse and amorphous cluster-scale ICL envelope at later times. Finally, we also see a correlation between the evolution of ICL at different surface brightnesses, including a time delay between the evolution of faint and extremely faint surface brightness features which is traced to the differing dynamical timescales in the group and cluster environment., 12 pages, 10 figures, 6 figures in color; Accepted for publication in ApJ. A full version including figures can be found at http://astroweb.cwru.edu/craig/diffuse_light/papers/icl_sim.pdf
Published: 2006
Full Text: View/download PDF

32. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Modeling the clustering and halo occupation distribution of BOSS-CMASS galaxies in the Final Data Release

Author: Yiping Shu, Claudia Maraston, Cameron K. McBride, David J. Schlegel, ChangHoon Hahn, Ginevra Favole, Jeremy L. Tinker, Antonio D. Montero-Dorta, Joel R. Brownstein, Daniel Thomas, Anatoly Klypin, Hong Guo, Adam S. Bolton, Francisco Prada, Francisco-Shu Kitaura, Roman Scoccimarro, Gustavo Yepes, Stefan Gottlöber, Chia-Hsun Chuang, Johan Comparat, Donald P. Schneider, Lado Samushia, Peter Behroozi, and Sergio Rodríguez-Torres
Subjects: Cosmology and Gravitation, Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), 01 natural sciences, Halo occupation distribution, 0103 physical sciences, abundances [galaxies], 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, numerical [methods], Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, haloes [galaxies], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Halo, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a study of the clustering and halo occupation distribution of BOSS CMASS galaxies in the redshift range 0.43 < z < 0.7 drawn from the Final SDSS-III Data Release. We compare the BOSS results with the predictions of a Halo Abundance Matching (HAM) clustering model that assigns galaxies to dark matter halos selected from the large BigMultiDark $N$-body simulation of a flat $\Lambda$CDM Planck cosmology. We compare the observational data with the simulated ones on a light-cone constructed from 20 subsequent outputs of the simulation. Observational effects such as incompleteness, geometry, veto masks and fiber collisions are included in the model, which reproduces within 1-$\sigma$ errors the observed monopole of the 2-point correlation function at all relevant scales: from the smallest scales, 0.5 $h^{-1}$ Mpc, up to scales beyond the Baryonic Acoustic Oscillation feature. This model also agrees remarkably well with the BOSS galaxy power spectrum (up to $k\sim1$ $h$ Mpc$^{-1}$), and the Three-point correlation function. The quadrupole of the correlation function presents some tensions with observations. We discuss possible causes that can explain this disagreement, including target selection effects. Overall, the standard HAM model describes remarkably well the clustering statistics of the CMASS sample. We compare the stellar to halo mass relation for the CMASS sample measured using weak lensing in the CFHT Stripe 82 Survey with the prediction of our clustering model, and find a good agreement within 1-$\sigma$. The BigMD-BOSS light-cone including properties of BOSS galaxies and halo properties is made publicly available., Comment: 16 pages, 16 figures. See companion papers that share the "The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey:" title
Published: 2015
Full Text: View/download PDF

33. The Spatial Distribution of Satellite Galaxies Within Halos: Measuring the Very Small Scale Angular Clustering of SDSS Galaxies

Author: Andreas A. Berlind, Cameron K. McBride, Roman Scoccimarro, and Jennifer Piscionere
Subjects: Luminous infrared galaxy, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dwarf galaxy problem, Dark matter, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Disc galaxy, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Satellite galaxy, Galaxy formation and evolution, Halo, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the angular clustering of galaxies from the Sloan Digital Sky Survey Data Release 7 in order to probe the spatial distribution of satellite galaxies within their dark matter halos. Specifically, we measure the angular correlation function on very small scales (7-320") in a range of luminosity threshold samples (absolute r-band magnitudes of -18 up to -21) that are constructed from the subset of SDSS that has been spectroscopically observed more than once (the so-called plate overlap region). We choose to measure angular clustering in this reduced survey footprint in order to minimize the effects of fiber collision incompleteness, which are otherwise substantial on these small scales. We model our clustering measurements using a fully numerical halo model that populates dark matter halos in N-body simulations to create realistic mock galaxy catalogs. The model has free parameters that specify both the number and spatial distribution of galaxies within their host halos. We adopt a flexible density profile for the spatial distribution of satellite galaxies that is similar to the dark matter Navarro-Frenk-White (NFW) profile, except that the inner slope is allowed to vary. We find that the angular clustering of our most luminous samples (Mr< -20 and -21) suggests that luminous satellite galaxies have substantially steeper inner density profiles than NFW. Lower luminosity samples are less constraining, however, and are consistent with satellite galaxies having shallow density profiles. Our results confirm the findings of Watson et al. 2012 while using different clustering measurements and modeling methodology., 13 pages, 8 figures. Published in the Astrophysical Journal
Published: 2014

34. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: modelling of the luminosity and colour dependence in the Data Release 10

Author: Ashley J. Ross, Andreas A. Berlind, Rita Tojeiro, Cameron K. McBride, Zheng Zheng, Johan Comparat, Daniel J. Eisenstein, Molly E. C. Swanson, Hong Guo, David H. Weinberg, David A. Wake, Ramin A. Skibba, Donald P. Schneider, Idit Zehavi, Neta A. Bahcall, Jeremy L. Tinker, Haojie Xu, Aix Marseille Université (AMU), 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), and University of St Andrews. School of Physics and Astronomy
Subjects: statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy group, 0103 physical sciences, Galaxy formation and evolution, QB Astronomy, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Luminosity function (astronomy), Luminous infrared galaxy, Physics, theory [cosmology], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, observations [cosmology], Galaxy, haloes [galaxies], QC Physics, Space and Planetary Science, Elliptical galaxy, distances and redshifts [galaxies], large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the luminosity and colour dependence of clustering of CMASS galaxies in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey Tenth Data Release. The halo occupation distribution framework is adopted to model the projected two-point correlation function measurements on small and intermediate scales (from $0.02$ to $60\,h^{-1}{\rm {Mpc}}$) and to interpret the observed trends and infer the connection of galaxies to dark matter halos. We find that luminous red galaxies reside in massive halos of mass $M{\sim}10^{13}$--$10^{14}\,h^{-1}{\rm M_\odot}$ and more luminous galaxies are more clustered and hosted by more massive halos. The strong small-scale clustering requires a fraction of these galaxies to be satellites in massive halos, with the fraction at the level of 5--8 per cent and decreasing with luminosity. The characteristic mass of a halo hosting on average one satellite galaxy above a luminosity threshold is about a factor $8.7$ larger than that of a halo hosting a central galaxy above the same threshold. At a fixed luminosity, progressively redder galaxies are more strongly clustered on small scales, which can be explained by having a larger fraction of these galaxies in the form of satellites in massive halos. Our clustering measurements on scales below $0.4\,h^{-1}{\rm {Mpc}}$ allow us to study the small-scale spatial distribution of satellites inside halos. While the clustering of luminosity-threshold samples can be well described by a Navarro-Frenk-White (NFW) profile, that of the reddest galaxies prefers a steeper or more concentrated profile. Finally, we also use galaxy samples of constant number density at different redshifts to study the evolution of luminous galaxies, and find the clustering to be consistent with passive evolution in the redshift range of $0.5 \lesssim z \lesssim 0.6$., Comment: MNRAS Accepted. Minor revisions from the last version
Published: 2014
Full Text: View/download PDF

35. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations in the Data Release 10 and 11 galaxy samples

Author: John K. Parejko, David J. Schlegel, Beth Reid, Matthew D. Olmstead, Natalie A. Roe, Antonio J. Cuesta, Stephanie Escoffier, Claudia Maraston, Vaishali Bhardwaj, Xiaoying Xu, Lauren Anderson, Kyle S. Dawson, Mariana Vargas Magaña, Molly E. C. Swanson, Francisco Prada, Adrian M. Price-Whelan, Marc Manera, Robert C. Nichol, Hee-Jong Seo, David A. Wake, Idit Zehavi, Francesco Montesano, Olga Mena, Gong-Bo Zhao, Will J. Percival, Donald P. Schneider, Chia-Hsun Chuang, Daniel J. Eisenstein, J. Brinkmann, Daniel Thomas, Jeremy L. Tinker, Élric Aubourg, Sebastián E. Nuza, Patrick Petitjean, Adam S. Bolton, Cameron K. McBride, Robert H. Lupton, D. Kirkby, Michael R. Blanton, Angela Burden, Ashley J. Ross, Cristiano G. Sabiu, Shun Saito, Cullan Howlett, James E. Gunn, Martin White, Rita Tojeiro, Hong Guo, Florian Beutler, Stephen Bailey, Ariel G. Sánchez, Joel R. Brownstein, Licia Verde, Shirley Ho, David H. Weinberg, Lado Samushia, Michael A. Strauss, Benjamin A. Weaver, Claudia G. Scóccola, Christophe Yèche, Nicholas P. Ross, Nikhil Padmanabhan, Nathalie Palanque-Delabrouille, Ramin A. Skibba, K. Honscheid, AstroParticule et Cosmologie (APC (UMR_7164)), 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 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), 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), Universitat de Barcelona, and University of St Andrews. School of Physics and Astronomy
Subjects: Astrofísica, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, 01 natural sciences, Observacions astronòmiques, 0103 physical sciences, QB Astronomy, cosmological parameters, dark energy, 010303 astronomy & astrophysics, QC, STFC, Astrophysics::Galaxy Astrophysics, QB, Physics, Cosmologia, 010308 nuclear & particles physics, Angular diameter distance, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, RCUK, Astronomy and Astrophysics, Espectroscòpia de microones, Galaxy, Redshift, observations [cosmology], Cosmology, Baryon, QC Physics, 13. Climate action, Space and Planetary Science, Microwave spectroscopy, Baryon acoustic oscillations, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Astronomical observations
Abstract: We present a one per cent measurement of the cosmic distance scale from the detections of the baryon acoustic oscillations in the clustering of galaxies from the Baryon Oscillation Spectroscopic Survey (BOSS), which is part of the Sloan Digital Sky Survey III (SDSS-III). Our results come from the Data Release 11 (DR11) sample, containing nearly one million galaxies and covering approximately $8\,500$ square degrees and the redshift range $0.2, Comment: 40 pages, 29 figures; replaced with final version in journal
Published: 2014
Full Text: View/download PDF

36. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey:including covariance matrix errors

Author: Francesco Montesano, Mariana Vargas Magaña, Lado Samushia, Robert Crittenden, Beth Reid, Cameron K. McBride, Nikhil Padmanabhan, Chia-Hsun Chuang, Angela Burden, Ariel G. Sánchez, Benjamin A. Weaver, Florian Beutler, Antonio J. Cuesta, Will J. Percival, Donald P. Schneider, Hee-Jong Seo, Daniel J. Eisenstein, Rita Tojeiro, Shirley Ho, Marc Manera, Shun Saito, Ashley J. Ross, Universitat de Barcelona, and University of St Andrews. School of Physics and Astronomy
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), distance scale, Theoretical physics, Observacions astronòmiques, QB Astronomy, Statistical physics, Cluster analysis, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB, Physics, Cosmologia, Oscillation, Covariance matrix, Spectral density, Astronomy and Astrophysics, Covariance, Espectroscòpia de microones, observations [cosmology], Cosmology, Baryon, QC Physics, Boss, Space and Planetary Science, Microwave spectroscopy, large-scale structure of Universe, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astronomical observations
Abstract: We present improved methodology for including covariance matrices in the error budget of Baryon Oscillation Spectroscopic Survey (BOSS) galaxy clustering measurements, revisiting Data Release 9 (DR9) analyses, and describing a method that is used in DR10/11 analyses presented in companion papers. The precise analysis method adopted is becoming increasingly important, due to the precision that BOSS can now reach: even using as many as 600 mock catalogues to estimate covariance of 2-point clustering measurements can still lead to an increase in the errors of ~20%, depending on how the cosmological parameters of interest are measured. In this paper we extend previous work on this contribution to the error budget, deriving formulae for errors measured by integrating over the likelihood, and to the distribution of recovered best-fit parameters fitting the simulations also used to estimate the covariance matrix. Both are situations that previous analyses of BOSS have considered. We apply the formulae derived to Baryon Acoustic Oscillation (BAO) and Redshift-Space Distortion (RSD) measurements from BOSS in our companion papers. To further aid these analyses, we consider the optimum number of bins to use for 2-point measurements using the monopole power spectrum or correlation function for BAO, and the monopole and quadrupole moments of the correlation function for anisotropic-BAO and RSD measurements., Comment: 11 pages, 5 figures, MNRAS submitted
Published: 2014
Full Text: View/download PDF

37. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the full shape of the clustering wedges in the data release 10 and 11 galaxy samples

