2011A&A...531A.128O

We present near-IR spectroscopy of a sample of luminous (M_B-27.5; L_bol>10¹⁴L_☉), sub-millimeter-detected, dusty (M_d∼10⁹M_☉), radio-quiet quasi-stellar objects (QSOs) at z∼2. A primary aim is to provide a more accurate QSO redshift determination in order to trace kinematics and inflows/outflows in these sub-mm bright QSOs. Additionally, the Hα and continuum properties allow an estimation of the black hole mass and accretion rate, offering insights into the starburst-AGN connection in sub-mm bright QSOs. We measure the redshift, width, and luminosity of the Hα line, and the continuum luminosity near Hα. Relative velocity differences between Hα and rest-frame UV emission lines are used to study the presence and strength of outflows/inflows. Luminosities and line widths are used to estimate the black hole masses, bolometric luminosities, Eddington fractions, and accretion rates; these are compared to the star-formation-rate (SFR), estimated from the sub-mm derived far-infrared (FIR) luminosity. Finally our sub-mm-bright QSO sample is compared with other QSO samples at similar redshifts. The Hα emission line was strongly detected in all sources. Two components - a very broad (>5000km/s) Gaussian and an intermediate-width (>1500km/s) Gaussian, were required to fit the Hα profile of all observed QSOs. Narrow (≲1000km/s) lines were not detected in the sample QSOs. The rest-frame UV emission lines in these sub-mm bright QSOs show larger than average blue-shifted velocities, potentially tracing strong - up to 3000km/s - outflows in the broad line region. With the exception of the one QSO which shows exceptionally broad Hα lines, the black hole masses of the QSO sample are in the range log M_BH=9.0-9.7 and the Eddington fractions are between 0.5 and ∼1. In black hole mass and accretion rate, this sub-mm bright QSO sample is indistinguishable from the Shemmer et al. (2004ApJ...614..547S) optically-bright QSO sample at z∼2; the latter is likely dominated by sub-mm dim QSOs. Previous authors have demonstrated a correlation, over six orders of magnitude, between SFR and accretion rate in active galaxies: the sub-mm bright QSOs lie at the upper extremes of both quantities and their SFR is an order of magnitude higher than that predicted from the correlation.