SNAPSHOT METALLICITY ESTIMATE OF RESOLVED STELLAR SYSTEMS THROUGH LICK Fe5270 DIAGNOSTIC
- INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna (Italy)
- INAOE-Instituto Nacional de AstrofIsica Optica y Electronica, Luis Enrique Erro 1, 72840 Tonantzintla, Puebla (Mexico)
We outline a new method to derive a 'snapshot' metallicity estimate of stellar systems (providing one resolves at least the brightest part of the color-magnitude diagram) on the basis of low-resolution (i.e., 6-8 A FWHM) spectroscopy of a small stellar sample. Our method relies on the Fe5270 Lick index measurements and takes advantage of the special behavior of this spectral feature that reaches its maximum strength among the ubiquitous component of K-type giants. This makes the Fe5270{sub max} estimate a robust and model-independent tracer of cluster [Fe/H], being particularly insensitive to the age of the stellar population. A comparison of the Fe5270{sub max} distribution derived from globular and open clusters, as well as from the field giant population in the Galaxy disk, confirms a tight correlation of the index maximum versus cluster [Fe/H] over the entire metallicity range for a stellar population with [Fe/H] approx>-2.0. Relying on a theoretical calibration of the feature, we trust to infer effectively cluster metallicity within a typical uncertainty of 0.1-0.2 dex, depending on red giant branch (RGB) luminosity sampling of the observations. A handful of stars (5-10 objects) is required for the method to be applied, with low-metallicity stellar populations more easily managed, being Fe5270{sub max} located within the few brightest RGB stars of the system. In any case, we show that even the observation of a coarse stellar set would allow us to place a confident lower limit on cluster metallicity.
- OSTI ID:
- 21371881
- Journal Information:
- Astrophysical Journal (Online), Journal Name: Astrophysical Journal (Online) Journal Issue: 2 Vol. 703; ISSN 1538-4357
- Country of Publication:
- United States
- Language:
- English
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