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SN 2008ha: An Extremely Low Luminosity and Extremely Low Energy Supernova | Ryan J. Foley
; Ryan Chornock
; Alexei V. Filippenko
; Mohan Ganeshalingam
; Robert P. Kirshner
; Weidong Li
; S. Bradley Cenko
; Pete Challis
; Andrew S. Friedman
; Maryam Modjaz
; W. Michael Wood-Vasey
; | Date: |
16 Feb 2009 | Abstract: | We present ultraviolet, optical, and near-infrared photometry as well as
optical spectra of the peculiar supernova (SN) 2008ha. SN 2008ha had a very low
peak luminosity, reaching only M_V = -14.2 mag, and low line velocities of only
~2000 km/s near maximum brightness, indicating a very small kinetic energy per
unit mass of ejecta. Spectroscopically, SN 2008ha is a member of the SN
2002cx-like class of SNe, a peculiar subclass of SNe Ia; however, SN 2008ha is
an extreme member, being significantly fainter and having lower line velocities
than the typical member, which is already ~2 mag fainter and has line
velocities ~5000 km/s smaller (near maximum brightness) than a normal SN Ia. SN
2008ha had a remarkably short rise time of only ~10 days, significantly shorter
than both SN 2002cx-like objects (~15 days) and normal SNe Ia (~19.5 days). The
bolometric light curve of SN 2008ha indicates that SN 2008ha peaked at L_peak =
(9.5 +/- 1.4) x 10^40 ergs/s, making SN 2008ha perhaps the least luminous SN
ever observed. From its peak luminosity and rise time, we infer that SN 2008ha
generated (3.0 +/- 0.9) x 10^-3 M_sun of 56Ni, had a kinetic energy of ~2 x
10^48 ergs, and ejected 0.15 M_sun of material. We classify three new (and one
potential) members of the SN 2002cx-like class, expanding the sample to 14 (and
one potential) members. The host-galaxy morphology distribution of the class is
consistent with that of SNe Ia, Ib, Ic, and II. Several models for generating
low-luminosity SNe can explain the observations of SN 2008ha; however, if a
single model is to describe all SN 2002cx-like objects, either electron capture
in Ne-Mg white dwarfs causing a core collapse, or deflagration of C-O white
dwarfs with SN 2008ha being a partial deflagration and not unbinding the
progenitor star, are preferred. Abridged. | Source: | arXiv, 0902.2794 | Services: | Forum | Review | PDF | Favorites |
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