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J/ApJ/713/L1    Lithium and proton-capture elements in 47 Tuc   (D'Orazi+, 2010)

Lithium and proton-capture elements in globular cluster dwarfs: the case of 47 Tuc. D'Orazi V., Lucatello S., Gratton R., Bragaglia A., Carretta E., Shen Z., Zaggia S. <Astrophys. J., 713, L1-L5 (2010)> =2010ApJ...713L...1D
ADC_Keywords: Abundances ; Clusters, globular ; Effective temperatures ; Stars, dwarfs Keywords: globular clusters: individual (NGC 104) - stars: abundances - stars: individual (Population II) Abstract: Previous surveys in a few metal-poor globular clusters (GCs) showed that the determination of abundances for Li and proton-capture elements offers a key tool to address the intracluster pollution scenario. In this Letter, we present Na, O, and Li abundances in a large sample of dwarf stars in the metal-rich GC 47 Tucanae. We found a clear Na-O anticorrelation, in good agreement with what obtained for giant members by Carretta et al. (2009, Cat. J/A+A/505/117). While lithium and oxygen abundances appear to be positively correlated with each other, there is a large scatter, well exceeding observational errors, and no anticorrelation with sodium. These findings suggest that Li depletion, due to mechanisms internal to the stars (which are cooler and more metal-rich than those on the Spite plateau), combines with the usual pollution scenario responsible for the Na-O anticorrelation. Description: We retrieved from the ESO Archive FLAMES-Giraffe spectra (MEDUSA configuration) of 109 unevolved members of the metal-rich GC 47 Tuc (Program 081.D-0287; PI: Z. Shen). The observations were carried out in Service mode in 2008 August-September; gratings HR15n (R∼17000), HR18 (R∼18400), and HR20A (R∼16000) were used to cover LiI (6707Å), OI (7771, 7773, 7774Å), and NaI (8183, 8194Å) features, respectively. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 80 100 Properties of target stars
See also: VII/202 : Globular Clusters in the Milky Way (Harris, 1997) J/A+A/505/117 : Abundances of red giants in 15 GCs (Carretta+, 2009) J/A+A/503/545 : Equivalent widths of Li, Na, Fe, Ca in NGC 6397 (Lind+, 2009) J/AJ/135/1551 : Abundances of stars in 47 Tuc (Koch+, 2008) J/AJ/125/197 : CN abundances of the 47 Tuc main sequence (Harbeck+, 2003) J/A+AS/117/227 : Dwarf effective temperatures (Alonso+ 1996) J/A+AS/106/161 : (V,I) photometry in NGC 6356 and 47 Tuc (Bica+ 1994) J/ApJS/85/293 : HST Observations of core of 47 Tuc (de Marchi+ 1993) J/PASP/99/739 : BV photometry in 4 fields of 47 Tuc (Hesser+, 1987) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- ID [1/114] Stellar identification number (<[DLG2010] NNN> in Simbad) 5- 11 F7.5 deg RAdeg Right Ascension (J2000) 13- 20 F8.4 deg DEdeg Declination (J2000) 22- 27 F6.3 mag Vmag The V band magnitude (1) 29- 34 F6.3 mag Bmag The B band magnitude (1) 36- 39 I4 K Teff Effective temperature (1) 41- 44 F4.2 [cm/s2] log(g) Log of the gravity 46- 50 F5.3 [-] lognO ?=9.999 Log of the oxygen number abundance (2) 52- 56 F5.3 [-] e_lognO ?=9.999 Error in LognO 58- 62 F5.3 [-] lognNa ?=9.999 Log of the sodium number abundance (2) 64- 68 F5.3 [-] e_lognNa ?=9.999 Error in LognNa 70- 74 F5.3 [-] lognLi ?=9.999 Log of the lithium number abundance (2) 76- 80 F5.3 [-] e_lognLi ?=0.000 Error in LognLi
Note (1): We obtained initial effective temperatures (Teff) from the de-reddened (E(B-V)=0.04; Harris 1996, see Cat. VII/202) B-V colors (data are from unpublished photometry by Y. Momany (2004, private communication) and the calibration by Alonso et al. (1996, Cat. J/A+AS/117/227). The adopted values were derived from a relation between V magnitude and color-based Teff. See section 2 for further details. Note (2): the Solar values are: lognO = 8.79; lognNa = 6.21; lognLi = 2.78±0.08
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 16-Apr-2012
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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