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Supernova 2010as: the lowest-velocity member of a family of flat-velocity type IIb supernovae

Universidad de Chile. Repositorio Académico

Título Supernova 2010as: the lowest-velocity member of a family of flat-velocity type IIb supernovae
Autor Elliott, Jonny
Moore, Justin P.
Kuncarayakti, Hanindyo
Pignata, Giuliano
Greiner, Jochen
Morrell, Nidia
Holmbo, Simon
Olivares Estay, Felipe
Folatelli, Gastón
Phillips, Mark M.
LaCluyze, Aaron P.
Reichart, Daniel E.
Haislip, Joshua B.
Nomoto, Ken’ichi
Forster, Francisco
Maeda, Keiichi
Afonso, Paulo
Prieto, José Luis
Altenmuller, Konrad
Stritzinger, Maximilian
Bersten, Melina C.
Valenti, Stefano
Anderson, Joseph P.
Updike, Adria
Contreras, Carlos
Hamuy Wackenhut, Mario Andrés
Tema supernovae: general
Descripción Artículo de publicación de ISI.
We present extensive optical and near-infrared photometric and spectroscopic observations of the stripped-envelope
supernova SN 2010as. Spectroscopic peculiarities such as initially weak helium features and low expansion
velocities with a nearly flat evolution place this object in the small family of events previously identified as
transitional Type Ib/c supernovae (SNe). There is ubiquitous evidence of hydrogen, albeit weak, in this family of
SNe, indicating that they are in fact a peculiar kind of Type IIb SNe that we name “flat-velocity Type IIb. The
flat-velocity evolution—which occurs at different levels between 6000 and 8000 km s−1 for different SNe—suggests
the presence of a dense shell in the ejecta. Despite the spectroscopic similarities, these objects show surprisingly
diverse luminosities. We discuss the possible physical or geometrical unification picture for such diversity. Using
archival Hubble Space Telescope images, we associate SN 2010as with a massive cluster and derive a progenitor
age of ≈6 Myr, assuming a single star-formation burst, which is compatible with a Wolf–Rayet progenitor. Our
hydrodynamical modeling, on the contrary, indicates that the pre-explosion mass was relatively low, ≈4 M . The
seeming contradiction between a young age and low pre-SN mass may be solved by a massive interacting binary
Fecha 2014-09-02T15:33:42Z
Tipo Artículo de revista
Enlace The Astrophysical Journal, 792:7 (24pp), 2014 September 1
Idioma en_US
Publicador The American Astronomical Society