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J/MNRAS/414/1227    Mg/Fe ratio of MILES stars               (Milone+, 2011)

Element abundances in the stars of the MILES spectral library: the Mg/Fe ratio. Milone A.DE C., Sansom A.E., Sanchez-Blazquez P. <Mon. Not. R. Astron. Soc., 414, 1227-1252 (2011)> =2011MNRAS.414.1227M
ADC_Keywords: Stars, nearby ; Abundances Keywords: techniques: spectroscopic - astronomical data bases: miscellaneous - catalogues - stars: abundances - stars: atmospheres - solar neighbourhood Abstract: We have obtained [Mg/Fe] measurements for 76.3 per cent of the stars in the Mid-resolution Isaac Newton Telescope Library of Empirical Spectra (MILES) spectral library used for understanding stellar atmospheres and stellar populations in galaxies and star clusters. These abundance ratios were obtained through (1) a compilation of values from the literature using abundances from high-resolution (HR) spectroscopic studies and (2) a robust spectroscopic analysis using the MILES mid-resolution (MR) optical spectra. All the [Mg/Fe] values were carefully calibrated to a single uniform scale, by using an extensive control sample with results from HR spectra. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 84 687 The MILES [Mg/Fe] catalogue for field stars table5.dat 105 65 The MILES [Mg/Fe] catalogue for star cluster stars
See also: J/MNRAS/371/703 : MILES lib. of empirical spectra (Sanchez-Blazquez+, 2006) J/MNRAS/374/664 : MILES lib. stellar atmospheric parameters (Cenarro+, 2007) J/MNRAS/404/1639 : MILES base models + new line index system (Vazdekis+, 2010) J/MNRAS/406/165 : Comparison of Lick indexes (Johansson+, 2010) J/A+A/531/A165 : MILES atmospheric parameters (Prugniel+, 2011) Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Miles Miles identification 9- 11 I3 --- CaT ? Identification number in the CaT library (Cenarro et al. 2002MNRAS.329..863C) 15- 27 A13 --- Name Star name 34- 38 I5 K Teff Effective temperature 42- 46 F5.2 [cm/s2] logg Surface gravity 50- 54 F5.2 [Sun] [Fe/H] Metallicity 58- 62 F5.2 [Sun] [Mg/Fe] Abundance [Mg/Fe] 66- 69 F4.2 [Sun] e_[Mg/Fe] rms uncertainty on [Mg/Fe] 73- 74 A2 --- src [HR mr] high/mid-resolution origin (G2) 76- 84 A9 --- Ref Reference (G1)
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Miles Miles identification 9- 11 I3 --- CaT ? Identification number if the CaT library (Cenarro et al. 2002MNRAS.329..863C) 15- 22 A8 --- Cluster Cluster name 26- 33 A8 --- Type [open globular] Type of cluster 37- 52 A16 --- Name Star name 56- 60 I5 K Teff Effective temperature 64- 68 F5.2 [cm/s2] logg Surface gravity 72- 76 F5.2 [Sun] [Fe/H] Metallicity 80- 84 F5.2 [Sun] [Mg/Fe] Abundance [Mg/Fe] 88- 91 F4.2 [Sun] e_[Mg/Fe] rms uncertainty on [Mg/Fe] 95- 96 A2 --- src [HR mr] high/mid-resolution origin (G2) 98-105 A8 --- Ref Reference (G1)
Global notes: Note (G1): References as follows: "*" = if the MR measurement represents an α-enhancement model atmosphere extrapolation as described in Section 3.5 BothMg = Mg5183 and Mg5528 Mg5183 = Mg5183 Mg5528 = Mg5528 Ae01 = Adelman et al. 2001, Cat. J/A+A/371/1078 Ae06 = Adelman et al. 2006, Cat. J/A+A/447/685 Be05 = Bensby et al. 2005, Cat. J/A+A/433/185 BM05 = Borkova & Marsakov, 2005, Cat. J/AZh/82/453 Ce00 = Carretta, Gratton & Sneden 2000, Cat. J/A+A/356/238 Ce02 = Caliskan et al. 2002, Cat. J/A+A/394/187 Ce09 = Cenarro et al. 2009, Cat. J/MNRAS/396/1895 EN03 = Erspamer & North 2003, Cat. J/A+A/398/1121 F00 = Fulbright 2000, Cat. J/AJ/120/1841) FG98 = Feltzing & Gustafsson 1998, Cat. J/A+AS/129/237 FK99 = Fulbright & Kraft, 1999AJ....118..527F Ge03 = Gratton et al. 2003, Cat. J/A+A/404/187 H02 = Heiter 2002, Cat., J/A+A/381/959 LH05 = Luck & Heiter 2005, Cat. J/AJ/129/1063 Re06 = Reddy, Lambert & Allende Prieto, 2006, Cat. J/MNRAS/367/1329 T98 = Thevenin 1998, Cat. III/193 Note (G2): * "HR" indicates a compilation of values from the literature using abundances from high-resolution (HR) spectroscopic studies * "mr" indicates a robust spectroscopic analysis using our MILES mid-resolution (MR) optical spectra.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 31-Jan-2012
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