Active and Star-forming Galaxies and Their Supernovae

Петросян, А. Р.; Navasardyan, H.; McLean, B.; Allen, R. J.; Panagia, N.; Leitherer, Claus; MacKenty, John; Turatto, M.

doi:10.1086/427712

Cited by 35 publications

(54 citation statements)

References 61 publications

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“…6, as well as Table 5). This result has been known for some time (e.g., van den Bergh 1997; Wang et al 1997;Petrosian et al 2005;Hakobyan 2008) for the distribution of radii normalized to R 25 , but we confirm the more centrally concentrated distribution of SNe Ib/c with our normalization to the disk scale lengths (Fig. 6 and Table 5).…”

Section: Discussionsupporting

confidence: 87%

“…Petrosian & Turatto (1990) found that their sample of 8 SNe II and SNe Ib within galaxies hosting AGN were significantly more radially concentrated in their galaxy hosts than analogous CCSNe in galaxies without active nuclei. Petrosian et al (2005) studying a sample of 12 SNe II and SNe Ib/c in galaxies hosting AGN, confirmed this result and found that SNe Ib/c in active/star-forming galaxies are more centrally concentrated than are the SNe II, but given the small sample, this difference was not statistically significant. These results were confirmed with larger samples of CCSNe by Hakobyan (2008), who used both one-dimensional and multivariate statistics.…”

Section: Introductionmentioning

confidence: 78%

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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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Section: Discussionsupporting

confidence: 87%

Section: Introductionmentioning

confidence: 78%

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

Hakobyan¹,

Mamon

Петросян³

et al. 2009

A&A

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“…For example, Wang et al (2010) directly measured number and surface density distributions of SNe II in their hosts, and indicated that SNe II detected in star-forming galaxies follow an exponential law, in contrast, the distribution of SNe II detected in Active Galactic Nuclei (AGN) hosts significantly deviates from an exponential law. Petrosian et al (2005) studying a sample of CC SNe in galaxies hosting AGN found that SNe Ibc in active/star-forming galaxies are more centrally concentrated than are the SNe II, but given the small sample, this difference was not statistically significant. The results of Petrosian et al were confirmed with larger samples of CC SNe by Hakobyan (2008).…”

Section: Introductionmentioning

confidence: 96%

“…However, other authors have shown that the SNe distributions in galaxies with various activity levels might be different (e.g., Petrosian & Turatto 1990;Petrosian et al 2005;Hakobyan 2008;Wang et al 2010;Herrero-Illana et al 2012). For example, Wang et al (2010) directly measured number and surface density distributions of SNe II in their hosts, and indicated that SNe II detected in star-forming galaxies follow an exponential law, in contrast, the distribution of SNe II detected in Active Galactic Nuclei (AGN) hosts significantly deviates from an exponential law.…”

Section: Introductionmentioning

confidence: 98%

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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“…They also found that the ratio N Ibc /NII measured in Sy galaxies exceeds that in normal host galaxies by a factor of 4. Studying a sample of CC SNe in galaxies hosting AGN, Petrosian et al (2005) and Hakobyan (2008) found that the SNe in active/star-forming (SF) galaxies are more centrally concentrated than those in normal galaxies. Herrero-Illana, Pérez-Torres & Alberdi (2012) modelled the radial distribution of SNe in the nuclear starbursts of M 82, Arp 220, and Arp 299A galaxies, and interpreted the results as evidence of galaxy-galaxy interactions that are expected to trigger massive star formation down to the central kiloparsec region of galaxies.…”

Section: Introductionmentioning

confidence: 99%

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Hakobyan¹,

Nazaryan²,

Adibekyan³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the relative frequencies of different supernova (SN) types in spirals with various morphologies and in barred or unbarred galaxies. We use a well-defined and homogeneous sample of spiral host galaxies of 692 SNe from the Sloan Digital Sky Survey in different stages of galaxy-galaxy interaction and activity classes of nucleus. We propose that the underlying mechanisms shaping the number ratios of SNe types can be interpreted within the framework of interaction-induced star formation, in addition to the known relations between morphologies and stellar populations. We find a strong trend in behaviour of the N Ia /N CC ratio depending on host morphology, such that early spirals include more Type Ia SNe. The N Ibc /N II ratio is higher in a broad bin of early-type hosts. The N Ia /N CC ratio is nearly constant when changing from normal, perturbed to interacting galaxies, then declines in merging galaxies, whereas it jumps to the highest value in post-merging/remnant galaxies. In contrast, the N Ibc /N II ratio jumps to the highest value in merging galaxies and slightly declines in post-merging/remnant subsample. The interpretation is that the star formation rates and morphologies of galaxies, which are strongly affected in the final stages of interaction, have an impact on the number ratios of SNe types. The N Ia /N CC (N Ibc /N II ) ratio increases (decreases) from star-forming to active galactic nuclei (AGN) classes of galaxies. These variations are consistent with the scenario of an interaction-triggered starburst evolving into AGN during the later stages of interaction, accompanied with the change of star formation and transformation of the galaxy morphology into an earlier type.

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Active and Star-forming Galaxies and Their Supernovae

Cited by 35 publications

References 61 publications

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

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

Supernovae and their host galaxies

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

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