Galaxies with a UV excess in which supernovae have been observed

Kazarian, M. A.

doi:10.1007/bf03035744

Cited by 5 publications

(5 citation statements)

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“…This study of the radial distribution of Hii regions in normal, LINER and Seyfert galaxies agrees with a large number of detailed spectroscopic and imaging studies of Seyfert galaxies. Consistently, the radial distribution of supernovae appears to be more strongly peaked in Seyfert galaxies than in normal galaxies in several samples (Kazarian 1997;Petrosian & Turatto 1990) as well as in our own. However, enhancement of star formation rate in the inner galactic regions cannot explain the relative excess of type Ib/c supernovae found in Seyfert galaxies.…”

Section: Seyfert Galaxiessupporting

confidence: 89%

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On core-collapse supernovae in normal and in Seyfert galaxies

Bressan¹,

Valle²,

Marziani³

2002

Monthly Notices of the Royal Astronomical Society

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This paper estimates the relative frequency of different types of core‐collapse supernovae, in terms of the ratio 𝒮 between the number of Type Ib–Ic and of Type II supernovae. We estimate 𝒮 independently for all normal and Seyfert galaxies whose radial velocity is ≤14 000 km s−1, and which had at least one supernova event recorded in the Asiago catalogue from 1986 January to 2000 August. We find that the ratio 𝒮 is ≈0.23±0.05 in normal galaxies. This value is consistent with constant star formation rate and with a Salpeter initial mass function and an average binary rate ≈50 per cent. On the contrary, Seyfert galaxies exceed the ratio 𝒮 in normal galaxies by a factor ≈4 at a confidence level ≳2σ. A caveat is that the numbers for Seyferts are still small (six of Type Ib–Ic and six of Type II supernovae discovered as yet). Assumed to be real, this excess of Type Ib/c supernovae may indicate a burst of low‐age star formation(τ≲20 Myr), a high incidence of binary systems in the inner regions (r≲0.4R25) of Seyfert galaxies, or a top‐loaded mass function.

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Section: Seyfert Galaxiessupporting

confidence: 89%

“…A Kolmogorov–Smirnov test suggests that the distributions are different to a statistical significance of 0.999. This result has been known for some time (Petrosian & Turatto 1990; Kazarian 1997) from the analysis of supernova data in different samples.…”

Section: Resultsmentioning

confidence: 61%

On core-collapse supernovae in normal and in Seyfert galaxies

Bressan¹,

Valle²,

Marziani³

2002

Monthly Notices of the Royal Astronomical Society

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“…In this context, the properties of SN host galaxies, such as the morphology, color, nuclear activity, star formation rate, metallicity, stellar population, age etc. provide strong clues to the understanding of the progenitors Full Table 7 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/cgi-bin/qcat?J/A+A/544/A81 (e.g., Petrosian & Turatto 1995;Kazarian 1997;Bressan et al 2002;Prantzos & Boissier 2003;Mannucci et al 2005;Prieto et al 2008;Boissier & Prantzos 2009;Arcavi et al 2010;Han et al 2010;Kelly & Kirshner 2011). In addition, valuable information of the nature of progenitors can be obtained through the study of the spatial distribution of SNe (e.g., Förster & Schawinski 2008;Hakobyan et al 2009;Wang et al 2010) and environments (e.g., Anderson & James 2008;Modjaz et al 2011;Leloudas et al 2011).…”

Section: Introductionmentioning

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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“…It is generally accepted that progenitor stars of Types II and Ib/c SNe are young massive stars born in recent episodes of star formation in galaxies (e.g., Branch et al 1990;Hamuy 2003;Van Dyk et al 2003), with possible differences in their nature (e.g., Van Dyk et al 2003). Core-collapse SNe, in particular, have been considered to be tracers of recent star formation in galaxies (e.g., Petrosian & Turatto 1990, 1995Kazarian 1997;Cappellaro et al 1999;Navasardyan et al 2001).…”

Section: Introductionmentioning

confidence: 99%

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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Galaxies with a UV excess in which supernovae have been observed

Cited by 5 publications

References 1 publication

On core-collapse supernovae in normal and in Seyfert galaxies

On core-collapse supernovae in normal and in Seyfert galaxies

Supernovae and their host galaxies

Active and Star-forming Galaxies and Their Supernovae

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