2010ApJ...721.1492P


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.29CET21:19:04

2010ApJ...721.1492P - Astrophys. J., 721, 1492-1508 (2010/October-1)

Non-thermal X-ray emission from the northwestern rim of the galactic supernova remnant G266.2-1.2 (RX J0852.0-4622).

PANNUTI T.G., ALLEN G.E., FILIPOVIC M.D., DE HORTA A., STUPAR M. and AGRAWAL R.

Abstract (from CDS):

We present a detailed spatially resolved spectroscopic analysis of two observations (with a total integration time of 73280 s) made of the X-ray-luminous northwestern rim complex of the Galactic supernova remnant (SNR) G266.2-1.2 (RX J0852.0-4622) with the Chandra X-ray Observatory. G266.2-1.2 is a member of a class of Galactic SNRs which feature X-ray spectra dominated by non-thermal emission: in the cases of these SNRs, the emission is believed to have a synchrotron origin and studies of the X-ray spectra of these SNRs can lend insight into how SNRs accelerate cosmic-ray particles. The Chandra observations have clearly revealed fine structure in this rim complex (including a remarkably well-defined leading shock) and the spectra of these features are dominated by non-thermal emission. We have measured the length scales of the upstream structures at eight positions along the rim and derive lengths of 0.02-0.08 pc (assuming a distance of 750 pc to G266.2-1.2). We have also extracted spectra from seven regions in the rim complex (as sampled by the ACIS-S2, -S3, and -S4 chips) and fit these spectra with such models as a simple power law as well as the synchrotron models SRCUT and SRESC. We have constrained our fits to the latter two models using estimates for the flux densities of these filaments at 1 GHz as determined from radio observations of this rim complex made with the Australia Telescope Compact Array. Statistically acceptable fits to all seven regions are derived using each model: differences in the fit parameters (such as photon index and cutoff frequency) are seen in different regions, which may indicate variations in shock conditions and the maximum energies of the cosmic-ray electrons accelerated at each region. Finally, we estimate the maximum energy of cosmic-ray electrons accelerated along this rim complex to be approximately 40 TeV (corresponding to one of the regions of the leading shock structure assuming a magnetic field strength of 10 µG). We include a summary of estimated maximum energies for both Galactic SNRs as well as SNRs located in the Large Magellanic Cloud. Like these other SNRs, it does not appear that G266.2-1.2 is currently accelerating electrons to the knee energy (∼3000 TeV) of the cosmic-ray spectrum. This result is not surprising, as there is some evidence that loss mechanisms which are not important for the accelerated cosmic-ray nucleons at energies just below the knee might cut off electron acceleration.

Abstract Copyright:

Journal keyword(s): acceleration of particles - cosmic rays - ISM: supernova remnants - X-rays: individual: G266.2-1.2

Simbad objects: 43

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Number of rows : 43

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SN 1572A SN* 00 25 21.5 +64 08 27           B8 1082 1
2 LHA 120-N 2 G 04 43 20.4 -67 56 25           ~ 4 0
3 SNR G156.2+05.7 SNR 04 58 51.300 +51 50 28.00           ~ 112 1
4 SNR B0505-67.9 SNR 05 05 42.0 -67 52 29           ~ 126 0
5 SNR J050555-680150 SNR 05 05 55.00 -68 01 54.0           ~ 80 0
6 LHA 120-N 103B EmO 05 08 47.8 -68 45 39           ~ 183 1
7 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14998 1
8 SNR J052501-693842 SNR 05 25 02.20 -69 38 39.0           ~ 351 1
9 SNR B0525-66.0 SNR 05 25 27.1 -65 59 11           ~ 92 1
10 SNR B0535-66.0 SNR 05 35 43.1 -66 01 59           ~ 159 1
11 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1124 2
12 NAME Vela Jr SN SNR 08 52.0 -46 20           ~ 408 2
13 2XMM J085201.4-461753 X 08 52 01.4 -46 17 53           ~ 40 1
14 NAME VELA MOL RIDGE MoC 08 53 -45.0           ~ 134 0
15 NAME Vela Z Rad 08 53 30 -45 35.0           ~ 29 0
16 PSR J0855-4644 Psr 08 55 36.18 -46 44 13.4           ~ 35 1
17 RCW 38 SFR 08 59 05.50 -47 30 39.4           ~ 270 2
18 CTB 31 SNR 08 59 07 -47 31.4           ~ 13 0
19 NGC 2736 HII 09 00.2 -45 57           ~ 18 0
20 ESO 134-11 HII 14 40 29 -62 38.7           ~ 508 1
21 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1219 1
22 SNR G330.2+01.0 SNR 16 01.1 -51 34           ~ 65 1
23 PKS 1613-50 Rad 16 17 33.000 -51 02 00.00           ~ 459 3
24 SNR G346.6-00.2 SNR 17 10.3 -40 11           ~ 80 0
25 SNR G347.3-00.5 SNR 17 12 27 -39 41.2           ~ 619 1
26 SNR G348.7+00.3 SNR 17 13 43.0 -38 10 12           ~ 109 2
27 SNR G349.7+00.2 SNR 17 18 10.160 -37 18 53.80           ~ 169 0
28 SNR G352.7-00.1 Rad 17 27 43 -35 06.5           ~ 61 1
29 NAME Kepler SNR Rad 17 30 35.976 -21 28 56.23           ~ 717 4
30 SNR G001.9+00.3 SNR 17 48 46.10 -27 09 50.9           ~ 167 1
31 SNR G011.0+00.0 SNR 18 10.1 -19 25           ~ 25 1
32 SNR G011.2-00.3 SNR 18 11 28.9 -19 25 29           ~ 252 1
33 SNR G011.2-01.1 SNR 18 14.0 -19 46           ~ 59 1
34 PSR J1838-0655 Psr 18 38 03.13 -06 55 33.4           ~ 81 1
35 SNR G026.6-00.1 SR? 18 40 -05.7           ~ 14 0
36 4C -04.71 Rad 18 41 19.8 -04 56 06           ~ 300 3
37 SNR G028.6-00.1 Rad 18 43 55 -03 53.0           ~ 45 1
38 3C 391.0 Rad 18 49 23.3 -00 55 38           ~ 320 2
39 SNR G032.5+00.1 SNR 18 50 05.000 -00 25 00.00           ~ 36 1
40 SNR G039.2-00.3 SNR 19 04 04.50 +05 27 12.0           ~ 172 1
41 3C 397 SNR 19 07 33.20 +07 08 32.0           ~ 192 2
42 W 49b SNR 19 11 09.000 +09 06 24.00           ~ 398 1
43 NAME Cas A SNR 23 23 24.000 +58 48 54.00           ~ 2441 1

    Equat.    Gal    SGal    Ecl

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2020.10.29-21:19:04

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