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J/A+A/497/497  Physical parameters from JHK flux   (Gonzalez-Hernandez+, 2009)

A new implementation of the infrared flux method using the 2MASS catalogue. Gonzalez Hernandez J.I., Bonifacio P. <Astron. Astrophys. 497, 497 (2009)> =2009A&A...497..497G
ADC_Keywords: Stars, giant ; Stars, dwarfs ; Photometry, UBVRI ; Photometry, infrared ; Models, atmosphere Keywords: infrared: stars - stars: abundances - stars: atmospheres - stars: fundamental parameters Abstract: The effective temperature scale of FGK stars, especially at the lowest metallicities remains a major problem in the chemical abundance analysis of metal-poor stars. We present a new implementation of the infrared flux method (IRFM) using the 2MASS catalogue. Description: We have made use of the infrared flux method (IRFM) to determine effective temperatures of 555 dwarf and subgiant field stars, and 264 giant field stars. Our implementation of the IRFM uses the 2MASS photometric system as a reference system to perform all the calculations. Bolometric fluxes are derived using UBV(RI)cJHKs accurate photometric data. In tables dwarf.dat and giants.dat, we provide the photometric data and reddenings used in this paper, stellar parameters and metallicity, bolometric fluxes and IRFM temperatures and angular diameters for all the stars in our samples. In tables a*.dat, we provide A factors and Bx-B coefficients, necessary for the determination of bolometric fluxes, computed from the ATLAS theoretical fluxes of Castelli & Kurucz (2003, arXiv:astro-ph/0405087v1) We used the fluxes in the ranges 3500K<Teff<50000K, 0.0<log(g)<5.0 and -4<[Fe/H]<+0.5, for metal-poor models with [Fe/H]≤-0.5 we used the fluxes computed from the α-enhanced models. Different A factor corresponding to the different ratios between the bolometric flux and the observed integrated flux, determined from observed magnitudes: - A1: when using the UBV(RI)cJHKs magnitudes - A2: when using the UBVJHKs magnitudes - A3: when using the BVJHKs magnitudes - A4: when using the BV(RI)cJHKs magnitudes In tables qr*.dat, we provide Q and R factors, necessary for the implementation of the IRFM, computed from the ATLAS theoretical fluxes of Castelli & Kurucz (2003, arXiv:astro-ph/0405087v1) We used the fluxes in the ranges 3500K<Teff<50000K, 0.0<log(g)<5.0 and -4<[Fe/H]<+0.5, for metal-poor models with [Fe/H]≤-0.5 we used the fluxes computed from the α-enhanced models. We also provide the theoretical color V-K and the magnitudes JHKs in the 2MASS system for each atmospheric model. The theoretical magnitudes are normalized to Vega (J=H=Ks=0 in the 2MASS photometric system). The model Flux for Vega is that computed by F. Castelli (http://wwwuser.oats.inaf.it/castelli/vega/fm05t9550g395k2odfnew.dat) and assumes parameters Teff=9550, logg=3.95, vturb=2km/s and metallicity -0.5 (see Castelli & Kurucz 1994, Cat. J/A+A/281/817). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file dwarfs.dat 146 555 Dwarfs photometric data and reddenings used in the paper giants.dat 146 264 Giants photometric data and reddenings used in the paper am05k2.dat 88 476 A factors and Bx-B coefficients for [Fe/H]=-0.5 model am10ak2.dat 88 476 A factors and Bx-B coefficients for [Fe/H]=-1.0 α-enhanced model am15ak2.dat 88 476 A factors and Bx-B coefficients for [Fe/H]=-1.5 α-enhanced model am20ak2.dat 88 476 A factors and Bx-B coefficients for [Fe/H]=-2.0 α-enhanced model am25ak2.dat 88 476 A factors and Bx-B coefficients for [Fe/H]=-2.5 α-enhanced model am40ak2.dat 88 476 A factors and Bx-B coefficients for [Fe/H]=-4.0 α-enhanced model ap00k2.dat 88 476 A factors and Bx-B coefficients for [Fe/H]=+0.0 model ap05k2.dat 88 476 A factors and Bx-B coefficients for [Fe/H]=+0.5 model qrm05k2.dat 127 476 Q and R factors for [Fe/H]=-0.5 model qrm10ak2.dat 127 476 Q and R factors for [Fe/H]=-1.0, α-enhanced model qrm15ak2.dat 127 476 Q and R factors for [Fe/H]=-1.5, α-enhanced model qrm20ak2.dat 127 476 Q and R factors for [Fe/H]=-2.0, α-enhanced model qrm25ak2.dat 127 476 Q and R factors for [Fe/H]=-2.5, α-enhanced model qrm40ak2.dat 127 476 Q and R factors for [Fe/H]=-4.0, α-enhanced model qrp00k2.dat 127 476 Q and R factors for [Fe/H]=+0.0 model qrp05k2.dat 127 476 Q and R factors for [Fe/H]=+0.5 model
