A Local Baseline for the Black Hole Mass Scaling Relations for Active Galaxies. II. Stellar Kinematics: Results and Practical Guidelines for Future Studies

Details A Local Baseline for the Black Hole Mass Scaling Relations for Active Galaxies. II. Stellar Kinematics: Results and Practical Guidelines for Future Studies A Local Baseline for the Black Hole Mass Scaling Relations for Active Galaxies. II. Stellar Kinematics: Results and Practical Guidelines for Future Studies

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21924609h&link_type=abstract

American Astronomical Society, AAS Meeting #219, #246.09

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the latest results from an ongoing comprehensive survey of 113 local type-1 AGN selected from the SDSS database. The goal is to obtain a more accurate measurement of the slope, intercept, and scatter correlations of the between central black hole mass and host bulge luminosity and stellar velocity dispersion. To meet this goal we collected at the Keck Telescope high signal to noise ratio and spatially resolved long slit spectra, suitable to measure rotation curves and bulge dispersion profiles. In addition to improving the calibration of the local correlations by reducing uncertainties in host galaxy properties, a main goal of our program is to apply what we learn in the local universe to minimize systematic uncertainties in the study of their cosmic evolution. Results from a pilot study are given in paper I (Bennert et al. 2011).
We present here the full spectroscopic sample and stellar kinematics measurements, which are challenging owing to the presence of AGN emission. To produce the most accurate measurements and investigate potential biases, we focus on three different spectroscopic regions, including the strong stellar features: CaHK, MgIb, and CaII IR triplet. We achieve the following goals: (1) cross-calibrate the three spectroscopic regions, using the Ca triplet as a benchmark; (2) determine the reliability of each region as a function of S/N ; (3) determine the reliability of the regions when various strong stellar absorption features are excluded from a given region; and (4) estimate the success rate of measuring sigma_stellar from the Ca H+K region based on simple parameters available for many target candidates in the SDSS survey catalogue. We investigate each issue both as a function of offset from galactic center and also for synthetic spatially unresolved spectroscopy, mimicking what would be observed in the SDSS-fibers or for high redshift sources.

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