Author: Shirley Ho, Florian Beutler, Daniel J. Eisenstein, Jeremy L. Tinker, Eyal A. Kazin, Benjamin A. Weaver, Ashley J. Ross, Francesco Montesano, Idit Zehavi, Daniel Thomas, Kyle S. Dawson, Will J. Percival, David A. Wake, Joel R. Brownstein, K. Honscheid, Martin White, Lado Samushia, Donald P. Schneider, Jon Brinkmann, Cameron K. McBride, David J. Schlegel, Ariel G. Sánchez, Éric Aubourg, Antonio J. Cuesta, Ramin A. Skibba, Claudia Maraston, Marc Manera, Rita Tojeiro, AstroParticule et Cosmologie (APC (UMR_7164)), 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), University of Utah, McMaster University [Hamilton, Ontario], Ohio State University [Columbus] (OSU), Institute of cosmology and gravitation, University of Portsmouth, Institut Lagrange de Paris, Sorbonne Université (SU), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Pennsylvania State University (Penn State), Penn State System, Institut de Génétique et Développement de Rennes (IGDR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)-Structure Fédérative de Recherche en Biologie et Santé de Rennes ( Biosit : Biologie - Santé - Innovation Technologique ), New York University [New York] (NYU), NYU System (NYU), University of St Andrews [Scotland], College of William and Mary [Williamsburg] (WM), Universitat de Barcelona, University of St Andrews. School of Physics and Astronomy, 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, and 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)
Subjects: Astrofísica, Cosmology and Gravitation, Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), Astronomy & Astrophysics, 01 natural sciences, Observacions astronòmiques, 0103 physical sciences, cosmological parameters, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Physics, [PHYS]Physics [physics], Cosmologia, 010308 nuclear & particles physics, Oscillation, Astronomy, Astronomy and Astrophysics, Galaxy, Cosmology, Baryon, Space and Planetary Science, Sky, astro-ph.CO, High Energy Physics::Experiment, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Astronomical observations
Abstract: We explore the cosmological implications of the angle-averaged correlation function, xi(s), and the clustering wedges, xi_perp(s) and xi_para(s), of the LOWZ and CMASS galaxy samples from Data Release 10 and 11 of the SDSS-III Baryon Oscillation Spectroscopic Survey. Our results show no significant evidence for a deviation from the standard LCDM model. The combination of the information from our clustering measurements with recent data from the cosmic microwave background is sufficient to constrain the curvature of the Universe to Omega_k = 0.0010 +- 0.0029, the total neutrino mass to Sum m_nu < 0.23 eV (95% confidence level), the effective number of relativistic species to N_eff=3.31 +- 0.27, and the dark energy equation of state to w_DE = -1.051 +- 0.076. These limits are further improved by adding information from type Ia supernovae and baryon acoustic oscillations from other samples. In particular, this data set combination is completely consistent with a time-independent dark energy equation of state, in which case we find w_DE=-1.024 +- 0.052. We explore the constraints on the growth-rate of cosmic structures assuming f(z)=Omega_m(z)^gamma and obtain gamma=0.69 +- 0.15, in agreement with the predictions from general relativity of gamma=0.55., 24 pages, 14 figures. Submitted to MNRAS. Measurements and covariance matrices are available at https://sdss3.org/science/boss_publications.php
Published: 2014
Full Text: View/download PDF

38. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: galaxy clustering measurements in the low redshift sample of Data Release 11

Author: Donald P. Schneider, Beth Reid, Matthew D. Olmstead, Kyle S. Dawson, Florian Beutler, Ariel G. Sánchez, Jeremy L. Tinker, Joel R. Brownstein, Lado Samushia, Francisco Montesano, Martin White, Antonio J. Cuesta, Shirley Ho, Ashley J. Ross, Jon Brinkmann, John K. Parejko, David J. Schlegel, Marc Manera, Daniel J. Eisenstein, Rita Tojeiro, Cameron K. McBride, Angela Burden, Mariana Vargas Magaña, Cullan Howlett, Will J. Percival, Universitat de Barcelona, and University of St Andrews. School of Physics and Astronomy
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, ComputingMilieux_LEGALASPECTSOFCOMPUTING, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, distance scale, GeneralLiterature_MISCELLANEOUS, surveys, Universe, Observacions astronòmiques, ComputingMilieux_COMPUTERSANDEDUCATION, QB Astronomy, Cluster analysis, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Univers, Cosmologia, ComputingMilieux_THECOMPUTINGPROFESSION, Oscillation, European research, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Sample (graphics), observations [cosmology], Redshift, Galaxy, Cosmology, Baryon, QC Physics, Space and Planetary Science, large-scale structure of Universe, BDC, Data release, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Astronomical observations
Abstract: We present the distance measurement to z = 0.32 using the 11th data release of the Sloan Digital Sky Survey-III Baryon Acoustic Oscillation Survey (BOSS). We use 313,780 galaxies of the low-redshift (LOWZ) sample over 7,341 square-degrees to compute $D_V = (1264 \pm 25)(r_d/r_{d,fid})$ - a sub 2% measurement - using the baryon acoustic feature measured in the galaxy two-point correlation function and power-spectrum. We compare our results to those obtained in DR10. We study observational systematics in the LOWZ sample and quantify potential effects due to photometric offsets between the northern and southern Galactic caps. We find the sample to be robust to all systematic effects found to impact on the targeting of higher-redshift BOSS galaxies, and that the observed north-south tensions can be explained by either limitations in photometric calibration or by sample variance, and have no impact on our final result. Our measurement, combined with the baryonic acoustic scale at z = 0.57, is used in Anderson et al. (2013a) to constrain cosmological parameters., Comment: 17 pages. Submitted to MNRAS
Published: 2014
Full Text: View/download PDF

39. Modelling The Redshift-Space Three-Point Correlation Function in SDSS-III

Author: Zheng Zheng, David H. Weinberg, Robert C. Nichol, Cristiano G. Sabiu, Hong Guo, Cameron K. McBride, Cheng Li, Donald P. Schneider, Idit Zehavi, Yipeng Jing, Graziano Rossi, and Ramin A. Skibba
Subjects: statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Criminology, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Halo occupation distribution, Galactic halo, Galaxy group, Galaxy formation and evolution, Lenticular galaxy, STFC, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics, Physics, theory [cosmology], RCUK, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, observations [cosmology], haloes [galaxies], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Elliptical galaxy, distances and redshifts [galaxies], large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the measurements of the redshift-space three-point correlation function (3PCF) for z~0.5 luminous red galaxies of the CMASS sample in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey Data Release 11. The 3PCF measurements are interpreted within the halo occupation distribution framework using high-resolution N-body simulations, and the model successfully reproduces the 3PCF on scales larger than 1Mpc/h. As with the case for the redshift-space two-point correlation functions, we find that the redshift-space 3PCF measurements also favour the inclusion of galaxy velocity bias in the model. In particular, the central galaxy in a halo is on average in motion with respect to the core of the halo. We discuss the potential of the small-scale 3PCF to tighten the constraints on the relation between galaxies and dark matter haloes and on the phase-space distribution of galaxies., Comment: MNRAS Letter accepted
Published: 2014
Full Text: View/download PDF

40. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles

Author: Kyle S. Dawson, David J. Schlegel, Benjamin A. Weaver, Will J. Percival, Nicholas P. Ross, Francesco Montesano, Andreu Font-Ribera, Jon Brinkmann, Florian Beutler, Cameron K. McBride, Jeremy L. Tinker, Shun Saito, Daniel J. Eisenstein, Ashley J. Ross, Shirley Ho, Hee-Jong Seo, Ariel G. Sánchez, and Lado Samushia
Subjects: Physics, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, observations [cosmology], Galaxy, Redshift, Redshift-space distortions, Baryon, symbols.namesake, surveys, gravitation, Space and Planetary Science, Dark energy, symbols, large-scale structure of Universe, Baryon acoustic oscillations, cosmological parameters, Planck, dark energy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We analyse the anisotropic clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) CMASS Data Release 11 (DR11) sample, which consists of $690\,827$ galaxies in the redshift range $0.43 < z < 0.7$ and has a sky coverage of $8\,498\,\text{deg}^2$. We perform our analysis in Fourier space using a power spectrum estimator suggested by Yamamoto et al. (2006). We measure the multipole power spectra in a self-consistent manner for the first time in the sense that we provide a proper way to treat the survey window function and the integral constraint, without the commonly used assumption of an isotropic power spectrum and without the need to split the survey into sub-regions. The main cosmological signals exploited in our analysis are the Baryon Acoustic Oscillations and the signal of redshift space distortions, both of which are distorted by the Alcock-Paczynski effect. Together, these signals allow us to constrain the distance ratio $D_V(z_{\rm eff})/r_s(z_d) = 13.89\pm 0.18$, the Alcock-Paczynski parameter $F_{\rm AP}(z_{\rm eff}) = 0.679\pm0.031$ and the growth rate of structure $f(z_{\rm eff})\sigma_8(z_{\rm eff}) = 0.419\pm0.044$ at the effective redshift $z_{\rm eff}=0.57$. We did not find significant systematic uncertainties for $D_V/r_s$ or $F_{\rm AP}$ but include a systematic error for $f\sigma_8$ of $3.1\%$. Combining our dataset with Planck to test General Relativity (GR) through the simple $\gamma$-parameterisation, reveals a $\sim 2\sigma$ tension between the data and the prediction by GR. The tension between our result and GR can be traced back to a tension in the clustering amplitude $\sigma_8$ between CMASS and Planck., Comment: 30 pages, 3 Tables, 17 Figures
Published: 2013
Full Text: View/download PDF

41. Structure finding in cosmological simulations: the state of affairs

Author: Frazer R. Pearce, Doug Potter, Pascal J. Elahi, Mark C. Neyrinck, H. Lux, Stefan Gottlöber, Fabrice Roy, Julian Onions, J. Casado, Marcel Zemp, Juerg Diemand, Volker Springel, Bridget Falck, Joachim Stadel, Rosa Domínguez-Tenreiro, Yago Ascasibar, Peter Behroozi, Paul M. Ricker, Andrés N. Ruiz, Yann Rasera, Klaus Dolag, Manuel Merchán, Vicent Quilis, Mario Agustín Sgró, Zarija Lukić, S. Planelles, Jiaxin Han, C. Corbett Moran, Anatoly Klypin, Cameron K. McBride, Alexander Knebe, Michal Maciejewski, Paul M. Sutter, Stuart I. Muldrew, Dylan Tweed, Universitats-Sternwarte [München], Ludwig-Maximilians-Universität München (LMU), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Asociación Chelonia, 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 Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Ciencias Físicas, Dark matter, FOS: Physical sciences, Astrophysics, GALAXIES HALOES, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, purl.org/becyt/ford/1 [https], 0103 physical sciences, Galaxy formation and evolution, Statistical physics, 010303 astronomy & astrophysics, Galaxy rotation curve, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], COSMIC cancer database, 010308 nuclear & particles physics, Astronomy and Astrophysics, Observable, purl.org/becyt/ford/1.3 [https], Astronomía, Gravitational lens, Space and Planetary Science, LUMINOSITY FUNCTION, Halo, GALAXIES EVOLUTION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CIENCIAS NATURALES Y EXACTAS, Astrophysics - Cosmology and Nongalactic Astrophysics, GALAXIES STATISTICS
Abstract: The ever increasing size and complexity of data coming from simulations of cosmic structure formation demands equally sophisticated tools for their analysis. During the past decade, the art of object finding in these simulations has hence developed into an important discipline itself. A multitude of codes based upon a huge variety of methods and techniques have been spawned yet the question remained as to whether or not they will provide the same (physical) information about the structures of interest. Here we summarize and extent previous work of the "halo finder comparison project": we investigate in detail the (possible) origin of any deviations across finders. To this extent we decipher and discuss differences in halo finding methods, clearly separating them from the disparity in definitions of halo properties. We observe that different codes not only find different numbers of objects leading to a scatter of up to 20 per cent in the halo mass and Vmax function, but also that the particulars of those objects that are identified by all finders differ. The strength of the variation, however, depends on the property studied, e.g. the scatter in position, bulk velocity, mass, and the peak value of the rotation curve is practically below a few per cent, whereas derived quantities such as spin and shape show larger deviations. Our study indicates that the prime contribution to differences in halo properties across codes stems from the distinct particle collection methods and -- to a minor extent -- the particular aspects of how the procedure for removing unbound particles is implemented. We close with a discussion of the relevance and implications of the scatter across different codes for other fields such as semi-analytical galaxy formation models, gravitational lensing, and observables in general., Comment: 28 pages containing 13 figures & 4 tables + 9 pages appendix containing another 4 tables + 4 pages of references, accepted for publication in MNRAS
Published: 2013
Full Text: View/download PDF

42. THE CLUSTERING OF GALAXIES IN THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: LUMINOSITY AND COLOR DEPENDENCE AND REDSHIFT EVOLUTION

Author: Luiz N. da Costa, Lado Samushia, Dmitry Bizyaev, Elena Malanushenko, Ariel G. Sánchez, Graziano Rossi, Audrey Simmons, John K. Parejko, Kevin Bundy, David J. Schlegel, Idit Zehavi, Andreas A. Berlind, Neta A. Bahcall, Daniel J. Eisenstein, Jeremy L. Tinker, Martin White, Eyal A. Kazin, Ashley J. Ross, Yanmei Chen, Daniel Thomas, Michael R. Blanton, Nicholas P. Ross, Viktor Malanushenko, Alina Streblyanska, Sebastián E. Nuza, Shirley Ho, Will J. Percival, Garrett Ebelke, Zheng Zheng, Howard Brewington, David A. Wake, Molly E. C. Swanson, Cameron K. McBride, Hong Guo, Donald P. Schneider, Nikhil Padmanabhan, Ramin A. Skibba, Daniel Oravetz, Stephanie A. Snedden, David H. Weinberg, Rita Tojeiro, Claudia Maraston, Marc Manera, University of Utah, Texas Tech University Health Sciences Center, Texas Tech University [Lubbock] (TTU), McMaster University [Hamilton, Ontario], Institute of cosmology and gravitation, University of Portsmouth, Institut Lagrange de Paris, Sorbonne Université (SU), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Pennsylvania State University (Penn State), Penn State System, New York University [New York] (NYU), NYU System (NYU), University of St Andrews [Scotland], College of William and Mary [Williamsburg] (WM), California Institute of Technology (CALTECH), 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)), 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), Institut de Génétique et Développement de Rennes (IGDR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)-Structure Fédérative de Recherche en Biologie et Santé de Rennes ( Biosit : Biologie - Santé - Innovation Technologique ), 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), and University of St Andrews. School of Physics and Astronomy
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, statistics [Galaxies], theory [Cosmology], 0103 physical sciences, Galaxy formation and evolution, distances and redshifts [Galaxies], QB Astronomy, observations [Cosmology], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, QB, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Galaxy, Baryon, Space and Planetary Science, Sky, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], halos [Galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the luminosity and color dependence and the redshift evolution of galaxy clustering in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey Ninth Data Release. We focus on the projected two-point correlation function (2PCF) of subsets of its CMASS sample, which includes about 260,000 galaxies over ~3,300 sq. deg in the redshift range 0.43, Comment: Accepted for publication in ApJ. Matched to the accepted version
Published: 2013
Full Text: View/download PDF

