Optical identification of 2S 1417-62

Details Optical identification of 2S 1417-62 Optical identification of 2S 1417-62

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...276..621g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 15, 1984, p. 621-624.

Astronomy and Astrophysics

Astronomy

24

Astronomical Spectroscopy, Binary Stars, Pulsars, Visible Spectrum, X Ray Sources, X Ray Stars, B Stars, O Stars, Spectral Resolution, Ubv Spectra, X Ray Astronomy, X Ray Spectra

Scientific paper

The 17 s X-ray pulsar 2S 1417-62 has been identified with a V of approximately 16.9 mag OB star on the basis of an X-ray position obtained with the Einstein X-Ray Observatory and spectrophotometry with the 4-m telescope at Cerro Tololo Inter-American Observatory. Strong H-alpha emission is observed as well as significant changes in X-ray luminosity. The optical counterpart may be either a Be or a B I star, but the H-alpha emission strength and galactic position suggest that a Be star is more likely. A Be star identification also further supports the limit of approximately 15 days or more on the system binary period obtained by Kelley et al. (1981) from pulse timing studies.

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