The co-evolution of black hole growth and star formation from a cross-correlation analysis between quasars and the cosmic infrared background

Abstract

We present the first cross-correlation measurement between Sloan Digital Sky Survey (SDSS) Type 1 quasars and the cosmic infrared background (CIB) measured by Herschel. The distribution of the quasars at 0.15<z<3.5 covers the redshift range where we expect most of the CIB to originate. We detect the sub-mm emission of the quasars, which dominates on small scales, as well as correlated emission from dusty star-forming galaxies (DSFGs) dominant on larger scales. The mean sub-mm flux densities of the DR7 quasars (median redshift <z>=1.4) is $11.1_{-1.4}^{+1.6}$, $7.1_{-1.3}^{+1.6}$ and $3.6_{-1.0}^{+1.4}$ mJy at 250, 350 and 500 microns, respectively, while the mean sub-mm flux densities of the DR9 quasars (<z>=2.5) is $5.7_{-0.6}^{+0.7}$, $5.0_{-0.7}^{+0.8}$ and $1.8_{-0.4}^{+0.5}$ mJy. We find that the correlated sub-mm emission includes both the emission from satellite DSFGs in the same halo as the central quasar and the emission from DSFGs in separate halos (correlated with the quasar-hosting halo). The amplitude of the one-halo term is ~10 times smaller than the sub-mm emission of the quasars, implying the the satellites have a lower star-formation rate than the quasars. The satellite fraction for the DR7 quasars is $0.008_{-0.005}^{+0.008}$ and the host halo mass scale for the central and satellite quasars is $10^{12.36\pm 0.87}$ M${}_{\odot }$ and $10^{13.60\pm 0.38}$ M${}_{\odot }$, respectively. The satellite fraction of the DR9 quasars is $0.065_{-0.031}^{+0.021}$ and the host halo mass scale for the central and satellite quasars is $10^{12.29\pm 0.62}$ M${}_{\odot }$ and $10^{12.82\pm 0.39}$ M${}_{\odot }$, respectively. Thus, the typical halo environment of the SDSS Type 1 quasars is found to be similar to that of DSFGs, which supports the generally accepted view that dusty starburst and quasar activity are evolutionarily linked.

arXiv comment20 pages, 14 pages, submitted to MNRAS

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