The flux distribution of VEGA for the wavelength region from 10 to 100 microns, and the calibration of IRAS at 12 microns and 25 microns

Details The flux distribution of VEGA for the wavelength region from 10 to 100 microns, and the calibration of IRAS at 12 microns and 25 microns The flux distribution of VEGA for the wavelength region from 10 to 100 microns, and the calibration of IRAS at 12 microns and 25 microns

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...153..273l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 153, no. 1, Dec. 1985, p. 273-277.

Astronomy and Astrophysics

Astronomy

6

A Stars, Infrared Astronomy Satellite, O Stars, Stellar Atmospheres, Stellar Envelopes, Stellar Temperature, B Stars, Calibrating, Early Stars, Infrared Radiation, Stellar Luminosity, Stellar Spectrophotometry

Scientific paper

The IRAS data have been used to investigate the flux distribution of Vega to ascertain whether the circumstellar dust cloud described by Aumann et al., which causes the large excess at λ ≥ 60 μm, could be contributing at shorter wavelengths. Fluxes have been derived around 12 μm (band 1) and 25 μm (band 2) by two methods. One is to use the band 1 and band 2 data for Vega together with the calibration as given in Beichman et al. The other is the application of the infrared flux method to derive effective temperatures for 23 bright stars. Using Vega as calibration, the band 1 and band 2 fluxes are adjusted until the temperatures derived for these stars at these wavelengths agree with those derived at (1 - 5) μm, as in Blackwell et al. and Leggett et al. The 12 μm and 25 μm fluxes determined in these two ways agree well with each other. Vega is then compared to stars of similar spectral types; the observations of Sirius and 33 survey stars are used.

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