See also: J/A+A/281/817 : Model atmospheres for Vega (Castelli+ 1994) Byte-by-byte Description of file: dwarfs.dat giants.dat
Bytes Format Units Label Explanations
1- 14 A14 -- Name Name of the star 15- 21 F7.1 K Tirfm Effective temperature from IR flux method 23- 28 F6.1 K e_Tirfm Uncertainty on the IRFM temperature 30- 34 F5.3 mas theta Angular diameter 36- 40 F5.3 mas e_theta Uncertainty on the angular diameter 42- 46 F5.2 [cm/s2] logg Surface gravity 48- 52 F5.2 [Sun] [Fe/H] Metallicity 54- 63 E10.5 mW/m2 Fbol Bolometric flux 65- 69 F5.3 mag E(B-V) Reddening corrections 71- 76 F6.3 mag Vmag V magnitude in the Johnson system 78- 83 F6.3 mag B-V ?=99.999 Johnson B-V colour index (1) 85- 90 F6.3 mag U-B ?=99.999 Johnson U-B colour index (1) 92- 97 F6.3 mag V-Rc ?=99.999 Johnson-Cousins V-R colour index (1) 99-104 F6.3 mag V-Ic ?=99.999 Johnson-Cousins V-I colour index (1) 106-111 F6.3 mag Jmag 2MASS J magnitude 113-118 F6.3 mag e_Jmag Uncertainty on 2MASS J magnitude 120-125 F6.3 mag Hmag 2MASS H magnitude 127-132 F6.3 mag e_Hmag Uncertainty on 2MASS H magnitude 134-139 F6.3 mag Kmag 2MASS K magnitude 141-146 F6.3 mag e_Kmag Uncertainty on 2MASS K magnitude
Note (1): When the photometric colour is equal to 99.999, this means there is no available data in the literature.
Byte-by-byte Description of file: a*.dat
Bytes Format Units Label Explanations
3- 7 I5 K Teff Effective temperature 9- 13 F5.2 [cm/s2] logg Surface gravity 14- 19 F6.2 [Sun] [Fe/H] Metallicity 21- 25 F5.2 km/s Vturb Microturbulence 27- 31 F5.2 -- l/H Mixing length parameter (1) 32- 43 E12.5 -- A1 A1-factor when using UBV(RI)cJHKs magnitudes (1) 44- 55 E12.5 -- A2 A2-factor when using UBVJHKs magnitudes (1) 56- 67 E12.5 -- A3 A3-factor when using BVJHKs magnitudes (1) 68- 79 E12.5 -- A4 A4-factor when using BV(RI)cJHKs magnitudes (1) 80- 88 F9.4 mag Bx-B Bx-B correction factor (2)
Note (1): Dimensionless parameter. The A factors represent the fit of φ = Fbol/(dexp(-0.4m)) [m is the magnitude in I, J or K] as a function of the color index X = (V-m): φ = Ao + A1.X + A2.X2 + A3.X3 + A4.X.[Fe/H] + A5.[Fe/H] Note (2): Bx-B is the correction used to compute the synthetic U magnitude from the observed magnitudes and colors of the star V, (U-B) (B-V): U = (U-B) + V + (B-V) + (Bx-B)
Byte-by-byte Description of file: qr*.dat
Bytes Format Units Label Explanations
3- 7 I5 K Teff Effective temperature 9- 13 F5.2 [cm/s2] logg Surface gravity 14- 19 F6.2 [Sun] [Fe/H] Metallicity 21- 25 F5.2 km/s Vturb Microturbulence 27- 31 F5.2 --- l/H Mixing length parameter (1) 33- 42 E10.5 --- RJ R-factor in 2MASS J filter 45- 51 F7.5 --- qJ q-factor in 2MASS J filter (1) 53- 62 E10.5 --- RH R-factor in 2MASS H filter 65- 71 F7.5 --- qH q-factor in 2MASS H filter (1) 73- 82 E10.5 --- RK R-factor in 2MASS Ks filter 85- 91 F7.5 --- qK q-factor in 2MASS Ks filter (1) 95-100 F6.3 mag V-K Theoretical V-K colour index 104-109 F6.3 mag JMAG Theoretical J absolute magnitude 113-118 F6.3 mag HMAG Theoretical H absolute magnitude 122-127 F6.3 mag KMAG Theoretical K absolute magnitude
Note (1): Dimensionless parameter. The factors relate the bolometric flux Fbol to the calibrated flux of Vega from the calibrated ATLAS9 flux: Fbol/Fcal = q . R . dexp(-0.4(m-m(cal))) where q and R are function of wavelength, and stellar parameters.
Acknowledgements: Jonay Isai Gonzalez Hernandez, Jonay.Gonzalez-Hernandez(at)obspm.fr History: * 20-Jan-2009: Original version * 11-Jan-2010: Unit of diameter (parameter "theta" in tables "giants" and "dwarfs" corrected from "arcsec" to "mas"
(End) Patricia Vannier [CDS] 20-Jan-2009
(End) Patricia Vannier [CDS] 20-Jan-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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