2012/03/09 by Jesse Rogerson, Jesse A. Rogerson, Rogerson, Jesse A. +8
Engineering · Mathematics · Physics and Astronomy · #Astronomical Observations and Instrumentation #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Statistical and numerical algorithms #astro-ph.CO
paper · pdf · doi:10.48550/arxiv.1203.2162
2 pages, 1 figure, The proceedings of the "AGN Winds in Charleston" meeting, Charleston, SC, 15-18 Oct 2011. To be published by ASP
arxiv created 2012/03/09 · openalex publication_date 2012/03/09 · arxiv updated 2012/03/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Broad Absorption Line (BAL) trough variability is predominantly due to cloud motion transverse to our line of sight. The rate at which the variability occurs indicates the velocity of the cloud, which can provide constraints on the cloud's distance from the central source. This requires detailed spectroscopy during a variability event. Such spectra have proven elusive, suggesting either the timescale of variability is too short to be caught, or too long to notice until a sufficient amount of time has passed. Photometric monitoring of BAL quasar colours may potentially be used as an early warning system to trigger time resolved spectroscopic monitoring of BAL variability. Towards this end, we are analyzing both BAL and non-BAL colour variability using time series photometry from Stripe 82 in the Sloan Digital Sky Survey.