SCYON Abstract

Received on May 22 2002

Keck Spectroscopy of Globular Clusters in the Sombrero Galaxy

Authors	S. S. Larsen (¹), J. P. Brodie (¹), M. A. Beasley (²), D. A. Forbes (²)
Affiliation	(¹) UC Observatories / Lick Observatory, University of California, Santa Cruz, CA 95064, USA, (²) Astrophysics & Supercomputing, Swinburne University, Hawthorn VIC 3 122, Australia
Accepted by	Astronomical Journal
Contact	soeren@ucolick.org
URL	http://xxx.lanl.gov/abs/astro-ph/0204420
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Abstract

We analyze high signal-to-noise spectra for 14 globular clusters (GCs) in the Sombrero galaxy, NGC 4594 = M104, obtained with the LRIS spectrograph on the Keck I telescope. We find generally good agreement between spectroscopic metallicities and previous photometric metallicities based on V-I colors. Further, we use measurements of various Balmer line indices on co-added spectra of metal-poor and metal-rich GCs to estimate ages for the GC subpopulations and find ages of 10-15 Gyrs, with preferred ages around 11-12 Gyrs and no detectable differences between the metal-rich and metal-poor subpopulations. However, because of model and measurement uncertainties, age differences of a few (2-3) Gyrs cannot be ruled out. We also measure alpha to iron abundance ratios from Mg and TiO features and find enhancements on the order of [alpha/Fe] = +0.4, similar to the [alpha/Fe] abundance ratios observed in other old stellar populations. Finally, we combine our sample with radial velocities for 34 GCs from Bridges et al (1997) and obtain virial and projected masses for the Sombrero of M_VT = (8.1 ± 1.8) x 10¹¹ Msun and M_P = (5.3 ± 1.0) x 10¹¹ Msun within 17 kpc, respectively. Using 12 clusters within the central 4.5 kpc the corresponding numbers are M_VT = (2.1 ± 1.1) x 10¹¹ Msun and M_P = (2.0 ± 1.3) x 10¹¹ Msun.