The M$_BH$-M$_*$ relation for X-ray-obscured, red QSOs at 1.2 łt} z łt} 2.6

TitleThe M$_BH$-M$_*$ relation for X-ray-obscured, red QSOs at 1.2 łt} z łt} 2.6
Publication TypeJournal Article
Year of Publication2014
AuthorsBongiorno, A, Maiolino, R, Brusa, M, Marconi, A, Piconcelli, E, Lamastra, A, Cano-Díaz, M, Schulze, A, Magnelli, B, Vignali, C, Fiore, F, Menci, N, Cresci, G, La Franca, F, Merloni, A
Keywordscosmology: observations, galaxies: active, galaxies: evolution, quasars: emission lines, quasars: supermassive black holes

{We present near-infrared (NIR) spectra, obtained with SINFONI and XShooter observations at ESO VLT, of nine dusty, red QSOs at 1.2 łt} z łt} 2.6. The sources are hard X-ray detected, characterized by cold absorption (N$_{H}$ {\gt} 10$^{21}$-10$^{22}$ cm$^{-2}$) and show a broad H{$\alpha$} component in the NIR spectra. We complement this sample with 12 additional sources taken from the literature with similar properties resulting in a total sample of 21 X-ray-obscured, intermediate-type (1.8-1.9), dusty reddened QSOs. From the broad H{$\alpha$} line, we have computed the black hole (BH) masses through the virial formula and derived Eddington ratios. Moreover, from optical/IR multicomponent spectral energy distribution fitting we have derived the stellar mass of their host galaxies and their star formation rates. We find that most of the sources in our sample are hosted in starburst and main-sequence star-forming galaxies with Eddington ratios {$łambda$} {\gt} 0.1. We find a strong trend with the BH mass, i.e. less massive objects are scattered below and above the local relation while the most massive ones are mainly located above it. We also studied the evolution of these sources on the M$_{BH}$-M$_{*}$ plane compared to a sample of optically blue type-1 QSOs and we find that obscured red QSOs show a ratio of M$_{BH}$ to M$_{*}$ that increases with redshift which is consistent with or slightly lower than what has been found for blue QSOs. These sources may represent the blow-out phase at the end of the rapid BH growth and immediately preceding the classical blue QSOs typically sampled in optical surveys. They in fact show evidence of outflows in the ionized gas component, but their BH has already fully formed. }