43. Cosmic Voids in the SDSS DR12 BOSS Galaxy Sample: the Alcock–Paczyński test

Author: Andreas A. Berlind, Mark C. Neyrinck, Robert J. Scherrer, Donald P. Schneider, Qingqing Mao, Cameron K. McBride, Roman Scoccimarro, and Jeremy L. Tinker
Subjects: Physics, Void (astronomy), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Line-of-sight, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, Cosmology, Baryon, Redshift-space distortions, Boss, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We apply the Alcock-Paczynski (AP) test to the stacked voids identified using the large-scale structure galaxy catalog from the Baryon Oscillation Spectroscopic Survey (BOSS). This galaxy catalog is part of the Sloan Digital Sky Survey (SDSS) Data Release 12 and is the final catalog of SDSS-III. We also use 1000 mock galaxy catalogs that match the geometry, density, and clustering properties of the BOSS sample in order to characterize the statistical uncertainties of our measurements and take into account systematic errors such as redshift space distortions. For both BOSS data and mock catalogs, we use the ZOBOV algorithm to identify voids, we stack together all voids with effective radii of 30-100Mpc/h in the redshift range 0.43-0.7, and we accurately measure the shape of the stacked voids. Our tests with the mock catalogs show that we measure the stacked void ellipticity with a statistical precision of 2.6%. We find that the stacked voids in redshift space are slightly squashed along the line of sight, which is consistent with previous studies. We repeat this measurement of stacked void shape in the BOSS data assuming several values of Omega_m within the flat LCDM model, and we compare to the mock catalogs in redshift space in order to perform the AP test. We obtain a constraint of $\Omega_m = 0.38^{+0.18}_{-0.15}$ at the 68% confidence level from the AP test. We discuss the various sources of statistical and systematic noise that affect the constraining power of this method. In particular, we find that the measured ellipticity of stacked voids scales more weakly with cosmology than the standard AP prediction, leading to significantly weaker constraints. We discuss how AP constraints will improve in future surveys with larger volumes and densities., Comment: 10 pages, 7 figures. Submitted to the ApJ. Replaced with updated version
Published: 2017
Full Text: View/download PDF

44. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: the low-redshift sample

Author: Will J. Percival, Elena Malanushenko, David A. Wake, Tomomi Sunayama, Daniel Oravetz, Daniel J. Eisenstein, Andreas A. Berlind, Benjamin A. Weaver, John K. Parejko, Joel R. Brownstein, Nicholas P. Ross, Frank C. van den Bosch, Claudia Maraston, Nikhil Padmanabhan, Audrey Simmons, David J. Schlegel, Jon Brinkmann, Zheng Zheng, Idit Zehavi, Daniel Thomas, Ramin A. Skibba, Cameron K. McBride, Martin White, Jeremy L. Tinker, Kaike Pan, Marcio A. G. Maia, Dmitry Bizyaev, David H. Weinberg, Adam S. Bolton, Ashley J. Ross, Francisco Prada, Luiz N. da Costa, Rita Tojeiro, Robert C. Nichol, Michael R. Blanton, Hong Guo, Andrew Wetzel, Eyal A. Kazin, Donald P. Schneider, and University of St Andrews. School of Physics and Astronomy
Subjects: statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Halo occupation distribution, surveys, QB Astronomy, Astrophysics::Galaxy Astrophysics, evolution [galaxies], QB, Physics, Luminous infrared galaxy, Oscillation, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Baryon, haloes [galaxies], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Halo, large-scale structure of Universe, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report on the small scale (0.5, Comment: 20 pages, 12 figures, accepted to MNRAS, catalogs available at http://www.sdss3.org/dr9/data_access/vac.php
Published: 2013
Full Text: View/download PDF

45. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: a large sample of mock galaxy catalogues

Author: Andreas A. Berlind, Beth Reid, Ravi K. Sheth, Lado Samushia, Will J. Percival, Benjamin A. Weaver, Roland de Putter, Bob Nichol, Ariel G. Sánchez, Nikhil Padmanabhan, Francesco Montesano, Cameron K. McBride, Ramin A. Skibba, Martin White, Roman Scoccimarro, Ashley J. Ross, Rita Tojeiro, Claudia Maraston, Jonathan Brinkmann, Xiaoying Xu, Marc Manera, and University of St Andrews. School of Physics and Astronomy
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Halo occupation distribution, 0103 physical sciences, QB Astronomy, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, Oscillation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Covariance, Galaxy, Baryon, haloes [galaxies], Space and Planetary Science, Perturbation theory (quantum mechanics), large-scale structure of Universe, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a fast method of producing mock galaxy catalogues that can be used to compute covariance matrices of large-scale clustering measurements and test the methods of analysis. Our method populates a 2nd-order Lagrangian Perturbation Theory (2LPT) matter field, where we calibrate masses of dark matter halos by detailed comparisons with N-body simulations. We demonstrate the clustering of halos is recovered at ~10 per cent accuracy. We populate halos with mock galaxies using a Halo Occupation Distribution (HOD) prescription, which has been calibrated to reproduce the clustering measurements on scales between 30 and 80 Mpc/h. We compare the sample covariance matrix from our mocks with analytic estimates, and discuss differences. We have used this method to make catalogues corresponding to Data Release 9 of the Baryon Oscillation Spectroscopic Survey (BOSS),producing 600 mock catalogues of the "CMASS" galaxy sample. These mocks enabled detailed tests of methods and errors that formed an integral part of companion analyses of these galaxy data., Comment: 21 pages, 18 figures, 2 tables. See companion papers that share the "The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey:" title. Mocks and covariance matrices will be available at http://www.marcmanera.net/mocks when the paper is accepted and DR9 released. Minor edits. Amended author's names. Submitted to MNRAS
Published: 2013

