2018MNRAS.475.1046I


Query : 2018MNRAS.475.1046I

2018MNRAS.475.1046I - Mon. Not. R. Astron. Soc., 475, 1046-1072 (2018/March-3)

On the nature of hydrogen-rich superluminous supernovae.

INSERRA C., SMARTT S.J., GALL E.E.E., LELOUDAS G., CHEN T.-W., SCHULZE S., JERKSTRAND A., NICHOLL M., ANDERSON J.P., ARCAVI I., BENETTI S., CARTIER R.A., CHILDRESS M., DELLA VALLE M., FLEWELLING H., FRASER M., GAL-YAM A., GUTIERREZ C.P., HOSSEINZADEH G., HOWELL D.A., HUBER M., KANKARE E., KRUHLER T., MAGNIER E.A., MAGUIRE K., McCULLY C., PRAJS S., PRIMAK N., SCALZO R., SCHMIDT B.P., SMITH M., SMITH K.W., TUCKER B.E., VALENTI S., WILMAN M., YOUNG D.R. and YUAN F.

Abstract (from CDS):

We present two hydrogen-rich superluminous supernovae (SLSNe): SN2103hx and PS15br. These objects, together with SN2008es, are the only SLSNe showing a distinct, broad H α feature during the photospheric phase; also, they show no sign of strong interaction between fast moving ejecta and circumstellar shells in their early spectra. Despite the fact that the peak luminosity of PS15br is fainter than that of the other two objects, the spectrophotometric evolution is similar to SN2103hx and different from any other supernova in a similar luminosity space. We group all of them as SLSNe II and hence they are distinct from the known class of SLSN IIn. Both transients show a strong, multicomponent H α emission after 200 d past maximum, which we interpret as an indication of the interaction of the ejecta with an asymmetric, clumpy circumstellar material. The spectra and photometric evolution of the two objects are similar to Type II supernovae, although they have much higher luminosity and evolve on slower time-scales. This is qualitatively similar to how SLSNe I compare with normal type Ic, in that the former are brighter and evolve more slowly. We apply a magnetar and an interaction semi-analytical code to fit the light curves of our two objects and SN2008es. The overall observational data set would tend to favour the magnetar, or central engine, model as the source of the peak luminosity, although the clear signature of late-time interaction indicates that interaction can play a role in the luminosity evolution of SLSNe II at some phases.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): circumstellar matter - stars: magnetars - supernovae: general - supernovae: individual: SN2103hx - supernovae: individual: PS15br - supernovae: individual: SN2008es

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 - 2021
#notes
1 iPTF 13iqb SN* 00 34 04.84 -09 42 17.9           SNIIn 57 0
2 CRTS CSS121015 J004244+132827 SN* 00 42 44.380 +13 28 26.20           SNII/IIB 28 0
3 SN 2007pk SN* 01 31 47.07 +33 36 54.1     17.0     SNIInpec 35 1
4 SN 2013hx SN* 01 35 33.28 -57 57 50.6           SNIc 14 1
5 SN 2013fc SN* 02 45 08.95 -55 44 27.3           SNIIn 12 0
6 SN 2006gy SN* 03 17 27.06 +41 24 19.5       14.20   SNIIn 305 1
7 SN 2009bw SN* 03 56 06.92 +72 55 40.9           SNII 58 1
8 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4626 2
9 iPTF 13ehe SN* 06 53 21.50 +67 07 56.0           SLSN-I 55 0
10 LSQ 14mo ev 10 22 41.53 -16 55 14.4           SLSN-I 44 0
11 SDSS J112519.21+081417.9 G 11 25 19.2279923293 +08 14 18.533047404           ~ 1 0
12 NAME PS 15br SN* 11 25 19.23 +08 14 18.5           SNSL 10 0
13 SN 2010gx SN* 11 25 46.71 -08 49 41.4           SNIc 145 1
14 SN 2015bn SN* 11 33 41.57 +00 43 32.2           SNIc 93 0
15 SN 1998S SN* 11 46 06.13 +47 28 55.4     12.2     SNIIn 406 1
16 SN 2008es SN* 11 56 49.13 +54 27 25.7           SNIIL 105 1
17 SN 1986E SN* 12 21 41.19 +14 37 54.8   14.2       SNIIL 62 1
18 SN 1979C SN* 12 22 58.58 +15 47 52.7   11.6       SNIIL 557 1
19 SN 2011ke SN* 13 50 57.77 +26 16 42.8     18.6     SLSNIc 75 1
20 SN 2013cu SN* 14 33 58.97 +40 14 20.7           SNII: 67 1
21 SN 2009kf SN* 16 12 54.00 +55 38 13.8           SNIIP 44 1
22 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1704 2
23 SN 1980K SN* 20 35 30.07 +60 06 23.7   11.6       SNIIL 441 1

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2021.10.24-05:01:52

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