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. (arXiv:2007.08999v2 [astro-ph.CO] UPDATED)

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. (arXiv:2007.08999v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Neveux_R/0/1/0/all/0/1">Richard Neveux</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Burtin_E/0/1/0/all/0/1">Etienne Burtin</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Mattia_A/0/1/0/all/0/1">Arnaud de Mattia</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_A/0/1/0/all/0/1">Alex Smith</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Ross_A/0/1/0/all/0/1">Ashley J. Ross</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Hou_J/0/1/0/all/0/1">Jiamin Hou</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Bautista_J/0/1/0/all/0/1">Julian Bautista</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Brinkmann_J/0/1/0/all/0/1">Jonathan Brinkmann</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Chuang_C/0/1/0/all/0/1">Chia-Hsun Chuang</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_K/0/1/0/all/0/1">Kyle S. Dawson</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Gil_Marin_H/0/1/0/all/0/1">Héctor Gil-Marín</a> (8 and 9), <a href="http://arxiv.org/find/astro-ph/1/au:+Lyke_B/0/1/0/all/0/1">Brad W. Lyke</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Macorra_A/0/1/0/all/0/1">Axel de la Macorra</a> (11), <a href="http://arxiv.org/find/astro-ph/1/au:+Bourboux_H/0/1/0/all/0/1">Hélion du Mas des Bourboux</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Mohammad_F/0/1/0/all/0/1">Faizan G. Mohammad</a> (12,13) <a href="http://arxiv.org/find/astro-ph/1/au:+Muller_E/0/1/0/all/0/1">Eva-Maria Müller</a> (14), <a href="http://arxiv.org/find/astro-ph/1/au:+Myers_A/0/1/0/all/0/1">Adam D. Myers</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Newman_J/0/1/0/all/0/1">Jeffrey A. Newman</a> (15), <a href="http://arxiv.org/find/astro-ph/1/au:+Percival_W/0/1/0/all/0/1">Will J. Percival</a> (12 and 13 and 16), <a href="http://arxiv.org/find/astro-ph/1/au:+Rossi_G/0/1/0/all/0/1">Graziano Rossi</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_D/0/1/0/all/0/1">Donald Schneider</a> (18), <a href="http://arxiv.org/find/astro-ph/1/au:+Vivek_M/0/1/0/all/0/1">M. Vivek</a> (19 and 20), <a href="http://arxiv.org/find/astro-ph/1/au:+Zarrouk_P/0/1/0/all/0/1">Pauline Zarrouk</a> (1 and 21), <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_C/0/1/0/all/0/1">Cheng Zhao</a> (22), <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_G/0/1/0/all/0/1">Gong-Bo Zhao</a> (23) ((1) IRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France, (2) Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, Ohio, USA, (3) Max-Planck-Institut für Extraterrestrische Physik, Garching bei München, Germany, (4) Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, UK, (5) Apache Point Observatory, Sunspot, NM, (6) Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA, USA, (7) Department Physics and Astronomy, University of Utah, Salt Lake City, UT, USA, (8) Institut de Ciències del Cosmos, Universitat de Barcelona, ICCUB, Barcelona, Spain, (9) Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain, (10) University of Wyoming, Laramie, WY, USA, (11) Instituto de Física, Universidad Nacional Autónoma de México, México, (12) Waterloo Centre for Astrophysics, University of Waterloo, Waterloo, ON, Canada, (13) Department of Physics and Astronomy, University of Waterloo, Waterloo, ON, Canada, (14) Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, (15) PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA, USA, (16) Perimeter Institute for Theoretical Physics, Waterloo, ON, Canada, (17) Department of Physics and Astronomy, Sejong University, Seoul, Korea, (18) Institute for Gravitation and the Cosmos, Pennsylvania State University, University Park, PA, USA, (19) Department of Astronomy & Astrophysics, Pennsylvania State University, University Park, PA, USA, (20) Indian Institute of Astrophysics, Koramangala, Bangalore, India, (21) Institute for Computational Cosmology, Dept. of Physics, Univ. of Durham, South Road, Durham, UK, (22) Institute of Physics, Laboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, Switzerland, (23) National Astronomy Observatories, Chinese Academy of Science, Beijing, P.R. China)

We measure the clustering of quasars of the final data release (DR16) of
eBOSS. The sample contains $343,708$ quasars between redshifts $0.8leq
zleq2.2$ over $4699,mathrm{deg}^2$. We calculate the Legendre multipoles
(0,2,4) of the anisotropic power spectrum and perform a BAO and a Full-Shape
(FS) analysis at the effective redshift $z{rm eff}=1.480$. The errors include
systematic errors that amount to 1/3 of the statistical error. The systematic
errors comprise a modelling part studied using a blind N-Body mock challenge
and observational effects studied with approximate mocks to account for various
types of redshift smearing and fibre collisions. For the BAO analysis, we
measure the transverse comoving distance $D_{rm M}(z_{rm eff})/r_{rm
drag}=30.60pm{0.90}$ and the Hubble distance $D_{rm H}(z_{rm eff})/r_{rm
drag}=13.34pm{0.60}$. This agrees with the configuration space analysis, and
the consensus yields: $D_{rm M}(z_{rm eff})/r_{rm drag}=30.69pm{0.80}$ and
$D_{rm H}(z_{rm eff})/r_{rm drag}=13.26pm{0.55}$. In the FS analysis, we
fit the power spectrum using a model based on Regularised Perturbation Theory,
which includes Redshift Space Distortions and the Alcock-Paczynski effect. The
results are $D_{rm M}(z_{rm eff})/r_{rm drag}=30.68pm{0.90}$ and $D_{rm
H}(z_{rm eff})/r_{rm drag}=13.52pm{0.51}$ and we constrain the linear growth
rate of structure $f(z_{rm eff})sigma_8(z_{rm eff})=0.476pm{0.047}$. Our
results agree with the configuration space analysis. The consensus analysis of
the eBOSS quasar sample yields: $D_{rm M}(z_{rm eff})/r_{rm
drag}=30.21pm{0.79}$, $D_{rm H}(z_{rm eff})/r_{rm drag}=3.23pm{0.47}$ and
$f(z_{rm eff})sigma_8(z_{rm eff})=0.462pm{0.045}$ and is consistent with a
flat $Lambda {rm CDM}$ cosmological model using Planck results.

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