Clustering of intermediate redshift quasars using the final SDSS III-BOSS sample

By S. Eftekharzadeh, Adam D. Myers, M. White, D. Weinberg, D. Schneider, Yue Shen, A. Font-Ribera, N. Ross, Iap Paris, A. Streblyanska. 2015

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Author(s): Eftekharzadeh, S; Myers, AD; White, M; Weinberg, DH; Schneider, DP; Shen, Y; Font-Ribera, A; Ross, NP; Paris, I; Streblyanska, A | Abstract: © 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. We measure the two-point clustering of spectroscopically confirmed quasars from the final sample of the Baryon Oscillation Spectroscopic Survey (BOSS) on comoving scales of 4 ≲ s ≲ 22 h-1 Mpc. The sample covers 6950 deg2 [~19 (h-1Gpc)3] and, over the redshift range 2.2 ≲ z ≲ 2.8, contains 55 826 homogeneously selected quasars, which is twice as many as in any similar work. We deduce bQ = 3.54 ± 0.10; the most precise measurement of quasar bias to date at these redshifts. This corresponds to a host halo mass of ~2 × 1012 h-1M⊙ with an implied quasar duty cycle of ~1 per cent. The real-space projected correlation function is well fitted by a power law of index 2 and correlation length r0 = (8.12 ± 0.22) h-1 Mpc over scales of 4 ≲ rp ≲ 25 h-1 Mpc. To better study the evolution of quasar clustering at moderate redshift, we extend the redshift range of our study to z ~ 3.4 and measure the bias and correlation length of three subsamples over 2.2 ≲ z ≲ 3.4. We find no significant evolution of r0 or bias over this range, implying that the host halo mass of quasars decreases somewhat with increasing redshift. We find quasar clustering remains similar over a decade in luminosity, contradicting a scenario in which quasar luminosity is monotonically related to halo mass at z ≈ 2.5. Our results are broadly consistent with previous BOSS measurements, but they yield more precise constraints based upon a larger and more uniform data set.

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Citations in the corpus

The Sloan Digital Sky Survey Quasar Catalog: Twelfth data release (2016, background): “Conversely there is the desire to perform demographic measurements and quasar physics studies using a uniformly-selected quasar sample (e.g. White et al. 2012; Ross et al. 2013; Eftekharzadeh et al. 2015).”
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 redshift 0.8 and 2.2 (2018, methodology): “Further studies to constrain the dark matter halo mass and duty cycle using the final eBOSS quasar clustering measurements would provide a superior statistical power to investigate these effects, following the approach developed in Eftekharzadeh et al. (2015) and Laurent et al. (2017).”
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, background): “Due to their high intrinsic luminosity, quasars can be used as tracers of the large scale structure at high redshifts (Croom et al. 2009; Myers et al. 2007; Ross et al. 2009; Shen et al. 2009; White et al. 2012; Karagiannis et al. 2014; Eftekharzadeh et al. 2015; Laurent et al. 2016).”
THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: QUASAR TARGET SELECTION (2015, background): “(e.g Filiz Ak et al. 2012, 2013, 2014; White et al. 2012; Alexandroff et al. 2013; Finley et al. 2013; McGreer et al. 2013; Ross et al. 2013; Vikas et al. 2013; Greene et al. 2014; Eftekharzadeh et al. 2015). eBOSS will seek to augment many of these measurements.”
The realm of the galaxy protoclusters (2016, background): “However, several recent works based on spectroscopic observations of LBGs and LAEs more similar to the Venemans et al. (2007) work on radio galaxy environments, have found evidence for protoclusters near luminous QSOs in about 10 % of the cases (Trainor & Steidel, 2012; Adams et al., 2015; Hennawi e”
The Sloan Digital Sky Survey Quasar Catalog: Fourteenth data release (2017, methodology): “This sample was also used to study the luminosity function of quasars (Ross et al. 2013; Palanque-Delabrouille et al. 2013), moderate-scale clustering of z ∼ 2.5 quasars (e.g. Eftekharzadeh et al. 2015).”