2006MNRAS.368.1169P


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.23CEST04:37:00

2006MNRAS.368.1169P - Mon. Not. R. Astron. Soc., 368, 1169-1195 (2006/May-3)

Optical and infrared observations of the TypeIIP SN2002hh from days 3 to 397.

POZZO M., MEIKLE W.P.S., RAYNER J.T., JOSEPH R.D., FILIPPENKO A.V., FOLEY R.J., LI W., MATTILA S. and SOLLERMAN J.

Abstract (from CDS):

We present optical and infrared (IR) observations of the TypeII SN2002hh from 3 to 397d after explosion. The optical spectroscopic (4-397d) and photometric (3-278d) data are complemented by spectroscopic (137-381d) and photometric (137-314d) data acquired at IR wavelengths. This is the first time L-band spectra have ever been successfully obtained for a supernova (SN) at a distance beyond the Local Group. The VRI light curves in the first 40d reveal SN2002hh to be an SNIIP (plateau) - the most common of all core-collapse SNe. SN2002hh is one of the most highly extinguished SNe ever investigated. To provide a match between its early-time spectrum and a coeval spectrum of the TypeIIP SN1999em, as well as maintaining consistency with Ki interstellar absorption, we invoke a two-component extinction model. One component is due to the combined effect of the interstellar medium (ISM) of our Milky Way Galaxy and the SN host galaxy, while the other component is due to a `dust pocket' where the grains have a mean size smaller than in the ISM. The early-time optical light curves of SNe1999em and 2002hh are generally well matched, as are the radioactive tails of these two SNe and SN1987A. The late-time similarity of the SN2002hh optical light curves to those of SN1987A, together with measurements of the optical/IR luminosity and [Feii]1.257µm emission indicate that 0.07±0.02Mof 56Ni was ejected by SN2002hh. However, during the nebular phase the HKL' luminosities of SN2002hh exhibit a growing excess with respect to those of SN1987A. We attribute much of this excess to an IR-echo from a pre-existing, dusty circumstellar medium. Based on an IR-echo interpretation of the near-IR (NIR) excess, we deduce that the progenitor of SN2002hh underwent recent mass-loss of ∼0.3M. A detailed comparison of the late-time optical and NIR spectra of SNe1987A and 2002hh is presented. While the overall impression is one of similarity between the spectra of the two events, there are notable differences. The Mgi1.503µm luminosity of SN2002hh is a factor of 2.5 greater than in SN1987A at similar epochs, yet coeval silicon and calcium lines in SN2002hh are fainter. Interpreting these differences as being due to abundance variations, the overall abundance trend between SN1987A and 2002hh is not consistent with explosion model predictions. It appears that during the burning to intermediate-mass elements, the nucleosynthesis did not progress as far as might have been expected given the mass of iron ejected. Evidence for mixing in the ejecta is presented. Pronounced blueshifts seen in the more isolated lines are attributed to asymmetry in the ejecta. However, during the time-span of these observations (∼1-yr post-explosion) we find no evidence of dust condensation in the ejecta such as might have been revealed by an increasing blueshift and/or attenuation of the red wings of the emission lines. Nevertheless, the clear detection of first overtone CO emission by 200d and the reddening trend in (K - L')0suggest that dust formation in the ejecta may occur at later epochs. From the [Oi] λλ6300, 6364Å doublet luminosity we infer a 16-18Mmain-sequence progenitor star. The progenitor of SN2002hh was probably a red supergiant with a substantial, dusty wind.

Abstract Copyright: 2006 The Authors. Journal compilation © 2006 RAS

Journal keyword(s): circumstellar matter - supernovae: individual: SN2002hh - infrared: stars

Errata: vol. 375, p. 416 (2007)

CDS comments: Fig. 1 and Table 1 : Comparison stars not in simbad.

