2016ApJ...819..160B


Query : 2016ApJ...819..160B

2016ApJ...819..160B - Astrophys. J., 819, 160 (2016/March-2)

G11.2-0.3: the young remnant of a stripped-envelope supernova.

BORKOWSKI K.J., REYNOLDS S.P. and ROBERTS M.S.E.

Abstract (from CDS):

We present results of a 400 ks Chandra observation of the young shell supernova remnant (SNR) G11.2-0.3, containing a pulsar and pulsar-wind nebula (PWN). We measure a mean expansion rate for the shell since 2000 of 0.0277±0.0018%/yr, implying an age between 1400 and 2400 yr, and making G11.2-0.3 one of the youngest core-collapse SNRs in the Galaxy. However, we find very high absorption (AV∼ 16m±2m), confirming near-IR determinations and ruling out a claimed association with the possible historical SN of 386 CE. The PWN shows strong jets and a faint torus within a larger, more diffuse region of radio emission and nonthermal X-rays. Central soft thermal X-ray emission is anticorrelated with the PWN; that, and more detailed morphological evidence, indicates that the reverse shock has already reheated all ejecta and compressed the PWN. The pulsar characteristic energy-loss timescale is well in excess of the remnant age, and we suggest that the bright jets have been produced since the recompression. The relatively pronounced shell and diffuse hard X-ray emission in the interior, enhanced at the inner edge of the shell, indicate that the immediate circumstellar medium into which G11.2-0.3 is expanding was quite anisotropic. We propose a possible origin for G11.2-0.3 in a stripped-envelope progenitor that had lost almost all its envelope mass, in an anisotropic wind or due to binary interaction, leaving a compact core whose fast winds swept previously lost mass into a dense irregular shell, and which exploded as a SN cIIb or Ibc.

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Journal keyword(s): ISM: individual: G11.20.3 - ISM: supernova remnants - X-rays: ISM

Simbad objects: 20

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Number of rows : 20
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 1572A SN* 00 25 21.5 +64 08 27           B8 1140 1
2 3C 48 QSO 01 37 41.2996631208 +33 09 35.080388820   16.62 16.20     ~ 2698 2
3 WOH G 64 Mi* 04 55 10.5236094912 -68 20 30.019011036     18.46 15.69 12.795 M7.5 88 0
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16284 1
5 M 1 SNR 05 34 32 +22 00.8           ~ 5957 1
6 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4741 2
7 NAME Vela Jr SN SNR 08 52.0 -46 20           ~ 450 2
8 SN 2008ax SN* 12 30 40.80 +41 38 16.1   23.6 23.5 14.1 22.6 SNIIb 238 1
9 SN 2011dh SN* 13 30 05.10555 +47 10 10.9227           SNIIb 343 1
10 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4121 2
11 ESO 134-11 HII 14 40 29 -62 38.7           ~ 545 1
12 SNR G315.0-02.3 SNR 14 43 00 -62 30.0           ~ 358 1
13 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1279 1
14 SNR G347.3-00.5 SNR 17 12 27 -39 41.2     12.27     ~ 686 1
15 NAME Kepler SNR Rad 17 30 35.976 -21 28 56.23           ~ 762 4
16 SNR G001.9+00.3 SNR 17 48 46.10 -27 09 50.9           ~ 187 1
17 SNR G011.2-00.3 SNR 18 11 28.9 -19 25 29           ~ 270 1
18 SNR G011.2-01.1 SNR 18 14.0 -19 46           ~ 63 1
19 SNR G029.7-00.2 SNR 18 46 25.5 -02 59 14           ~ 322 2
20 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2633 1

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2022.10.06-20:51:32

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