2022ApJ...927..180P


Query : 2022ApJ...927..180P

2022ApJ...927..180P - Astrophys. J., 927, 180-180 (2022/March-2)

The Type Icn SN 2021csp: Implications for the Origins of the Fastest Supernovae and the Fates of Wolf-Rayet Stars.

PERLEY D.A., SOLLERMAN J., SCHULZE S., YAO Y., FREMLING C., GAL-YAM A., HO A.Y.Q., YANG Y., KOOL E.C., IRANI I., YAN L., ANDREONI I., BAADE D., BELLM E.C., BRINK T.G., CHEN T.-W., CIKOTA A., COUGHLIN M.W., DAHIWALE A., DEKANY R., DUEV D.A., FILIPPENKO A.V., HOEFLICH P., KASLIWAL M.M., KULKARNI S.R., LUNNAN R., MASCI F.J., MAUND J.R., MEDFORD M.S., RIDDLE R., ROSNET P., SHUPE D.L., STROTJOHANN N.L., TZANIDAKIS A. and ZHENG W.

Abstract (from CDS):

We present observations of SN 2021csp, the second example of a newly identified type of supernova (SN) hallmarked by strong, narrow, P Cygni carbon features at early times (Type Icn). The SN appears as a fast and luminous blue transient at early times, reaching a peak absolute magnitude of -20 within 3 days due to strong interaction between fast SN ejecta (v ≃ 30,000 km s–1) and a massive, dense, fast-moving C/O wind shed by the WC-like progenitor months before explosion. The narrow-line features disappear from the spectrum 10-20 days after explosion and are replaced by a blue continuum dominated by broad Fe features, reminiscent of Type Ibn and IIn supernovae and indicative of weaker interaction with more extended H/He-poor material. The transient then abruptly fades ∼60 days post-explosion when interaction ceases. Deep limits at later phases suggest minimal heavy-element nucleosynthesis, a low ejecta mass, or both, and imply an origin distinct from that of classical Type Ic SNe. We place SN 2021csp in context with other fast-evolving interacting transients, and discuss various progenitor scenarios: an ultrastripped progenitor star, a pulsational pair-instability eruption, or a jet-driven fallback SN from a Wolf-Rayet (W-R) star. The fallback scenario would naturally explain the similarity between these events and radio-loud fast transients, and suggests a picture in which most stars massive enough to undergo a W-R phase collapse directly to black holes at the end of their lives.

Abstract Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Supernovae - Core-collapse supernovae - Wolf-Rayet stars - Stellar mass black holes - Transient sources

Status at CDS : Associated data (images, light curves, etc...) being ingested in VizieR.

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 AT 2018lug ev 02 00 15.19 +16 47 57.3           ~ 34 0
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 17265 1
3 SN 2010al SN* 08 14 15.91 +18 26 18.2           SNIInpec 64 1
4 SN 2021ckj SN* 09 05 51.083 -08 35 07.56           SNIcn 9 0
5 SN 2008D SN* 09 09 30.625 +33 08 20.16     17.5     SNIb 402 1
6 SN 2006jc SN* 09 17 20.78 +41 54 32.7     13.8     SNIbn 341 1
7 SN 2020eyj SN* 11 11 47.180 +29 23 06.36           SNIa 15 0
8 SN 2019uo SN* 12 02 36.602 +41 03 41.92           SNIbn 17 0
9 SN 2020oi SN* 12 22 54.930 +15 49 24.96           SNIc 50 0
10 SN 1994I SN* 13 29 54.072 +47 11 30.50     12.9     SNIc 624 1
11 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4314 2
12 SN 2021csp SN* 14 26 22.114 +05 51 33.18           SNIcn 13 0
13 QSO J1430+1043 QSO 14 30 09.73880343 +10 43 26.8623079     18.5 18.67   ~ 91 1
14 SN 2020bvc SN* 14 33 57.009 +40 14 37.62           SNIc-BL 31 0
15 SN 2019hgp SN* 15 36 12.90 +39 44 00.6           SN.Icn 20 0
16 SN 2018cow SN* 16 16 00.254 +22 16 05.10           SNIb 231 0
17 SN 2018gep SN* 16 43 48.2 +41 02 43           SNIc 48 0
18 ASASSN -15ed SN* 16 48 25.16 +50 59 30.7           SNIbn 23 0
19 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1814 2
20 AT 2020xnd ev 22 20 02.030 -02 50 25.30           ~ 43 0
21 SN 2020nxt SN* 22 37 36.235 +35 00 07.68           SNIbn 5 0
22 NAME Local Group GrG ~ ~           ~ 8312 0
23 GRB 210210B gB ~ ~           ~ 3 0

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