J/A+A/480/79 Abundances of giants in five Galactic clusters (Bragaglia+, 2008)
Old open clusters as key tracers of Galactic chemical evolution.
II. Iron and elemental abundances in NGC 2324, NGC 2477, NGC 2660, NGC 3960,
and Berkeley 32.
Bragaglia A., Sestito P., Villanova S., Carretta E., Randich S., Tosi M.
<Astron. Astrophys. 480, 79 (2008)>
=2008A&A...480...79B 2008A&A...480...79B
ADC_Keywords: Clusters, open ; Stars, giant ; Equivalent widths ; Abundances
Keywords: stars: evolution - stars: abundances - Galaxy: disk -
open clusters and associations: general
Abstract:
To constrain the formation and chemical evolution of the Galactic
disk, we surveyed open clusters of different ages, metal contents, and
distances form the Galactic centre.
We employed FLAMES on VLT-UT2 to collect UVES spectra of five to ten
giant stars in each of the selected clusters, and used them to derive
the iron abundance and the detailed chemical composition. Equivalent
widths were measured and abundance analysis was performed using the
MOOG code and Kurucz model atmospheres on all stars accepted as
cluster member on the basis of their radial velocity.
We derived the atmospheric parameters and the abundance of Fe for
NGC 2324 and NGC 2477 (average [Fe/H]=-0.17 with rms 0.05dex, and
+0.07 with rms 0.03dex, respectively), two clusters never analyzed
using high resolution spectroscopy. We also derived the abundances of
Mg, Al, Ca, Si, Ti, Cr, Ni, and Ba for these two clusters and for
NGC 2660, NGC 3960, and Berkeley 32, whose atmospheric parameters and
metallicities were measured in a previous paper. We determined the
reddening values for the five clusters, based on the spectroscopically
determined temperatures, literature photometry, and a
colour-temperature relation.
All clusters show solar-scaled abundances for alpha- and Fe-peak
elements, while [Na/Fe] appears slightly enhances and and [Ba/Fe]
significantly enhanced. Our findings were compared to thin-disk stars
and other open clusters, and no significant deviation from the
standard behavior was found.
Description:
Spectra for 5 to 10 (mostly) giant stars in NGC 2324, NGC 2477,
NGC 2660, NGC 3960, Berkeley 32 were obtained with FLAMES@VLT using
the fiber link to UVES. Abundances of Fe, Na, Mg, Al, Si, Ca, Ti, Cr,
Ni and Ba were derived using equivalent widths, model atmospheres and
input atmospheric parameters based on photometry.
For each member star in the five clusters we give the measured EWs.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 108 33 List of stars observed
table4.dat 28 209 WL, EP, log(gf), source of damping
ew.dat 34 13002 Equivalent widths (tables 6-10 of the paper)
table13.dat 116 33 Abundances for Na, Si, Ca, TiI, TiII, CrI, CrII,
Ni, Ba in the five clusters
table14.dat 42 132 Line-by-line abundances for Mg and Al
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See also:
J/MNRAS/299/834 : Berkeley 21 BVI photometry (Tosi+, 1998)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Cluster Cluster name
9- 13 A5 --- Star Star name in the cluster
15- 16 I2 h RAh Right ascension (J2000)
18- 19 I2 min RAm Right ascension (J2000)
21- 25 F5.2 s RAs Right ascension (J2000)
27 A1 --- DE- Declination sign (J2000)
28- 29 I2 deg DEd Declination (J2000)
31- 32 I2 arcmin DEm Declination (J2000)
34- 37 F4.1 arcsec DEs Declination (J2000)
39- 55 A17 --- Name Original name in the paper (cluster-star)
57- 79 A23 --- SName Simbad name (1)
81 A1 --- --- [=]
83-108 A26 --- SName2 Second Simbad name
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Note (1): Cl* NGC 2477 KVI 2447 is not in Sinbad
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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- 4 A4 --- Ion Atom and ionization stage
6- 13 F8.3 0.1nm lambda Wavelength
15- 19 F5.3 --- EP Energy potential
21- 26 F6.3 --- loggf Oscillator strength
28 I1 --- Flag [1/4] Flag indicating source of damping (1)
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Note (1): Source of damping as follows:
1 = MOOG code
2 = Barklem et al. (2000A&A...363.1091B 2000A&A...363.1091B)
3 = Gratton et al. (2003, Cat. J/A+A/404/187)
4 = Unsold (1955, Physik der Sternatmosphaeren
(Berlin: Springer-Verlag))
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Byte-by-byte Description of file: ew.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Cluster Cluster name
9- 13 A5 --- Star Star name in the cluster
16- 22 F7.2 0.1nm lambda Wavelength
25- 28 F4.1 --- El Element (1)
30- 34 F5.1 0.1pm EW Equivalent width for the star (mÅ)
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Note (1): Element is the atomic number; ZZ.0 is neutral, ZZ.1 is ionized.
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Byte-by-byte Description of file: table13.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Cluster Cluster name
9- 13 A5 --- Star Star name in the cluster
15- 18 F4.2 [-] [Na/Fe]LTE LTE abundance [Na/Fe]
20- 23 F4.2 [-] [Na/Fe]NLTE NLTE abundance [Na/Fe]
25- 28 F4.2 [-] e_[Na/Fe]LTE rms uncertainty on [Na/Fe]LTE and [Na/Fe]NLTE
30- 34 F5.2 [-] [Si/Fe] Abundance [Si/Fe]
36- 39 F4.2 [-] e_[Si/Fe] rms uncertainty on [Si/Fe]
41- 45 F5.2 [-] [Ca/Fe] Abundance [Ca/Fe]
47- 50 F4.2 [-] e_[Ca/Fe] rms uncertainty on [Ca/Fe]
52- 56 F5.2 [-] [TiI/Fe] Abundance [Ti/Fe]I
58- 61 F4.2 [-] e_[TiI/Fe] rms uncertainty on [TiI/Fe]
63- 67 F5.2 [-] [TiII/Fe] Abundance [Ti/Fe]II
69- 72 F4.2 [-] e_[TiII/Fe] rms uncertainty on [TiII/Fe]
74- 78 F5.2 [-] [CrI/Fe] Abundance [Cr/Fe]I
80- 83 F4.2 [-] e_[CrI/Fe] rms uncertainty on [CrI/Fe]
85- 89 F5.2 [-] [CrII/Fe] Abundance [Cr/Fe]II
91- 94 F4.2 [-] e_[CrII/Fe] rms uncertainty on [CrII/Fe]
96-100 F5.2 [-] [Ni/Fe] Abundance [Ni/Fe]
102-105 F4.2 [-] e_[Ni/Fe] rms uncertainty on [Ni/Fe]
107-111 F5.2 [-] [Ba/Fe] Abundance [Ba/Fe]
113-116 F4.2 [-] e_[Ba/Fe] rms uncertainty on [Ba/Fe]
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Byte-by-byte Description of file: table14.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Cluster Cluster name
10- 14 A5 --- Star Star name in the cluster
16- 17 A2 --- El Element (Al or Mg)
19- 26 F8.3 0.1nm lambda Wavelength of line
28- 31 F4.2 [-] LogNSun LogN(X) for this element in Sun
33- 36 F4.2 [-] LogN(X) ?=- LogN(X) for this element in the star
38- 42 F5.2 [-] [X/Fe] ?=- Abundance [X/Fe] for this element in the star
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Acknowledgements:
Angela Bragaglia, angela.bragaglia(at)oabo.inaf.it
References:
Sestito et al., Paper I 2006A&A...458..121S 2006A&A...458..121S
(End) Patricia Vannier [CDS] 10-Jan-2008