The Quasar-LBG Two-point Angular Cross-correlation Function at z~4 in the COSMOS Field

August 2015 • 2015ApJ...809..138I

Authors • Ikeda, H. • Nagao, T. • Taniguchi, Y. • Matsuoka, K. • Kajisawa, M. • Akiyama, M. • Miyaji, T. • Kashikawa, N. • Morokuma, T. • Shioya, Y. • Enoki, M. • Capak, P. • Koekemoer, A. M. • Masters, D. • Salvato, M. • Sanders, D. B. • Schinnerer, E. • Scoville, N. Z.

Abstract • In order to investigate the origin of quasars, we estimate the bias factor for low-luminosity quasars at high redshift for the first time. In this study, we use the two-point angular cross-correlation function (CCF) for both low-luminosity quasars at -24\lt {M}₁₄₅₀\lt -22 and Lyman-break galaxies (LBGs). Our sample consists of both 25 low-luminosity quasars (16 objects are spectroscopically confirmed low-luminosity quasars) in the redshift range 3.1\lt z\lt 4.5 and 835 color-selected LBGs with {z}_{LBG}^\prime\lt 25.0 at z ∼ 4 in the COSMOS field. We have performed our analysis for the following two quasar samples: (1) the spectroscopic sample (the 16 quasars confirmed by spectroscopy), and (2) the total sample (the 25 quasars including 9 quasars with photometric redshifts). The bias factor for low-luminosity quasars at z ∼ 4 is derived by utilizing the quasar-LBG CCF and the LBG auto-correlation function. We then obtain the 86% upper limits of the bias factors for low-luminosity quasars, which are 5.63 and 10.50 for the total and the spectroscopic samples, respectively. These bias factors correspond to the typical dark matter halo masses, log ({M}_{DM}/({h}^-1{M}_⊙)) = 12.7 and 13.5, respectively. This result is not inconsistent with the predicted bias for quasars that is estimated by the major merger models.

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IPAC Authors
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Elise Furlan

Associate Scientist

Daniel Masters

Assistant Scientist