2014ApJ...795L...4K

Query : 2014ApJ...795L...4K

2014ApJ...795L...4K - Astrophys. J., 795, L4 (2014/November-1)

Optical and near-infrared polarimetry of highly reddened type Ia supernova 2014J: peculiar properties of dust in M82.

KAWABATA K.S., AKITAYA H., YAMANAKA M., ITOH R., MAEDA K., MORITANI Y., UI T., KAWABATA M., MORI K., NOGAMI D., NOMOTO K., SUZUKI N., TAKAKI K., TANAKA M., UENO I., CHIYONOBU S., HARAO T., MATSUI R., MIYAMOTO H., NAGAE O., NAKASHIMA A., NAKAYA H., OHASHI Y., OHSUGI T., KOMATSU T., SAKIMOTO K., SASADA M., SATO H., TANAKA H., URANO T., YAMASHITA T., YOSHIDA M., ARAI A., EBISUDA N., FUKAZAWA Y., FUKUI A., HASHIMOTO O., HONDA S., IZUMIURA H., KANDA Y., KAWAGUCHI K., KAWAI N., KURODA D., MASUMOTO K., MATSUMOTO K., NAKAOKA T., TAKATA K., UEMURA M. and YANAGISAWA K.

Abstract (from CDS):

We present optical and near-infrared multi-band linear polarimetry of the highly reddened Type Ia supernova (SN) 2014J that appeared in M82. SN 2014J exhibits large polarization at shorter wavelengths, e.g., 4.8% in the B band, which decreases rapidly at longer wavelengths, while the position angle of the polarization remains at approximately 40° over the observed wavelength range. These polarimetric properties suggest that the observed polarization is likely predominantly caused by the interstellar dust within M82. Further analysis shows that the polarization peaks at a wavelengths much shorter than those obtained for the Galactic dust. The wavelength dependence of the polarization can be better described by an inverse power law rather than by the Serkowski law for Galactic interstellar polarization. These points suggest that the nature of the dust in M82 may be different from that in our Galaxy, with polarizing dust grains having a mean radius of <0.1 µm.

Abstract Copyright: ∼

Journal keyword(s): circumstellar matter - dust, extinction - galaxies: individual: Messier 82 - polarization - supernovae: individual: SN 2014J

Simbad objects: 17

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Number of rows : 17
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 HD 283701 * 04 34 54.9740171088 +27 12 11.277228744   10.44 9.6     A5 29 0
2 HD 30168 * 04 46 12.0584752704 +26 02 07.768021776 8.000 8.010 7.700     B9/A0 38 0
3 MCG-05-18-002 Sy2 07 16 31.2062162520 -29 19 28.882826364   13.28 13.52 11.61   ~ 288 4
4 SN 2008fp SN* 07 16 32.60 -29 19 31.7           SNIa 79 1
5 BD+70 587 * 09 55 34.9430916672 +69 38 55.297587156   10.64 10.04 9.0   G5 15 0
6 SN 2014J SN* 09 55 42.12 +69 40 25.9           SNIa-norm 456 1
7 M 82 AGN 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 6156 6
8 HD 94851 * 10 56 44.2560073776 -20 39 52.617699576   9.47 9.29     A5V 44 0
9 HD 98281 PM* 11 18 22.0116141258 -05 04 02.288928836 8.278 7.993 7.232 6.822 6.438 G8V 184 0
10 SN 2006X SN* 12 22 53.93 +15 48 32.0     15.3     SNIa 347 1
11 M 100 AGN 12 22 54.9299993592 +15 49 20.296257960 10.04 10.05 9.35     ~ 1963 2
12 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
13 NAME Centaurus A BLL 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4774 3
14 SN 1986G SN* 13 25 36.46 -43 01 53.6   12.45 11.44     SNIapec 422 1
15 SN 2011fe SN* 14 03 05.711 +54 16 25.22   10.12 10.06     SNIa-norm 747 1
16 HD 150193 Ae* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   A3Va(e) 336 0
17 BD+41 3807 SB* 20 34 08.5147948176 +41 36 59.408503092 11.74 11.52 10.03     O5.5Ifc 137 0

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