Uv Photometry of the Degenerate X-Ray Binary in NGC6712

Details Uv Photometry of the Degenerate X-Ray Binary in NGC6712 Uv Photometry of the Degenerate X-Ray Binary in NGC6712

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6121c&link_type=abstract

HST Proposal ID #6121

Physics

Hst Proposal Id #6121 Hot Stars

Scientific paper

Ground-based imaging has revealed the optical counterpart of the luminous X- ray binary in the globular cluster NGC6712. It is a faint UV star with an indication of up to 0.4 mag variability. However, at B=21.2 and crowded by two brighter stars within 1 arcsec, only HST WFPC photometry will enable a detailed light curve of the X-ray source to be obtained. Given the distance to the cluster the X-ray source has M_V=5.6 which makes it a prime candidate for an underluminous and hence degenerate secondary. The orbital period will thus lie below 80 mins and is likely to be in the range 10--60 mins. With evidence already for variability we propose here for time -resolved CCD photometry to measure the orbital period and light curve in the UV, and thus confirm its degenerate nature. This would be a remarkable result as 2 of the 3 identified (optical/UV) sources in globular clusters would be degenerate, with important implications for the formation and evolution of globular cluster X-ray binaries.

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