The radial distribution of supernovae compared to star formation tracers

Audcent-Ross, Fiona; Meurer, G. R.; Audcent, James R.; Ryder, S. D.; Wong, O. I.; Phan, Jennifer A.; Williamson, A. R.; Kim, Ji Hoon

doi:10.1093/mnras/stz3282

Cited by 20 publications

(19 citation statements)

References 210 publications

(290 reference statements)

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“…This has been interpreted as Type Ibc SN progenitors having shorter stellar life times than Type IIP SNe, which is expected from single stellar evolution models. Similar results have also been found by Crowther (2013), Aramyan et al (2016), andAudcent-Ross et al (2020), among others. Furthermore, Kangas et al (2017) corroborated these previous results with their statistical study combining spatial distribution of massive stars to those of different CCSN classes in local galaxies.…”

Section: Introductionsupporting

confidence: 90%

Core-collapse supernova subtypes in luminous infrared galaxies

Kankare

Efstathiou

Kotak

et al. 2021

A&A

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The fraction of core-collapse supernovae (CCSNe) occurring in the central regions of galaxies is not well constrained at present. This is partly because large-scale transient surveys operate at optical wavelengths, making it challenging to detect transient sources that occur in regions susceptible to high extinction factors. Here we present the discovery and follow-up observations of two CCSNe that occurred in the luminous infrared galaxy (LIRG) NGC 3256. The first, SN 2018ec, was discovered using the ESO HAWK-I/GRAAL adaptive optics seeing enhancer, and was classified as a Type Ic with a host galaxy extinction of AV = 2.1−0.1+0.3 mag. The second, AT 2018cux, was discovered during the course of follow-up observations of SN 2018ec, and is consistent with a subluminous Type IIP classification with an AV = 2.1 ± 0.4 mag of host extinction. A third CCSN, PSN J10275082−4354034 in NGC 3256, was previously reported in 2014, and we recovered the source in late-time archival Hubble Space Telescope imaging. Based on template light curve fitting, we favour a Type IIn classification for it with modest host galaxy extinction of AV = 0.3−0.3+0.4 mag. We also extend our study with follow-up data of the recent Type IIb SN 2019lqo and Type Ib SN 2020fkb that occurred in the LIRG system Arp 299 with host extinctions of AV = 2.1−0.3+0.1 and AV = 0.4−0.2+0.1 mag, respectively. Motivated by the above, we inspected, for the first time, a sample of 29 CCSNe located within a projected distance of 2.5 kpc from the host galaxy nuclei in a sample of 16 LIRGs. We find, if star formation within these galaxies is modelled assuming a global starburst episode and normal IMF, that there is evidence of a correlation between the starburst age and the CCSN subtype. We infer that the two subgroups of 14 H-poor (Type IIb/Ib/Ic/Ibn) and 15 H-rich (Type II/IIn) CCSNe have different underlying progenitor age distributions, with the H-poor progenitors being younger at 3σ significance. However, we note that the currently available sample sizes of CCSNe and host LIRGs are small, and the statistical comparisons between subgroups do not take into account possible systematic or model errors related to the estimated starburst ages.

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Section: Introductionsupporting

confidence: 90%

Core-collapse supernova subtypes in luminous infrared galaxies

Kankare

Efstathiou

Kotak

et al. 2021

A&A

View full text Add to dashboard Cite

show abstract

“…Similar results have also been found e.g. by Crowther (2013), Aramyan et al (2016), andAudcent-Ross et al (2020). Furthermore, Kangas et al (2017) corroborated these previous results with their statistical study combining spatial distribution of massive stars to those of different CCSN classes in local galaxies.…”

Section: Introductionsupporting

confidence: 88%

Core-collapse supernova subtypes in luminous infrared galaxies

Kankare,

Efstathiou,

Kotak

et al. 2021

Preprint

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The fraction of core-collapse supernovae (CCSNe) occurring in the central regions of galaxies is not well-constrained at present. This is partly because large-scale transient surveys operate at optical wavelengths, making it challenging to detect transient sources that occur in regions susceptible to high extinction factors. Here we present the discovery and follow-up observations of two CCSNe that occurred in the luminous infrared galaxy (LIRG), NGC 3256. The first, SN 2018ec, was discovered using the ESO HAWK-I/GRAAL adaptive optics seeing enhancer, and was classified as a Type Ic with a host galaxy extinction of A V = 2.1 +0.3 −0.1 mag. The second, AT 2018cux, was discovered during the course of follow-up observations of SN 2018ec, and is consistent with a sub-luminous Type IIP classification with an A V = 2.1 ± 0.4 mag of host extinction. A third CCSN, PSN J10275082-4354034 in NGC 3256, has previously been reported in 2014, and we recovered the source in late time archival Hubble Space Telescope imaging. Based on template light-curve fitting, we favour a Type IIn classification for it with modest host galaxy extinction of A V = 0.3 +0.4 −0.3 mag. We also extend our study with follow-up data of the recent Type IIb SN 2019lqo and Type Ib SN 2020fkb that occurred in the LIRG system Arp 299 with host extinctions of A V = 2.1 +0.1 −0.3 and A V = 0.4 +0.1 −0.2 mag, respectively. Motivated by the above, we inspected, for the first time, a sample of 29 CCSNe located within a projected distance of 2.5 kpc from the host galaxy nuclei in a sample of 16 LIRGs. We find that, if star formation within these galaxies is modelled assuming a global starburst episode and normal IMF, there is evidence of a correlation between the starburst age and the CCSN subtype. We infer that the two subgroups of 14 H-poor (Type IIb/Ib/Ic/Ibn) and 15 H-rich (Type II/IIn) CCSNe have different underlying progenitor age distributions, with the H-poor progenitors being younger at 3 σ significance. However, we do note that the available sample sizes of CCSNe and host LIRGs are so far small, and the statistical comparisons between subgroups do not take into account possible systematic or model errors related to the estimated starburst ages.

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“…Meurer et al [42] and Audcent-Ross et al [43] pointed out that the burstlike nature of star formation in low-mass galaxies shows up in their average surface brightness. The left-side panel in Fig.…”

Section: Resultsmentioning

confidence: 99%

Star Formation in Nearby Dwarf Galaxies

Кайсин

Караченцев

2019

Astrophys. Bull.

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We report the measured Hα fluxes and images of 66 nearby objects observed with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences.Three of these objects IC 2233, UGC 4704, and NGC 3432 are late-type spiral galaxies, six objects are distant globular clusters of the M31 galaxy, and the remaining ones are dwarf galaxies. We used the measured Hα fluxes to estimate the integrated and specific starformation rates and analyzed some of the main features of star formation in dwarf galaxies and late-type spirals based on a sample of more than 500 Local-volume galaxies.

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The radial distribution of supernovae compared to star formation tracers

Cited by 20 publications

References 210 publications

Core-collapse supernova subtypes in luminous infrared galaxies

Core-collapse supernova subtypes in luminous infrared galaxies

Core-collapse supernova subtypes in luminous infrared galaxies

Star Formation in Nearby Dwarf Galaxies

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