Classification of Supernovae

Turatto, M.

doi:10.1007/3-540-45863-8_3

Cited by 63 publications

(58 citation statements)

References 127 publications

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“…The spectral type of an SN provides a crucial diagnostic of the initial mass, age and metallicity of the progenitor, as well as of the explosion mechanism (e.g., Turatto 2003;Turatto et al 2007). We have thus attempted to homogenize the spectral types for SNe that have been assign different types in different SN catalogs.…”

Section: Spectroscopic Classes Of Supernovaementioning

confidence: 99%

Supernovae and their host galaxies

Hakobyan

Adibekyan

Aramyan

et al. 2012

A&A

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Context. In this first paper of a series, we report the creation of large and well-defined database that combines extensive new measurements and a literature search of 3876 supernovae (SNe) and their 3679 host galaxies located in the sky area covered by the Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8). Aims. This database should be much larger than previous ones, and should contain a homogenous set of global parameters of SN hosts, including morphological classifications and measures of nuclear activity. Methods. The measurements of apparent magnitudes, diameters (D 25 ), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies. Results. Identification of the host galaxy sample is 91% complete (with 3536 SNe in 3340 hosts), of which the SDSS names of ∼1100 anonymous hosts are listed for the first time. The morphological classification is available for 2104 host galaxies, including 73 (56) hosts in interacting (merging) systems. The total sample of host galaxies collects heliocentric redshifts for 3317 (∼90%) galaxies. The g-band magnitudes, D 25 , b/a, and PA are available for 2030 hosts of the morphologically classified sample of galaxies. Nuclear activity measures are provided for 1189 host galaxies. We analyze and discuss many selection effects and biases that can significantly affect any future analysis of our sample. Conclusions. The creation of this large database will help to better understand how the different types of SNe are correlated with the properties of the nuclei and global physical parameters of the host galaxies, and minimize possible selection effects and errors that often arise when data are selected from different sources and catalogs.

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Section: Spectroscopic Classes Of Supernovaementioning

confidence: 99%

Supernovae and their host galaxies

Hakobyan

Adibekyan

Aramyan

et al. 2012

A&A

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“…Most SNe can be assigned to two main physical classes (e.g., Turatto 2003;Turatto et al 2007): the gravitational collapse of young massive stellar cores (Types Ib, Ic and II SNe) and the thermonuclear explosions of a white dwarf in close binary systems (Type Ia SNe). While SNe with no or weak hydrogen lines were classified into type I, it is now understood that there are actually three spectroscopically and photometrically distinct subclasses of SNe I.…”

Section: Introductionmentioning

confidence: 99%

The radial distribution of core-collapse supernovae in spiral host galaxies

Hakobyan¹,

Mamon

Петросян³

et al. 2009

A&A

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Aims. With the goal of providing constraints on the nature of the progenitors of core-collapse (CC) supernovae (SNe), we compare their radial distribution within their spiral host galaxies with the distributions of stars and ionized gas in spiral disks. Methods. SNe positions are taken from the Asiago catalog for a well-defined sample of 224 SNe within 204 host galaxies. The SN radial distances are estimated from the deprojected separations from the host galaxy nuclei, and normalized both to the 25th mag arcsec −2 blue-band isophotal radius and (for the first time) to the statistically-estimated disk scale length. Results. The normalized radial distribution of all CCSNe is consistent with an exponential law, as previously found, with a possible depletion of CCSNe within one-fifth of the isophotal radius (less significant with scale-length normalization). There are no signs of truncation of the exponential distribution of CCSNe out to 7 disk scale lengths. The scale length of the distribution of type II SNe appears to be significantly larger than that of the stellar disks of their host galaxies, but consistent with the scale lengths of Freeman disks. SNe Ib/c have a significantly smaller scale length than SNe II, with little difference between types Ib and Ic. The radial distribution of type Ib/c SNe is more centrally concentrated than that of the stars in a Freeman disk, but is similar to the stellar disk distribution that we infer for the host galaxies. All CCSN subsamples are consistent with the still uncertain distribution of H ii regions. The scale length of the CCSN radial distribution shows no significant correlation with the host galaxy morphological type, or the presence of bars. However, low luminosity as well as inclined hosts have a less concentrated distribution (with the scale-length normalized radial distances) of CCSNe, which are probably a consequence of metallicity and selection effects, respectively. Conclusions. The exponential distribution of CCSNe shows a scale length consistent with that of the ionized gas confirming the generally accepted hypothesis that the progenitors of these SNe are young massive stars. Given the lack of correlation of the normalized radial distances of CCSNe with the morphological type of the host galaxy, we conclude that the more concentrated distribution of SNe Ib/c relative to SNe II must arise from the higher metallicity of their progenitors or possibly from a shallower initial mass function in the inner regions of spirals.

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“…Supernovae, the catastrophic events terminating the life of several kinds of stars, arise from two fundamentally different paths (Turatto 2003): the core collapse of a massive star that has exhausted the nuclear fuel, or the thermonuclear explosion of a white dwarf that overcomes the Chandrasekhar mass limit (about 1.4 M , ) after accretion of material from a companion star.…”

Section: Introductionmentioning

confidence: 99%

Supernova 2002ic: The Collapse of a Stripped-Envelope, Massive Star in a Dense Medium?

Benetti

Turatto

Taubenberger

et al. 2006

ApJ

101

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We revisit the case of SN 2002ic, which recently revived the debate about the progenitors of Type Ia supernovae (SNe Ia) after the claim of the unprecedented presence of hydrogen lines over a diluted SN Ia spectrum. As an alternative to the previous interpretation, we suggest that SN 2002ic actually was a Type Ic SN, the core collapse of a massive star that lost its hydrogen and helium envelope. In this scenario the observed interaction with a dense circumstellar material (CSM) is the predictable consequence of the intense mass loss of the progenitor and/or of the presence of a gas-rich environment. With this view we establish a link between energetic SNe Ic and highly interacting SNe IIn and add some credits to the proposed association of some SNe IIn with gamma-bursts (GRBs).

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Classification of Supernovae

Cited by 63 publications

References 127 publications

Supernovae and their host galaxies

Supernovae and their host galaxies

The radial distribution of core-collapse supernovae in spiral host galaxies

Supernova 2002ic: The Collapse of a Stripped-Envelope, Massive Star in a Dense Medium?

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