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J/A+A/496/441       Radial velocities of Berkeley 32 stars   (Randich+, 2009)

Membership and lithium in the old, metal-poor open cluster Berkeley 32. Randich S., Pace G., Pastori L., Bragaglia A. <Astron. Astrophys., 496, 441-451 (2009)> =2009A&A...496..441R
ADC_Keywords: Clusters, open ; Photometry ; Radial velocities Keywords: stars: abundances - stars: evolution - stars: interiors - open clusters and associations: individual: Berkeley 32 Abstract: Measurements of lithium (Li) abundances in open clusters provide a unique tool for following the evolution of this element with age, metallicity, and stellar mass. In spite of the plethora of Li data already available, the behavior of Li in solar-type stars has so far been poorly understood. Using FLAMES/Giraffe on the VLT, we obtained spectra of 157 candidate members of the old, metal-poor cluster Berkeley 32, to determine membership and to study the Li behavior of confirmed members. Radial velocities were measured, allowing us to derive both the cluster velocity and membership information for the sample stars. The Li abundances were obtained from the equivalent width of the Li I 670.8nm feature, using curves of growth. Description: Be 32 was observed with two different FLAMES configurations (A and B) centered at RA(2000)=06:58:04.2 and Dec(2000)=-06:28:21.1 and RA(2000)=06:58:02.0 and Dec(2000)=-06:22:41.4, respectively. We obtained four and one 3600s long exposures for configurations A and B, respectively. Observations were obtained in Visitor mode on Jan. 20, 2005 (configuration A) and Jan. 21, 2005 (configuration B). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 99 157 Sample stars table3.dat 37 57 Final results of our analysis
See also: J/A+A/480/79 : Abundances of giants in five Galactic clusters (Bragaglia+ 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Seq Sequential number 6- 7 I2 h RAh Right ascension (J2000) 9- 10 I2 min RAm Right ascension (J2000) 12- 17 F6.3 s RAs Right ascension (J2000) 19 A1 --- DE- Declination sign (J2000) 20- 21 I2 deg DEd Declination (J2000) 23- 24 I2 arcmin DEm Declination (J2000) 26- 30 F5.2 arcsec DEs Declination (J2000) 32- 34 A3 --- Conf [A,B ] Configuration of the FLAMES instrument 36- 41 F6.3 mag Bmag ?=- D'Orazi et al. (2006MNRAS.368..471D) B magnitude 43- 48 F6.3 mag V(B-V) ?=- D'Orazi et al. (2006MNRAS.368..471D) V magnitude from (B-V) colour index 50- 55 F6.3 mag V(V-I) ?=- D'Orazi et al. (2006MNRAS.368..471D) V magnitude from (V-I) colour index 57- 62 F6.3 mag Imag ?=- D'Orazi et al. (2006MNRAS.368..471D) I magnitude 64- 69 F6.3 mag Vmag Litterature V magnitude (1) 71- 75 F5.3 mag B-V ?=- Kaluzny & Mazur (1991AcA....41..167K) B-V colour index 77- 81 F5.3 mag V-I Richtler & Sagar (2001BASI...29...53R) V-I colour index 83- 87 F5.1 km/s RV ?=- Radial velocity 89- 92 F4.2 km/s e_RV ? rms uncertainty on RV 94 A1 --- Mm [mn?] Membership flag 96- 99 A4 --- Note Note
Note (1): V magnitude from Kaluzny & Mazur (1991AcA....41..167K) if the star is present in their catalog otherwise from Richtler & Sagar (2001BASI...29...53R).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Seq Sequential number 6- 10 F5.3 mag (B-V)0 Dereddened B-V colour index 11- 13 A3 --- n_(B-V)0 [ab*, ] Note on the origin of (B-V)0 (1) 15- 18 I4 K Teff Effective temperature 20- 21 A2 --- l_EW [≤ ] Limit flag on EW 22- 23 I2 0.1pm EW Li equivalent width 25- 26 I2 0.1pm e_EW ? rms uncertainty on EW 27- 28 A2 --- l_logN [≤ ] Limit flag on logn 29- 32 F4.2 [-] logN Li abundance (log(H)=12) 34- 37 F4.2 [-] e_logN ? rms uncertainty on logn
Note (1): Notes as follows: a = B-V from Richtler & Sagar (2001BASI...29...53R) b = (B-V)0 derived from (V-I) (see text) * = B-V from D'Orazi et al. (2006MNRAS.368..471D) available, but not used (see text)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 26-Apr-2009
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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