Photometric observations of the supernova 2009nr

Tsvetkov, D. Yu.; Balanutsa, P.; Lipunov, V.; Volkov, I. M.; Tuchin, O.; Kudelina, I.; Pruzhinskaya, M.; Gorbovskoy, E.; Корнилов, В. Г.; Belinski, A. A.; Tyurina, N.; Yurkov, V.; Sergienko, Y.; Tlatov, A. G.; Пархоменко, А.; Dormidontov, D.; Senik, V.; Крушинский, В. В.

doi:10.1134/s1063773711110053

Cited by 13 publications

(12 citation statements)

References 43 publications

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“…In the first attempts to estimate the mean value of the vertical coordinates of SNe, Tsvetkov (1981Tsvetkov ( , 1987 used the distribution of SN colour excesses without precise information on their spectroscopic types and host galaxy morphology in a sample of non-edge-on spirals. No difference was found in the vertical distributions of Type I and II SNe with indication that both types belong to the young population I.…”

Section: The Vertical Distribution and Scale Height Of Snementioning

confidence: 99%

Supernovae and their host galaxies – V. The vertical distribution of supernovae in disc galaxies

Hakobyan

Barkhudaryan

Karapetyan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the height distributions of the different types of supernovae (SNe) from the plane of their host galaxies. We use a well-defined sample of 102 nearby SNe appeared inside high-inclined (i 85 • ), morphologically non-disturbed S0-Sd host galaxies from the Sloan Digital Sky Survey. For the first time, we show that in all the subsamples of spirals, the vertical distribution of core-collapse (CC) SNe is about twice closer to the plane of host disc than the distribution of SNe Ia. In Sb-Sc hosts, the exponential scale height of CC SNe is consistent with those of the younger stellar population in the Milky Way (MW) thin disc, while the scale height of SNe Ia is consistent with those of the old population in the MW thick disc. We show that the ratio of scale lengths to scale heights of the distribution of CC SNe is consistent with those of the resolved young stars with ages from ∼ 10 Myr up to ∼ 100 Myr in nearby edge-on galaxies and the unresolved stellar population of extragalactic thin discs. The corresponding ratio for SNe Ia is consistent with the same ratios of the two populations of resolved stars with ages from a few 100 Myr up to a few Gyr and from a few Gyr up to ∼ 10 Gyr, as well as with the unresolved population of the thick disc. These results can be explained considering the age-scale height relation of the distribution of stellar population and the mean age difference between Type Ia and CC SNe progenitors.

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Section: The Vertical Distribution and Scale Height Of Snementioning

confidence: 99%

Supernovae and their host galaxies – V. The vertical distribution of supernovae in disc galaxies

Hakobyan

Barkhudaryan

Karapetyan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Model 150M and Model 250M are those of 150 M ⊙ and 250 M ⊙ PISNe simulated in the frame of present study. Labeled 'R190.D', 'B190.D' and 'B210.D' are models from (Dessart et al 2013) and 'R150.K' and 'R250.K' are models simulated by (Kasen et al 2011 Institute Supernova Light Curve Catalogue (Tsvetkov et al 2010;Tsvetkov & Pavlyuk 2013) and are compiled from the original data (Tsvetkov 1994;Clocchiatti et al 1996;Hamuy 2001;Botticella et al 2010). Model 150M has a plateau phase during the first 115 days which is not unusual for SNe IIP.…”

Section: Relatively Low-mass Pisne and Type Iip Snementioning

confidence: 99%

Observational properties of low-redshift pair instability supernovae

Kozyreva

Блинников

Langer

et al. 2014

A&A

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Context. So-called superluminous supernovae have been recently discovered in the local Universe. It appears possible that some of them originate in stellar explosions induced by the pair instability mechanism. Recent stellar evolution models also predict pair instability supernovae from very massive stars at fairly high metallicities (i.e., Z ∼ 0.004). Aims. We provide supernova models and synthetic light curves for two progenitor models, a 150 M red supergiant and a 250 M yellow supergiant at a metallicity of Z = 0.001, for which the evolution from the main sequence to collapse and the initiation of the pair instability supernova itself has been previously computed in a realistic and self-consistent way. Methods. We use the radiation hydrodynamics code STELLA to describe the supernova evolution of both models in a time frame of about 500 days. Results. We describe the shock-breakout phases of both supernovae, which are characterized by higher luminosity, longer duration, and a lower effective temperature than those of ordinary Type IIP supernovae. We derive the bolometric, as well as the U, B, V, R, and I, light curves of our pair instability supernova models, which show a long-lasting plateau phase with maxima at M bol −19.3 mag and −21.3 mag for our lower and higher mass models, respectively. While we do not produce synthetic spectra, we also describe the photospheric composition and velocity as a function of time. Conclusions. We conclude that the light curve of the explosion of our initially 150 M star resembles those of relatively bright type IIP supernovae, whereas its photospheric velocity at early times is somewhat lower. Its 56 Ni mass of 0.04 M also falls well into the range found in ordinary core collapse supernovae. The light curve and photospheric velocity of our 250 M models has a striking resemblance to that of the superluminous SN 2007bi, strengthening its interpretation as pair instability supernova. We conclude that pair instability supernovae may occur more frequently in the local universe than previously assumed.

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“…The statistics of "bad" nights over 2.5 years included mainly the Ural and Moscow-region sites, which have the poorest weather conditions. The supernovae 2008gy [172] and 2009nr [184] discovered in the robotic MASTER survey are among the best-studied, nearby Type Ia supernovae, and are practically located in intergalactic space. Supernovae similar to 2008gy and 2009nr can be distinguished as a special class of Type Ia supernovae that are not subject to the effects of ordinary and additional extragalactic gray absorption and chemical evolution.…”

Section: Observations Of Supernovaementioning

confidence: 99%

The MASTER-II network of robotic optical telescopes. First results

et al. 2013

Self Cite

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Abstract-The main stages in the creation of the Russian segment of the MASTER network of robotic telescopes is described. This network is designed for studies of the prompt optical emission of gammaray bursts (GRBs; optical emission synchronous with the gamma-ray radiation) and surveys of the sky aimed at discovering uncataloged objects and photometric studies for various programs. The first results obtained by the network, during its construction and immediately after its completion in December 2010, are presented. Eighty-nine alert pointings at GRBs (in most cases, being the first ground telescopes to point at the GRBs) were made from September 2006 through July 2011. The MASTER network holds first place in the world in terms of the total number of first pointings, and currently more than half of first pointings at GRBs by ground telescopes are made by the MASTER network. Photometric light curves of GRB

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Photometric observations of the supernova 2009nr

Cited by 13 publications

References 43 publications

Supernovae and their host galaxies – V. The vertical distribution of supernovae in disc galaxies

Supernovae and their host galaxies – V. The vertical distribution of supernovae in disc galaxies

Observational properties of low-redshift pair instability supernovae

The MASTER-II network of robotic optical telescopes. First results

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