2018ApJ...856..133R


Query : 2018ApJ...856..133R

2018ApJ...856..133R - Astrophys. J., 856, 133-133 (2018/April-1)

Expansion and brightness changes in the pulsar-wind nebula in the composite supernova remnant Kes 75.

REYNOLDS S.P., BORKOWSKI K.J. and GWYNNE P.H.

Abstract (from CDS):

We report new Chandra X-ray observations of the shell supernova remnant Kes 75 (G29.7-0.3) containing a pulsar and pulsar-wind nebula (PWN). Expansion of the PWN is apparent across four epochs-2000, 2006, 2009, and 2016. We find an expansion rate between 2000 and 2016 of the northwest edge of the PWN of 0.249% ± 0.023% yr–1, for an expansion age R/(dR/dt) of 400 ± 40 yr and an expansion velocity of about 1000 km s–1. We suggest that the PWN is expanding into an asymmetric nickel bubble in a conventional Type IIP supernova. Some acceleration of the PWN expansion is likely, giving a true age of 480 ± 50 yr. The pulsar's birth luminosity was larger than the current value by a factor of 3-8, while the initial period was within a factor of 2 of its current value. We confirm directly that Kes 75 contains the youngest known PWN, and hence the youngest known pulsar. The pulsar PSR J1846-0258 has a spindown-inferred magnetic field of 5 x 1013 G; in 2006, it emitted five magnetar-like short X-ray bursts, but its spindown luminosity has not changed significantly. However, the flux of the PWN has decreased by about 10% between 2009 and 2016, almost entirely in the northern half. A bright knot has declined by 30% since 2006. During this time, the photon indices of the power-law models did not change. This flux change is too rapid to be due to normal PWN evolution in one-zone models.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): ISM: individual objects: Kes 75 - ISM: supernova remnants - pulsars: individual: PSR J1846-0258 - 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 1139 1
2 SNR G130.7+03.1 SNR 02 05 37.0 +64 49 42           ~ 592 4
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16253 1
4 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5076 0
5 M 1 SNR 05 34 32 +22 00.8           ~ 5956 1
6 SNR B0540-69.7 SNR 05 40 -69.7           ~ 14 0
7 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 852 3
8 SN 1993J SN* 09 55 24.77476 +69 01 13.7026   10.8 12.0     SNIIb 1344 1
9 SN 2008ax SN* 12 30 40.80 +41 38 16.1   23.6 23.5 14.1 22.6 SNIIb 237 1
10 SN 2011dh SN* 13 30 05.10555 +47 10 10.9227           SNIIb 341 1
11 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1279 1
12 NAME Kepler SNR Rad 17 30 35.976 -21 28 56.23           ~ 760 4
13 SNR G001.9+00.3 SNR 17 48 46.10 -27 09 50.9           ~ 187 1
14 SNR G011.2-00.3 SNR 18 11 28.9 -19 25 29           ~ 270 1
15 4C -04.71 Rad 18 41 19.8 -04 56 06           ~ 314 3
16 PSR J1846-0258 Psr 18 46 24.94 -02 58 30.1           ~ 328 2
17 SNR G029.7-00.2 SNR 18 46 25.5 -02 59 14           ~ 321 2
18 SNR G054.1+00.3 SNR 19 30 31 +18 52.0           ~ 212 1
19 SN 2004et SN* 20 35 25.33 +60 07 17.7   12.88       SNIIP 453 1
20 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2630 1

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2022.09.28-09:00:26

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