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The Nature of Galactic Bulges from SAURON Absorption Line Strength Maps

Published online by Cambridge University Press:  01 December 2006

Reynier F. Peletier ,
Jesús Falcón-Barroso ,
Katia Ganda ,
Roland Bacon ,
Michele Cappellari ,
Roger L. Davies ,
P. Tim de Zeeuw ,
Eric Emsellem ,
Davor Krajnović  and
Harald Kuntschner
...Show all authors
Reynier F. Peletier
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, NL-9700 AV Groningen email: peletier@astro.rug.nl
Jesús Falcón-Barroso
Affiliation:
European Space Agency/ESTEC, Keplerlaan 1, NL-2200 AG Noordwijk
Katia Ganda
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, NL-9700 AV Groningen email: peletier@astro.rug.nl
Roland Bacon
Affiliation:
Observatoire de Lyon, 9 av. Charles André, F-69230 Saint-Genis Laval
Michele Cappellari
Affiliation:
Sub-Department of Astrophysics, University of Oxford, Oxford OX1 3RH, UK
Roger L. Davies
Affiliation:
Sub-Department of Astrophysics, University of Oxford, Oxford OX1 3RH, UK
P. Tim de Zeeuw
Affiliation:
Sterrewacht Leiden, University of Leiden, NL-2333 CA Leiden
Eric Emsellem
Affiliation:
Observatoire de Lyon, 9 av. Charles André, F-69230 Saint-Genis Laval
Davor Krajnović
Affiliation:
Sub-Department of Astrophysics, University of Oxford, Oxford OX1 3RH, UK
Harald Kuntschner
Affiliation:
ST-ECF, European Southern Observatory, D-85748 Garching bei München
Richard M. McDermid
Affiliation:
Sterrewacht Leiden, University of Leiden, NL-2333 CA Leiden
Marc Sarzi
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire, Hatfield, UK
Glenn van de Ven
Affiliation:
Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA
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Abstract

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We discuss SAURON absorption line strength maps of a sample of 24 early-type spirals, mostly Sa. From the Lick indices Hβ, Mgb and Fe 5015 we derive SSP-ages and metallicities. By comparing the scaling relations of Mg b and Hβ and central velocity dispersion with the same relation for the edge-on sample of Falcón-Barroso et al. (2002) we derive a picture in which the central regions of Sa galaxies contain at least 2 components: one (or more) thin, disc-like component, often containing recent star formation, and another, elliptical-like component, consisting of old stars and rotating more slowly, dominating the light above the plane. If one defines a bulge to be the component responsible for the light in excess of the outer exponential disc, then many Sa-bulges are dominated by a thin, disc-like component containing recent star formation.

Keywords

galaxies: spiralgalaxies: stellar contentgalaxies: bulges
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 485 - 488
Copyright
Copyright © International Astronomical Union 2007

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