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Franckowiak, Melissa; Nader, Nader D.

doi:10.1016/b978-1-4160-2215-2.50234-9

Cited by 1 publication

(1 citation statement)

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“…The bulk of the energy expelled from a supernova is in the form of neutrinos (for a recent review see Haxton 2008). However, although experiments are underway to measure such neutrinos (Kowarik et al 2009, Franckowiak et al 2009), the amount of energy is not as readily measured for distant SN as is their optical emission. The amount of optical energy in the explosion of SN 2006gy was found to require a progenitor with mass > 40M ⊙ and suggests either the explosion of a luminous blue variable (LBV) like η Carinae, or the pair-instability destruction of a very massive, low metallicity star (Woosley et al 2007;Ofek et al 2007).…”

Section: Introductionmentioning

confidence: 99%

DISCOVERY OF THE EXTREMELY ENERGETIC SUPERNOVA 2008fz

Drake¹,

Djorgovski²,

Prieto³

et al. 2010

ApJ

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We report on the discovery and initial observations of the energetic type IIn supernova (SN), 2008fz. The optical energy emitted by SN 2008fz (based on the light curve over a 88 day period), is possibly the most ever observed for a supernova (1.4×10 51 erg). The event was more luminous than the type IIn SN 2006gy, but exhibited same smooth, slowly evolving light curve. As is characteristic of type IIn SN, the early spectra of 2008fz initially exhibited narrow Balmer lines which were replaced by a broader component at later times. The spectra also show a blue continuum with no signs of Ca or Na absorption, suggesting that there is little extinction due to intragalatic dust in the host or circumstellar material. No host galaxy is identified in prior coadded images reaching R ∼ 22. From the supernova's redshift, z = 0.133, we place an upper limit on the host of M R = −17. The presence of the SN within such a faint host follows the majority of recently discovered highly luminous SN. A possible reason for this occurrence is the very high star formation rate occurring in low-mass galaxies in combination with the low metallicity environment, which makes the production of very massive stars possible. We determine the peak absolute magnitude of the event to be M V = −22.3 from the initial photometry and the redshift distance, placing it among the most luminous supernovae discovered.

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