2001ApJ...559.1019M


Query : 2001ApJ...559.1019M

2001ApJ...559.1019M - Astrophys. J., 559, 1019-1031 (2001/October-1)

Late light curves of type Ia supernovae.

MILNE P.A., THE L.-S. and LEISING M.D.

Abstract (from CDS):

We extend earlier efforts to determine whether the late (t≥60 days) light curves of Type Ia SNe are better explained by the escape of positrons from the ejecta or by the complete deposition of positron kinetic energy in a trapping magnetic field. We refine our selection of Ia SNe, using those that have extensive BVRI photometry 35 days or more after maximum light. Assuming that all SNe within a given Δm15(B) range form a distinct subclass, we fit a combined light curve for all class members with a variety of models. We improve our previous calculations of energy deposition rates by including the transport of the Comptonized electrons. Their nonlocal and time-dependent energy deposition produces a correction of as much as 0.10 mag for Chandrasekhar-mass models and 0.18 mag for sub-Chandrasekhar-mass models.

We produce bolometric corrections, derived from measured spectra, to B, V, R, and I light curves after day 50. Comparisons of the resulting bolometric light curves with simulated energy deposition rates demonstrate that the energy deposition from the photons and positrons created in 56Co⟶56Fe decays are consistent with the observations if positron escape is assumed. This implies that there is no evidence of additional sources of energy deposition or of a shift of emission into unobserved wavelength ranges between days 60 and 900. The V band is shown to be an accurate indicator of total emission in the 3500-9700 Å range, with a constant fraction (∼25%) appearing in the V band after day 50. This suggests that the V band scales with the bolometric luminosity and that the deposited energy is instantaneously recycled into optical emission during this epoch. We see significant evolution of the colors of SNe Ia between days 50 and 170. We suggest that this may be due to the transition from spectra dominated by emission lines from the radioactive nucleus, 56Co, to those from the stable daughter nucleus, 56Fe.


Abstract Copyright:

Journal keyword(s): Gamma Rays: Observations - Gamma Rays: Theory - Stars: Supernovae: General