46. An optimized correlation function estimator for galaxy surveys

Author: M. Vargas-Magaña, Julian E. Bautista, J.-M. Le Goff, A. Labatie, J.-Ch. Hamilton, Cameron K. McBride, Marc Manera, Christopher N. A. Willmer, Stephanie Escoffier, Donald P. Schneider, Nicolás G. Busca, E. Aubourg, 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), 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), 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, 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), 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), 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), Département de Physique des Particules (ex SPP) (DPP), 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), APC - Cosmologie, 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, Département d'Astrophysique (ex SAP) (DAP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), BOSS, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), distance scale, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, 0103 physical sciences, Applied mathematics, Linear combination, 010303 astronomy & astrophysics, galaxies: statistics, media_common, Physics, 010308 nuclear & particles physics, Estimator, Astronomy and Astrophysics, methods: data analysis, Galaxy, Universe, Space and Planetary Science, cosmology: observations, Log-normal distribution, Dark energy, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Measuring the two-point correlation function of the galaxies in the Universe gives access to the underlying dark matter distribution, which is related to cosmological parameters and to the physics of the primordial Universe. The estimation of the correlation function for current galaxy surveys makes use of the Landy-Szalay estimator, which is supposed to reach minimal variance. This is only true, however, for a vanishing correlation function. We study the Landy-Szalay estimator when these conditions are not fulfilled and propose a new estimator that provides the smallest variance for a given survey geometry. Our estimator is a linear combination of ratios between paircounts of data and/or random catalogues (DD, RR and DR). The optimal combination for a given geometry is determined by using lognormal mock catalogues. The resulting estimator is biased in a model-dependent way, but we propose a simple iterative procedure for obtaining an unbiased model- independent estimator.Our method can be easily applied to any dataset and requires few extra mock catalogues compared to the standard Landy-Szalay analysis. Using various sets of simulated data (lognormal, second-order LPT and N-Body), we obtain a 20-25% gain on the error bars on the two-point correlation function for the SDSS geometry and $\Lambda$CDM correlation function. When applied to SDSS data (DR7 and DR9), we achieve a similar gain on the correlation functions, which translates into a 10-15% improvement over the estimation of the densities of matter $\Omega_m$ and dark energy $\Omega_\Lambda$ in an open $\Lambda$CDM model. The constraints derived from DR7 data with our estimator are similar to those obtained with the DR9 data and the Landy-Szalay estimator, which covers a volume twice as large and has a density that is three times higher., Comment: Accepted for publication A&A
Published: 2013
Full Text: View/download PDF

47. The Baryon Oscillation Spectroscopic Survey of SDSS-III

Author: Dan Long, Jean-Paul Kneib, Timothée Delubac, Ricardo Genova-Santos, Oliver Steele, Guinevere Kauffmann, Rupert A. C. Croft, Nicolás G. Busca, Will J. Percival, Marcio A. G. Maia, Tomer Tal, James Rich, Cullen H. Blake, Stephen A. Smee, Adam S. Bolton, Ashley J. Ross, Yiping Shu, Beatrice Jordan, Janine Pforr, Andreas A. Berlind, John K. Parejko, Kevin Bundy, Hayley Finley, Joel R. Brownstein, Johan Comparat, David J. Schlegel, Stephanie A. Snedden, Ian D. McGreer, Shirley Ho, D. Kirkby, Howard Brewington, Anže Slosar, James E. Gunn, Michael R. Blanton, Nao Suzuki, Christopher P. Ahn, Karen L. Masters, Fritz Stauffer, Licia Verde, Russell Owen, Jeremy L. Tinker, Jordi Miralda-Escudé, Anne Ealet, Éric Aubourg, M. Jordan Raddick, Nathalie Palanque-Delabrouille, Benjamin A. Weaver, Francisco Prada, Mark A. Klaene, Claudia G. Scóccola, Michael A. Strauss, Alina Streblyanska, Kaike Pan, Arnaud Borde, Craig Loomis, Adrian M. Price-Whelan, Natalia Connolly, Joe Huehnerhoff, Martin Makler, Daryl Haggard, Benjamin J. Weiner, Gong-Bo Zhao, Robert Pfaffenberger, A. Carnero, Martin White, Pasquier Noterdaeme, Antonio J. Cuesta, Jose Alberto Rubino-Martin, Stephen Bailey, Alessandra Beifiori, Patrick McDonald, Khee-Gan Lee, Jo Bovy, Nicholas P. Ross, Jean-Marc Le Goff, Francesco Montesano, Jon Brinkmann, Stephanie Escoffier, Matthew D. Olmstead, M. G. Watson, Natalie A. Roe, Michael A. Carr, Isabelle Pâris, Zheng Zheng, Rafael Rebolo, Gordon T. Richards, Hee-Jong Seo, Daniel J. Eisenstein, Britt Lundgren, Olga Mena, Yue Shen, Audrey Oravetz, Cameron K. McBride, Xiaohui Fan, Molly E. C. Swanson, Frances Cope, K. Honscheid, Graziano Rossi, Tracy Naugle, Matthew M. Pieri, David H. Weinberg, Robert H. Lupton, Viktor Malanushenko, Erin S. Sheldon, Michael Blomqvist, Donald P. Schneider, Luiz N. da Costa, Ben Harris, David W. Harris, Robert C. Nichol, Julian E. Bautista, James R. A. Davenport, Peter J. Brown, Saurav Dhital, Garrett Ebelke, Daniel Margala, Ignasi Pérez-Ràfols, Hong Guo, Robert H. Barkhouser, N. Filiz Ak, Demitri Muna, Scott F. Anderson, Andrew A. West, Elena Malanushenko, Patrick B. Hall, Alaina Shelden, Yanmei Chen, M. Vargas Magaña, Ariel G. Sánchez, William Carithers, Lado Samushia, Dmitry Bizyaev, Kyle S. Dawson, Christy Tremonti, Conor Sayres, Sebastián E. Nuza, Roland de Putter, Diana Holder, Sarah J. Schmidt, Eyal A. Kazin, Richard G. McMahon, Wendell P. Jordan, W. M. Wood-Vasey, Idit Zehavi, Andreu Font-Ribera, W. N. Brandt, Jean-Christophe Hamilton, Christophe Yèche, Patrick Petitjean, Daniel Oravetz, Nikhil Padmanabhan, Ismael Perez-Fournon, Antonio D. Montero-Dorta, Rita Tojeiro, David W. Hogg, Adam D. Myers, Daniel Thomas, Vaishali Bhardwaj, Matteo Viel, David A. Wake, Rachel Mandelbaum, Claudia Maraston, Constance M. Rockosi, Masayuki Tanaka, Marc Manera, University of St Andrews. School of Physics and Astronomy, APC - Cosmologie, 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)-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)-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)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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), BOSS, 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), Aix Marseille Université (AMU)-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)-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, and 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)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, Observacions astronòmiques, 0103 physical sciences, Physical Sciences and Mathematics, observations [Cosmology], 010303 astronomy & astrophysics, Observations, Astrophysics::Galaxy Astrophysics, Physics, Cosmologia, 010308 nuclear & particles physics, Angular diameter distance, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Quasar, Cosmology and Extragalactic Astrophysics, Lyman-alpha forest, Redshift, Galaxy, Cosmology, Baryon, Boss, Space and Planetary Science, Astronomia, Baryon acoustic oscillations, Astronomical observations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Baryon Oscillation Spectroscopic Survey (BOSS) is designed to measure the scale of baryon acoustic oscillations (BAO) in the clustering of matter over a larger volume than the combined efforts of all previous spectroscopic surveys of large-scale structure. BOSS uses 1.5 million luminous galaxies as faint as i = 19.9 over 10,000 deg(2) to measure BAO to redshifts z < 0.7. Observations of neutral hydrogen in the Ly alpha forest in more than 150,000 quasar spectra (g < 22) will constrain BAO over the redshift range 2.15 < z < 3.5. Early results from BOSS include the first detection of the large-scale three-dimensional clustering of the Ly alpha forest and a strong detection from the Data Release 9 data set of the BAO in the clustering of massive galaxies at an effective redshift z = 0.57. We project that BOSS will yield measurements of the angular diameter distance d(A) to an accuracy of 1.0% at redshifts z = 0.3 and z = 0.57 and measurements of H(z) to 1.8% and 1.7% at the same redshifts. Forecasts for Ly alpha forest constraints predict a measurement of an overall dilation factor that scales the highly degenerate D-A(z) and H-1(z) parameters to an accuracy of 1.9% at z similar to 2.5 when the survey is complete. Here, we provide an overview of the selection of spectroscopic targets, planning of observations, and analysis of data and data quality of BOSS, The successful installation, commissioning, and operation of the Pierre Auger Observatory would not have been possible without the strong commitment and effort fromthe technical and administrative staff in Malarg¨ue. The authors are very grateful to the following agencies and organizations for financial support: Comisi´on Nacional de Energ´ıa At´omica, Fundaci ´on Antorchas, Gobierno De La Provincia de Mendoza, Municipalidad de Malarg¨ue, NDM Holdings and Valle Las Le˜nas, in gratitude for their continuing cooperation over land access,Argentina; theAustralian ResearchCouncil;Conselho Nacional de Desenvolvimento Cient´ıfico e Tecnol´ogico (CNPq), Financiadora de Estudos e Projetos (FINEP), Fundacao de Amparo a Pesquisa do Estado de Rio de Janeiro (FAPERJ), Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Minist´erio de Ciˆencia e Tecnologia (MCT), Brazil; AVCR AV0Z10100502 and AV0Z10100522, GAAV KJB100100904, MSMT-CR LA08016, LG11044, MEB111003, MSM0021620859, LA08015, and TACR TA01010517, Czech Republic; Centre de Calcul IN2P3/CNRS, CentreNational de la Recherche Scientifique (CNRS), Conseil R´egional Ile-de- France, D´epartement Physique Nucleaire et Corpusculaire (PNC-IN2P3/CNRS), D´epartement Sciences de l’Univers (SDU-INSU/CNRS), France; Bundesministerium fur Bildung und Forschung (BMBF), Deutsche Forschungsgemeinschaft (DFG), Finanzministerium Baden-W¨urttemberg, Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF), Ministerium fur Wissenschaft und Forschung, Nordrhein-Westfalen, Ministerium f¨ur Wissenschaft, Forschung und Kunst, Baden-W¨urttemberg, Germany; Istituto Nazionale di Fisica Nucleare (INFN), Ministero dell’Istruzione, dell’Universita e della Ricerca (MIUR), Italy; Consejo Nacional de Ciencia y Tecnolog´ıa (CONACYT), Mexico; Ministerie van Onderwijs, Cultuur en Wetenschap, Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO), Stichting voor Fundamenteel Onderzoek der Materie (FOM), The Netherlands; Ministry of Science and Higher Education, Grants no. N N202 200239 and N N202 2038, Poland; Fundacao para a Ciˆencia e a Tecnologia, Portugal; Ministry for Higher Education, Science, and Technology, Slovenian Research Agency, Slovenia; Comunidad de Madrid, Consejer´ıa de Educaci´on de la Comunidad de Castilla La Mancha, FEDER funds, Ministerio de Ciencia e Innovaci´on and Consolider- Ingenio 2010 (CPAN), Xunta de Galicia, Spain; Science and Technology Facilities Council, UK; Department of Energy, Contract nos. DE-AC02-07CH11359 and DEFR02- 04ER41300, National Science Foundation, Grant no. 0450696, The Grainger Foundation, USA; NAFOSTED, Vietnam; ALFA-EC/HELEN and UNESCO.
Published: 2013
Full Text: View/download PDF

