Stellar velocity dispersions in AGN – II: Methods

• Published in: Proceedings of the International Astronomical Union 2004-03, Vol.2004 (IAUS222), p.153-154
• Main Authors: Asari, Natalia Vale, Garcia-Rissmann, Aurea, Neme, Luis Rodolfo Vega, Fernandes, Roberto Cid
• Format: Article
• Language: English
• ISSN: 1743-9213; 1743-9221
• DOI: 10.1017/S1743921304001802

Stellar velocity dispersions in AGN are useful indicators of the black-hole mass (through the M[bull ]−σ[sstarf ] relation) and nuclear stellar populations (through the M/L ratio). We have collected near-infrared spectra of ∼40 Seyferts in the CaII triplet range in order to measure σ[sstarf ] and investigate the connection between stellar populations and AGN properties. In this poster we present a comparison between two methods to measure velocity dispersions: (1) direct fitting (DFM) and (2) cross-correlation (CCM). (1) In DFM the spectra in the CaII triplet range is modeled as a combination of a broadened and shifted stellar spectrum (observed through the same instrumental setup) and a featureless continuum. This method has the advantage of making it easy to mask out noisy regions and sky residuals. (2) CCM converts the width of the star-galaxy cross-correlation function onto a velocity dispersion. We find that these methods yield velocity dispersions consistent to within 20 km s−1 on-average. Our results are consistent to within 20 km s−1 with those objects available in the literature.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html