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Table 1.

Confirmed and likely CCSNe at the central regions (dproj ≤ 2.5 kpc) of LIRGs with SED model based global star formation properties of LIRG hosts (see compilations of Kool et al. 2018; Kool 2019, and references therein).

Host Dl log(LIR) tSB SNRSB SFR LAGN SED DOF CCSN Type dproj Disc. Ref.
(Mpc) (L) (Myr) (SN yr−1) (M yr−1) (%) host (kpc) (mag)
IRAS 18293−3413 84.1 11.89 S 22 AT 2012iz IIP 0.6 1.8 IR (1)
IRAS 18293−3413 SN 2013if IIP 0.2 0 IR (2)
IC 883 107.1 11.73 D 27 SN 2010cu IIP 0.2 0 IR (3)
IC 883 SN 2011hi IIP 0.4 6 IR (3)
NGC 5331 150.0 11.66 D 5 AT 2017chi IIn 1.5 12 IR (1)
Arp 299 44.8 11.82 0.0 S 5 SN 1998T Ib 1.5 ? Opt (4)
Arp 299 SN 2005U IIb 1.4 ? IR (4)
Arp 299 SN 2010O Ib 1.2 1.9 Opt (5)
Arp 299 SN 2010P IIb 0.2 7 IR (5)
Arp 299 SN 2019lqo IIb 2.0 2.1 Opt (6)
Arp 299 SN 2020fkb Ib 0.7 0.4 Opt (6)
NGC 1614 66.8 11.66 S 33 SN 1996D Ic 2.1 ? Opt (2)
NGC 1614 SN 2020cuj II 2.5 2.8 Opt (5)
NGC 838 53.3 11.05 S 7 SN 2005H II 0.4 ? Opt (2)
IRAS 17138−1017 82.2 11.49 S 22 SN 2008cs IIn 1.5 16 IR (7)
IRAS 17138−1017 SN 2015cb IIP 0.6 4.6 IR (2)
NGC 2388 61.1 11.28 D 8 SN 2015U Ibn 1.8 3.1 Opt (8)
NGC 317B 77.0 11.19 S 30 SN 1999gl II 1.9 ? Opt (2)
NGC 317B SN 2014dj Ic 1.5 ? Opt (2)
NGC 3256 37.4 11.61 S 16 SN 2001db II 2.1 5.5 IR (6)
NGC 3256 PSN102750 IIn 2.1 0.3 Opt (6)
NGC 3256 SN 2018ec Ic 1.7 2.1 IR (6)
NGC 3256 AT 2018cux IIP 0.8 2.1 Opt (6)
ESO 138−G27 96.1 11.41 S 27 SN 2009ap Ic 1.2 ? Opt (2)
NGC 6907 49.2 11.11 S 2 SN 2008fq II 1.4 ? Opt (2)
NGC 2146 18.0 11.15 S 8 SN 2005V Ib/c 0.5 ? IR (2)
MCG -02-01-052 115.2 11.48 S 3 SN 2010hp II 2.1 0.5 IR (9)
NGC 6000 28.1 10.95 S 4 SN 2010as IIb 0.6 1.8 Opt (10)
NGC 5433 70.3 11.01 < 0.03 S 2 SN 2010gk Ic 2.0 ? Opt (2)

Notes. Luminosity distances are obtained via NED. References for the CCSNe and their host galaxy extinction estimates, if available, are given in brackets.

References. 1) Kool (2019), 2) Kool et al. (2018), 3) Kankare et al. (2012), 4) Mattila et al. (2012), 5) Kankare et al. (2014a), 6) This work, 7) Kankare et al. (2008), 8) Pastorello et al. (2015), 9) Miluzio et al. (2013), 10) Folatelli et al. (2014).

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