2017ApJ...836..158H


Query : 2017ApJ...836..158H

2017ApJ...836..158H - Astrophys. J., 836, 158-158 (2017/February-3)

Type Ibn supernovae show photometric homogeneity and spectral diversity at maximum light.

HOSSEINZADEH G., ARCAVI I., VALENTI S., McCULLY C., HOWELL D.A., JOHANSSON J., SOLLERMAN J., PASTORELLO A., BENETTI S., CAO Y., CENKO S.B., CLUBB K.I., CORSI A., DUGGAN G., ELIAS-ROSA N., FILIPPENKO A.V., FOX O.D., FREMLING C., HORESH A., KARAMEHMETOGLU E., KASLIWAL M., MARION G.H., OFEK E., SAND D., TADDIA F., ZHENG W., FRASER M., GAL-YAM A., INSERRA C., LAHER R., MASCI F., REBBAPRAGADA U., SMARTT S., SMITH K.W., SULLIVAN M., SURACE J. and WOZNIAK P.

Abstract (from CDS):

Type Ibn supernovae (SNe) are a small yet intriguing class of explosions whose spectra are characterized by low-velocity helium emission lines with little to no evidence for hydrogen. The prevailing theory has been that these are the core-collapse explosions of very massive stars embedded in helium-rich circumstellar material (CSM). We report optical observations of six new SNe Ibn: PTF11rfh, PTF12ldy, iPTF14aki, iPTF15ul, SN 2015G, and iPTF15akq. This brings the sample size of such objects in the literature to 22. We also report new data, including a near-infrared spectrum, on the Type Ibn SN 2015U. In order to characterize the class as a whole, we analyze the photometric and spectroscopic properties of the full Type Ibn sample. We find that, despite the expectation that CSM interaction would generate a heterogeneous set of light curves, as seen in SNe IIn, most Type Ibn light curves are quite similar in shape, declining at rates around 0.1 mag day–1 during the first month after maximum light, with a few significant exceptions. Early spectra of SNe Ibn come in at least two varieties, one that shows narrow P Cygni lines and another dominated by broader emission lines, both around maximum light, which may be an indication of differences in the state of the progenitor system at the time of explosion. Alternatively, the spectral diversity could arise from viewing-angle effects or merely from a lack of early spectroscopic coverage. Together, the relative light curve homogeneity and narrow spectral features suggest that the CSM consists of a spatially confined shell of helium surrounded by a less dense extended wind.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): supernovae: general - supernovae: individual: (PTF11rfh, PTF12ldy, iPTF14aki, SN 2015U, iPTF15ul, SN 2015G, iPTF15akq) - supernovae: individual: (PTF11rfh, PTF12ldy, iPTF14aki, SN 2015U, iPTF15ul, SN 2015G, iPTF15akq)

Simbad objects: 37

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Number of rows : 37
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 SN 2005db SN* 00 41 26.79 +25 29 51.6     17.3     SNIIn 28 1
2 SN 2005gl SN* 00 49 50.02 +32 16 56.8       17.0   SNIIn 132 2
3 SN 2000er SN* 02 24 32.54 -58 26 18.0     15.1     SNIbn 24 1
4 NAME PS 15dpn SN* 02 32 59.75 +18 38 07.0           SNIbn 11 0
5 OGLE 2012-SN-6 SN* 03 33 34.79 -74 23 40.1           SNIbn 26 0
6 SN 2004gq SN* 05 12 04.81 -15 40 54.2     15.5     SNIb 82 1
7 SN 2015U SN* 07 28 53.87 +33 49 10.6           SNIbn 29 1
8 ASASSN -14dd SN* 07 45 14.380 -71 24 14.04     15.6     SNIbn 6 0
9 PTF 11kx SN* 08 09 12.87 +46 18 48.8           SNIa 124 0
10 SN 2016Q SN* 08 10 19.86 +19 26 48.2           SNIbn 3 0
11 SN 2010al SN* 08 14 15.91 +18 26 18.2           SNIInpec 57 1
12 PS1-12sk SN* 08 44 54.860 +42 58 16.89           SNIbn 27 0
13 SN 2014av SN* 09 00 20.02 +52 29 28.0           SNIb: 15 1
14 SN 2006jc SN* 09 17 20.78 +41 54 32.7     13.8     SNIbn 301 1
15 UGC 4904 GiP 09 17 21.709 +41 54 38.92   15.0       ~ 66 0
16 SN 2010jl SN* 09 42 53.33 +09 29 41.8           SNIIn 237 1
17 LSQ 12btw SN* 10 10 28.820 +05 32 12.48           SNIbn 18 0
18 iPTF 15ul SN* 12 14 03.76 +47 54 03.9           ~ 12 0
19 SN 2005la SN* 12 52 15.68 +27 31 52.5     17.6     SNIbn/IIbn 57 1
20 SN 2014bk SN* 13 54 02.42 +20 00 24.3           SNIbpec 6 1
21 CRTS CSS140421 J142042+031602 SN* 14 20 41.70 +03 16 01.5           SNIbn 10 0
22 SN 2002ao SN* 14 29 35.74 -00 00 55.8     14.3     SNIb/cpec 49 1
23 iPTF 13bvn SN* 15 00 00.152 +01 52 53.17           SNIb 135 0
24 iPTF 15akq SN* 15 03 51.29 +33 33 18.1           ~ 5 0
25 iPTF 13beo SN* 16 12 26.63 +14 19 18.0           SNIbn 22 0
26 ASASSN -15ed SN* 16 48 25.16 +50 59 30.7           SNIbn 20 0
27 SN 1999cq SN* 18 32 07.10 +37 36 44.3     15.8     SNIb/c 51 1
28 SN 2015G SN* 20 37 25.58 +66 07 11.5           SNIbn 22 1
29 SN 2005cl SN* 21 02 02.35 -06 17 35.7     18.3     SNIIn 28 1
30 LSQ 13ccw SN* 21 35 51.64 -18 32 52.0           SNIbn 21 0
31 SN 2009ip s*b 22 23 08.26 -28 56 52.4           LBV 305 0
32 SN 2011hw SN* 22 26 14.54 +34 12 59.1           SNIIn: 47 1
33 PTF 11rfh SN* 22 35 49.58 -00 22 26.1           ~ 5 0
34 SN 2014C SN* 22 37 05.60 +34 24 31.9           SNIb 85 1
35 SN 2008ha SN* 23 34 52.69 +18 13 35.4           SNIax 169 1
36 PTF 12ldy SN* 23 45 11.04 +23 09 18.8           ~ 6 0
37 GrW 151226 GWE ~ ~           ~ 234 1

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2022.06.27-05:15:14

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