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A photometric and spectroscopic study of the new dwarf spheroidal galaxy in Hercules Metallicity, velocities, and a clean list of RGB members

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journal contribution
posted on 24.10.2012, 09:15 by D. Aden, S. Feltzing, A. Koch, M. I. Wilkinson, E. K. Grebel, I. Lundstrom, G. F. Gilmore, D. B. Zucker, V. Belokurov, N. W. Evans, D. Faria
Context. Dwarf spheroidal (dSph) galaxies are the least luminous, least massive galaxies known. Recently, the number of observed galaxies in this class has greatly increased thanks to large surveys. Determining their properties, such as mass, luminosity and metallicity, provides key information in our understanding of galaxy formation and evolution. Aims. Our aim is to provide as clean and as complete a sample as possible of red giant branch stars that are members of the Hercules dSph galaxy. With this sample we explore the velocity dispersion and the metallicity of the system. Methods. Strömgren photometry and multi-fibre spectroscopy are combined to provide information about the evolutionary state of the stars (via the Strömgren c1 index) and their radial velocities. Based on this information we have selected a clean sample of red giant branch stars, and show that foreground contamination by Milky Way dwarf stars can greatly distort the results. Results. Our final sample consists of 28 red giant branch stars in the Hercules dSph galaxy. Based on these stars we find a mean photometric metallicity of $-2.35 \pm 0.31$ dex which is consistent with previous studies. We find evidence for an abundance spread. Using those stars for which we have determined radial velocities we find a systemic velocity of $45.20 \pm 1.09 {\rm\, km\, s^{-1}}$ with a dispersion of 3.72 km s-1, this is lower than values found in the literature. Furthermore we identify the horizontal branch and estimate the mean magnitude of the horizontal branch of the Hercules dSph galaxy to be $V_0=21.17 \pm 0.05$, which corresponds to a distance of 147+8-7 kpc. Conclusions. When studying sparsely populated and/or heavily foreground contaminated dSph galaxies it is necessary to include knowledge about the evolutionary stage of the stars. This can be done in several ways. Here we have explored the power of the $c_{{\rm 1}}$ index in Strömgren photometry. This index is able to clearly identify red giant branch stars redder than the horizontal branch, enabling a separation of red giant branch dSph stars and foreground dwarf stars. Additionally, this index is also capable of correctly identifying both red and blue horizontal branch stars. We have shown that a proper cleaning of the sample results in a smaller value for the velocity dispersion of the system. This has implications for galaxy properties derived from such velocity dispersions.

History

Citation

Astronomy & Astrophysics, 2009, 506 (3), pp. 1147-1168

Version

VoR (Version of Record)

Published in

Astronomy & Astrophysics

Publisher

EDP Sciences for European Southern Observatory (ESO)

issn

0004-6361

Copyright date

2009

Available date

24/10/2012

Publisher version

http://www.aanda.org/articles/aa/abs/2009/42/aa12718-09/aa12718-09.html

Language

English