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dc.contributor.authorBhandari, S.
dc.contributor.authorKeane, E.
dc.contributor.authorBarr, E.
dc.contributor.authorJameson, A.
dc.contributor.authorPetroff, E.
dc.contributor.authorJohnston, S.
dc.contributor.authorBailes, M.
dc.contributor.authorBhat, Ramesh
dc.contributor.authorBurgay, M.
dc.contributor.authorBurke-Spolaor, S.
dc.contributor.authorCaleb, M.
dc.contributor.authorEatough, R.
dc.contributor.authorFlynn, C.
dc.contributor.authorGreen, J.
dc.contributor.authorJankowski, F.
dc.contributor.authorKramer, M.
dc.contributor.authorVenkatraman Krishnan, V.
dc.contributor.authorMorello, V.
dc.contributor.authorPossenti, A.
dc.contributor.authorStappers, B.
dc.contributor.authorTiburzi, C.
dc.contributor.authorvan Straten, W.
dc.contributor.authorAndreoni, I.
dc.contributor.authorButterley, T.
dc.contributor.authorChandra, P.
dc.contributor.authorCooke, J.
dc.contributor.authorCorongiu, A.
dc.contributor.authorCoward, D.
dc.contributor.authorDhillon, V.
dc.contributor.authorDodson, R.
dc.contributor.authorHardy, L.
dc.contributor.authorHowell, E.
dc.contributor.authorJaroenjittichai, P.
dc.contributor.authorKlotz, A.
dc.contributor.authorLittlefair, S.
dc.contributor.authorMarsh, T.
dc.contributor.authorMickaliger, M.
dc.contributor.authorMuxlow, T.
dc.contributor.authorPerrodin, D.
dc.contributor.authorPritchard, T.
dc.contributor.authorSawangwit, U.
dc.contributor.authorTerai, T.
dc.contributor.authorTominaga, N.
dc.contributor.authorTorne, P.
dc.contributor.authorTotani, T.
dc.contributor.authorTrois, A.
dc.contributor.authorTurpin, D.
dc.contributor.authorNiino, Y.
dc.contributor.authorWilson, R.
dc.contributor.authorAlbert, A.
dc.contributor.authorAndré, M.
dc.contributor.authorAnghinolfi, M.
dc.contributor.authorAnton, G.
dc.contributor.authorArdid, M.
dc.contributor.authorAubert, J.
dc.contributor.authorAvgitas, T.
dc.contributor.authorBaret, B.
dc.contributor.authorBarrios-Martí, J.
dc.contributor.authorBasa, S.
dc.contributor.authorBelhorma, B.
dc.contributor.authorBertin, V.
dc.contributor.authorBiagi, S.
dc.contributor.authorBormuth, R.
dc.contributor.authorBourret, S.
dc.contributor.authorBouwhuis, M.
dc.contributor.authorBranzas, H.
dc.contributor.authorBruijn, R.
dc.contributor.authorBrunner, J.
dc.contributor.authorBusto, J.
dc.contributor.authorCapone, A.
dc.date.accessioned2018-05-18T07:56:16Z
dc.date.available2018-05-18T07:56:16Z
dc.date.created2018-05-18T00:23:02Z
dc.date.issued2018
dc.identifier.citationBhandari, S. and Keane, E. and Barr, E. and Jameson, A. and Petroff, E. and Johnston, S. and Bailes, M. et al. 2018. The survey for pulsars and extragalactic radio bursts - II. new FRB discoveries and their follow-up. Monthly Notices of the Royal Astronomical Society. 475 (2): pp. 1427-1446.
dc.identifier.urihttp://hdl.handle.net/20.500.11937/66816
dc.identifier.doi10.1093/mnras/stx3074
dc.description.abstract

We report the discovery of four Fast Radio Bursts (FRBs) in the ongoing SUrvey for Pulsars and Extragalactic Radio Bursts at the Parkes Radio Telescope: FRBs 150610, 151206, 151230 and 160102. Our real-time discoveries have enabled us to conduct extensive, rapid multimessenger follow-up at 12 major facilities sensitive to radio, optical, X-ray, gamma-ray photons and neutrinos on time-scales ranging from an hour to a few months post-burst. No counterparts to the FRBs were found and we provide upper limits on afterglow luminosities. None of the FRBs were seen to repeat. Formal fits to all FRBs show hints of scattering while their intrinsic widths are unresolved in time. FRB 151206 is at low Galactic latitude, FRB 151230 shows a sharp spectral cut-off, and FRB 160102 has the highest dispersion measure (DM = 2596.1 ± 0.3 pc cm -3 ) detected to date. Three of the FRBs have high dispersion measures (DM > 1500 pc cm -3 ), favouring a scenario where theDMis dominated by contributions from the intergalactic medium. The slope of the Parkes FRB source counts distribution with fluences > 2 Jyms is α = -2.2 +0.6 -1.2 and still consistent with a Euclidean distribution (α = -3/2). We also find that the all-sky rate is 1.7 +1.5 -0.9 × 10 3 FRBs/(4π sr)/day above ~2 Jy ms and there is currently no strong evidence for a latitude-dependent FRB sky rate.

dc.publisherOxford University Press
dc.titleThe survey for pulsars and extragalactic radio bursts - II. new FRB discoveries and their follow-up
dc.typeJournal Article
dcterms.source.volume475
dcterms.source.number2
dcterms.source.startPage1427
dcterms.source.endPage1446
dcterms.source.issn0035-8711
dcterms.source.titleMonthly Notices of the Royal Astronomical Society
curtin.note

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

curtin.departmentCurtin Institute of Radio Astronomy (Physics)
curtin.accessStatusOpen access


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