48. Recovering Redshift Distributions with Cross-Correlations: Pushing The Boundaries

Author: Cameron K. McBride, Brice Ménard, S. J. Schmidt, Christopher B. Morrison, and Ryan Scranton
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift quantization, Redshift survey, Residual, 01 natural sciences, Cosmology, Galaxy, Redshift, Space and Planetary Science, 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Determining accurate redshift distributions for very large samples of objects has become increasingly important in cosmology. We investigate the impact of extending cross-correlation based redshift distribution recovery methods to include small scale clustering information. The major concern in such work is the ability to disentangle the amplitude of the underlying redshift distribution from the influence of evolving galaxy bias. Using multiple simulations covering a variety of galaxy bias evolution scenarios, we demonstrate reliable redshift recoveries using linear clustering assumptions well into the non-linear regime for redshift distributions of narrow redshift width. Including information from intermediate physical scales balances the increased information available from clustering and the residual bias incurred from relaxing of linear constraints. We discuss how breaking a broad sample into tomographic bins can improve estimates of the redshift distribution, and present a simple bias removal technique using clustering information from the spectroscopic sample alone., Comment: 13 pages, 9 figures. Submitted to MNRAS
Published: 2013
Full Text: View/download PDF

49. Mock galaxy catalogs using the quick particle mesh method

Author: Cameron K. McBride, Jeremy L. Tinker, and Martin White
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, Volume (computing), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Observable, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Computational science, Set (abstract data type), Space and Planetary Science, Particle Mesh, Halo, Reduction (mathematics), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Sophisticated analysis of modern large-scale structure surveys requires mock catalogs. Mock catalogs are used to optimize survey design, test reduction and analysis pipelines, make theoretical predictions for basic observables and propagate errors through complex analysis chains. We present a new method, which we call "quick particle mesh", for generating many large-volume, approximate mock catalogs at low computational cost. The method is based on using rapid, low-resolution particle mesh simulations that accurately reproduce the large-scale dark matter density field. Particles are sampled from the density field based on their local density such that they have N-point statistics nearly equivalent to the halos resolved in high-resolution simulations, creating a set of mock halos that can be populated using halo occupation methods to create galaxy mocks for a variety of possible target classes., Comment: 13 pages, 16 figures. Matches version accepted by MNRAS. Code available at http://github.com/mockFactory
Published: 2013
Full Text: View/download PDF

