Characterizing the Stellar Population in NGC 1705-1
We observed the brightest super-star cluster NGC 1705-1 in the nearby dwarf galaxy NGC 1705 with the Space Telescope Imaging Spectrograph in the echelle mode between 1200 and 3100 Aa. The data allow a study of the young stellar population at hitherto unprecedented spectral resolution and signal-to-n...
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Published in | The Astrophysical journal Vol. 600; no. 1; pp. 162 - 181 |
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Main Authors | , , , , , , |
Format | Journal Article |
Language | English |
Published |
IOP Publishing
01.01.2004
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Online Access | Get full text |
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Summary: | We observed the brightest super-star cluster NGC 1705-1 in the nearby dwarf galaxy NGC 1705 with the Space Telescope Imaging Spectrograph in the echelle mode between 1200 and 3100 Aa. The data allow a study of the young stellar population at hitherto unprecedented spectral resolution and signal-to-noise ratios. A comprehensive list of strong and weak stellar and interstellar absorption lines is given, together with the measured line parameters. Four distinct velocity systems are identified: stellar lines at the measured H I velocity, blueshifted interstellar lines from outflowing gas, Milky Way foreground absorption, and a high-velocity cloud. Comparison with stellar template spectra indicates an equivalent spectral type of B0 to B1, with mostly dwarf and giant stars contributing. When placed on a theoretical Hertzsprung- Russell diagram, these stars constrain the age of NGC 1705-1 to 12 plus or minus [image] Myr. Since this age is derived purely from spectroscopy, it is independent of reddening corrections. A comparison of the observed and theoretical mass-to- light ratio for the derived age was performed. We find no significant evidence for an anomalous initial mass function at the low-mass end, contrary to suggestions found in the literature. The stellar population of NGC 1705-1 is similar to that in other massive clusters, such as 30 Doradus or NGC 1569-A, after taking into account age differences and model uncertainties. We discuss the difficulty of relating observed and theoretical mass-to-light ratios because of the unknown gas mass fraction lost by the cluster and the uncertain mass-loss rates of asymptotic giant branch stars in population synthesis models. |
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Bibliography: | ObjectType-Article-2 SourceType-Scholarly Journals-1 ObjectType-Feature-1 content type line 23 |
ISSN: | 0004-637X 1538-4357 |
DOI: | 10.1086/379805 |