A Study of SN 1992H in NGC 5377

Clocchiatti, A.; Benetti, S.; Wheeler, J. C.; Wren, W.; Boisseau, John R.; Cappellaro, E.; Turatto, M.; Patat, F.; Swartz, Douglas A.; Harkness, Robert; Brotherton, Michael S.; Wills, B.; Hemenway, P. D.; Cornell, Mark E.; Frueh, M.; Kaiser, M.

doi:10.1086/117874

Cited by 64 publications

(71 citation statements)

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“…However, it follows the correlation shown in Figure 2 and is consistent with the range of values found in previous studies (Hamuy 2003;Spiro et al 2014). It is worth noting that Schmidt et al (1994) and Clocchiatti et al (1996) have calculated the distance to the host galaxy of SN 1992H, GC 5377, obtaining values of ∼ 30 Mpc and ∼ 20 Mpc (compared to ∼ 40 Mpc with our method), respectively. These values give lower M Ni than ours for the same reddening, ∼ 0.15 M ⊙ and ∼ 0.06 M ⊙ , respectively.…”

Section: Ni Distribution: Observations Vs Theorysupporting

confidence: 91%

The Nickel Mass Distribution of Normal Type II Supernovae

Müller

Prieto

Pejcha

et al. 2017

ApJ

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109

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Core-collapse supernova explosions expose the structure and environment of massive stars at the moment of their death. We use the global fitting technique of Pejcha & Prieto (2015a,b) to estimate a set of physical parameters of 19 normal Type II SNe, such as their distance moduli, reddenings, 56 Ni masses M Ni , and explosion energies E exp from multicolor light curves and photospheric velocity curves. We confirm and characterize known correlations between M Ni and bolometric luminosity at 50 days after the explosion, and between M Ni and E exp . We pay special attention to the observed distribution of M Ni coming from a joint sample of 38 Type II SNe, which can be described as a skewed-Gaussian-like distribution between 0.005 M ⊙ and 0.280 M ⊙ , with a median of 0.031 M ⊙ , mean of 0.046 M ⊙ , standard deviation of 0.048 M ⊙ and skewness of 3.050. We use twosample Kolmogorov-Smirnov test and two-sample Anderson-Darling test to compare the observed distribution of M Ni to results from theoretical hydrodynamical codes of core-collapse explosions with the neutrino mechanism presented in the literature. Our results show that the theoretical distributions obtained from the codes tested in this work, KEPLER and Prometheus Hot Bubble, are compatible with the observations irrespective of different pre-supernova calibrations and different maximum mass of the progenitors.

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Section: Ni Distribution: Observations Vs Theorysupporting

confidence: 91%

The Nickel Mass Distribution of Normal Type II Supernovae

Müller

Prieto

Pejcha

et al. 2017

ApJ

Self Cite

109

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“…It was followed by a plateau lasting about 50-70 days, more clearly visible in the R and I bands. The luminous peak, m V ∼15.5 corresponding to M V ∼ −16.6 is slightly higher than the average for SNIIP (M V ∼ −15.9, Patat et al 1994;Li et al 2011) and fainter than the luminous IIP 1992H (M V ∼ −17.3, Clocchiatti et al 1996) mag in ∼20d in the V band, somewhat lower than the value of 2 mag in normal SNe IIP. The late decline rates in the various bands are similar.…”

Section: Sn 2009ddmentioning

confidence: 59%

“…Intermediate cases have been found with light curves showing less pronounced plateaus, e.g. SNe 1992H (Clocchiatti et al 1996). A common feature of SN IIP and IIL is the linear tail of the late light curve powered by the energy release of the radioactive decay of 56 Co to 56 Fe with the characteristic slope of 0.98 mag/100d, indicating complete γ-ray and e + trapping.…”

Section: Introductionmentioning

confidence: 98%

Moderately luminous Type II supernovae

Inserra

Pastorello

Turatto

et al. 2013

A&A

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Context. Core-collapse Supernovae (CC-SNe) descend from progenitors more massive than about 8 M . Because of the young age of the progenitors, the ejecta may eventually interact with the circumstellar medium (CSM) via highly energetic processes detectable in the radio, X-ray, ultraviolet (UV) and, sometimes, in the optical domains. Aims. In this paper we present ultraviolet, optical and near infrared observations of five type II SNe, namely SNe 2009dd, 2007pk, 2010aj, 1995ad, and 1996W. Together with few other SNe they form a group of moderately luminous type II events. We investigate the photometric similarities and differences among these bright objects. We also attempt to characterise them by analysing the spectral evolutions, in order to find some traces of CSM-ejecta interaction. Methods. We collected photometry and spectroscopy with several telescopes in order to construct well-sampled light curves and spectral evolutions from the photospheric to the nebular phases. Both photometry and spectroscopy indicate a degree of heterogeneity in this sample. Modelling the data of SNe 2009dd, 2010aj and 1995ad allows us to constrain the explosion parameters and the properties of the progenitor stars.

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“…SNIIL, on the other hand, show a linear, uninterrupted luminosity decline, probably because of a lower mass envelope. Indeed the two classes are not separated and there are a number of intermediate cases with short plateaus, e.g., SN1992H [36]. A quantitative criterion for the classification of the light curves has been proposed on the basis of the average decline rate of the first 100 days [93].…”

Section: Type II Supernovaementioning

confidence: 99%

Classification of Supernovae

Turatto

2003

Supernovae and Gamma-Ray Bursters

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Abstract. The current classification scheme for supernovae is presented. The main observational features of the supernova types are described and the physical implications briefly addressed. Differences between the homogeneous thermonuclear type Ia and similarities among the heterogeneous core collapse type Ib, Ic and II are highlighted. Transforming type IIb, narrow line type IIn, supernovae associated with GRBs and few peculiar objects are also discussed.

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A Study of SN 1992H in NGC 5377

Cited by 64 publications

References 0 publications

The Nickel Mass Distribution of Normal Type II Supernovae

The Nickel Mass Distribution of Normal Type II Supernovae

Moderately luminous Type II supernovae

Classification of Supernovae

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