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THE YOUNG AND BRIGHT TYPE IA SUPERNOVA ASASSN-141p: DISCOVERY, EARLY-TIME OBSERVATIONS, FIRST-LIGHT TIME, DISTANCE TO NGC 4666, AND PROGENITOR CONSTRAINTS
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Number of Authors: 33
2016 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 826, no 2, 144Article in journal (Refereed) Published
Abstract [en]

On 2014 December 9.61, the All-sky Automated Survey for SuperNovae (ASAS-SN or Assassin) discovered ASASSN-141p just similar to 2 days after first light using a global array of 14 cm diameter telescopes. ASASSN-141p went on to become a bright supernova (V = 11.94 mag), second only to SN 2014J for the year. We present prediscovery photometry (with a detection less than a day after first light) and ultraviolet through near-infrared photometric and spectroscopic data covering the rise and fall of ASASSN-141p for more than 100 days. We find that ASASSN-141p had a broad light curve (Delta m(15) (B) = 0.80 +/- 0.05), a B-band maximum at 2457015.82 +/- 0.03, a rise time of 16.941(-0.10)(+0.11) days, and moderate host-galaxy extinction (E (B - V)host = 0.33 +/- 0.06). Using ASASSN-141p, we derive a distance modulus for NGC 4666 of mu = 30.8 +/- 0.2, corresponding to a distance of 14.7 +/- 1.5 Mpc. However, adding ASASSN-141p to the calibrating sample of Type Ia supernovae still requires an independent distance to the host galaxy. Finally, using our early-time photometric and spectroscopic observations, we rule out red giant secondaries and, assuming a favorable viewing angle and explosion time, any nondegenerate companion larger than 0.34 RG(circle dot).

Place, publisher, year, edition, pages
2016. Vol. 826, no 2, 144
Keyword [en]
galaxies: distances and redshifts, supernovae: individual (ASASSN-141p, Type Ia, NGC 4666, ASASSN-141p), white dwarfs
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-134447DOI: 10.3847/0004-637x/826/2/144ISI: 000381977900044OAI: oai:DiVA.org:su-134447DiVA: diva2:1033851
Available from: 2016-10-10 Created: 2016-10-06 Last updated: 2017-11-30Bibliographically approved

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Taddia, Francesco
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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