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Spectroscopy of Red Giants of the Sagittarius Dwarf Galaxy

Published online by Cambridge University Press:  25 May 2016

G. Marconi ,
P. Bonifacio ,
L. Pasquini  and
P. Molaro
G. Marconi
Affiliation:
Osservatorio Astronomico di Roma
P. Bonifacio
Affiliation:
Osservatorio Astronomico di Trieste
L. Pasquini
Affiliation:
European Southern Observatory
P. Molaro
Affiliation:
Osservatorio Astronomico di Trieste

Abstract

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The photometric study of the Sagittarius dwarf galaxy by Marconi et al. (1998) has suggested the presence of a spread in metallicity (-0.7 ≤ [Fe/H] ≤ −1.6), which may result from different bursts of star formation. We present the results from a Multi Object Slit spectroscopy program carried out at the NTT with the aim to determine spectroscopic abundances of Sagittarius giants selected from the CCD photometry. From our intermediate resolution (R~1500) spectra, radial velocities are determined to confirm the membership and metallicities are derived by using spectral synthesis codes for stars down to V ~ 18, i.e. below the RGB clump. Out of 57 observed stars, 23 have a radial velocity consistent with Sagittarius membership; here we present results for 8 of these. No star with [Fe/H]< −1.0 is found, three stars are found to be metal-rich.

Type
Part 2: The Database
Information
Symposium - International Astronomical Union , Volume 192: The Stellar Content of Local Group Galaxies , 1999 , pp. 129 - 135
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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