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A 2.14 ms Candidate Optical Pulsar in SN1987A | J. Middleditch
; J. A. Kristian
; W. E. Kunkel
; K. M. Hill
; R. M. Watson
; R. Luicio
; J. N. Imamura
; T. Y. Steiman-Cameron
; A. Shearer
; M. Redfern
; R. Butler
; A. C. Danks.
; | Date: |
2 Oct 2000 | Subject: | astro-ph | Affiliation: | 2 and 3), W. E. Kunkel , K. M. Hill, R. M. Watson, R. Luicio, J. N. Imamura, T. Y. Steiman-Cameron, A. Shearer, M. Redfern and R. Butler, A. C. Danks. ( Los Alamos National Lab., The Carnegie Observatories, Deceased, U. of Tasmania, Indep. Consultan | Abstract: | We have monitored Supernova 1987A in optical/near-infrared bands from a few weeks following its birth until the present time in order to search for a pulsar remnant. We have found an apparent pattern of emission near the frequency of 467.5 Hz - a 2.14 ms pulsar candidate, first detected in data taken on the remnant at the Las Campanas Observatory (LCO) 2.5-m Dupont telescope during 14-16 Feb. 1992 UT. We detected further signals near the 2.14 ms period on numerous occasions over the next four years in data taken with a variety of telescopes, data systems and detectors, at a number of ground- and space-based observatories. The sequence of detections of this signal from Feb. `92 through August `93, prior to its apparent subsequent fading, is highly improbable (< 1.e-10) for any noise source). We also find evidence for modulation of the 2.14 ms period with a ~1,000 s period which, when taken with the high spindown of the source (2-3e-10 Hz/s), is consistent with precession and spindown via gravitational radiation of a neutron star with a non-axisymmetric oblateness of ~1e-6, and an implied gravitational luminosity exceeding that of the Crab Nebula pulsar by an order of magnitude. | Source: | arXiv, astro-ph/0010044 | Services: | Forum | Review | PDF | Favorites |
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