Lucas, P.Minniti, D.Kamble, A.Kaplan, D.Cross, N.Dekany, I.Ivanov, V.Kurtev, R.Saito, R.Smith, L.Catelan, M.Masetti, N.2021-07-152021-07-152020-01Monthly Notices of the Royal Astronomical Society, Volume 492, Issue 4, Pages 4847 - 4857, 20200035-8711http://repositorio.unab.cl/xmlui/handle/ria/19404Indexación: Scopus.A 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 2 yr. The 1.6-22 μm spectral energy distribution in March 2010 was well fit by a highly obscured blackbody 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 ≈ 0.01-0.02), which suggests a physical association, e.g. a collision between low mass protostars. However, blackbody 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 d after the explosion. Radio follow-up with the Australia Telescope Compact Array 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 = 0.13-0.24. After weighing several options, it appears likely that VVV-WIT-01 was a classical nova event located behind an IRDC.enInfrared: starsISM: cloudsNovaecataclysmic variablesStars: formationArtículoDOI: 10.1093/MNRAS/STAA155