NOAO > Observing Info > Approved Programs > 2011A-0609
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NOAO > Observing Info > Approved Programs > 2011A-0609 |
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PI: Paco Najarro, Center of Astrobiology, CAB, CSIC-INTA, Spain, najarro@damir.iem.csic.es
Address: Spain
CoI: Donald Figer, Rochester Institute of Technology (CIS)
CoI: Tom Geballe, Gemini Observatory - North
CoI: Diego de la Fuente, Center of Astrobiology, CAB, CSIC, Spain
Title: Metallicity in the Quintuplet Cluster and the Galactic Center: Evidence for a top-heavy star formation history?
Abstract:
Massive star clusters are the breeding grounds for stars of all masses, and
the primary birthplaces of the most massive stars in galaxies. The Quintuplet
cluster, in our Galaxy, is one of the most massive resolved young clusters in
the Local Group and is a test bed for studying the star formation history of
the region and testing for a top-heavy star formation scenario by measuring
the alpha-elements and iron absolute abundances and their corresponding
ratios. We have recently developed two different techniques to derive
metallicity from infrared observations of LBVs and WR stars. For LBVs,
absolute alpha-elements (Si, Mg) and iron abundances may be obtained, while
for WRs it is possible to derive the alpha-element (oxygen) abundance of the
natal cloud. The Quintuplet cluster offers a unique site to obtain metal
abundances using such techniques. Thus, we propose to obtain near-infrared
GNIRS spectra of the high-mass stars in the Quintuplet cluster and isolated
massive stars in the inner Galactic Center region in order to extract stellar
properties, ages, and abundances and hence address the top heavy question.
National Optical Astronomy Observatory, 950 North Cherry Avenue, P.O. Box 26732, Tucson, Arizona 85726, Phone: (520) 318-8000, Fax: (520) 318-8360
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NOAO > Observing Info > Approved Programs > 2011A-0609 |
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