J/A+AS/125/229 A standard stellar library (Lejeune+ 1997)
A standard stellar library for evolutionary synthesis.
I. Calibration of theoretical spectra.
Lejeune T., Cuisinier F., Buser R.
<Astron. Astrophys. Suppl. Ser. 125, 229 (1997)>
=1997A&AS..125..229L 1997A&AS..125..229L (SIMBAD/NED BibCode)
ADC_Keywords: Atlases ; Models, evolutionary ; Spectrophotometry
Keywords: atlases - stars: fundamental parameters
Description:
The present library provides an extensive and homogeneous grid of
low-resolution theoretical flux distributions for a large range of
stellar parameters : Teff=50,000K to K, logg=5.50 to -1.02 and
[M/H]=-5.0 to +1.0. The library has been constructed from different
grids of blanketed stellar atmosphere models (Bessell et al.
(1989A&AS...77....1B 1989A&AS...77....1B, 1991A&AS...89..335B 1991A&AS...89..335B), Fluks et al.
(1994, Cat. J/A+AS/105/311), Kurucz (1995, priv. comm.), Allard &
Hauschildt (1995ApJ...445..433A 1995ApJ...445..433A). The models described in the
accompanying paper (Lejeune et al. (1997A&AS..125..229L 1997A&AS..125..229L) are given
here as part of a more extensive data set including M dwarf model
spectra, which will be presented in a forthcoming paper (Lejeune et
al., 1998, Cat. J/A+AS/130/65). A correction procedure has been
applied to the theoretical energy in order to calibrate fluxes on
empirical-temperature relations (see also Lejeune et al., 1998, Cat.
J/A+AS/130/65). The library is given here in its two versions : the
first one (files *.ori) containing the "original" flux distributions
-- as given by the original grids of atmosphere models --, but
rebinned on a common wavelength scale (see also Leitherer et al.
1996PASP..108..996L 1996PASP..108..996L) and the second one (files *.cor) which provides
the "corrected" flux distributions. Each version of the library
contains an ASCII file of models for each of the 19 values of the
metallicity ([M/H]=-5.0, -4.5, -4.0, -3.5, -3.0, -2.5, -2.0, -1.5,
-1.0, -0.5, -0.3, -0.2, -0.1, 0.0, +0.1, +0.2, +0.3, +0.5 and +1.0),
named as lcbxxx.yyy, where xxx designates the metallicity (ex:
'm15' --> [M/H]=-1.5), and yyy identifies the library version. For
each model (out of the total of 8315 models), a flux spectrum is given
for the (same) set of 1221 wavelength points covering the range 9.1 to
160000 nm, with a mean resolution of 10Å in the UV and 20Å in
the visible. In addition to the 19 metallicity files, two individual
files originating from the Kurucz (1991, in Precision Photometry:
Astrophysics of the Galaxy, Davis Philip A.G., Upgren A.R. & Janes
K.A. (eds.). Schenectady, NY, L. Davis Press, Inc., 1991, pp. 27-44))
models are given, lcbsun.ori and lcbvega.ori, which provide
theoretical flux distributions for the Sun and Vega respectively.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
models.dat 62 8382 Summary of parameters
lcbm01.ori 80 79881 Original flux distributions for [M/H] = -0.1
lcbm02.ori 80 79881 Original flux distributions for [M/H] = -0.2
lcbm03.ori 80 79881 Original flux distributions for [M/H] = -0.3
lcbm05.ori 80 80409 Original flux distributions for [M/H] = -0.5
lcbm10.ori 80 80057 Original flux distributions for [M/H] = -1.0
lcbm15.ori 80 80409 Original flux distributions for [M/H] = -1.5
lcbm20.ori 80 75657 Original flux distributions for [M/H] = -2.0
lcbm25.ori 80 75305 Original flux distributions for [M/H] = -2.5
lcbm30.ori 80 76889 Original flux distributions for [M/H] = -3.0
lcbm35.ori 80 75833 Original flux distributions for [M/H] = -3.5
lcbm40.ori 80 74601 Original flux distributions for [M/H] = -4.0
lcbm45.ori 80 69321 Original flux distributions for [M/H] = -4.5
lcbm50.ori 80 68265 Original flux distributions for [M/H] = -5.0
lcbp00.ori 80 82345 Original flux distributions for [M/H] = 0.0
lcbp01.ori 80 81289 Original flux distributions for [M/H] = 0.1
lcbp02.ori 80 80585 Original flux distributions for [M/H] = 0.2
lcbp03.ori 80 80057 Original flux distributions for [M/H] = 0.3
lcbp05.ori 80 79705 Original flux distributions for [M/H] = 0.5
lcbp10.ori 80 66153 Original flux distributions for [M/H] = 1.0
lcbvega.ori 80 329 Original flux distributions for Vega
lcbsun.ori 80 329 Original flux distributions for the Sun
lcbm01.cor 80 79881 Corrected flux distributions for [M/H] = -0.1
