PSR B1951+32 and PSR J0537-6910 - where are the optical counterparts?

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dc.creatorButler, R. F.
dc.creatorGolden, A.
dc.creatorShearer, A.
dc.creatorGouiffes, C.
dc.date2002-08-29
dc.date2002-09-09
dc.date.accessioned2026-07-07T02:04:51Z
dc.date.available2026-07-07T02:04:51Z
dc.descriptionThere remain several definitive gamma-ray pulsars that are as yet undetected in the optical regime. A classic case is the pulsar PSR B1951+32, associated with the complex CTB 80 SNR. Previous ground based high speed 2-d optical studies have ruled out candidates to m_V ~ 24. Hester (2000) has reported an analysis of archival HST/WFPC2 observations of the CTB 80 complex which suggest a compact synchrotron nebula coincident with the pulsar's radio position. Performing a similar analysis, we have identified a possible optical counterpart within this synchrotron nebula at m_V ~ 25.5, and another optical counterpart candidate nearby at m_V ~ 24.2. PSR J0537-6910 is a young (canonical age ~ 5000 years), 16ms pulsar in the LMC. We report a search for optical pulsations from the region around the X-ray position. We see no obvious candidate exhibiting optical pulsations at the X-ray period, with a 3 sigma upper limit of m_V ~ 23.6. We have also examined recent Chandra results (Wang et al. 2001) and show that their X-ray-Optical astrometry is in error by about 7''.
dc.description4 pages, 4 figures, 2 tables. To appear in the Proceedings of the 270. WE-Heraeus Seminar on Neutron Stars, Pulsars and Supernova Remnants, Jan. 21-25, 2002, Physikzentrum Bad Honnef, eds W.Becker, H.Lesch & J.Truemper. Proceedings are available as MPE-Report 278
dc.identifierhttps://arxiv.org/abs/astro-ph/0208534
dc.identifierhttp://arxiv.org/abs/astro-ph/0208534
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/4918
dc.subjectAstrophysics
dc.titlePSR B1951+32 and PSR J0537-6910 - where are the optical counterparts?
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