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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
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:
FileName Lrecl Records Explanations
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
See also: J/MNRAS/299/834 : Berkeley 21 BVI photometry (Tosi+, 1998) Byte-by-byte Description of file: stars.dat
Bytes Format Units Label Explanations
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
Note (1): Cl* NGC 2477 KVI 2447 is not in Sinbad
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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)
Note (1): Source of damping as follows: 1 = MOOG code 2 = Barklem et al. (2000A&A...363.1091B) 3 = Gratton et al. (2003, Cat. J/A+A/404/187) 4 = Unsold (1955, Physik der Sternatmosphaeren (Berlin: Springer-Verlag))
Byte-by-byte Description of file: ew.dat
Bytes Format Units Label Explanations
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)
Note (1): Element is the atomic number; ZZ.0 is neutral, ZZ.1 is ionized.
Byte-by-byte Description of file: table13.dat
Bytes Format Units Label Explanations
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]
Byte-by-byte Description of file: table14.dat
Bytes Format Units Label Explanations
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
Acknowledgements: Angela Bragaglia, angela.bragaglia(at)oabo.inaf.it References: Sestito et al., Paper I 2006A&A...458..121S
(End) Patricia Vannier [CDS] 10-Jan-2008
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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