2000A&A...359..337R


Query : 2000A&A...359..337R

2000A&A...359..337R - Astronomy and Astrophysics, volume 359, 337-346 (2000/7-1)

Observations of the supernova remnant W28 at TeV energies.

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

Abstract (from CDS):

The atmospheric Cerenkov imaging technique has been used to search for point-like and diffuse TeV gamma-ray emission from the southern supernova remnant, W28, and surrounding region. The search, made with the CANGAROO 3.8m telescope, encompasses a number of interesting features, the supernova remnant itself, the EGRET source 3EG J1800-2338, the pulsar PSR J1801-23, strong 1720MHz OH masers and molecular clouds on the north and east boundaries of the remnant. An analysis tailored to extended and off-axis point sources was used, and no evidence for TeV gamma-ray emission from any of the features described above was found in data taken over the 1994 and 1995 seasons. Our upper limit (E>1.5TeV) for a diffuse source of radius 0.25° encompassing both molecular clouds was calculated at 6.64x10–12cm–2.s–1 (from 1994 data), and interpreted within the framework of a model predicting TeV gamma-rays from shocked-accelerated hadrons. Our upper limit suggests the need for some cutoff in the parent spectrum of accelerated hadrons and/or slightly steeper parent spectra than that used here (-2.1). As to the nature of 3EG J1800-2338, it possibly does not result entirely from π° decay, a conclusion also consistent with its location in relation to W28.

Abstract Copyright:

Journal keyword(s): ISM: supernova remnants - ISM: individual objects: W28 - gamma rays: observations

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 - 2022
#notes
1 SN 1572A SN* 00 25 21.5 +64 08 27           B8 1124 1
2 IC 443 SNR 06 18 02.7 +22 39 36     10.11     ~ 1165 1
3 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2185 1
4 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1260 1
5 SNR G347.3-00.5 SNR 17 12 27 -39 41.2     12.27     ~ 669 1
6 [CFG97b] W28 OH A Mas 18 00 49.924 -23 20 26.66           ~ 5 0
7 GRS G006.60 -00.10 Rad 18 00 50.4 -23 20 39           ~ 7 0
8 [CFG97b] W28 OH B Mas 18 01 -23.3           ~ 4 0
9 [CFG97b] W28 OH E Mas 18 01 -23.3           ~ 5 0
10 PSR B1758-23 Psr 18 01 19.829 -23 04 44.20           ~ 133 0
11 SNR G006.4-00.1 SNR 18 01 22.7 -23 17 20           ~ 693 1
12 [CFG97b] W28 OH C Mas 18 01 44.041 -23 24 23.05           ~ 5 0
13 [CFG97b] W28 OH F Mas 18 01 50.002 -23 18 46.58           ~ 7 0
14 [CFG97b] W28 OH D Mas 18 11 41.444 -23 25 05.26           ~ 5 0
15 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 891 2
16 W 51 SNR 19 23 50 +14 06.0           ~ 1209 1
17 NAME gam Cyg SNR SNR 20 20 17.100 +40 26 09.00           ~ 210 2

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2022.05.24-07:31:32

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