Optical identification of the X-ray source GS 2023 + 338 as V404 Cygni

Details Optical identification of the X-ray source GS 2023 + 338 as V404 Cygni Optical identification of the X-ray source GS 2023 + 338 as V404 Cygni

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...378..293w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 378, Sept. 1, 1991, p. 293-297.

Other

27

Balmer Series, Emission Spectra, Iue, Light Curve, X Ray Sources, Accretion Disks, Helium, Nitrogen, Oxygen

Scientific paper

A bright new X-ray transient is identified with V404 Cygni. Photometry with the fine error sensor on the IUE satellite on May 27.3, 1989, yielded about 12.6, about 6 mag brighter than the quiescent magnitude. Optical spectroscopy on May 27.4, 1989, revealed a strong and rich emission-line spectrum superposed on a reddened continuum. The outburst spectrum shows strong Balmer, He I, He II 4686 A, and N III 4634-42 A emission lines as well as numerous interstellar absorption lines. The near-ultraviolet O III Bowen fluorescence lines at 3429-3444 A and possibly the complex between 3750-3790 A are present in these early spectra. These emission features are characteristics of the optical counterparts of various X-ray sources including X-ray bursters and two other X-ray novae. Photometrically, the source exhibits fluctuations of a magnitude or more on time scales of days, minutes, and possible seconds. The optical light curve exhibits a similarity to the X-ray light curve, suggesting that X-ray heating of an accretion disk plays a role in producing the optical emission.

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