Show simple item record

Very high‐energy observations of psr b1951+32

dc.contributor.authorSrinivasan, R.
dc.contributor.authorBoyle, P. J.
dc.contributor.authorBuckley, J. H.
dc.contributor.authorCarter‐Lewis, D. A.
dc.contributor.authorCatanese, M.
dc.contributor.authorCawley, M. F.
dc.contributor.authorColombo, E.
dc.contributor.authorFegan, D. J.
dc.contributor.authorFinley, J. P.
dc.contributor.authorGaidos, J. A.
dc.contributor.authorGordo, J. Bussons
dc.contributor.authorHillas, A. M.
dc.contributor.authorKrennrich, F.
dc.contributor.authorLamb, R. C.
dc.contributor.authorLessard, R. W.
dc.contributor.authorMcEnery, J. M.
dc.contributor.authorMoriarty, P.
dc.contributor.authorQuinn, J.
dc.contributor.authorRose, H. J.
dc.contributor.authorSamuelson, F. W.
dc.contributor.authorSembroski, G.
dc.contributor.authorWeekes, T. C.
dc.contributor.authorWilson, C.
dc.contributor.authorZweerink, J.
dc.date.accessioned2018-08-24T08:26:28Z
dc.date.available2018-08-24T08:26:28Z
dc.date.issued1997-11-01
dc.identifier.citationSrinivasan, R. Boyle, P. J.; Buckley, J. H.; Carter‐Lewis, D. A.; Catanese, M.; Cawley, M. F.; Colombo, E.; Fegan, D. J.; Finley, J. P.; Gaidos, J. A.; Gordo, J. Bussons; Hillas, A. M.; Krennrich, F.; Lamb, R. C.; Lessard, R. W.; McEnery, J. M.; Moriarty, P.; Quinn, J.; Rose, H. J.; Samuelson, F. W.; Sembroski, G.; Weekes, T. C.; Wilson, C.; Zweerink, J. (1997). Very high‐energy observations of psr b1951+32. The Astrophysical Journal 489 (1), 170-174
dc.identifier.issn0004-637X,1538-4357
dc.identifier.urihttp://hdl.handle.net/10379/9902
dc.description.abstractPSR B1951 + 32 is a gamma-ray pulsar detected by the Energetic Gamma Ray Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The pulsar energy spectrum is consistent with an unbroken power law with differential photon index of -1.8 +/- 0.1 between 50 MeV and 10 GeV. The EGRET data shows no evidence for a spectral turnover. Here we report on the first observations of PSR B1951 + 32 beyond 30 GeV. The observations were carried out with the 10 m gamma-ray telescope at the Whipple Observatory on Mount Hopkins, Arizona. In 8.1 hours of observation we find no evidence for steady or periodic emission from PSR B1951 + 32 above similar to 260 GeV, Flux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models.
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.subjectgamma rays, observations
dc.subjectpulsars, individual (psr b1951+32)
dc.subjectsupernova remnants
dc.subjectgamma-rays
dc.subjectpulsar
dc.subjectradiation
dc.subjectnebula
dc.titleVery high‐energy observations of psr b1951+32
dc.typeArticle
dc.identifier.doi10.1086/304781
dc.local.publishedsourcehttp://iopscience.iop.org/article/10.1086/304781/pdf
nui.item.downloads0


Files in this item

Thumbnail
Name:
license.txt
Size:
5.659Kb
Format:
Text file
View/Open

This item appears in the following Collection(s)

Show simple item record

Attribution-NonCommercial-NoDerivs 3.0 Ireland
Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 Ireland