Simbad objects: 50

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Number of rows : 50
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 NGC 252 GiG 00 48 01.5069897792 +27 37 26.093379360   13.4 12.49     ~ 81 0
2 SN 1998de SN* 00 48 06.88 +27 37 28.5   17.56       SNIapec 84 1
3 SN 1992bc SN* 03 05 16.05 -39 33 34.6   15.15 15.17     SNIa 126 1
4 SN 1992A SN* 03 36 27.41 -34 57 31.4   12.56 12.50     SNIa 395 1
5 NGC 1380 GiP 03 36 27.590 -34 58 34.68 11.32 10.94 9.93 9.37   ~ 406 1
6 UGC 3151 GiG 04 45 19.616 +11 04 04.53   16.5       ~ 52 0
7 SN 1995bd SN* 04 45 21.24 +11 04 02.5   17.29       SNIapec 65 1
8 SN 1987L SN* 07 27 26.42 +80 09 30.6   13.2 18.2     SNIa 25 1
9 NGC 2441 GiG 07 51 54.6864254040 +73 00 56.553791256   12.7       ~ 97 0
10 SN 1995E SN* 07 51 56.75 +73 00 34.6   16.81 15.9     SNIa 115 1
11 NGC 2935 EmG 09 36 44.8527810504 -21 07 41.560449096   11.84 10.04 10.44 11.6 ~ 127 1
12 NGC 2962 GiP 09 40 53.9321546928 +05 09 57.032828496   13.1       ~ 194 0
13 SN 1995D SN* 09 40 54.753 +05 08 26.16   13.42 13.22     SNIa 147 1
14 SN 1995al SN* 09 50 55.97 +33 33 09.4   13.36 13.22     SNIa 99 1
15 NGC 3021 GiG 09 50 57.1456156056 +33 33 12.934404072   12.6       ~ 179 0
16 SN 1993ag SN* 10 03 35.00 -35 27 47.6   18.30 17.78     SNIa 66 1
17 2MASX J10033546-3527410 G 10 03 35.4396402456 -35 27 41.044198860   17.05   15.69   ~ 13 1
18 M 96 GiP 10 46 45.744 +11 49 11.78 10.42 10.15 9.25 8.99   ~ 790 1
19 SN 1998bu SN* 10 46 46.01 +11 50 07.5   12.11       SNIa 309 1
20 SN 1994ae SN* 10 47 01.94 +17 16 30.8   13.20 12.99     SNIa 167 1
21 SN 1989B SN* 11 20 13.93 +13 00 18.9   12.25       SNIa 354 1
22 SN 1991bg SN* 12 25 03.70 +12 52 15.6   14.75 14.3     SNIapec 570 1
23 M 84 Sy2 12 25 03.74333 +12 53 13.1393 12.67 12.09 10.49     ~ 1715 2
24 SN 1984A SN* 12 26 55.73 +15 03 17.1   12.40 12.20     SNIa 133 1
25 SN 1994D SN* 12 34 02.395 +07 42 05.70   11.75 12.03     SNIa 536 1
26 IRAS 12315+0758 GiG 12 34 03.029 +07 41 56.90   10.6       ~ 642 0
27 NGC 4527 GiP 12 34 08.496 +02 39 13.72   12.4       ~ 519 2
28 SN 1991T SN* 12 34 10.20 +02 39 56.4   11.70 11.51     SNIapec 749 1
29 SN 1981B SN* 12 34 29.57 +02 11 59.3   11.74       SNIa 394 1
30 NGC 4639 GiP 12 42 52.3785000336 +13 15 26.706153600   13.62 12.72     ~ 589 0
31 SN 1990N SN* 12 42 56.68 +13 15 23.4   12.69 12.62     SNIa 384 1
32 SN 1937C SN* 13 05 53.2 +37 36 07   8.80 8.77     SNIa 202 1
33 SN 1992K SN* 13 10 04.20 -46 26 30.3   16.30 16.2     SNIapec 72 1
34 ESO 269-57 GiG 13 10 04.4423275416 -46 26 14.476741944   12.49   11.30 11.9 ~ 54 0
35 SN 1996X SN* 13 18 01.13 -26 50 45.3   12.99 13.00     SNIa 185 1
36 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4319 3
37 SN 1986G SN* 13 25 36.46 -43 01 53.6   12.45 11.44     SNIapec 399 1
38 SN 1972E SN* 13 39 52.7 -31 40 09   8.49 8.30     SNIa 301 1
39 ESO 445-66 GiG 13 52 50.2668050616 -30 42 35.755878420   14.64   13.26   ~ 30 0
40 SN 1993H SN* 13 52 50.34 -30 42 23.3   16.99       SNIa 87 1
41 NGC 5490 rG 14 09 57.330 +17 32 43.53   13.4 15.5     ~ 161 1
42 SN 1997cn SN* 14 09 57.76 +17 32 32.3   17.2 16.7     SNIapec 81 1
43 MCG+03-44-003 G 17 15 34.3738986216 +16 19 29.713024704   15.1       ~ 27 0
44 SN 1990O SN* 17 15 35.92 +16 19 25.8   16.59 16.22     SNIa 75 1
45 SN 1991ag SN* 20 00 08.61 -55 22 03.1   14.67 14.39     SNIa 56 1
46 IC 4919 G 20 00 09.05 -55 22 24.2   15.03   14.31 14.2 ~ 30 0
47 ESO 234-69 GiG 20 45 54.5263393944 -51 23 28.491578376   14.18   13.09 13.8 ~ 43 0
48 SN 1992al SN* 20 45 56.49 -51 23 39.9   14.59 14.54     SNIa 83 2
49 SN 1995ac SN* 22 45 34.14 -08 45 04.7   17.23 17.10     SNIapec 78 2
50 SN 1993L SN* 22 57 52.86 -35 51 26.8     13.20     SNIa 32 1

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2023.01.28-10:57:23

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