Dwarf galaxies in the Coma cluster – I. Velocity dispersion measurements
Article first published online: 10 FEB 2012
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
Monthly Notices of the Royal Astronomical Society
Volume 420, Issue 4, pages 2819–2834, March 2012
How to Cite
Kourkchi, E., Khosroshahi, H. G., Carter, D., Karick, A. M., Mármol-Queraltó, E., Chiboucas, K., Tully, R. B., Mobasher, B., Guzmán, R., Matković, A. and Gruel, N. (2012), Dwarf galaxies in the Coma cluster – I. Velocity dispersion measurements. Monthly Notices of the Royal Astronomical Society, 420: 2819–2834. doi: 10.1111/j.1365-2966.2011.19899.x
- Issue published online: 1 MAR 2012
- Article first published online: 10 FEB 2012
- Accepted 2011 September 27. Received 2011 September 13; in original form 2010 December 18
- galaxies: clusters: individual: Coma;
- galaxies: dwarf;
- galaxies: elliptical and lenticular, cD;
- galaxies: evolution;
- galaxies: fundamental parameters;
- galaxies: kinematics and dynamics
We present the study of a large sample of early-type dwarf galaxies in the Coma cluster observed with DEIMOS on the Keck II to determine their internal velocity dispersion. We focus on a subsample of 41 member dwarf elliptical galaxies for which the velocity dispersion can be reliably measured, 26 of which were studied for the first time. The magnitude range of our sample is −21 < MR < −15 mag.
This paper (Paper I) focuses on the measurement of the velocity dispersion and their error estimates. The measurements were performed using penalized pixel fitting (ppxf) and using the calcium triplet absorption lines. We use Monte Carlo bootstrapping to study various sources of uncertainty in our measurements, namely statistical uncertainty, template mismatch and other systematics. We find that the main source of uncertainty is the template mismatch effect which is reduced by using templates with a range of spectral types.
Combining our measurements with those from the literature, we study the Faber–Jackson relation (L∝σα) and find that the slope of the relation is α= 1.99 ± 0.14 for galaxies brighter than MR≃−16 mag. A comprehensive analysis of the results combined with the photometric properties of these galaxies is reported in Paper II.