Spatial distributions of core-collapse supernovae in infrared-bright galaxies

Kangas, T.; Mattila, S.; Kankare, E.; Kotilainen, Jari; Vaïsänen, P.; Greimel, R.; Takalo, A.

doi:10.1093/mnras/stt1833

Cited by 33 publications

(36 citation statements)

References 57 publications

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“…It was concluded that the association of SNe Ic to g ′ -band light implied a minimum progenitor mass for SNe Ic of 25 M ⊙ . Kangas et al (2013) investigated specifically the local environments of CC SNe within infrared-bright galaxies. Using NCR pixel statistics they presented similar distributions and relative differences in distributions between SNe II and SNe Ic populations to the Anderson et al results.…”

Section: Pixel Statisticsmentioning

confidence: 99%

“…Both of these possibilities were also considered in the radial analysis of Hakobyan et al (2009), and are further discussed below. Kangas et al (2013) also analysed CC SN host galaxies using the same radial analysis as discussed above. These authors concentrated on SNe within infrared bright galaxies (many of which are starbursts), finding very similar results our analysis where we combine their sample into our large radial analysis database.…”

Section: Sn Radial Distributionsmentioning

confidence: 99%

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Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

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Mapping the diversity of supernovae (SNe) to progenitor properties is key to our understanding of stellar evolution and explosive stellar death. Investigations of the immediate environments of SNe allow statistical constraints to be made on progenitor properties such as mass and metallicity. Here we review the progress that has been made in this field. Pixel statistics using tracers of e.g. star formation within galaxies show intriguing differences in the explosion sites of, in particular SNe types II and Ibc (SNe II and SNe Ibc respectively), suggesting statistical differences in population ages. Of particular interest is that SNe Ic are significantly more associated with host galaxy Hα emission than SNe Ib, implying shorter lifetimes for the former. In addition, such studies have shown (unexpectedly) that the interacting SNe IIn do not explode in regions containing the most massive stars, which suggests that at least a significant fraction of their progenitors arise from the lower end of the core-collapse SN mass range. Host H ii region spectroscopy has been obtained for a significant number of core-collapse events, however definitive conclusions on differences between distinct SN types have to-date been elusive. Single stellar evolution models predict that the relative fraction of SNe Ibc to SNe II should increase with increasing metallicity, due to the dependence of mass-loss rates on progenitor metallicity. We present a meta-analysis of all current host H ii region oxygen abundances for CC SNe. It is concluded that the SN II to SN Ibc ratio shows little variation with oxygen abundance, with only a suggestion that the ratio increases in the lowest bin. Radial distributions of different SNe are discussed, where a central excess of SNe Ibc has been observed within disturbed galaxy systems, which is difficult to ascribe to metallicity or selection effects. Environment studies are also being undertaken for SNe Ia, where constraints can be made on the shortest delay times of progenitor systems. It is shown that 'redder' SNe Ia are more often found within star-forming regions. Environment studies are evolving to enable studies at higher spatial resolutions than previously possible, while in addition the advent of widefield integral field unit instruments allows galaxy-wide spectral analyses which will provide fruitful results to this field. Some example contemporary results are shown in that direction.

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Section: Pixel Statisticsmentioning

confidence: 99%

Section: Sn Radial Distributionsmentioning

confidence: 99%

Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

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“…The deprojected GCD, recovered from the inclination and the orientation of the galaxy, which is the best estimate for the real GCD if the SN lies in the galactic plane. Examples of previous works using this approach are Hakobyan et al (2009), Wang et al (2010, Galbany et al (2012) and Kangas et al (2013). The galaxy inclinations and orientations were obtained from an analysis of the 2D Hα velocity maps using the procedure previously described in Sect.…”

Section: Distance Deprojection and Azimuthal Averagementioning

confidence: 99%

Nearby supernova host galaxies from the CALIFA Survey

Galbany

Stanishev²,

Mourão³

et al. 2014

A&A

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We use optical integral field spectroscopy (IFS) of nearby supernova (SN) host galaxies (0.005 < z < 0.03) provided by the Calar Alto Legacy Integral Field Area (CALIFA) Survey with the goal of finding correlations in the environmental parameters at the location of different SN types. In this first study of a series we focus on the properties related with star formation (SF). We recover the sequence in association of different SN types to the star-forming regions by using several indicators of the ongoing and recent SF related to both the ionized gas and the stellar populations. While the total ongoing SF is on average the same for the three SN types, SNe Ibc/IIb tend to occur closer to star-forming regions and in higher SF density locations than SNe II and SNe Ia; the latter shows the weakest correlation. SNe Ia host galaxies have masses that are on average ∼0.3−0.8 dex higher than those of the core collapse (CC) SNe hosts because the SNe Ia hosts contain a larger fraction of old stellar populations. Using the recent SN Ia delay-time distribution and the SFHs of the galaxies, we show that the SN Ia hosts in our sample are expected to produce twice as many SNe Ia as the CC SN hosts. Since both types occur in hosts with a similar SF rate and hence similar CC SN rate, this can explain the mass difference between the SN Ia and CC SN hosts, and reinforces the finding that at least part of the SNe Ia originate from very old progenitors. By comparing the mean SFH of the eight least massive galaxies with that of the massive SF SN Ia hosts, we find that the low-mass galaxies formed their stars during a longer time (0.65%, 24.46%, and 74.89% in the intervals 0-0.42 Gyr, 0.42-2.4 Gyr, and >2.4 Gyr, respectively) than the massive SN Ia hosts (0.04%, 2.01%, and 97.95% in these intervals). We estimate that the low-mass galaxies produce ten times fewer SNe Ia and three times fewer CC SNe than the high-mass group. Therefore the ratio between the number of CC SNe and SNe Ia is expected to increase with decreasing galaxy mass. CC SNe tend to explode at positions with younger stellar populations than the galaxy average, but the galaxy properties at SNe Ia locations are one average the same as the global galaxy properties.

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“…However, in the central regions of merging galaxies where the excess of Ibc SNe is observed, metallicities are systematically lower (∼ 0.2 dex from Kewley et al 2006) than those of normal and weakly interacting galaxies. The possible roles of metallicity, age, fraction of binary systems, and IMF shape are discussed in detail in Anderson et al (2011Anderson et al ( , 2012, Habergham et al (2012), and Kangas et al (2013). In the final stage of interactions, i.e.…”

Section: Dependence Of Relative Frequencies Of Sne Types On Host Distmentioning

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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Spatial distributions of core-collapse supernovae in infrared-bright galaxies

Cited by 33 publications

References 57 publications

Statistical Studies of Supernova Environments

Statistical Studies of Supernova Environments

Nearby supernova host galaxies from the CALIFA Survey

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

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