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The stellar populations in the central parsecs of galactic bulges

Published online by Cambridge University Press:  24 November 2004

Marc Sarzi
Affiliation:
University of Oxford, Astrophysics, Keble Road, OX13RH Oxford, UK email: [email protected]
H.-W. Rix
Affiliation:
University of Oxford, Astrophysics, Keble Road, OX13RH Oxford, UK email: [email protected]
J. C. Shields
Affiliation:
University of Oxford, Astrophysics, Keble Road, OX13RH Oxford, UK email: [email protected]
L. C. Ho
Affiliation:
University of Oxford, Astrophysics, Keble Road, OX13RH Oxford, UK email: [email protected]
A. J. Barth
Affiliation:
University of Oxford, Astrophysics, Keble Road, OX13RH Oxford, UK email: [email protected]
G. Rudnick
Affiliation:
University of Oxford, Astrophysics, Keble Road, OX13RH Oxford, UK email: [email protected]
A. V. Filippenko
Affiliation:
University of Oxford, Astrophysics, Keble Road, OX13RH Oxford, UK email: [email protected]
W. L. W. Sargent
Affiliation:
University of Oxford, Astrophysics, Keble Road, OX13RH Oxford, UK email: [email protected]
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Abstract

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We present the analysis of Hubble Space Telescope blue spectra at intermediate spectral resolution for the nuclei of 23 nearby disk galaxies. These objects were selected to have nebular emission in their nuclei, and span a range of emission-line classifications as well as Hubble types. Here we focus on the stellar population as revealed by the continuum spectral energy distribution measured within the central 0.″13 (∼8 pc) of these galaxies. The data were modeled with linear combinations of single-age stellar population synthesis models. The large majority (∼80%) of the surveyed nuclei have spectra whose features are consistent with a predominantly old ($\gtrsim 5 \times 10^9$ yr) stellar population. Approximately 25% of these nuclei show evidence of a component with age younger than 1 Gyr, with the incidence of these stars related to the nebular classification. Successful model fits imply an average reddening corresponding to AV∼0.4 mag and stellar metallicity of (1–2.5)$Z_\odot$. Our findings reinforce the picture wherein Seyfert nuclei and the majority of low-ionization nuclear emission-line regions (LINERs) are predominantly accretion-powered, and suggest that much of the central star formation in HII nuclei is actually circumnuclear.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
ORAL CONTRIBUTIONS
Copyright
© 2004 International Astronomical Union