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J/A+A/488/943   Abundances of giants in four Galactic clusters  (Sestito+, 2008)

Old open clusters as key tracers of Galactic chemical evolution. III. Element abundances Berkeley 20, Berkeley 29, Collinder 261 and Melotte 66. Sestito P., Bragaglia A., Randich S., Pallavicini R., Andrievsky S.M., Korotin S.A. <Astron. Astrophys. 488, 943 (2008)> =2008A&A...488..943S
ADC_Keywords: Clusters, open ; Stars, giant ; Abundances Keywords: stars: abundances - stars: evolution - Galaxy: disk - Galaxy: open clusters and associations: general - open clusters and associations: individual: Berkeley 20, Berkeley 29, Collinder 261, Melotte 66 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 bright 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. We derived the abundance of Fe for Mg, Al, Ca, Si, Ti, Cr, Ni, and Ba. We employed direct line profile fitting to derive non-LTE Na abundances. We found [Fe/H]=-0.30, -0.31, +0.13, -0.33 for Be 20, Be 29, Cr 261, and Melotte 66, respectively (with rms values of 0.02 to 0.05dex). Alpha- and Fe-peak elements have solar ratios, Ba is enhanced, and Na has solar ratios, suggesting that treatment of non-LTE is very important. We confirm the presence of a metallicity gradient in the inner disk, and a flattening in the outer part. Description: Spectra for 2 to 6 giant stars in Be 20, Be 29, Cr 261, and Mel 66 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 (and synthesis for Na), model atmospheres and input atmospheric parameters based on photometry. For each member star in the four clusters we give the measured EWs. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file stars.dat 91 21 Star positions, photometry and radial velocities ew.dat 32 6482 Equivalent widths
See also: J/A+A/480/79 : Abundances of giants in five Galactic clusters (Bragaglia+ 2008) Byte-by-byte Description of file: stars.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Cluster Cluster name (1) 8- 11 I4 --- Star Star number within cluster 12- 23 A12 --- Name Star name 25- 26 I2 h RAh Right ascension (J2000) 28- 29 I2 min RAm Right ascension (J2000) 31- 36 F6.3 s RAs Right ascension (J2000) 38 A1 --- DE- Declination sign (J2000) 39- 40 I2 deg DEd Declination (J2000) 42- 43 I2 arcmin DEm Declination (J2000) 45- 50 F6.3 arcsec DEs Declination (J2000) 51- 56 F6.3 mag Bmag ?=- B magnitude 58- 63 F6.3 mag Vmag V magnitude 65- 70 F6.3 mag Imag I magnitude 72- 77 F6.2 km/s RV Radial velocity 79- 82 F4.2 km/s e_RV rms uncertainty on RV 84- 86 A3 --- Mm Membership notes 88- 91 I4 --- WEBDA ?=- WEBDA number
Note (1): Origin of data as follows: Be 20 = ID is ours, from the FLAMES pointing, based on EIS; magnitudes from MacMinn et al. (1994AJ....107.1806M) or from EIS photometry, aligned to it), or Andreuzzi et al. (2008, MNRAS, subm.) Be 29 = ID, BVI from Tosi et al. (2004MNRAS.354..225T) Cr 261 = ID is ours, from the FLAMES pointing, BVI private communication (EIS data) by L. Prisinzano Mel 66 = ID, VI from EIS data (Spano, priv. comm.) calibrated to Kassis et al. (1997AJ....113.1723K)
Byte-by-byte Description of file: ew.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Cluster Cluster name 8- 11 I4 --- Star Star number within cluster 14- 20 F7.2 0.1nm lambda Wavelength 22- 26 A5 --- El Element 28- 32 F5.1 0.1pm EW Equivalent width
Acknowledgements: Angela Bragaglia, angela.bragaglia(at)oabo.inaf.it References: Sestito et al., Paper I 2006A&A...458..121S Bragaglia et al., Paper II 2008A&A...480...79B, Cat. J/A+A/480/79
(End) Patricia Vannier [CDS] 06-Jul-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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