The Stellar Initial Mass Function in Early-Type Galaxies From Absorption Line Spectroscopy. II. Results

TL;DR

This study uses advanced spectral modeling to analyze early-type galaxy spectra, revealing that the stellar initial mass function becomes more bottom-heavy with higher velocity dispersion and metallicity, aligning with dynamical constraints.

Contribution

Introduces a new population synthesis model accounting for variable element abundances to constrain the IMF in early-type galaxies using high-quality spectra.

Findings

IMF becomes more bottom-heavy with increasing velocity dispersion.

Derived stellar mass-to-light ratios align with dynamical measurements.

Globular cluster spectra suggest fewer low-mass stars than a Milky Way IMF.

Abstract

The spectral absorption lines in early-type galaxies contain a wealth of information regarding the detailed abundance pattern, star formation history, and stellar initial mass function (IMF) of the underlying stellar population. Using our new population synthesis model that accounts for the effect of variable abundance ratios of 11 elements, we analyze very high quality absorption line spectra of 38 early-type galaxies and the nuclear bulge of M31. These data extend to 1um and they therefore include the IMF-sensitive spectral features NaI, CaII, and FeH at 0.82um, 0.86um and 0.99um, respectively. The models fit the data well, with typical rms residuals ~1%. Strong constraints on the IMF and therefore the stellar mass-to-light ratio, (M/L)_stars, are derived for individual galaxies. We find that the IMF becomes increasingly bottom-heavy with increasing velocity dispersion and [Mg/Fe]. At the lowest dispersions and [Mg/Fe] values the derived IMF is consistent with the Milky Way IMF, while at the highest dispersions and [Mg/Fe] values the derived IMF contains more low-mass stars (is more bottom-heavy) than even a Salpeter IMF. Our best-fit (M/L)_stars values do not exceed dynamically-based M/L values. We also apply our models to stacked spectra of four metal-rich globular clusters in M31 and find an (M/L)_stars that implies fewer low-mass stars than a Milky Way IMF, again agreeing with dynamical constraints. We discuss other possible explanations for the observed trends and conclude that variation in the IMF is the simplest and most plausible.