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dc.contributor.authorLucas, P. W.
dc.contributor.authorMinniti, D.
dc.contributor.authorKamble, A.
dc.contributor.authorKaplan, D. L.
dc.contributor.authorCross, N.
dc.contributor.authorDekany, I.
dc.contributor.authorIvanov, V. D.
dc.contributor.authorKurtev, R.
dc.contributor.authorSaito, R. K.
dc.contributor.authorSmith, L. C.
dc.contributor.authorCatelan, M.
dc.contributor.authorMasetti, N.
dc.contributor.authorToledo, I.
dc.contributor.authorHempel, M.
dc.contributor.authorThompson, M. A.
dc.contributor.authorPeña, C. Contreras
dc.contributor.authorForbrich, J.
dc.contributor.authorKrause, M.
dc.contributor.authorDale, J.
dc.contributor.authorBorissova, J.
dc.contributor.authorEmerson, J.P.
dc.date.accessioned2020-02-07T01:06:40Z
dc.date.available2020-02-07T01:06:40Z
dc.date.issued2020-03
dc.identifier.citationLucas , P W , Minniti , D , Kamble , A , Kaplan , D L , Cross , N , Dekany , I , Ivanov , V D , Kurtev , R , Saito , R K , Smith , L C , Catelan , M , Masetti , N , Toledo , I , Hempel , M , Thompson , M A , Peña , C C , Forbrich , J , Krause , M , Dale , J , Borissova , J & Emerson , J P 2020 , ' VVV-WIT-01: highly obscured classical nova or protostellar collision? ' , Monthly Notices of the Royal Astronomical Society , vol. 492 , no. 4 , pp. 4847–4857 . https://doi.org/10.1093/mnras/staa155
dc.identifier.issn0035-8711
dc.identifier.otherArXiv: http://arxiv.org/abs/2001.05536v1
dc.identifier.otherORCID: /0000-0001-5392-909X/work/68611415
dc.identifier.otherORCID: /0000-0002-8872-4462/work/68611478
dc.identifier.otherORCID: /0000-0002-9610-5629/work/68611751
dc.identifier.otherORCID: /0000-0001-5252-5771/work/68611752
dc.identifier.otherORCID: /0000-0001-8694-4966/work/68611754
dc.identifier.urihttp://hdl.handle.net/2299/22166
dc.description© 2020 The Author(s).
dc.description.abstractA search of the first Data Release of the VISTA Variables in the Via Lactea (VVV) Survey discovered the exceptionally red transient VVV-WIT-01 (H-Ks=5.2). It peaked before March 2010, then faded by ~9.5 mag over the following two years. The 1.6-22 µm spectral energy distribution in March 2010 was well fit by a highly obscured black body with T ~ 1000 K and AKs ~ 6.6 mag. The source is projected against the Infrared Dark Cloud (IRDC) SDC G331.062-0.294. The chance projection probability is small for any single event (p ≈ 0.01 to 0.02) which suggests a physical association, e.g. a collision between low mass protostars. However, black body emission at T ~ 1000 K is common in classical novae (especially CO novae) at the infrared peak in the light curve, due to condensation of dust ~30-60 days after the explosion. Radio follow up with the Australia Telescope Compact Array (ATCA) detected a fading continuum source with properties consistent with a classical nova but probably inconsistent with colliding protostars. Considering all VVV transients that could have been projected against a catalogued IRDC raises the probability of a chance association to p=0.13 to 0.24. After weighing several options, it appears likely that VVV-WIT-01 was a classical nova event located behind an IRDC.en
dc.format.extent11
dc.format.extent3040829
dc.format.extent2894371
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectastro-ph.SR
dc.subjectastro-ph.GA
dc.titleVVV-WIT-01: highly obscured classical nova or protostellar collision?en
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecord10.1093/mnras/staa155
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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