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Connection between dynamically derived IMF normalisation and stellar population parameters

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arxiv 1408.3189 v1 pith:52MTWJZI submitted 2014-08-14 astro-ph.GA

Richard M. McDermid , Michele Cappellari , Katherine Alatalo , Estelle Bayet , Leo Blitz , Maxime Bois , Frederic Bournaud , Martin Bureau
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Alison F. Crocker Roger L. Davies Timothy A. Davis P. T. de Zeeuw Pierre-Alain Duc Eric Emsellem Sadegh Khochfar Davor Krajnovic Harald Kuntschner Raffaella Morganti Thorsten Naab Tom Oosterloo Marc Sarzi Nicholas Scott Paolo Serra Anne-Marie Weijmans Lisa M. Young
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We report on empirical trends between the dynamically determined stellar initial mass function (IMF) and stellar population properties for a complete, volume-limited sample of 260 early-type galaxies from the Atlas3D project. We study trends between our dynamically-derived IMF normalisation and absorption line strengths, and interpret these via single stellar population- (SSP-) equivalent ages, abundance ratios (measured as [alpha/Fe]), and total metallicity, [Z/H]. We find that old and alpha-enhanced galaxies tend to have on average heavier (Salpeter-like) mass normalisation of the IMF, but stellar population does not appear to be a good predictor of the IMF, with a large range of normalisation at a given population parameter. As a result, we find weak IMF-[alpha/Fe] and IMF-age correlations, and no significant IMF-[Z/H] correlation. The observed trends appear significantly weaker than those reported in studies that measure the IMF normalisation via low-mass star demographics inferred through stellar spectral analysis.

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Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Hector Galaxy Survey: Linking the low- and high-mass ends of the initial mass function in star-forming galaxies

    astro-ph.GA 2026-06 unverdicted novelty 7.0 of 10

    Simultaneous measurement of low- and high-mass IMF slopes in 214 star-forming galaxies reveals diversity, weak correlation between ends, and links to stellar mass, star formation rate, and metallicity.

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