2012
DOI: 10.1051/0004-6361/201219712
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A new visual – near-infrared diagnostic to estimate the metallicity of cluster and field dwarf stars

Abstract: We present a theoretical calibration of a new metallicity diagnostic based on the Strömgren 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 α-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 dwar… Show more

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Cited by 5 publications
(13 citation statements)
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“…Unfortunately, we do not have an α-enhancement abundance measurement for our field star sample, but only an estimate of the α-enhancement proxy, that is [α/Fe] ≈ [Ca/Fe], for 12 out of the 61 RGs, with a median value of [α/Fe] = 0.35, and a dispersion of 0.08 dex. It is worth mentioning that we found a similar shift, ≈−0.1 dex, when we adopted the visual-NIR α-enhanced MIC relations to estimate photometric metallicities of field dwarfs in Calamida et al (2012). When we assumed an α-enhancement of 0.2 for the stars without the [α/Fe] spectroscopic estimate, we found a very good agreement between spectroscopic and photometric abundance estimates.…”
Section: × E(b-y ) (Ca07) and E(y − J) = 223 × E(b−v) E(y−h) = 256supporting
confidence: 75%
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“…Unfortunately, we do not have an α-enhancement abundance measurement for our field star sample, but only an estimate of the α-enhancement proxy, that is [α/Fe] ≈ [Ca/Fe], for 12 out of the 61 RGs, with a median value of [α/Fe] = 0.35, and a dispersion of 0.08 dex. It is worth mentioning that we found a similar shift, ≈−0.1 dex, when we adopted the visual-NIR α-enhanced MIC relations to estimate photometric metallicities of field dwarfs in Calamida et al (2012). When we assumed an α-enhancement of 0.2 for the stars without the [α/Fe] spectroscopic estimate, we found a very good agreement between spectroscopic and photometric abundance estimates.…”
Section: × E(b-y ) (Ca07) and E(y − J) = 223 × E(b−v) E(y−h) = 256supporting
confidence: 75%
“…The residual spread is caused by the effect of CN/CH/NH molecular bands on the m 1 index; M 92 shows the typical variations in [C/Fe] and [N/Fe] (Langer et al 1986;Bellman et al 2001) together with the typical anticorrelations of most GGCs (Pilachowski et al 1983;Sneden et al 1991;Kraft 1994). We also found a similar effect when applying the visual-NIR metallicity calibration to M 92 MS stars (Calamida et al 2012).…”
Section: Using Cluster Data Brings Three Indisputable Advantagessupporting
confidence: 69%
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“…We used the m 1 vs. b−y, m 1 vs. v−y, V vs. b−y, and V vs. v − y diagrams as discriminators between giant, subgiant, and dwarf stars (thus weeding out foreground stars) to select RGB stars in stellar populations (Faria 2007;Arnadottir 2010;Calamida et al 2012Calamida et al , 2014. We contrained our search to RGB stars located inside the cluster radii estimated by Piatti & Mackey (2018), and brighter that the respective cluster horizontal branch (Frank et al 2015).…”
Section: Metallicity Estimatesmentioning
confidence: 99%