Chemical Abundances and Kinematics of the Stellar Populations of M33

Details Chemical Abundances and Kinematics of the Stellar Populations of M33 Chemical Abundances and Kinematics of the Stellar Populations of M33

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...206.1311h&link_type=abstract

American Astronomical Society Meeting 206, #13.11; Bulletin of the American Astronomical Society, Vol. 37, p.791

Astronomy and Astrophysics

Astronomy

Scientific paper

Our goal is to quantify the kinematics and chemical abundances of the stellar populations (thin disk and thick disk and/or halo) of the nearby spiral galaxy M33. M33 is unique in that it is a low luminosity (Mv=-19 mag, Lv=5 * 109 Lo) galaxy with a point-like nucleus and no bulge. Photometry from Ferguson et al. (2005, in preparation) suggests M33 is a pure disk galaxy, but the high velocity dispersion of globular clusters suggests the existence of a thick disk or halo (Chandar et al. 2002). We are using the DEIMOS spectrograph at the Keck II 10-meter telescope to obtain spectra surrounding the Ca II near-infrared triplet lines for approximately 2000 individual red giant stars throughout M33's disk and halo. We will present our initial radial velocity data from approximately 20% of our expected sample. From the spectra we expect to measure the radial velocities and chemical abundances of the stars with typical 1-sigma random errors of 15 km/s and 0.12 dex, respectively. We will make use of photometric observations we have made with the narrow-band DDO51 filter at the Kitt Peak 4-meter telescope to separate foreground Milky Way dwarf stars from M33 red giants, as M33's small (negative) radial velocity (-179 km/s) renders membership determination from velocity alone impossible. The large number of spectra in this project will allow for determination of the fraction of stars in each galactic component, based on kinematics.
We gratefully acknowledge financial support from grant NSF AST-0307863 to Tammy Smecker-Hane.

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