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Pulsed optical emission from psr 0656+14

dc.contributor.authorShearer, A.
dc.contributor.authorRedfern, R. M.
dc.contributor.authorGorman, G.
dc.contributor.authorButler, R.
dc.contributor.authorGolden, A.
dc.contributor.authorO'Kane, P.
dc.contributor.authorBeskin, G. M.
dc.contributor.authorNeizvestny, S. I.
dc.contributor.authorNeustroev, V. V.
dc.contributor.authorPlokhotnichenko, V. L.
dc.contributor.authorCullum, M.
dc.date.accessioned2018-08-24T08:26:24Z
dc.date.available2018-08-24T08:26:24Z
dc.date.issued1997-10-01
dc.identifier.citationShearer, A. Redfern, R. M.; Gorman, G.; Butler, R.; Golden, A.; O'Kane, P.; Beskin, G. M.; Neizvestny, S. I.; Neustroev, V. V.; Plokhotnichenko, V. L.; Cullum, M. (1997). Pulsed optical emission from psr 0656+14. The Astrophysical Journal 487 (2), L181-L185
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/10379/9877
dc.description.abstractUsing data collected with the Special Astrophysical Observatory (SAG) 6 m telescope and the University College Galway (UCG) Transputer Instrument for Fast Image Deconvolution (TRIFFID) imaging photometer, we show that the radio, X-ray, and gamma-ray pulsar PSR 0656+14 exhibits pulsed optical emission. We observed that the pulsed fraction was consistent with 100% and that the flux was higher than that expected from a thermal source. The magnitude of PSR 0656+14 in the B band was observed to be 25.1 +/- 0.3, consistent with previous CCD observations. The peak of the optical signal is at phase 0.2 compared to the radio and in phase with the weak gamma-ray pulse.
dc.publisherIOP Publishing
dc.relation.ispartofThe Astrophysical Journal
dc.rightsAttribution-NonCommercial-NoDerivs 3.0 Ireland
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/3.0/ie/
dc.subjectinstrumentation, detectors
dc.subjectpulsars, individual (psr 0656+14)
dc.subjectx-ray emission
dc.subjectradio pulsars
dc.subjectproper-motion
dc.subjectpsr-0656+14
dc.subjectphenomenology
dc.subjectstars
dc.titlePulsed optical emission from psr 0656+14
dc.typeArticle
dc.identifier.doi10.1086/310888
dc.local.publishedsourcehttp://iopscience.iop.org/article/10.1086/310888/pdf
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