50. The Ninth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Baryon Oscillation Spectroscopic Survey

Author: Christopher P. Ahn, Rachael Alexandroff, Carlos Allende Prieto, Scott F. Anderson, Timothy Anderton, Brett H. Andrews, Éric Aubourg, Stephen Bailey, Eduardo Balbinot, Rory Barnes, Julian Bautista, Timothy C. Beers, Alessandra Beifiori, Andreas A. Berlind, Vaishali Bhardwaj, Dmitry Bizyaev, Cullen H. Blake, Michael R. Blanton, Michael Blomqvist, John J. Bochanski, Adam S. Bolton, Arnaud Borde, Jo Bovy, W. N. Brandt, J. Brinkmann, Peter J. Brown, Joel R. Brownstein, Kevin Bundy, N. G. Busca, William Carithers, Aurelio R. Carnero, Michael A. Carr, Dana I. Casetti-Dinescu, Yanmei Chen, Cristina Chiappini, Johan Comparat, Natalia Connolly, Justin R. Crepp, Stefano Cristiani, Rupert A. C. Croft, Antonio J. Cuesta, Luiz N. da Costa, James R. A. Davenport, Kyle S. Dawson, Roland de Putter, Nathan De Lee, Timothée Delubac, Saurav Dhital, Anne Ealet, Garrett L. Ebelke, Edward M. Edmondson, Daniel J. Eisenstein, S. Escoffier, Massimiliano Esposito, Michael L. Evans, Xiaohui Fan, Bruno Femenía Castellá, Emma Fernández Alvar, Leticia D. Ferreira, N. Filiz Ak, Hayley Finley, Scott W. Fleming, Andreu Font-Ribera, Peter M. Frinchaboy, D. A. García-Hernández, A. E. García Pérez, Jian Ge, R. Génova-Santos, Bruce A. Gillespie, Léo Girardi, Jonay I. González Hernández, Eva K. Grebel, James E. Gunn, Hong Guo, Daryl Haggard, Jean-Christophe Hamilton, David W. Harris, Suzanne L. Hawley, Frederick R. Hearty, Shirley Ho, David W. Hogg, Jon A. Holtzman, Klaus Honscheid, J. Huehnerhoff, Inese I. Ivans, Željko Ivezić, Heather R. Jacobson, Linhua Jiang, Jonas Johansson, Jennifer A. Johnson, Guinevere Kauffmann, David Kirkby, Jessica A. Kirkpatrick, Mark A. Klaene, Gillian R. Knapp, Jean-Paul Kneib, Jean-Marc Le Goff, Alexie Leauthaud, Khee-Gan Lee, Young Sun Lee, Daniel C. Long, Craig P. Loomis, Sara Lucatello, Britt Lundgren, Robert H. Lupton, Bo Ma, Zhibo Ma, Nicholas MacDonald, Claude E. Mack, Suvrath Mahadevan, Marcio A. G. Maia, Steven R. Majewski, Martin Makler, Elena Malanushenko, Viktor Malanushenko, A. Manchado, Rachel Mandelbaum, Marc Manera, Claudia Maraston, Daniel Margala, Sarah L. Martell, Cameron K. McBride, Ian D. McGreer, Richard G. McMahon, Brice Ménard, Sz. Meszaros, Jordi Miralda-Escudé, Antonio D. Montero-Dorta, Francesco Montesano, Heather L. Morrison, Demitri Muna, Jeffrey A. Munn, Hitoshi Murayama, Adam D. Myers, A. F. Neto, Duy Cuong Nguyen, Robert C. Nichol, David L. Nidever, Pasquier Noterdaeme, Sebastián E. Nuza, Ricardo L. C. Ogando, Matthew D. Olmstead, Daniel J. Oravetz, Russell Owen, Nikhil Padmanabhan, Nathalie Palanque-Delabrouille, Kaike Pan, John K. Parejko, Prachi Parihar, Isabelle Pâris, Petchara Pattarakijwanich, Joshua Pepper, Will J. Percival, Ismael Pérez-Fournon, Ignasi Pérez-Ràfols, Patrick Petitjean, Janine Pforr, Matthew M. Pieri, Marc H. Pinsonneault, G. F. Porto de Mello, Francisco Prada, Adrian M. Price-Whelan, M. Jordan Raddick, Rafael Rebolo, James Rich, Gordon T. Richards, Annie C. Robin, Helio J. Rocha-Pinto, Constance M. Rockosi, Natalie A. Roe, Ashley J. Ross, Nicholas P. Ross, Graziano Rossi, J. A. Rubiño-Martin, Lado Samushia, J. Sanchez Almeida, Ariel G. Sánchez, Basílio Santiago, Conor Sayres, David J. Schlegel, Katharine J. Schlesinger, Sarah J. Schmidt, Donald P. Schneider, Mathias Schultheis, Axel D. Schwope, C. G. Scóccola, Uros Seljak, Erin Sheldon, Yue Shen, Yiping Shu, Jennifer Simmerer, Audrey E. Simmons, Ramin A. Skibba, M. F. Skrutskie, A. Slosar, Flavia Sobreira, Jennifer S. Sobeck, Keivan G. Stassun, Oliver Steele, Matthias Steinmetz, Michael A. Strauss, Alina Streblyanska, Nao Suzuki, Molly E. C. Swanson, Tomer Tal, Aniruddha R. Thakar, Daniel Thomas, Benjamin A. Thompson, Jeremy L. Tinker, Rita Tojeiro, Christy A. Tremonti, M. Vargas Magaña, Licia Verde, Matteo Viel, Shailendra K. Vikas, Nicole P. Vogt, David A. Wake, Ji Wang, Benjamin A. Weaver, David H. Weinberg, Benjamin J. Weiner, Andrew A. West, Martin White, John C. Wilson, John P. Wisniewski, W. M. Wood-Vasey, Brian Yanny, Christophe Yèche, Donald G. York, O. Zamora, Gail Zasowski, Idit Zehavi, Gong-Bo Zhao, Zheng Zheng, Guangtun Zhu, Joel C. Zinn, APC - Cosmologie, 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), AstroParticule et Cosmologie (APC (UMR_7164)), 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), BOSS, Instituto de Astrofisica de Canarias (IAC), 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), Elon University [NC, USA], Department of Astronomy [Seattle], University of Washington [Seattle], The University of Notre Dame [Sydney], Apache point observatory, 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), 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, Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), 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), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Universitat de Barcelona, Observatoire des Sciences de l'Univers en région Centre (OSUC), and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Atles, Astrophysics, Surveys, 01 natural sciences, Astronomical spectroscopy, Via láctea, Observatory, Observacions astronòmiques, Physical Sciences and Mathematics, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Mapeamentos astronômicos, Physics, [PHYS]Physics [physics], Astrophysics::Instrumentation and Methods for Astrophysics, Atlases, Astrometry, Cosmology, atlases, Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astronomical observations, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, catalogs, surveys, Formacao de galaxias, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), Spectrograph, Astrophysics::Galaxy Astrophysics, Cosmologia, 010308 nuclear & particles physics, Astronomy and Astrophysics, Quasar, Cosmology and Extragalactic Astrophysics, Espectroscòpia, Galaxy, Spectrum analysis, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Stars, Space and Planetary Science, Sky, Catalogs, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Sloan Digital Sky Survey III (SDSS-III) presents the first spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS). This ninth data release (DR9) of the SDSS project includes 535,995 new galaxy spectra (median z=0.52), 102,100 new quasar spectra (median z=2.32), and 90,897 new stellar spectra, along with the data presented in previous data releases. These spectra were obtained with the new BOSS spectrograph and were taken between 2009 December and 2011 July. In addition, the stellar parameters pipeline, which determines radial velocities, surface temperatures, surface gravities, and metallicities of stars, has been updated and refined with improvements in temperature estimates for stars with T_eff-0.5. DR9 includes new stellar parameters for all stars presented in DR8, including stars from SDSS-I and II, as well as those observed as part of the SDSS-III Sloan Extension for Galactic Understanding and Exploration-2 (SEGUE-2). The astrometry error introduced in the DR8 imaging catalogs has been corrected in the DR9 data products. The next data release for SDSS-III will be in Summer 2013, which will present the first data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) along with another year of data from BOSS, followed by the final SDSS-III data release in December 2014., 9 figures; 2 tables. Submitted to ApJS. DR9 is available at http://www.sdss3.org/dr9
Published: 2012
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Database

Publisher

72 results on '"Cameron K. McBride"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources