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J/MNRAS/445/2223    Mass estimation for FGK stars            (Pinheiro+, 2014)

On the mass estimation for FGK stars: comparison of several methods. Pinheiro F.J.G., Fernandes J.M., Cunha M.S., Monteiro M.J.P.F.G., Santos N.C., Sousa S.G., Marques J.P., Fang J.-J., Mortier A., Sousa J. <Mon. Not. R. Astron. Soc., 445, 2223-2231 (2014)> =2014MNRAS.445.2223P
ADC_Keywords: Stars, F-type ; Stars, G-type ; Stars, K-type ; Stars, masses Keywords: methods: numerical - binaries: general - stars: fundamental parameters - Hertzsprung-Russell and colour-magnitude diagrams Abstract: Stellar evolutionary models simulate well binary stars when individual stellar mass and system metallicity are known. The mass can be derived directly from observations only in the case of multiple stellar systems, mainly binaries. Yet, the number of such stars for which accurate stellar masses are available is rather small. The main goal of this project is to provide realistic mass estimates for a homogeneous sample of about a thousand FGK single stars, using four different methods and techniques. We present the masses inferred according to each one of these methods as well as a final mass estimate consisting in the median of the four mass estimates. The procedures evaluated here include the use of stellar evolutionary models, mass-luminosity relation and surface gravity spectroscopic observations. By combining the results obtained with different methods, we determine the best mass value for each individual star, as well as the associated error budget. Our results confirm the expected consistency between the different mass estimation methods. None the less, for masses above 1.2M, the spectroscopic surface gravities seem to overestimate the mass. This result may be a consequence of the spectroscopic surface gravities used in this analysis. Nevertheless, this problem is minimized by the fact that we have several approaches available for deriving stellar masses. Moreover, we suggest an empirical procedure to overcome this issue. Description: The objects used in our analysis were taken from the works of Sousa et al. (2008A&A...487..373S, Cat. J/A+A/487/373, 2011A&A...533A.141S, Cat. J/A+A/533/A141) for which information on their effective temperature (Teff), luminosity (L), surface gravity (logg) and metal abundance ([Fe/H]) has been derived in a consistent way. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 98 451 Mass estimate for the targets from Sousa et al. 2008 (J/A+A/487/373) according to different methods tablea2.dat 97 582 Mass estimate for the targets from Sousa et al. 2011 (J/A+A/533/A141) according to different methods tablea3.dat 75 22 Mass estimate for the targets from Bruntt et al. (2010MNRAS.405.1907B) according to different methods
See also: J/AJ/106/773 : Mass-luminosity relation (Henry+, 1993) J/A+A/487/373 : Spectroscopic parameters of 451 HARPS-GTO stars (Sousa+, 2008) J/A+A/533/A141 : Stellar parameters for 582 HARPS FGK stars (Sousa+, 2011) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/451] Sequential number 5- 14 A10 --- Name Star's identifier 16- 17 I2 h RAh Right ascension (J2000) 19- 20 I2 min RAm Right ascension (J2000) 22- 26 F5.2 s RAs Right ascension (J2000) 28 A1 --- DE- Declination sign (J2000) 29- 30 I2 deg DEd Declination (J2000) 32- 33 I2 arcmin DEm Declination (J2000) 35- 38 F4.1 arcsec DEs Declination (J2000) 40- 44 F5.3 Msun M1 [0.6/1.4] Direct estimation of the stellar mass using the spectroscopic surface gravity 46- 50 F5.3 Msun e_M1 [0.04/0.12] Error in M1 52- 56 F5.3 Msun M2 [0.1/2.9] Estimation of the stellar mass using the method of Torres et al. (2010AJ....140.1158T) 58- 62 F5.3 Msun e_M2 [0.03/2.5] Error in M2 64- 68 F5.3 Msun M3 [0.6/1.5] Estimation of the stellar mass using the method of Henry & McCarthy (1993AJ....106..773H) 70- 74 F5.3 Msun e_M3 [0.05/0.11] Error in M3 76- 80 F5.3 Msun M4 [0.5/1.4] Estimation of the stellar mass using the Padova models 82- 86 F5.3 Msun e_M4 [0.05/0.08] Error in M4 88- 92 F5.3 Msun M [0.6/1.5] Median of the previous 4 mass estimates 94- 98 F5.3 Msun e_M [0.03/0.08] Error in M
Byte-by-byte Description of file: tablea2.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/582] Sequential number 5- 14 A10 --- Name Star's identifier 16- 24 F9.5 deg RAdeg Right ascension (J2000) 26- 34 F9.5 deg DEdeg Declination (J2000) 36- 40 F5.3 Msun M1 [0.6/1.5] Direct estimation of the stellar mass using the spectroscopic surface gravity 42- 46 F5.3 Msun e_M1 [0.03/0.1] Error in M1 48- 52 F5.3 Msun M2 [0.037/4.1] Estimation of the stellar mass using the method of Torres et al. (2010AJ....140.1158T) 54- 61 F8.3 Msun e_M2 [0.03/1049] Error in M2 63- 67 F5.3 Msun M3 [0.6/1.8] Estimation of the stellar mass using method of Henry & McCarthy (1993AJ....106..773H) 69- 73 F5.3 Msun e_M3 [0.03/0.13] Error in M3 75- 79 F5.3 Msun M4 [0.5/1.8] Estimation of the stellar mass using the Padova models 81- 85 F5.3 Msun e_M4 [0.03/0.11] Error in M4 87- 91 F5.3 Msun M [0.5/1.8] Median of the previous 4 mass estimates 93- 97 F5.3 Msun e_M [0.02/0.12] Error in M
Byte-by-byte Description of file: tablea3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/22] Sequential number 5- 15 A11 --- Name Star's identifier 17- 21 F5.3 Msun M1 [0.7/2.2] Direct estimation of the stellar mass using the spectroscopic surface gravity 23- 27 F5.3 Msun e_M1 [0.05/0.3] Error in M1 29- 33 F5.3 Msun M2 [0.9/2.9] Estimation of the stellar mass using the method of Torres et al. (2010AJ....140.1158T) 35- 39 F5.3 Msun e_M2 [0.4/1.4] Error in M2 41- 45 F5.3 Msun M3 [0.9/2.5] Estimation of the stellar mass using method of Henry & McCarthy (1993AJ....106..773H) 47- 51 F5.3 Msun e_M3 [0.06/0.2] Error in M3 53- 57 F5.3 Msun M4 [0.7/2.9] Estimation of the stellar mass using the Padova models 59- 63 F5.3 Msun e_M4 [0.05/0.2] Error in M4 65- 69 F5.3 Msun M [0.8/2.7] Median of the previous 4 mass estimates 71- 75 F5.3 Msun e_M [0.05/0.24] Error in M
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 19-May-2015
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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