2009A&A...508..229P


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET22:23:55

2009A&A...508..229P - Astronomy and Astrophysics, volume 508, 229-246 (2009/12-2)

VLT spectropolarimetry of the fast expanding type Ia SN 2006X.

PATAT F., BAADE D., HOEFLICH P., MAUND J.R., WANG L. and WHEELER J.C.

Abstract (from CDS):

The main goal of this study is to probe the ejecta geometry and to get otherwise unobtainable information about the explosion mechanism of type Ia Supernovae (SNe). Using VLT-FORS1 we performed optical spectropolarimetric observations of the type Ia SN 2006X on 7 pre-maximum epochs (day -10 to day -1) and one post-maximum epoch (+39 days). The SN shows strong continuum interstellar polarization reaching about 8% at 4000Å, characterized by a wavelength dependency that is substantially different from that of the Milky-Way dust mixture. Several SN features, like SiII 6355Å and the CaII IR triplet, present a marked evolution. The CaII near-IR triplet shows a pronounced polarization (∼1.4%) already on day -10 in correspondence with a strong high-velocity feature (HVF). The SiII polarization peaks on day -6 at about 1.1% and decreases to 0.8% on day -1. By day +39 no polarization signal is detected for the SiII line, while the CaII IR triplet shows a marked re-polarization at the level of 1.2%. As in the case of another strongly polarized SN (2004dt), no polarization was detected across the OI 7774Å absorption. The fast-expanding SN 2006X lies on the upper edge of the relation between peak polarization and decline rate, and it confirms previous speculations about a correlation between degree of polarization, expansion velocity, and HVF strength. The polarization of CaII detected in our last epoch, the most advanced ever obtained for a type Ia SN, coincides in velocity with the outer boundary of the Ca synthesized during the explosion (15000-17000km/s) in delayed-detonation models. This suggests a large scale chemical inhomogeneity as produced by off-center detonations, a rather small amount of mixing, or a combination of both effects. In contrast, the absence of polarization at the inner edge of the Ca-rich layer (8000-10000km/s) implies a substantial amount of mixing in these deeper regions.

Abstract Copyright:

Journal keyword(s): stars: supernovae: general - stars: supernovae: individual: 2006X - ISM: general - dust, extinction

Simbad objects: 14

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Number of rows : 14

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 NGC 300 GiG 00 54 53.4460065856 -37 41 03.182962667 8.83 8.69 8.13 7.46   ~ 1338 2
2 SN 2004dt SN* 02 02 12.342 -00 06 02.10   15.33       SNIa 125 1
3 SN 2001el SN* 03 44 30.60 -44 38 23.4   12.81       SNIa 242 1
4 SN 1999by SN* 09 21 52.07 +51 00 06.6   13.66       SNIap 261 1
5 SN 2002bo SN* 10 18 06.51 +21 49 41.7   13.95       SNIa 280 1
6 SN 2006X SN* 12 22 53.93 +15 48 32.0     15.3     SNIa 284 1
7 M 100 AGN 12 22 54.9318850854 +15 49 20.294302163 10.04 10.05 9.35     ~ 1673 2
8 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5929 0
9 SN 1984A SN* 12 26 55.73 +15 03 17.1   12.40 12.20     SNIa 131 1
10 SN 1994D SN* 12 34 02.395 +07 42 05.70   11.75 12.03     SNIa 520 1
11 SN 2002dj SN* 13 13 00.34 -19 31 08.7     17.0     SNIa 103 1
12 SN 2003du SN* 14 34 35.80 +59 20 03.8   13.46       SNIa 317 1
13 SN 2004du SN* 21 08 26.51 +18 11 23.7     18.4     SNIIP 19 1
14 SN 2005cg SN* 21 10 50.44 +00 12 06.8     18.2     SNIa 32 1

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2020.11.28-22:23:55

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