SED for 7 stellar calibrators (Dehaes+, 2011)

Details SED for 7 stellar calibrators (Dehaes+, 2011) SED for 7 stellar calibrators (Dehaes+, 2011)

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ycat..35339107d&link_type=abstract

VizieR On-line Data Catalog: J/A+A/533/A107. Originally published in: 2011A&A...533A.107D

Physics

Stars: Giant, Models, Spectroscopy, Energy Distributions

Scientific paper

This catalogue presents the theoretical spectral energy distributions for 7 stellar calibrators of the ESA Herschel satellite in the wavelength range from 2 to 200 micron.
The stellar atmosphere model and theoretical spectrum are generated using the MARCS theoretical stellar atmosphere code (Gustafsson et al., 1975A&A....42..407G and further updates; Gustafsson et al. 2003A&A...400..709D) and the TURBOSPECTRUM synthetic spectrum code (Plez et al., 1992A&A...256..551P). Stellar parameters (and uncertainties thereon) have been derived by Decin et al. (2003A&A...400..709D) and are described in the text files added to this catalogue. The line lists used in the spectrum calculation are discussed in Decin (2000, PhD Thesis, Leuven University) and Decin and Eriksson (2007A&A...472.1041D).
The outermost depth point of the theoretical atmosphere model was taken at log(taulambda)=-7.2 with lambda being 2.2 micron. The atmosphere model was calculated with a spherically symmetric (parallel for Sirius) geometry, under the assumption of radiative and hydrostatic equilibrium, local thermodynamic equilibrium (LTE) and homogeneous layers.
The original theoretical spectrum was calculated at a resolution of Δλ=0.5Å, and then degraded to a resolution of λ/Δλ=5000 applying a gaussian convolution. The wavelength coverage is from 2 to 200 micron.
Uncertainties on the theoretical spectrum predictions are discussed in depth in Decin & Eriksson (2007A&A...472.1041D).
Absolute flux calibration is based on Selby (1988A&AS...74..127S) K-band (TCS for Sirius) photometry
Zero-point is determined on the basis of an ideal 'Vega', i.e. the K-band photometry of Vega is corrected for a flux excess of 1.29% (cf. Absil et al. 2006A&A...452..237A). The determined Selby K-band zeropoint is 4.0517E-10 W/m2/um. The determined TCS K-band zeropoint is 4.4506E-10W/m2/um (for Sirius)
The estimated absolute flux uncertainty is 1%
These theoretical spectra should be referenced as Decin & Eriksson (2007A&A...472.1041D).
(3 data files).

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