J/MNRAS/373/13 Lower main-sequence stars fundamental param. (Casagrande+, 2006)
Accurate fundamental parameters for lower main-sequence stars.
Casagrande L., Portinari L., Flynn C.
<Mon. Not. R. Astron. Soc., 373, 13-44 (2006)>
=2006MNRAS.373...13C 2006MNRAS.373...13C
ADC_Keywords: Stars, dwarfs ; Stars, early-type ; Photometry ;
Effective temperatures
Keywords: techniques: photometric - stars: atmospheres -
stars: fundamental parameters - Hertzsprung-Russell (HR) diagram -
stars: late-type - infrared: stars
Abstract:
We derive an empirical effective temperature and bolometric luminosity
calibration for G and K dwarfs, by applying our own implementation of
the Infrared Flux Method to multiband photometry. Our study is based
on 104 stars for which we have excellent BV(RI)C JHKs photometry,
excellent parallaxes and good metallicities.
Colours computed from the most recent synthetic libraries (ATLAS9 and
MARCS) are found to be in good agreement with the empirical colours
in the optical bands, but some discrepancies still remain in the
infrared. Synthetic and empirical bolometric corrections also show
fair agreement.
Description:
To recover accurate bolometric fluxes and temperatures for the stars,
we have obtained accurate and homogeneous Johnson-Cousins BV(RI)C
and JHKs photometry for all the 186 stars in our initial sample. For
most of the stars in our sample with declination north of DE=-25°,
we have made our own photometric observations from April to December
2004. Observations were done from Finland in full remote mode, using
the 35-cm telescope piggybacked on the Swedish 60-cm telescope located
at La Palma in the Canary Islands. A SBIG charge-coupled device was
used through all the observations. Johnson-Cousins BV(RI)C colours
were obtained for all stars. Infrared JHKs photometry for the sample
has been taken from the Two-Micron All-Sky Survey (2MASS) catalogue.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 125 104 Observable and physical quantities for our
sample stars
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See also:
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Name (HD, BD or CD)
12- 17 I6 --- HIP HIP (Cat. I/239) number
19- 23 F5.2 mas Plx Trigonometric parallax
25- 28 F4.2 mas e_Plx rms uncertainty on Plx
30- 33 I4 K Teff Effective temperature (1)
35- 37 I3 K e_Teff rms uncertainty on Teff
39- 43 F5.3 mas Diam ? Angular diameter (1)
45- 49 F5.3 mas e_Diam rms uncertainty on Diam
51- 56 F6.3 mag mbol Apparent bolometric luminosity (2)
58- 63 F6.3 mag Vmag Johnson V magnitude
65- 69 F5.3 mag B-V Johnson B-V colour index
71- 75 F5.3 mag V-Rc Johnson-Cousins V-R colour index
77- 81 F5.3 mag R-Ic Cousins R-I colour index
83- 86 F4.2 mag Jmag 2MASS J magnitude
88- 91 F4.2 mag e_Jmag rms uncertainty on Jmag
93- 96 F4.2 mag Hmag 2MASS H magnitude
98-101 F4.2 mag e_Hmag rms uncertainty in Hmag
103-106 F4.2 mag Ksmag 2MASS Ks magnitude
108-111 F4.2 mag e_Ksmag rms uncertainty on Ks
113-117 F5.2 [Sun] [Fe/H] Metallicity
119-123 F5.2 [Sun] [alpha/Fe] Abundance [alpha/Fe]
125 A1 --- r_[alpha/Fe] Reference for [alpha/Fe] (3)
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Note (1): Effective temperatures and angular diameters are those computed
via IRFM as described in Section 4.
Note (2): Apparent bolometric magnitudes are obtained as described in Section 7,
where the absolute bolometric magnitude of the Sun is MBol=4.74.
Note (3): Source of metallicities as follows:
a = Mishenina et al. (2002A&A...396..189M 2002A&A...396..189M and 2004, Cat. J/A+A/418/551)
b = Valenti & Fischer (2005)
c = Pompeia, Barbuy & Grenon (2002ApJ...566..845P 2002ApJ...566..845P + 2003ApJ...592.1173P 2003ApJ...592.1173P)
d = Santos et al. (2005A&A...437.1127S 2005A&A...437.1127S)
e = Favata, Micela & Sciortino (1997A&A...323..809F 1997A&A...323..809F)
f = Gray et al. (2003, Cat. J/AJ/126/2048)
g = Paulson, Sneden & Cochran (2003AJ....125.3185P 2003AJ....125.3185P)
h = Santos et al. (2004, Cat. J/A+A/415/1153)
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History:
31-Aug-2007: From electronic version of the journal
27-Jan-2011: In ReadMe, Plx and Diam columns were inverted
(End) Patricia Vannier [CDS] 08-Jun-2007