MULTI-ELEMENT ABUNDANCE MEASUREMENTS FROM MEDIUM-RESOLUTION SPECTRA. II. CATALOG OF STARS IN MILKY WAY DWARF SATELLITE GALAXIES

By E. Kirby, P. Guhathakurta, J. Simon, M. Geha, C. Rockosi, C. Sneden, J. Cohen, S. Sohn, S. Majewski, M. Siegel. 2010

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We present a catalog of Fe, Mg, Si, Ca, and Ti abundances for 2961 stars in eight dwarf satellite galaxies of the Milky Way (MW): Sculptor, Fornax, Leo I, Sextans, Leo II, Canes Venatici I, Ursa Minor, and Draco. For the purposes of validating our measurements, we also observed 445 red giants in MW globular clusters and 21 field red giants in the MW halo. The measurements are based on Keck/DEIMOS medium-resolution spectroscopy (MRS) combined with spectral synthesis. We estimate uncertainties in [Fe/H] by quantifying the dispersion of [Fe/H] measurements in a sample of stars in monometallic globular clusters (GCs). We estimate uncertainties in Mg, Si, Ca, and Ti abundances by comparing to high-resolution spectroscopic abundances of the same stars. For this purpose, a sample of 132 stars with published high-resolution spectroscopy in GCs, the MW halo field, and dwarf galaxies has been observed with MRS. The standard deviations of the differences in [Fe/H] and 〈[α/Fe]〉 (the average of [Mg/Fe], [Si/Fe], [Ca/Fe], and [Ti/Fe]) between the two samples is 0.15 and 0.16, respectively. This catalog represents the largest sample of multi-element abundances in dwarf galaxies to date. The next papers in this series draw conclusions on the chemical evolution, gas dynamics, and star formation histories from the catalog presented here. The wide range of dwarf galaxy luminosity reveals the dependence of dwarf galaxy chemical evolution on galaxy stellar mass.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c0c0d36677fbc7cf641fafe1f6d2d859539cb3f4

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Citations in the corpus

THE UNIVERSAL STELLAR MASS–STELLAR METALLICITY RELATION FOR DWARF GALAXIES (2013, methodology): “The measurements also differ in many other ways, such as the method of taking the average (averaging individual stars versus light-weighted mean), the stellar population probed (red giants versus the entire stellar population), and the models used (Kirby et al. 2010 versus Bruzual & Charlot 2003).”
THE QUENCHING OF THE ULTRA-FAINT DWARF GALAXIES IN THE REIONIZATION ERA (2014, methodology): “We refer the reader to Kirby et al. (2010) and Vargas et al. (2013) for an in-depth description of the analysis.”
MULTI-ELEMENT ABUNDANCE MEASUREMENTS FROM MEDIUM-RESOLUTION SPECTRA. III. METALLICITY DISTRIBUTIONS OF MILKY WAY DWARF SATELLITE GALAXIES (2010, methodology): “We use the [Fe/H] measurements for individual stars in eight MW dSphs from Paper II (Kirby et al. 2010b).”
The star formation and chemical evolution history of the Fornax dwarf spheroidal galaxy (2012, methodology): “2c shows that the [Mg/Fe] derived for the highest signal-to-noise ratio (S/N) measurements from Kirby et al. (2010) are consistent with those determined from the HR spectroscopy of Letarte et al. (2010).”
Gaia DR2 proper motions of dwarf galaxies within 420 kpc (2018, unknown): “We use the catalog of Kirby et al. (2010).”
Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph (2012, methodology): “…medium-resolution survey atR = 5, 000 will yield stellar spectra similar to those provided by the Keck/DEIMOS instrument, with which we have sufficient experience and well-calibrated techniques to measure multi-elementα abundances and quantify their uncertainties (Kirby et al. 2008, 2010).”
A COMPLETE SPECTROSCOPIC SURVEY OF THE MILKY WAY SATELLITE SEGUE 1: THE DARKEST GALAXY (2010, methodology): “Nevertheless, experiments with globular cluster stars reaching several magnitudes below the main sequence turnoff from the compilation of Kirby et al. (2010) show that while W ′ does increase at constant metallicity toward fainter main sequence magnitudes, this increase is less than 2 Å for stars…”
The hidden giant: discovery of an enormous Galactic dwarf satellite in Gaia DR2 (2018, methodology): “Accordingly, for comparison we overplot the metallicity distributions of a couple of classical dwarf spheroidal galaxies (Leo II and Fornax) from Kirby et al. (2010), whose overall metallicities and MDF shapes are not dissimilar to those of Ant 2.”