2011MNRAS.412.2735T


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.28CET14:08:48

2011MNRAS.412.2735T - Mon. Not. R. Astron. Soc., 412, 2735-2762 (2011/April-3)

High luminosity, slow ejecta and persistent carbon lines: SN 2009dc challenges thermonuclear explosion scenarios.

TAUBENBERGER S., BENETTI S., CHILDRESS M., PAKMOR R., HACHINGER S., MAZZALI P.A., STANISHEV V., ELIAS-ROSA N., AGNOLETTO I., BUFANO F., ERGON M., HARUTYUNYAN A., INSERRA C., KANKARE E., KROMER M., NAVASARDYAN H., NICOLAS J., PASTORELLO A., PROSPERI E., SALGADO F., SOLLERMAN J., STRITZINGER M., TURATTO M., VALENTI S. and HILLEBRANDT W.

Abstract (from CDS):

Extended optical and near-IR observations reveal that SN 2009dc shares a number of similarities with normal Type Ia supernovae (SNe Ia), but is clearly overluminous, with a (pseudo-bolometric) peak luminosity of log (L) = 43.47 (erg/s). Its light curves decline slowly over half a year after maximum light [Δm15(B)true= 0.71], and the early-time near-IR light curves show secondary maxima, although the minima between the first and the second peaks are not very pronounced. The bluer bands exhibit an enhanced fading after ∼200 d, which might be caused by dust formation or an unexpectedly early IR catastrophe. The spectra of SN 2009dc are dominated by intermediate-mass elements and unburned material at early times, and by iron-group elements at late phases. Strong C II lines are present until ∼2 weeks past maximum, which is unprecedented in thermonuclear SNe. The ejecta velocities are significantly lower than in normal and even subluminous SNe Ia. No signatures of interaction with a circumstellar medium (CSM) are found in the spectra. Assuming that the light curves are powered by radioactive decay, analytic modelling suggests that SN 2009dc produced ∼1.8 M of 56Ni assuming the smallest possible rise time of 22 d. Together with a derived total ejecta mass of ∼2.8 M, this confirms that SN 2009dc is a member of the class of possible super-Chandrasekhar-mass SNe Ia similar to SNe 2003fg, 2006gz and 2007if. A study of the hosts of SN 2009dc and other superluminous SNe Ia reveals a tendency of these SNe to explode in low-mass galaxies. A low metallicity of the progenitor may therefore be an important prerequisite for producing superluminous SNe Ia. We discuss a number of possible explosion scenarios, ranging from super-Chandrasekhar-mass white-dwarf progenitors over dynamical white-dwarf mergers and Type I{img} SNe to a core-collapse origin of the explosion. None of the models seems capable of explaining all properties of SN 2009dc, so that the true nature of this SN and its peers remains nebulous.

Based on observations at ESO La Silla, Prog. 083.D-0970 and 184.D-1140 and ESO Paranal, Prog. 083.D-0728.


Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS

Journal keyword(s): supernovae: general - supernovae: individual: SN 2006gz - supernovae: individual: SN 2007if - supernovae: individual: SN 2009dc - galaxies: individual: UGC 10063 - galaxies: individual: UGC 10064

Simbad objects: 28

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Number of rows : 28

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SN 2005hk SN* 00 27 50.89 -01 11 53.3   15.92       SN.Iax 181 1
2 SN 2007if SN* 01 10 51.37 +15 27 39.9   23.3 19.5     SN.Iap 102 1
3 SN 2007gr SN* 02 43 27.98 +37 20 44.7       12.77   SNIc 179 1
4 SN 2001el SN* 03 44 30.60 -44 38 23.4   12.81       SN.Ia 237 1
5 SN 1999by SN* 09 21 52.07 +51 00 06.6   13.66       SN.Iap 252 1
6 SN 2002bo SN* 10 18 06.51 +21 49 41.7   13.95       SN.Ia 267 1
7 SN 2005bf SN* 10 23 56.99 -03 11 29.3     18.0     SNIb 165 1
8 NAME Great Attractor SCG 10 32 -46.0           ~ 449 0
9 SN 1991bg SN* 12 25 03.70 +12 52 15.6   14.75 14.3     SN.IaPec 521 1
10 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5704 0
11 SN 1991T SN* 12 34 10.20 +02 39 56.4   11.70 11.51     SN.IaPec 694 1
12 SN 2004gu SN* 12 46 24.72 +11 56 56.1     17.5     SN.Iap 36 1
13 2MFGC 10065 G 12 46 24.785 +11 56 57.72   17.34       ~ 14 0
14 NAME SHAPLEY-CENTAURUS CL SCG 13 06.0 -33 04           ~ 483 0
15 SN 2003fg SN* 14 16 18.924 +52 14 53.68           SNIa 112 1
16 SN 2003du SN* 14 34 35.80 +59 20 03.8   13.46       SN.Ia 308 1
17 SN 2009dr SN* 14 44 42.08 +49 43 44.9           SN.Ia: 7 1
18 SN 2005cf SN* 15 21 33.12 -07 26 57.1   13.54       SN.Ia 231 1
19 UGC 10063 EmG 15 51 08.422 +25 43 21.36   16.5       ~ 16 0
20 SN 2009dc SN* 15 51 12.12 +25 42 28.0           SN.Iap 125 1
21 UGC 10064 EmG 15 51 13.2751649076 +25 42 06.783972569   15.0       ~ 42 0
22 SNF 20080723-012 SN* 16 16 03.07 +03 03 16.9           ~ 8 0
23 SN 2006gz SN* 18 10 26.33 +30 59 44.4   16.6       SNIa 123 1
24 IC 1277 GiP 18 10 27.3021092989 +31 00 11.686097348   15.0       ~ 28 0
25 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1623 2
26 SN 2004eo SN* 20 32 54.19 +09 55 42.7   15.07 17.8     SN.Ia 161 1
27 SN 1999ee SN* 22 16 09.40 -36 50 31.5   14.85       SN.Ia 169 1
28 NAME Local Group GrG ~ ~           ~ 6771 0

    Equat.    Gal    SGal    Ecl

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2020.01.28-14:08:48

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