The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: measurement of the growth rate of structure from the anisotropic correlation function between…

By P. Zarrouk, É. Burtin, H. Gil-Marín, A. Ross, R. Tojeiro, Iap Paris, K. Dawson, Adam D. Myers, Will J. Percival, C. Chuang and 28 more. Monthly notices of the Royal Astronomical Society, 2018

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PZ and EB acknowledge support from the P2IO LabEx (reference ANR-10-LABX-0038). HGM acknowledges support from the Labex ILP (reference ANR-10-LABX-63) part of the Idex SUPER, and received financial state aid managed by the Agence Nationalede la Recherche, as part of the programme Investissements d'avenir under the reference ANR-11-IDEX-0004-02. AJR is grateful for support from the Ohio State University Center for Cosmology and ParticlePhysics. GBZ is supported by NSFC Grants 1171001024 and 11673025. GBZ is also supported by a Royal Society Newton Advanced Fellowship, hosted by University of Portsmouth. SH's and KH's work was supported under the U.S. Department of Energy contract DE-AC02-06CH11357. GBZ is supported by NSFC Grant No. 11673025, and by a Royal Society Newton Advanced Fellowship. GR acknowledges support from the National Research Foundation of Korea (NRF) through Grant No. 2017077508 funded by the Korean Ministry of Education, Science and Technology (MoEST), and from the faculty research fund of Sejong University in 2018. Funding for SDSS-III and SDSS-IV has been provided by the Alfred P. Sloan Foundation and Participating Institutions. Additional funding for SDSS-III comes from the National Science Foundation and the U.S. Department of Energy Office of Science. Further information about both projects is available at www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions in both collaborations. In SDSS-III, these include 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. The Participating Institutions in SDSS-IV are CarnegieMellon University, Colorado University, Boulder, Harvard-Smithsonian Center for Astrophysics Participation Group, Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe Max-Planck-Institut fuer Astrophysik (MPA Garching), Max-Planck-Institut fuer Extraterrestrische Physik (MPE), Max-Planck-Institut fuer Astronomie (MPIA Heidelberg), National Astronomical Observatories of China, New Mexico State University, New York University, The Ohio State University, Penn State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, University of Portsmouth, University of Utah, University of Wisconsin, and Yale University. This research used resources of the Argonne Leadership Computing Facility, which is a DOE Office of Science User Facility supported under contract DE-AC02-06CH11357. This work made use of the facilities and staff of the UK Sciama High Performance Computing cluster supported by the ICG, SEPNet, and the University of Portsmouth. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No.r DE-AC02-05CH11231.

Subfields: Astronomy and Astrophysics, Instrumentation

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Target Selection and Validation of DESI Quasars (2022, methodology): “This new field of research with quasars was pioneered by eBOSS (Zarrouk et al. 2018; Neveux et al. 2020; Alam et al. 2021; Hou et al. 2021).”
The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: BAO and RSD measurements from the anisotropic power spectrum of the quasar sample between redshift 0.8 and 2.2 (2020, methodology): “The Data Release 14 of the first two years of eBOSS data (Ata et al. 2018; Gil-Marin et al. 2018; Hou et al. 2018; Zarrouk et al. 2018) demonstrated how well quasars are suited for cosmological clustering analyses and currently provide the most precise clustering information on large scales in the…”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: a tomographic measurement of cosmic structure growth and expansion rate based on optimal redshift weights (2018, methodology): “(iii) The clustering analysis presented in Zarrouk et al. (2018) is based on the eBOSS DR14 quasar sample in the redshift range 0.8 ≤ z ≤ 2.2, using Legendre multipoles with = 0, 2, 4, and three wedges of the correlation function on the s range from 16 h−1Mpc to 138 h−1Mpc.”
Baryon acoustic oscillations from the cross-correlation of Lyα absorption and quasars in eBOSS DR14 (2019, background): “…the peak has been seen in the correlation function of quasars at a mean redshift z ∼ 1.5 (Ata et al. 2018; Gil-Marín et al. 2018; Hou et al. 2018; Zarrouk et al. 2018) and in the flux-transmission correlation function in Lyman-α (Lyα) forests at z ∼ 2.3 (Busca et al. 2013; Slosar et al. 2013;…”
The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: BAO and RSD measurements from anisotropic clustering analysis of the quasar sample in configuration space between redshift 0.8 and 2.2 (2020, methodology): “In the DR14 full-shape analysis (Hou et al. 2018; Zarrouk et al. 2018; Gil-Maŕın et al. 2018), it was demonstrated that quasars can be used as robust tracers of the underlying matter field, extending growth rate measurements to redshift z ∼ 1.5.”
Baryon acoustic oscillations at z = 2.34 from the correlations of Lyα absorption in eBOSS DR14 (2019, background): “…discrete objects like galaxies (Percival et al. 2010; Reid et al. 2010; Beutler et al. 2011; Blake et al. 2011; Anderson et al. 2012, 2014a,b; Ross et al. 2015; Alam et al. 2017; Bautista et al. 2018) or quasars (Ata et al. 2018; Gil-Marín et al. 2018; Hou et al. 2018; Zarrouk et al. 2018).”