SN 2009ib: a Type II-P supernova with an unusually long plateau
Author
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Takáts, K.
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Pignata Libralato, Giuliano
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Pumo, M. L.
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Paillas, E.
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Zampieri, L.
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Elias-Rosa, N.
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Benetti, S.
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Bufano, Filomena
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Cappellaro, E.
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Ergon, M.
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Fraser, M.
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Hamuy Wackenhut, Mario
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Inserra, C.
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Kankare, E.
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Smartt, S. J.
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Stritzinger, M. D.
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Van Dyk, S. D.
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Haislip, Joshua B.
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LaCluyze, A. P.
Author
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Moore, J. P.
Author
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Reichart, D.
Admission date
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2015-06-16T19:33:09Z
Available date
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2015-06-16T19:33:09Z
Publication date
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2015
Cita de ítem
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MNRAS 450, 3137–3154 (2015)
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Identifier
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DOI:10.1093/mnras/stv857
Identifier
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https://repositorio.uchile.cl/handle/2250/131145
General note
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Artículo de publicación ISI
en_US
Abstract
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We present optical and near-infrared photometry and spectroscopy of SN 2009ib, a Type
II-P supernova in NGC 1559. This object has moderate brightness, similar to those of the
intermediate-luminosity SNe 2008in and 2009N. Its plateau phase is unusually long, lasting
for about 130 d after explosion. The spectra are similar to those of the subluminous SN 2002gd,
with moderate expansion velocities. We estimate the 56Ni mass produced as 0.046 ± 0.015 M.
We determine the distance to SN 2009ib using both the expanding photosphere method (EPM)
and the standard candle method. We also apply EPM to SN 1986L, a Type II-P SN that
exploded in the same galaxy. Combining the results of different methods, we conclude the
distance to NGC 1559 as D = 19.8 ± 3.0 Mpc. We examine archival, pre-explosion images
of the field taken with the Hubble Space Telescope, and find a faint source at the position of
the SN, which has a yellow colour [(V − I)0 = 0.85 mag]. Assuming it is a single star, we
estimate its initial mass as MZAMS = 20 M. We also examine the possibility, that instead of
the yellow source the progenitor of SN 2009ib is a red supergiant star too faint to be detected.
In this case, we estimate the upper limit for the initial zero-age main sequence (ZAMS)
mass of the progenitor to be ∼14–17 M. In addition, we infer the physical properties of the
progenitor at the explosion via hydrodynamical modelling of the observables, and estimate
the total energy as ∼0.55 × 1051 erg, the pre-explosion radius as ∼400 R, and the ejected
envelope mass as ∼15 M, which implies that the mass of the progenitor before explosion
was ∼16.5–17 M.