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REU 2016: Quasar Imaging Papers

The Big Picture (what are quasars and how do we find them)
Selecting quasars for SDSS-I/II (Richards et al. 2002)
Selecting quasars for SDSS-III (Ross et al. 2012)
Selecting quasars for SDSS-IV (Myers et al. 2015)
The largest catalog of spectroscopically confirmed quasars to date (Paris et al. 2018)
An orientation-based model for low-luminosity, low-redshift quasars (Antonucci 1993)
An improved such model (Elvis 2000)
Evolution is critical for understanding quasars in a cosmological context (Hopkins et al. 2006)
A fairly recent review of the menagerie of AGN and what drives them (Alexander & Hickox 2012)

Classics (quasar evolution and clustering)
Accretion disks around black holes can power AGN (Shakura & Sunyaev 1973)
Most massive galaxies must contain a dead black hole (Lynden-Bell 1969)
Active quasars must have evolved into dead black holes (Soltan 1982)
Quasars are an evolutionary stage in a galaxy's life (Sanders et al. 1988)
Direct observations of dormant black holes in local galaxies (Magorrian et al. 1998)
The M-sigma relation (Ferrarese & Merritt 2000)
The M-sigma relation (Gebhardt et al. 2000)
Detection of the Baryon Acoustic Oscillation in galaxy clustering (Eisenstein et al. 2005)

z ~ 6 quasars
Where it all began (selecting z~6 quasars and completeness of selection)
Pioneering tests for reionization
Highest redshift quasar (focuses on reionization)
Intervening absorbers (metal poor gas)
Huge black hole mass at z>6

Photometric Calibration Using SDSS Point Sources
SDSS Stripe 82
The SDSS Stripe 82 Standard Star Catalog

Characterizing Quasar Variability
Quasar variability and the structure function
A turn-over in the structure function?
Measurements of SDSS quasar variability on ~2-year timescales
Characterizing quasar variability as a Damped Random Walk via (σ,τ)
Characterizing quasar variability as a Damped Random Walk on ~7 year time scales
AGN variability may not be a Damped Random Walk on all scales

Finding Quasars Behind Local Galaxies
Optical colors of quasars in the SDSS ugriz system
Targeting quasars using variability via GCL
Color Selection of Quasars (optical+mid-IR)
Variability selection of quasars via (A,γ) from a structure function model (note that this paper has an Erratum)
Mid-IR-selected AGN behind the Magellanic Clouds
Variability-selected quasars behind the Magellanic Clouds
Quasars behind M31 and M33
Using Quasar spectra to trace gas features in M31

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