J/A+A/561/A93 On the metallicity of open clusters. II. (Heiter+, 2014)
On the metallicity of open clusters. II. Spectroscopy.
Heiter U., Soubiran C., Netopil M., Paunzen E.
<Astron. Astrophys. 561, A93 (2014)>
=2014A&A...561A..93H 2014A&A...561A..93H
ADC_Keywords: Clusters, open ; Abundances, [Fe/H] ; Effective temperatures ;
Spectroscopy ; Cross identifications
Keywords: Galaxy: abundances - open clusters and associations: general -
stars: abundances
Abstract:
The literature was searched for [Fe/H] estimates of individual member
stars of open clusters (OCs) based on the analysis of high-resolution
spectra. The lower limit for spectral resolving power
(R=λ/Δλ) was set to 25000, and the lower limit for
signal-to-noise ratio was set to 50. We searched the PASTEL database
(2010A&A...515A.111S 2010A&A...515A.111S, Cat. B/pastel) and the recent literature for
such metallicity determinations in references posterior to 1990 and
until June 2013. Only stars with an effective temperature lower than
7000K were included to avoid rapid rotators and chemical
peculiarities. We eliminated confirmed non-members, spectroscopic
binaries, and chemically peculiar stars and kept only stars with a
high probability of membership. This resulted in a list of 571 stars
in 86 OCs, with 830 metallicity determinations from 94 papers, which
we call the starting sample.
Description:
In Table 1 we list the basic information for each star and each
metallicity determination in the starting sample, which should be
sufficient to extract the corresponding atmospheric parameters from
the PASTEL catalogue.
Table 4 lists the weighted mean metallicities for each OC and each
paper, which were computed using the metallicities from the references
in Table 1. For the weights we used the inverse square of the
individual errors quoted by the authors. Table 4 also gives the ranges
of effective temperature (Teff) and surface gravity (logg) of the
stars corresponding to each paper.
After removing all determinations with Teff outside the range 4400 to
6500K and with logg<2.0, we constructed a list of recommended
cluster metallicities, which we call the final high-resolution sample.
The weighted mean metallicities for each cluster in the final sample
are given in Table 11, and the individual determinations included in
the final sample are identified in Table 1 (first column).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 112 830 List of the full starting sample of cluster members
described in Sect. 2.1.
table4.dat 75 197 Weighted mean metallicity of OCs, computed for each
reference giving atmospheric parameters based on
high-resolution, high-S/N spectra
table11.dat 32 78 Weighted average metallicity and standard deviation
of OCs after restricting the Teff and logg ranges
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See also:
B/pastel : The PASTEL catalogue (Soubiran+, 2010-)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1 I1 --- Sample [1/2] Sample identification (1)
3- 14 A12 --- Cluster Cluster identification
24- 25 I2 h RAh ? Right ascension (J2000)
27- 28 I2 min RAm ? Right ascension (J2000)
30- 37 F8.5 s RAs ? Right ascension (J2000)
40 A1 --- DE- ? Declination sign
41- 42 I2 deg DEd ? Declination (J2000)
44- 45 I2 arcmin DEm ? Declination (J2000)
47- 53 F7.4 arcsec DEs ? Declination (J2000)
56- 61 F6.3 mag Vmag Magnitude (apparent) in V filter
64- 82 A19 --- BibCode Reference for metallicity (2)
84-112 A29 --- StarID Star identification (3)
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Note (1): Sample code as follows:
1 = measurements that are NOT included in the final high-resolution sample
2 = measurements that are included in the final high-resolution sample
Note (2): Bibcode of the article from which the metallicity determination was
taken.
Note (3): StarID is resolvable by Simbad, except for five stars in NGC 6791
measured by Geisler et al. (2012ApJ...756L..40G 2012ApJ...756L..40G), for which the numbers
from Stetson et al. (2003, Cat. J/PASP/115/413, SBG NNNNN), are given
as <Cl* NGC 6791 SBG NNNNN> in Simbad
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/86] Sequential number for open clusters
4- 15 A12 --- Cluster Cluster identification
23- 26 I4 K B_Teff Minimum value of the effective temperature
28- 31 I4 K b_Teff Maximum value of the effective temperature
33- 36 F4.2 [cm/s2] B_logg Minimum value of the surface gravity
38- 41 F4.2 [cm/s2] b_logg Maximum value of the surface gravity
43- 47 F5.2 [Sun] [Fe/H] Mean iron abundance relative to the Sun
49- 52 F4.2 [Sun] s_[Fe/H] ? Standard deviation of [Fe/H]
54- 55 I2 --- o_[Fe/H] Number of determinations (1)
57- 75 A19 --- BibCode Reference (2)
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Note (1): In most cases, the number of determinations corresponds to the number
of stars analysed in each reference. In the case of Santos et al.
(2009A&A...493..309S 2009A&A...493..309S) giant stars are counted twice because two different
line lists were used. In the cases of Tautvaisiene et al. (2000,
Cat. J/A+A/360/499) and Pasquini et al. (2004A&A...424..951P 2004A&A...424..951P), for three
of seven and three of 21 stars, respectively, two or three different spectra
were used. The resulting values were treated as independent determinations.
Note (2): Bibcode of the article from which the [Fe/H] determinations were
taken.
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/84] Sequential number for open clusters
4- 15 A12 --- Cluster Cluster name
17- 21 F5.2 [Sun] [Fe/H] Mean metallicity
23- 26 F4.2 [Sun] s_[Fe/H] ? Standard deviation of metallicity
28- 29 I2 --- o_[Fe/H] Number of metallicity determinations
31- 32 I2 --- Nm Number of individual member stars
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Acknowledgements:
Ulrike Heiter, ulrike.heiter(at)physics.uu.se
References:
Paunzen et al., Paper I 2010A&A...517A..32P 2010A&A...517A..32P
(End) Patricia Vannier [CDS] 18-Nov-2013