Simbad objects: 38

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Number of rows : 38

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 SN 1998dl SN* 02 46 01.47 -07 34 25.1     16.0     SNIIP 38 1
2 SN 1995V SN* 02 46 26.77 -00 29 55.6     15     SNII 49 1
3 HD 19445 PM* 03 08 25.5884 +26 19 51.400 8.29 8.52 8.06 7.60 7.27 G2VFe-3 748 0
4 NAME Per Arm PoG 03 30 +45.0           ~ 1313 0
5 SN 1999em SN* 04 41 27.04 -02 51 45.2   13.79 13.7     SNIIP 603 1
6 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4595 2
7 HD 84937 PM* 09 48 56.09801 +13 44 39.3237 8.49 8.68 8.32 7.97 7.70 F8Vm-5 736 0
8 SN 1993J SN* 09 55 24.77476 +69 01 13.7026   10.8 12.0     SNIIb 1293 1
9 SN 1999gi SN* 10 18 16.66 +41 26 28.2   14.8       SNIIP 213 1
10 Feige 34 HS* 10 39 36.7377085527 +43 06 09.209752646 9.613 10.91 11.14 11.319 11.464 sdOp 621 0
11 SN 1998bu SN* 10 46 46.01 +11 50 07.5   12.11       SNIa 299 1
12 SN 1989B SN* 11 20 13.93 +13 00 18.9   12.25       SNIa 345 1
13 SN 2000ew SN* 11 40 58.52 +11 27 55.9     14.9     SNIc 52 1
14 SN 1998S SN* 11 46 06.13 +47 28 55.4     12.2     SNIIn 400 1
15 SN 1979C SN* 12 22 58.58 +15 47 52.7   11.6       SNIIL 556 1
16 SN 1991T SN* 12 34 10.20 +02 39 56.4   11.70 11.51     SNIapec 713 1
17 SN 1985F SN* 12 41 33.01 +41 09 05.9   12.1       SNIb 126 1
18 SN 1996ad SN* 15 59 05.91 +19 48 08.1     18.5     ~ 5 1
19 HD 194354 * 20 22 49.55031 +53 25 03.0027   7.97 7.96     A0Vs 10 1
20 HD 340611 WD* 20 34 21.8849808924 +25 03 49.749569866 10.687 11.471 11.546 11.648 11.728 DA2.4 290 0
21 SN 1939C SN* 20 34 24.0680573946 +60 09 29.850424655   13.7 13.8     SNI: 39 1
22 2MASS J20344320+6007234 * 20 34 43.20 +60 07 23.4   16.1 15.2 14.3   ~ 5 0
23 SN 2002hh SN* 20 34 44.29 +60 07 19.0     17.18     SNIIP 137 1
24 SN 1917A SN* 20 34 46.9 +60 07 29   13.6       SNII 48 1
25 SN 1969P SN* 20 34 51.3 +60 06 14   14.2       ~ 31 1
26 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2313 2
27 SN 1968D SN* 20 34 58.40 +60 09 34.4   13.5 13.5     SNII 67 1
28 SN 1948B SN* 20 35 21.5 +60 10 16   14.0 14.0     SNIIP 69 1
29 SN 2004et SN* 20 35 25.33 +60 07 17.7   12.88       SNIIP 430 1
30 SN 1980K SN* 20 35 30.07 +60 06 23.7   11.6       SNIIL 439 1
31 BD+49 3325 * 20 36 08.3724299885 +49 38 23.625547863   11.53 11.07     G0 9 0
32 HD 199217 * 20 54 01.4352112387 +48 26 15.124087273   7.66 7.69     A0V 24 0
33 HD 201941 * 21 12 45.3250085732 +02 38 33.847389262   7.14 6.99     A2/3V 45 0
34 HD 203856 * 21 23 35.5297106889 +40 01 07.021382015   7.33 7.21     A0V 79 0
35 HD 205314 ** 21 32 56.5913653851 +49 58 39.470136422   5.721 5.755     A0V 65 0
36 BD+28 4211 HS* 21 51 11.0220905905 +28 51 50.366090892 8.922 10.25 10.58 10.656 10.831 sdO2VIIIHe5 751 0
37 BD+17 4708 SB* 22 11 31.3751899315 +18 05 34.158392398 9.73 9.91 9.46 9.03 8.70 sdF8 546 0
38 NAME Local Group GrG ~ ~           ~ 7298 0

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2021.06.23-04:37:00

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