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Optical Observations of PSR J0205+6449

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dc.contributor.author Shearer, Andrew en
dc.date.accessioned 2011-03-10T16:59:16Z en
dc.date.available 2011-03-10T16:59:16Z en
dc.date.issued 2008 en
dc.identifier.citation A. Shearer and V. V. Neustroev...(2008)Optical Observations of PSR J0205+6449, A. Shearer and V. V. Neustroev en
dc.identifier.uri http://hdl.handle.net/10379/1736 en
dc.description.abstract PSR J0205+6449 is a X-ray and radio pulsar in supernova remnant 3C 58. We report on observations of the central region of 3C 58 using the 4.2-m William Herschel Telescope with the intention of identifying the optical counterpart of PSR J0205+6449 and characterising its pulsar wind nebula. Around the pulsar position we identified extended emission with a magnitude of $B = 23 \fm 97 \pm 0.10$, $V = 22 \fm 95 \pm 0.05$ and $R = 22 \fm 15 \pm 0.03$ consistent with a pulsar wind nebula. From the R-band image we identified three knots with $m_R$ = $24 \fm 08 \pm 0.07$ (o1), $24 \fm 15 \pm 0.07$ (o2) and $24 \fm 24 \pm 0.08$ (o3). We confirm the presence of an optical pulsar wind nebula around PSR J0205+6449 and give an upper limit of $m_R \approx$ 24 for the optical magnitude of the pulsar. Furthermore we make the tentative suggestion that our object o1, with an $m_R \approx$ 24.08 is the optical counterpart. If confirmed the pulsar would have an $L_R/L_x\approx 0.004$ and an optical efficiency of about 5% of the Crab pulsar. Such a low efficiency is more consistent with the characteristic age of the pulsar rather than that of SN 1181. en
dc.format application/pdf en
dc.language.iso en en
dc.subject Astrophysics en
dc.title Optical Observations of PSR J0205+6449 en
dc.type Article en
dc.local.publishedsource http://arxiv.org/pdf/0807.0983 en
dc.description.peer-reviewed peer-reviewed en
dc.local.authors A. Shearer and V. V. Neustroev en
dc.local.arxivid 0807.0983 en

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