X-ray identification of the soft γ-ray repeater 1806 - 20

Details X-ray identification of the soft γ-ray repeater 1806 - 20 X-ray identification of the soft γ-ray repeater 1806 - 20

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994natur.368..127m&link_type=abstract

Nature, Volume 368, Issue 6467, pp. 127-129 (1994).

Astronomy and Astrophysics

Astronomy

139

Scientific paper

THE nature of γ-ray bursters-astrophysical sources that emit abrupt bursts of γ-rays-presents a long-standing question in high-energy astronomy. Soft γ-ray repeaters (SGRs) are distinguished from classical γ-ray bursters by the short duration, softer γ-ray spectrum and recurrent activity of their outbursts1-6. Millisecond-scale structure in these bursts suggests that SGRs are compact, and many models invoke neutron stars as the emitting objects1,5. This idea is supported by the association of two SGRs, SGR0526 - 66 (ref. 6) and SGR1806 - 20 (ref. 7), with supernova remnants, SNR N49 and the radio nebula G10.0 - 0.3 respectively. Very recently, Kulkarni et al.8,9 have suggested that a compact radio source in G10.0 - 0.3 corresponds to a young pulsar at the centre of this nebula, and can be identified with SGR1806 - 20. Here we report the detection of a burst from SGR1806 - 20 with the X-ray satellite ASCA10, which allows us to identify the burster with a new X-ray source which we designate AX1805.7 - 2025. The burst is coincident in time with that detected by the BATSE11,12 instrument on board the Compton Gamma Ray Observatory. This result provides strong evidence that SGRs are indeed neutron stars.

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