A new visual - near-infrared diagnostic to estimate the metallicity of cluster and field dwarf stars

被引：35
|
作者：
Calamida, A. [1 ]
Monelli, M. [2 ,3 ]
Milone, A. P. [2 ,3 ]
Bono, G. [4 ]
Pietrinferni, A. [5 ]
Lagioia, E. P. [4 ]
机构：
[1] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy
[2] Inst Astrofis Canarias, Tenerife 38200, Spain
[3] Univ La Laguna, Dept Astrophys, Tenerife 38200, Spain
[4] Univ Roma Tor Vergata, I-00133 Rome, Italy
[5] Osservatorio Astron Collurania, INAF, I-64100 Teramo, Italy
来源：
ASTRONOMY & ASTROPHYSICS | 2012年 / 544卷
关键词：
stars: abundances; stars: evolution; stars: Population II; stars: low-mass; UVBY-BETA PHOTOMETRY; METAL-POOR STARS; STELLAR EVOLUTION DATABASE; GALACTIC GLOBULAR-CLUSTERS; GENEVA-COPENHAGEN SURVEY; F-TYPE STARS; STROMGREN PHOTOMETRY; SOLAR NEIGHBORHOOD; MODEL ATMOSPHERES; HIGH-VELOCITY;
D O I：
10.1051/0004-6361/201219712
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present a theoretical calibration of a new metallicity diagnostic based on the Stromgren index m(1) and on visual - near-infrared (NIR) colors to estimate the global metal abundance of cluster and field dwarf stars. To perform the metallicity calibration we adopt alpha-enhanced evolutionary models transformed into the observational plane by using atmosphere models computed adopting the same chemical mixture. We apply the new visual-NIR metallicity-index-color (MIC) relations to two different samples of field dwarfs and we find that the difference between photometric estimates and spectroscopic measurements is on average smaller than 0.1 dex, with a dispersion smaller than sigma = 0.3 dex. We apply the same MIC relations to a metal-poor (M 92) and a metal-rich (47 Tuc) globular cluster. We find a peak of -2.01 +/- 0.08 (sigma = 0.30 dex) and -0.47 +/- 0.01 (sigma = 0.42 dex), respectively.
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页数：11
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