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THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: ENSEMBLE SPECTROSCOPIC VARIABILITY OF QUASAR BROAD EMISSION LINES
Journal article   Open access

THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: ENSEMBLE SPECTROSCOPIC VARIABILITY OF QUASAR BROAD EMISSION LINES

Mouyuan Sun, Jonathan R Trump, Yue Shen, W. N Brandt, Kyle Dawson, Kelly D Denney, Patrick B Hall, Luis C Ho, Keith Horne, Linhua Jiang, …
The Astrophysical journal, v 811(1), pp 1-19
17 Sep 2015
DOI: https://doi.org/10.1088/0004-637X/811/1/42
url
https://doi.org/10.1088/0004-637x/811/1/42View
Published, Version of Record (VoR)Open Access (License Unspecified),  Open
url
https://doi.org/10.1088/0004-637X/811/1/42View
Published, Version of Record (VoR) Open

Abstract

black hole physics galaxies: active quasars: emission lines quasars: general surveys
ABSTRACT We explore the variability of quasars in the Mg ii and broad emission lines and ultraviolet/optical continuum emission using the Sloan Digital Sky Survey Reverberation Mapping project (SDSS-RM). This is the largest spectroscopic study of quasar variability to date: our study includes 29 spectroscopic epochs from SDSS-RM over 6 months, containing 357 quasars with Mg ii and 41 quasars with . On longer timescales, the study is also supplemented with two-epoch data from SDSS-I/II. The SDSS-I/II data include an additional 2854 quasars with Mg ii and 572 quasars with . The Mg ii emission line is significantly variable ( on ∼100-day timescales), a necessary prerequisite for its use for reverberation mapping studies. The data also confirm that continuum variability increases with timescale and decreases with luminosity, and the continuum light curves are consistent with a damped random-walk model on rest-frame timescales of days. We compare the emission-line and continuum variability to investigate the structure of the broad-line region. Broad-line variability shows a shallower increase with timescale compared to the continuum emission, demonstrating that the broad-line transfer function is not a δ-function. is more variable than Mg ii (roughly by a factor of ∼1.5), suggesting different excitation mechanisms, optical depths and/or geometrical configuration for each emission line. The ensemble spectroscopic variability measurements enabled by the SDSS-RM project have important consequences for future studies of reverberation mapping and black hole mass estimation of quasars.

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