A glance at the host galaxy of high-redshift quasars using strong damped Lyman-α systems as coronagraphs^⋆

¹ Institut d’Astrophysique de Paris, CNRS-UPMC, UMR7095, 98bis Bd Arago, 75014 Paris, France
e-mail: finley@iap.fr
² Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
³ Apache Point Observatory, PO Box 59, Sunspot, NM 88349-0059, USA
⁴ Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA
⁵ Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 92420, USA
⁶ Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
⁷ Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA

Received: 20 April 2013
Accepted: 2 August 2013

Abstract

We searched quasar spectra from the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) for the rare occurrences where a strong damped Lyman-α absorber (DLA) blocks the Broad Line Region emission from the quasar and acts as a natural coronagraph to reveal narrow Lyα emission from the host galaxy. We define a statistical sample of 31 DLAs in Data Release 9 (DR9) with log N(H i) ≥ 21.3  cm^-2 located at less than 1500 km s^-1 from the quasar redshift. In 25% (8) of these DLAs, a strong narrow Lyα emission line is observed with flux ~25 × 10^-17  erg  s^-1  cm^-2 on average. For DLAs without this feature in their troughs, the average 3-σ upper limit is <0.8 × 10^-17  erg  s^-1  cm^-2. Our statistical sample is nearly 2.5 times larger than the anticipated number of intervening DLAs in DR9 within 1   500  km  s^-1 of the quasar redshift. We also define a sample of 26 DLAs from DR9 and DR10 with narrow Lyα emission detected and no limit on the H i column density to better characterize properties of the host galaxy emission. Analyzing the statistical sample, we do not find substantial differences in the kinematics, metals, or reddening for the two populations with and without emission detected. The highly symmetric narrow Lyα emission line profile centered in the HI trough indicates that the emitting region is separate from the absorber. The luminosity of the narrow Lyα emission peaks is intermediate between that of Lyα emitters and radio galaxies, implying that the Lyα emission is predominantly due to ionizing radiation from the AGN. Galaxies neighboring the quasar host are likely responsible for the majority (>75%) of these DLAs, with only a minority (<25%) arising from H i clouds located in the AGN host galaxy.