The clustering of theSDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: measuring the anisotropic baryon acoustic oscillations with redshift weights

Journal Article · 22 July 2018 · Monthly Notices of the Royal Astronomical Society

DOI: https://doi.org/10.1093/mnras/sty1955 · OSTI ID:1593672

Zhu, Fangzhou ^[1]; Padmanabhan, Nikhil  ^[2]; Ross, Ashley J.  ^[3]; White, Martin  ^[4]; Percival, Will J. ^[5]; Ruggeri, Rossana ^[5]; Zhao, Gong-bo ^[6]; Wang, Dandan ^[7]; Mueller, Eva-Maria ^[5]; Burtin, Etienne ^[8]; Gil-Marín, Héctor ^[9]; Bautista, Julian ^[10]; Beutler, Florian  ^[11]; Brinkmann, Jonathan ^[12]; Brownstein, Joel R.  ^[10]; Dawson, Kyle ^[10]; de la Macorra, Axel ^[13]; Rossi, Graziano ^[14]; Schneider, Donald P. ^[15]; Tojeiro, Rita  ^[16] ; Wang, Yuting ^[6]

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1. Department of Physics, Yale University, New Haven, CT 06511, USA; University of California, Berkeley
2. Department of Physics, Yale University, New Haven, CT 06511, USA
3. Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA
4. Department of Physics and Astronomy, U.C. Berkeley, Berkeley, CA 94720, USA
5. Institute of Cosmology, Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK
6. Institute of Cosmology, Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R. China
7. National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R. China
8. IRFU, CFA, Université Paris-Scalay, F-91191 Gif-sur-Yvette, France
9. Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, 75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, 75005 Paris, France
10. Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA
11. Institute of Cosmology, Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley CA 94720, USA
12. Apache Point Observatory, PO Box 59, Sunspot, NM 88349, USA
13. Instituto de Física, Universidad Nacional Autónoma de México, Apdo.Postal 20-364, 01000 México D.F., México
14. Department of Physics and Astronomy, Sejong University, Seoul 143-747, Korea
15. Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA
16. School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK

We present an anisotropic analysis of baryon acoustic oscillation (BAO) signal from the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey Data Release 14 quasar sample. The sample consists of 147 000 quasars distributed over a redshift range of 0.8 < z < 2.2. We apply the redshift weights technique to the clustering of quasars in this sample and achieve a 4.6 per cent measurement of the angular distance measurement DM at z = 2.2 and Hubble parameter H at z = 0.8. We parametrize the distance-redshift relation, relative to a fiducial model, as a Taylor series. The coefficients of this expansion are used to reconstruct the distance-redshift relation and obtain distance and Hubble parameter measurements at all redshifts within the redshift range of the sample. Reporting the result at two characteristic redshifts, we determine DM(z = 1) = 3405 ± 305 (rd/rd, fid) Mpc, H(z=1) = 120.7± 7.3 (r_d,fid / r_d) km s^{-1} Mpc^{-1} and DM(z = 2) = 5325 ± 249 (rd/rd, fid) Mpc, H(z=2) = 189.9± 32.9 (r_d,fid / r_d) km s^{-1} Mpc^{-1}. These measurements are highly correlated. We assess the outlook of BAO analysis from the final quasar sample by testing the method on a set of mocks that mimic the noise level in the final sample. We demonstrate on these mocks that redshift weighting shrinks the measurement error by over 25 per cent on average. We conclude redshift weighting can bring us closer to the cosmological goal of the final quasar sample.

• Research Organization: Univ. of California, Berkeley, CA (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
• Grant/Contract Number: SC0017860
• OSTI ID: 1593672
• Alternate ID(s): OSTI ID: 1594729
• Journal Information: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 1 Vol. 480; ISSN 0035-8711
• Publisher: Royal Astronomical SocietyCopyright Statement
• Country of Publication: United States
• Language: English