2009A&A...505..265L


Query : 2009A&A...505..265L

2009A&A...505..265L - Astronomy and Astrophysics, volume 505, 265-279 (2009/10-1)

The normal type Ia SN 2003hv out to very late phases.

LELOUDAS G., STRITZINGER M.D., SOLLERMAN J., BURNS C.R., KOZMA C., KRISCIUNAS K., MAUND J.R., MILNE P., FILIPPENKO A.V., FRANSSON C., GANESHALINGAM M., HAMUY M., LI W., PHILLIPS M.M., SCHMIDT B.P., SKOTTFELT J., TAUBENBERGER S., BOLDT L., FYNBO J.P.U., GONZALEZ L., SALVO M. and THOMAS-OSIP J.

Abstract (from CDS):

We study a thermonuclear supernova (SN), emphasizing very late phases. An extensive dataset for SN 2003hv that covers the flux evolution from maximum light to day +786 is presented. This includes 82 epochs of optical imaging, 24 epochs of near-infrared (NIR) imaging, and 10 epochs of optical spectroscopy. These data are combined with published nebular-phase IR spectra, and the observations are compared to model light curves and synthetic nebular spectra. SN 2003hv is a normal Type Ia supernova (SN Ia) with photometric and spectroscopic properties consistent with its rarely observed B-band decline-rate parameter, Δm15(B)=1.61±0.02. The blueshift of the most isolated [FeII] lines in the nebular-phase optical spectrum appears consistent with those observed in the IR at similar epochs. At late times there is a prevalent color evolution from the optical toward the NIR bands. We present the latest-ever detection of a SN Ia in the NIR in Hubble Space Telescope images. The study of the ultraviolet/optical/infrared (UVOIR) light curve reveals that a substantial fraction of the flux is ``missing'' at late times. Between 300 and 700 days past maximum brightness, the UVOIR light curve declines linearly following the decay of radioactive 56Co, assuming full and instantaneous positron trapping. At 700 days we detect a possible slowdown of the decline in optical-bands, mainly in the V-band. The data are incompatible with a dramatic infrared catastrophe (IRC). However, the idea that an IRC occurred in the densest regions before 350 days can explain the missing flux from the UVOIR wavelengths and the flat-topped profiles in the NIR. We argue that such a scenario is possible if the ejecta are clumpy. The observations suggest that positrons are most likely trapped in the ejecta.

Abstract Copyright:

Journal keyword(s): supernovae: general - supernovae: individual: SN 2003hv

CDS comments: Fig 1., Table 2 : stars 11 and 13 not detected in USNO. Star 12 may be USNO-B1.0 0639-0035415 or USNO-B1.0 0639-0035413.

Simbad objects: 30

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Number of rows : 30
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 2000cx SN* 01 24 46.1 +09 30 31           SNIap 207 1
2 PG 0231+051 WD* 02 33 41.3574299856 +05 18 43.649856216 14.562 15.776 16.096 16.267 16.639 DAO.6 143 0
3 USNO-B1.0 0638-00042615 * 03 03 54.4955467440 -26 07 27.186351564   16.978 16.428 16.093 15.766 ~ 1 0
4 USNO-B1.0 0639-00035347 * 03 03 58.2392878176 -26 05 07.758073824 19.522 20.123 19.933 19.586 19.064 ~ 1 0
5 USNO-B1.0 0639-00035353 * 03 03 59.9783451552 -26 02 26.410738128 21.801 21.665 20.925 20.459 20.043 ~ 1 0
6 USNO-B1.0 0638-00042630 * 03 04 01.5889809768 -26 06 51.567909948 17.308 16.195 14.919 14.123 13.431 ~ 1 0
7 USNO-B1.0 0639-00035377 PM* 03 04 03.1122844440 -26 05 26.917452852 19.712 19.254 18.071 17.323 16.644 ~ 1 0
8 USNO-B1.0 0639-00035381 * 03 04 04.7710723824 -26 03 04.464038628 18.22 18.000 17.261 16.849 16.431 ~ 1 0
9 USNO-B1.0 0639-00035394 * 03 04 07.50 -26 02 24.4 22.179 22.029 21.290 20.847 20.470 ~ 1 0
10 NGC 1201 GiG 03 04 07.9912913448 -26 04 10.874234136   11.78 10.64 10.35   ~ 135 0
11 USNO-B1.0 0638-00042649 * 03 04 09.2218687224 -26 07 14.921047884 17.879 16.738 15.502 14.731 14.062 ~ 1 0
12 SN 2003hv SN* 03 04 09.32 -26 05 07.5     12.5     SNIa 111 1
13 USNO-B1.0 0638-00042652 * 03 04 10.3581699456 -26 08 02.979898980   18.612 17.779 17.253 16.797 ~ 1 0
14 USNO-B1.0 0639-00035420 PM* 03 04 17.750 -26 04 44.38 22.384 21.850 20.885 20.302 19.834 ~ 1 0
15 USNO-B1.0 0638-00042680 * 03 04 21.7157593272 -26 08 08.577450960   16.228 15.754 15.432 15.123 ~ 1 0
16 GSPC S301-D * 03 26 54.0 -39 50 38           ~ 16 0
17 SN 1992A SN* 03 36 27.41 -34 57 31.4   12.56 12.50     SNIa 395 1
18 SN 2001el SN* 03 44 30.60 -44 38 23.4   12.81       SNIa 251 1
19 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4691 2
20 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A0mA1Va 1468 0
21 SN 1999by SN* 09 21 52.07 +51 00 06.6   13.66       SNIap 273 1
22 SN 2002bo SN* 10 18 06.51 +21 49 41.7   13.95       SNIa 294 1
23 SN 1994D SN* 12 34 02.395 +07 42 05.70   11.75 12.03     SNIa 533 1
24 SN 1996X SN* 13 18 01.13 -26 50 45.3   12.99 13.00     SNIa 185 1
25 SN 1986G SN* 13 25 36.46 -43 01 53.6   12.45 11.44     SNIapec 394 1
26 SN 2003du SN* 14 34 35.80 +59 20 03.8   13.46       SNIa 332 1
27 GSPC S279-F * 17 48 22.7 -45 25 45           ~ 29 0
28 SN 2006gz SN* 18 10 26.33 +30 59 44.4   16.6       SNIa 139 1
29 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2590 0
30 SN 2000E SN* 20 37 13.77 +66 05 50.2   12.85       SNIa 83 1

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2022.05.20-01:58:40

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