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 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:
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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
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See also:
J/A+A/281/817 : Model atmospheres for Vega (Castelli+ 1994)
Byte-by-byte Description of file: dwarfs.dat giants.dat
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Bytes Format Units Label Explanations
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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
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Note (1): When the photometric colour is equal to 99.999, this means there
is no available data in the literature.
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Byte-by-byte Description of file: a*.dat
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Bytes Format Units Label Explanations
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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)
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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)
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Byte-by-byte Description of file: qr*.dat
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Bytes Format Units Label Explanations
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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
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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.
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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