lcbm02.cor 80 79881 Corrected flux distributions for [M/H] = -0.2
lcbm03.cor 80 79881 Corrected flux distributions for [M/H] = -0.3
lcbm05.cor 80 80409 Corrected flux distributions for [M/H] = -0.5
lcbm10.cor 80 80057 Corrected flux distributions for [M/H] = -1.0
lcbm15.cor 80 80409 Corrected flux distributions for [M/H] = -1.5
lcbm20.cor 80 75657 Corrected flux distributions for [M/H] = -2.0
lcbm25.cor 80 75129 Corrected flux distributions for [M/H] = -2.5
lcbm30.cor 80 76889 Corrected flux distributions for [M/H] = -3.0
lcbm35.cor 80 75833 Corrected flux distributions for [M/H] = -3.5
lcbm40.cor 80 74601 Corrected flux distributions for [M/H] = -4.0
lcbm45.cor 80 69321 Corrected flux distributions for [M/H] = -4.5
lcbm50.cor 80 68265 Corrected flux distributions for [M/H] = -5.0
lcbp00.cor 80 82345 Corrected flux distributions for [M/H] = 0.0
lcbp01.cor 80 81289 Corrected flux distributions for [M/H] = 0.1
lcbp02.cor 80 80585 Corrected flux distributions for [M/H] = 0.2
lcbp03.cor 80 80057 Corrected flux distributions for [M/H] = 0.3
lcbp05.cor 80 79705 Corrected flux distributions for [M/H] = 0.5
lcbp10.cor 80 66153 Corrected flux distributions for [M/H] = 1.0
read_lcb.f 79 68 Fortran program to read the model spectra
--------------------------------------------------------------------------------
See also:
VI/39 : Model Atmospheres (Kurucz, 1979)
VI/78 : Theoretical Stellar Flux Spectra for F- to K-type Stars (Buser+ 1992)
J/A+AS/105/311 : M giants spectra and photometry (Fluks+, 1994)
J/A+AS/130/65 : A standard stellar library. II. (Lejeune+ 1998)
Byte-by-byte Description of file: models.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 K Teff Effective Temperature of Model
7- 11 F5.2 [cm/s2] logg Gravity of Model
13- 17 F5.2 [Sun] [M/H] Metallicity of Model
19- 23 F5.2 km/s Vturb Microturbulence velocity
25- 29 F5.2 ---- xh Mixing-length parameter
31- 41 A11 --- oFluxes Name of file containing the "original" fluxes
44- 46 I3 --- oMod Original model number within file oFluxes
48- 58 A11 --- cFluxes Name of file containing the "corrected" fluxes
60- 62 I3 --- cMod ? Corrected model number within file oFluxes
--------------------------------------------------------------------------------
Structure of file lcbxxx.yyy:
------------------------------------------------------------------------------
Records Format Explanations
------------------------------------------------------------------------------
1- 153 8F10.1 Set of 1221 wavelengths (in nm)
Blocks of model fluxes.
154 2I6, 4F6.2 Each block contains in the first line an
identifier as follows
model number, Teff, logg, [M/H] , Vturb, xh
155- 328 174(7E11.4) 1221 values of the blanketed emergent surface
329 3E11.4 flux, expressed as flux moment (in mW/m2/Hz
or ergs/s/cm/cm/Hz), Hnu
329-82345 2I6,4F6.2/7E11.4 Repeating the above for maximum 466 other
Teff, logg and [M/H] values
Note about the parameters:
Teff is the effective temperature
logg the logarithm of the surface gravity
[M/H] the metallicity
Vturb the microturbulent velocity
xh the mixing-length parameter
For the M stars (Teff<3500K), the parameters Vturb and xh have no
meaning here and have been arbitrary fixed to 0.0
Note about the units :
As Hnu is expressed as flux moment in the units erg/s/cm2/Hz
(SI: mW/m2/Hz),
Flambda, in units ergs/s/cm2/Angstrom, must be calculated from
Hnu using the equation
Flambda=0.4*Hnu*c/lambda/lambda, (1)
where c=2.997925e17.......is the velocity of light and
lambda........is the wavelength in nanometers (as tabulated at the
beginning of each file lcbxxx.yyy)
The numerical factor of 0.4 (=4*0.1) in equation (1) above comes from the
conversion of the flux moment into flux (*4) and from the conversion of flux
per nanometer into flux per Angstrom (*0.1).
NOTICE however that Flambda still is a surface flux; therefore, calculations
of absolute luminosities for the present models require additional assumptions
about the radii of the stars represented by the models.
Within each file, the individual models are listed with Teff increasing, and
logg increasing at a given Teff.
-----------------------------------------------------------------------------
Acknowledgements: Thibault Lejeune
(End) Lejeune [Ast. Inst. Univ. Basel], Patricia Bauer [CDS] 28-Nov-1997