The optical counterpart of the X-ray source H0253+193 - A distant, high-luminosity RS Canum Venaticorum system

Details The optical counterpart of the X-ray source H0253+193 - A distant, high-luminosity RS Canum Venaticorum system The optical counterpart of the X-ray source H0253+193 - A distant, high-luminosity RS Canum Venaticorum system

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...345..346c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 345, Oct. 1, 1989, p. 346-355. Research supported by the Research Corp., NA

Astronomy and Astrophysics

Astronomy

11

Astronomical Photometry, Infrared Photometry, Molecular Clouds, Stellar Luminosity, X Ray Binaries, Far Infrared Radiation, H Alpha Line, Infrared Astronomy Satellite, Optical Polarization, Reflection Nebulae

Scientific paper

Optical and near-infrared photometry in the VRIJHK and CO (2.35 microns) bands and optical spectroscopy and polarimetry reveal that the optical counterpart of the X-ray source H0253+193 is most likely a RS CVn binary system. The results show a visual extinction of 11.3 mag to the star, with an IR excess possibly due a cooler binary companion or circumstellar material. It is suggested that the I-band polarization of 8.1 + or - 1.8 may be induced in the starlight by passage through the molecular cloud. The lack of strong H-alpha emission in the optical spectrum argues against the possibility of a classical T Tauri star, and the IR excess argues against a naked T Tauri star. The wide energy spectrum found in the dereddened optical and near-infrared photometry supports the binary star model.

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