2000A&A...354L..57M


Query : 2000A&A...354L..57M

2000A&A...354L..57M - Astronomy and Astrophysics, volume 354, L57-61 (2000/2-1)

Evidence for TeV gamma-ray emission from the shell type SNR RXJ1713.7-3946.

MURAISHI H., TANIMORI T., YANAGITA S., YOSHIDA T., MORIYA M., KIFUNE T., DAZELEY S.A., EDWARDS P.G., GUNJI S., HARA S., HARA T., KAWACHI A., KUBO H., MATSUBARA Y., MIZUMOTO Y., MORI M., MURAKI Y., NAITO T., NISHIJIMA K., PATTERSON J.R., ROWELL G.P., SAKO T., SAKURAZAWA K., SUSUKITA R., TAMURA T. and YOSHIKOSHI T.

Abstract (from CDS):

We report the results of TeV gamma-ray observations of the shell type SNR RX J1713.7-3946 (G347.3-0.5). The discovery of strong non-thermal X-ray emission from the northwest part of the remnant strongly suggests the existence of electrons with energies up to ∼100TeV in the remnant, making the SNR a good candidate TeV gamma-ray source. We observed RX J1713.7-3946 from May to August 1998 with the CANGAROO 3.8m atmospheric imaging Cerenkov telescope and obtained evidence for TeV gamma-ray emission from the NW rim of the remnant with the significance of ∼5.6σ. The observed TeV gamma-ray flux from the NW rim region was estimated to be (5.3±0.9[statistical]±1.6[systematic])x10–12photons/cm2/s at energies ≥1.8±0.9TeV. The data indicate that the emitting region is much broader than the point spread function of our telescope. The extent of the emission is consistent with that of hard X-rays observed by ASCA. This TeV gamma-ray emission can be attributed to the Inverse Compton scattering of the Cosmic Microwave Background Radiation by shock accelerated ultra-relativistic electrons. Under this assumption, a rather low magnetic field of ∼11µG is deduced for the remnant from our observation.

Abstract Copyright:

Journal keyword(s): stars: supernovae: individual: RX J1713.7-3946 - gamma rays: observations

Simbad objects: 3

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Number of rows : 3
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 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1260 1
2 PSR B1706-44 Psr 17 09 42.7460 -44 29 07.200     13.30     ~ 605 1
3 SNR G347.3-00.5 SNR 17 12 27 -39 41.2     12.27     ~ 669 1

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2022.05.24-07:12:39

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