Optical photometry of the type Ia supernova 1999ee and the type Ib/c supernova 1999ex in IC 5179
Author
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Stritzinger, Maximiliam
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Hamuy Wackenhut, Mario
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Suntzeff, Nicholas B.
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Smith, R. C.
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Phillips, M. M.
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Maza Sancho, José
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Strolger, L. G.
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Antezana, Roberto
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González, Luis
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Wischnjewsky, Marina
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Candia, Pablo
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Espinoza, Juan
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González, David
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Stubbs, Christopher
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Becker, A. C.
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Rubenstein, Eric P.
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Author
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Galaz, Gaspar, 1967-
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Admission date
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2014-01-08T17:06:24Z
Available date
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2014-01-08T17:06:24Z
Publication date
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2002-10
Cita de ítem
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The Astronomical Journal, 124:2100–2117, 2002 October
en_US
Identifier
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https://repositorio.uchile.cl/handle/2250/126062
General note
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Artículo de publicación ISI
en_US
Abstract
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We present UBVRIz light curves of the Type Ia SN 1999ee and the Type Ib/c SN 1999ex, both located in
the galaxy IC 5179. SN 1999ee has an extremely well-sampled light curve spanning from 10 days before Bmax
through 53 days after peak. Near maximum, we find systematic differences of 0.05 mag in photometry measured
with two different telescopes, even though the photometry is reduced to the same local standards
around the supernova using the specific color terms for each instrumental system. We use models for our
bandpasses and spectrophotometry of SN 1999ee to derive magnitude corrections (S-corrections) and remedy
this problem. This exercise demonstrates the need of accurately characterizing the instrumental system
before great photometric accuracies of Type Ia supernovae can be claimed. It also shows that this effect can
have important astrophysical consequences, since a small systematic shift of 0.02 mag in the B V color can
introduce a 0.08 mag error in the extinction-corrected peak B magnitude of a supernova and thus lead to
biased cosmological parameters. The data for the Type Ib/c SN 1999ex present us with the first ever observed
shock breakout of a supernova of this class. These observations show that shock breakout occurred 18 days
before Bmax and support the idea that Type Ib/c supernovae are due to the core collapse of massive stars
rather than thermonuclear disruption of white dwarfs.