Spectroscopy of giants in LMC clusters. III - Velocities and abundances for NGC 1841 and Reticulum and the properties of the metal-poor clusters

Details Spectroscopy of giants in LMC clusters. III - Velocities and abundances for NGC 1841 and Reticulum and the properties of the metal-poor clusters Spectroscopy of giants in LMC clusters. III - Velocities and abundances for NGC 1841 and Reticulum and the properties of the metal-poor clusters

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aj....104.1743s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 104, no. 5, p. 1743-1764.

Astronomy and Astrophysics

Astronomy

71

Giant Stars, Globular Clusters, Magellanic Clouds, Metallicity, Stellar Motions, Stellar Spectra, Abundance, Luminosity, Stellar Mass

Scientific paper

Giant stars candidates have been observed in the red clusters NGC 1841 and Reticulum near the LMC. The velocity of the former is found to be 212.5 +/- 1.8 km/s for the former and 241.5 +/- 1.5 km/s for the latter, clearly indicating that these two clusters are distant members of the LMC. Spectra are used to measure very accurate abundances based on the calcium II infrared triplet line strengths. Both clusters are found to be metal-poor, with (Fe/H) = -1.71 for Reticulum and (Fe/H) = -2.11 for NGC 1841, with a dispersion of 0.06 dex relative to the calibrating clusters. Estimates of the intrinsic velocity dispersions, masses, and M/L(V) are derived for the objects which are consistent with populations and mass functions similar to Galactic globular clusters. The abundance and absolute magnitude estimates for the 13 known Population II clusters are used to show that the mean abundance of the LMC clusters is about 0.3 dex more metal-poor than the ensemble average for the entire Galactic globular cluster population.

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