Distribution of supernovae relative to spiral arms and H II regions

Bartunov, O. S.; Tsvetkov, D. Yu.; Филимонова, И.В.

doi:10.1086/133505

Cited by 82 publications

(76 citation statements)

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“…Types II and Ib/c SNe are strongly concentrated on spiral arms; Type Ia SNe show less concentration ( Maza & van den Bergh 1976;McMillan & Ciardullo 1996), although Bartunov et al (1994) did not reach the same conclusion.…”

Section: 2004mentioning

confidence: 80%

“…This problem has been addressed for the first time by Whipple (1939), and currently we count more than a dozen articles in this field (e.g., van den Bergh 1997; Wang et al 1997;Tsvetkov et al 2001). Previous studies of the radial distributions of different types of SNe in their host galaxies sometimes reached opposite conclusions (e.g., Bartunov et al 1994;van den Bergh 1997;Wang et al 1997;Howell & Wheeler 1999), which might be the result of some selection effects (e.g., Hatano et al 1998). In these studies, no segregation of the SNe hosts according to their activity class has been done.…”

Section: The Radial Distribution Of Supernov Vae In Their Host Galaxiesmentioning

confidence: 99%

“…An observational determination of the nature of the SNe progenitor stars can be obtained from their location in spiral galaxies, including the correlation of SNe with spiral arm structure, as well as their positions relative to the star-forming sites-H ii regions-in these galaxies. In the past several studies have been done in this field (e.g., Van Dyk 1992;Van Dyk et al 1996;Bartunov et al 1994;McMillan & Ciardullo 1996;Maza & van den Bergh 1976). The main results of these studies can be summarized as follows:…”

Section: 2004mentioning

confidence: 99%

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Active and Star-forming Galaxies and Their Supernovae

Петросян¹,

Navasardyan²,

McLean³

et al. 2005

Astron J

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To investigate the extent to which nuclear starbursts or other nuclear activity may be connected with enhanced star formation activity in the host galaxy, we perform a statistical investigation of supernovae (SNe) discovered in host galaxies from four samples: the Markarian galaxies sample, the Second Byurakan Survey (SBS) sample, the north Galactic pole ( NGP) sample of active or star-forming galaxies, and the NGP sample of normal galaxies. Forty-seven SNe in 41 Mrk galaxies, 10 SNe in six SBS galaxies, 29 SNe in 26 NGP active or star-forming galaxies, and 29 SNe in 26 NGP normal galaxies have been studied. We find that the rate of SNe, particularly core-collapse ( Types Ib/c and II) SNe, is higher in active or star-forming galaxies in comparison with normal galaxies. Active or star-forming host galaxies of SNe are generally of later morphological type and have lower luminosity and smaller linear size than normal host galaxies of SNe. The radial distribution of SNe in active and star-forming galaxies shows a higher concentration toward the center of the active host galaxy than is the case for normal host galaxies, and this effect is more pronounced for core-collapse SNe. Ib/c-type SNe have been discovered only in active and star-forming galaxies of our samples. About 78% of these SNe are associated with H ii regions or are located very close to the nuclear regions of these active galaxies, which are in turn hosting AGNs or starburst nuclei. Besides these new results, our study also supports the conclusions of several other earlier papers. We find that Type Ia SNe occur in all galaxy types, whereas core-collapse SNe of Types Ib/c and II are found only in spiral and irregular galaxies. The radial distribution of Type Ib SNe in their host galaxies is more centrally concentrated than that of Type II and Ia SNe. The radial distances of Types Ib/c and II SNe, from the nuclei of their host galaxies, is larger for barred spiral hosts. Core-collapse SNe are concentrated in spiral arms and are often close to or in the H ii regions, whereas Type Ia SNe show only a loose association with spiral arms and no clear association with H ii regions.

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Section: 2004mentioning

confidence: 80%

Section: The Radial Distribution Of Supernov Vae In Their Host Galaxiesmentioning

confidence: 99%

Section: 2004mentioning

confidence: 99%

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Active and Star-forming Galaxies and Their Supernovae

Петросян¹,

Navasardyan²,

McLean³

et al. 2005

Astron J

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“…CO), as well as ionized gas (see compilation by Boissier et al 2003) and even neutral gas, and by extending the analysis to two dimensions (extending previous analyses such as those by Johnson & MacLeod 1963;Bartunov et al 1994;Van Dyk et al 1996;and Tsvetkov et al 2001, making use of the much larger CCSN sample used here).…”

Section: Discussionmentioning

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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“…Many previous authors have attempted to estimate the age of SNe Ia, including Oemler & Tinsley (1979;10 7 -10 8 yr), Bartunov, Tsvetkov, & Filimonova (1994;≥10 7 yr), McMillan & Ciardullo (1996;≥ yr), and Yoshii,Tsujimoto, 5 # 10 moto [1996; yr]. The above studies assumed a 9 (0.5-3) # 10 single-progenitor population for SNe Ia.…”

Section: Introductionmentioning

confidence: 99%

The Progenitors of Subluminous Type I[CLC]a[/CLC] Supernovae

Howell

2001

The Astrophysical Journal

166

173

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We find that spectroscopically peculiar subluminous Type Ia supernovae (SNe Ia) come from an old population. Of the 16 subluminous SNe Ia known, 10 are found in E/S0 galaxies, and the remainder are found in early-type spiral galaxies. The probability that this is a chance occurrence is only 0.2%. The finding that subluminous SNe Ia are associated with an older stellar population indicates that for a sufficiently large look-back time (already accessible in current high-redshift searches) they will not be found. Due to a scarcity in old populations, hydrogen and helium main-sequence stars and He red giant stars that undergo Roche lobe overflow are unlikely to be the progenitors of subluminous SNe Ia. Earlier findings that overluminous SNe Ia [ ] come from a young progenitor Dm (B) Շ 0.95 15 population are confirmed. The fact that subluminous SNe Ia and overluminous SNe Ia come from different progenitor populations and also have different properties is a prediction of the CO white dwarf merger progenitor scenario.

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Distribution of supernovae relative to spiral arms and H II regions

Cited by 82 publications

References 10 publications

Active and Star-forming Galaxies and Their Supernovae

Active and Star-forming Galaxies and Their Supernovae

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

The Progenitors of Subluminous Type I[CLC]a[/CLC] Supernovae

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