Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.4311h&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #43.11; Bulletin of the American Astronomical Society, Vol. 24, p.1188
Other
Scientific paper
The globular cluster M3 was observed twice with the ROSAT HRI\null. The low luminosity X-ray source 1E1339.8+2837 was detected at a luminosity of 1.1*E(35) ergs s(-1) during January 1992. The source was not detected in June 1992, and the upper limit (<2.8times 10(33) ergs s(-1) ) is consistent with the flux observed with the Einstein IPC in January 1981. During its bright phase (January 1992), 1E1339.8+2837 was very soft, with no counts detected above PHA channel 5. The position of 1E1339.8+2837 has been measured with an uncertainty of <3''. It is located 1 core radius (r_c = 25'') from the optical center of M3. Searches for radio, optical, and ultraviolet counterparts have been unsuccessful, though the severe crowding in M3's core makes the task difficult. We discuss the implications of the factor of 40 variability and extremely soft color of 1E1339.8+2837 for models of low luminosity globular cluster X-ray sources. The low ratio of maximum to minimum X-ray luminosity is inconsistent with a transient X-ray binary (neutron star primary), and the maximum luminosity rules out a coronal outburst. A dwarf nova (white dwarf primary) in outburst is consistent with the observations. 1E1339.8+2837 is more X-ray luminous than dwarf novae outbursts observed in the galactic plane, and it appears similar to the low luminosity X-ray source in the core of the globular cluster 47 Tuc. The extremely low reddening to M3 (E_B-V < 0.01) allows the soft outburst to be seen; a similar outburst would probably not be visible from any other X-ray globular cluster.
Bailyn Charles D.
Grindlay Jonathon E.
Hertz Paul
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