Astron. Astrophys. 360, 559-561 (2000)

An EUVE observation of the globular cluster NGC 1851: The second EUV detection of a low mass X-ray binary?

P.J. Callanan ¹, J.J. Drake ², A. Fruscione ² and D. Christian <sup>3

1</sup> University College, Department of Physics, Cork, Ireland (paulc@ucc.ie)
² Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA (jdrake@head-cfa.harvard.edu; antonell@head-cfa.harvard.edu)
³ Space Telescope Science Institute, Computer Sciences Corporation, 3700 San Martin Drive, Baltimore, MD 21218, USA (dchrist@stsci.edu)

Received 10 January 2000 / Accepted 25 May 2000

Abstract

We have detected EUV emission from the globular cluster NGC 1851, using the Deep Survey Photometer aboard the Extreme Ultraviolet Explorer (EUVE). The minimum EUV luminosity implied by our detection is 10³⁵ - 10³⁶ ergs s^-1, for a distance and reddening appropriate to NGC 1851. This is only the second detection of a globular cluster at EUV energies. If this flux is due to the cluster LMXB X0512-401, then the observed EUV luminosity is likely to be comparable to the 2-10 keV X-ray luminosity of the LMXB. With the detection of EUV emission from M15, these observations suggest that the EUV flux of LMXBs in general may represent a sizable fraction of their total bolometric luminosity. However, additional observations are needed to conclusively show that these cluster LMXBs (X0512-401 and AC211) indeed dominate the cluster EUV emission. Finally, we compare our NGC 1851 measurement with the EUVE detection of the X-ray transient XTE J1118+480 during outburst, and show that these objects appear to have comparable EUV luminosities.

Key words: stars: binaries: close Galaxy: globular clusters: individual: NGC 1851 stars: individual: X0512-401 stars: individual: XTE J1118+480

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Contents

• 1. Introduction
• 2. Observations and data reduction
• 3. Discussion
• 4. The origin of the EUV emission from NGC 1851
• 5. Comparison with XTE J1118+480
• 6. Conclusions
• Acknowledgements
• References

© European Southern Observatory (ESO) 2000

Online publication: August 17, 2000
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