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J/ApJ/701/1053      Abundances of 8 stars in the Draco dSph       (Cohen+, 2009)

The chemical evolution of the Draco dwarf spheroidal galaxy. Cohen J.G., Huang W. <Astrophys. J., 701, 1053-1075 (2009)> =2009ApJ...701.1053C
ADC_Keywords: Equivalent widths ; Stars, giant ; Galaxies, nearby Keywords: galaxies: abundances - galaxies: dwarf - galaxies: individual (Draco) Abstract: We present an abundance analysis based on high-resolution spectra of eight stars selected to span the full range in metallicity in the Draco dwarf spheroidal (dSph) galaxy. We find that [Fe/H] for the sample stars ranges from -1.5 to -3.0dex. Combining our sample with previously published work for a total of 14 luminous Draco giants, we show that the abundance ratios [Na/Fe], [Mg/Fe], and [Si/Fe] for the Draco giants overlap those of Galactic halo giants at the lowest [Fe/H] probed, but are significantly lower for the higher Fe-metallicity Draco stars. Using a toy model we compare the behavior of the abundance ratios within the sample of Draco giants with those from the literature of Galactic globular clusters, and the Carina and Sgr dSph galaxies. Description: The Draco stars in our sample were observed with HIRES at the Keck I telescope during two runs, in 2005 June and in 2006 September. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file stars.dat 77 8 The sample of stars in the Draco dSph and their stellar parameters (table 1 and 2 of the paper) table3.dat 42 3056 Equivalent Widths for eight stars in the Draco dSph
See also: J/AJ/136/1921 : Variable stars of Draco dSph (Kinemuchi+, 2008) J/MNRAS/375/831 : Draco MegaCam, INT and HST photometry (Segall+, 2007) J/A+A/442/165 : IJKs photometry of late-type stars in Draco dSph (Cioni+, 2005) J/ApJS/145/245 : SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003) J/AJ/124/3222 : VI photometry of Draco and UMi galaxies (Bellazzini+, 2002) J/MNRAS/330/792 : Radial velocity in Draco (Kleyna+, 2002) J/AJ/123/2511 : RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002) Byte-by-byte Description of file: stars.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Name Star identification (1) 7- 8 I2 h RAh Hour of right ascension (J2000) (1) 10- 11 I2 min RAm Minute of right ascension (J2000) 13- 17 F5.2 s RAs Second of right ascension (J2000) 19 A1 --- DE- Sign of declination (J2000) (1) 20- 21 I2 deg DEd Degree of declination (J2000) 23- 24 I2 arcmin DEm Arcminute of declination (J2000) 26- 30 F5.2 arcsec DEs Arcsecond of declination (J2000) 32- 36 F5.2 mag Vmag SDSS V-band magnitude (2) 38- 42 F5.2 mag Imag SDSS I-band magnitude (2) 44- 50 A7 --- Date Observation date in "MM/YYYY" format 51 A1 --- n_Date [b] b: the 2hr exposure from 06/2005 is not as good and was not used. 53- 56 I4 s Exp Exposure time 58- 61 I4 K Teff Effective temperature from the spectra 63- 66 F4.2 [cm/s2] logg Surface gravity from the spectra 68- 70 F3.1 km/s Vt Turbulent velocity ξ 72- 77 F6.1 km/s HRV Heliocentric radial velocity
Note (1): The star names and coordinates are from Winnick (2003PhDT.........9W). Many of the names were originally assigned by Baade & Swope (1961AJ.....66..300B). Note (2): Optical photometry from the SDSS (York et al. 2000AJ....120.1579Y) using the transformation equations of Smith et al. (2002AJ....123.2121S).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Name Star identification 7- 13 F7.2 0.1nm Wave Wavelength in Angstroms 15- 19 A5 --- Ion Species identification 21- 24 F4.2 eV ExPot Excitation potential 26- 32 F7.3 [-] log(gf) Log of the oscillator strength 34- 35 A2 --- l_EW [≤] Limit flag on EW 36- 40 F5.1 10-13m EW ? Equivalent width (in mÅ) 42 A1 --- u_EW [a] a: indicates EW is very uncertain, could be an upper limit (concerns XI-2)
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 13-Sep-2011
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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