2018A&A...611A..58G


Query : 2018A&A...611A..58G

2018A&A...611A..58G - Astronomy and Astrophysics, volume 611A, 58-58 (2018/3-1)

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv.

GALL C., STRITZINGER M.D., ASHALL C., BARON E., BURNS C.R., HOEFLICH P., HSIAO E.Y., MAZZALI P.A., PHILLIPS M.M., FILIPPENKO A.V., ANDERSON J.P., BENETTI S., BROWN P.J., CAMPILLAY A., CHALLIS P., CONTRERAS C., ELIAS DE LA ROSA N., FOLATELLI G., FOLEY R.J., FRASER M., HOLMBO S., MARION G.H., MORRELL N., PAN Y.-C., PIGNATA G., SUNTZEFF N.B., TADDIA F., ROBLEDO S.T. and VALENTI S.

Abstract (from CDS):

We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN 2011iv are characterised by Δm15 (B) decline-rate values of 1.96mag and 1.77mag, respectively. Although they have similar decline rates, their peak B- and H-band magnitudes differ by ∼0.60mag and ∼0.35mag, respectively. After correcting for the luminosity vs. decline rate and the luminosity vs. colour relations, the peak B-band and H-band light curves provide distances that differ by ∼14% and ∼ 9%, respectively. These findings serve as a cautionary tale for the use of transitional SNe Ia located in early-type hosts in the quest to measure cosmological parameters. Interestingly, even though SN 2011iv is brighter and bluer at early times, by three weeks past maximum and extending over several months, its B-V colour is 0.12mag redder than that of SN 2007on. To reconcile this unusual behaviour, we turn to guidance from a suite of spherical one-dimensional Chandrasekhar-mass delayed-detonation explosion models. In this context, 56Ni production depends on both the so-called transition density and the central density of the progenitor white dwarf. To first order, the transition density drives the luminosity-width relation, while the central density is an important second-order parameter. Within this context, the differences in the B-V colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on.

Abstract Copyright: © ESO 2018

Journal keyword(s): supernovae: general - supernovae: individual: SN 2007on - supernovae: individual: SN 2011iv - dust, extinction

VizieR on-line data: <Available at CDS (J/A+A/611/A58): table1.dat table2.dat table3.dat table4.dat table5.dat>

Simbad objects: 26

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Number of rows : 26
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* S And No* 00 42 43.12368 +41 16 03.2124           ~ 179 2
2 iPTF 13ebh SN* 02 21 59.98 +33 16 13.7           SNIa 38 0
3 SN 2003gs SN* 02 27 38.36 -01 09 35.4     14.0     SNIap 53 1
4 SN 2009ig SN* 02 38 11.62 -01 18 45.3           SNIa 139 1
5 SN 2003hv SN* 03 04 09.32 -26 05 07.5     12.5     SNIa 114 1
6 SN 2006dd SN* 03 22 41.64 -37 12 13.2   14.5 15.0     SNIa 72 1
7 NGC 1316 GiP 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1321 1
8 SN 2006mr SN* 03 22 42.84 -37 12 28.5     15.6     SNIap 61 1
9 SN 1980N SN* 03 22 59 -37 12.8   12.5 12.37     SNIa 146 1
10 SN 1992A SN* 03 36 27.41 -34 57 31.4   12.56 12.50     SNIa 395 1
11 NGC 1399 BiC 03 38 29.083 -35 27 02.67 11.05 9.74 9.59 8.12   ~ 1530 1
12 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1725 0
13 SN 2007on SN* 03 38 50.90 -35 34 30.0       14.9   SNIa 122 1
14 SN 2011iv SN* 03 38 51.35 -35 35 32.0           SNIa 66 1
15 NGC 1404 GiP 03 38 51.917 -35 35 39.81 11.53 10.69 10.00 9.03   ~ 725 1
16 SN 1999em SN* 04 41 27.04 -02 51 45.2   13.79 13.7     SNIIP 647 1
17 SN 2014J SN* 09 55 42.12 +69 40 25.9           SNIa 377 1
18 SN 1991bg SN* 12 25 03.70 +12 52 15.6   14.75 14.3     SNIapec 570 1
19 SN 1991T SN* 12 34 10.20 +02 39 56.4   11.70 11.51     SNIapec 749 1
20 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4319 3
21 SN 1986G SN* 13 25 36.46 -43 01 53.6   12.45 11.44     SNIapec 399 1
22 SN 2011fe SN* 14 03 05.711 +54 16 25.22   10.12 10.06     SNIa 613 1
23 SN 2015bp SN? 15 05 30.07 +01 38 02.4           ~ 19 0
24 SN 2004eo SN* 20 32 54.19 +09 55 42.7   15.07 17.8     SNIa 192 1
25 SN 2013dy SN* 22 18 17.60 +40 34 09.6           SNIa 92 0
26 SN 2001ig SN* 22 57 30.69 -41 02 25.9     14.5     SNIIb 164 1

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2023.01.27-09:44:25

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