REANALYSIS OF DATA TAKEN BY THE CANGAROO 3.8 METER IMAGING ATMOSPHERIC CHERENKOV TELESCOPE: PSR B1706-44, SN 1006, AND VELA

被引：3

作者：

Yoshikoshi, T. ^{[1
]}

Mori, M. ^{[1
]}

Edwards, P. G. ^{[2
]}

Gunji, S. ^{[3
]}

Hara, S. ^{[4
]}

Hara, T. ^{[5
]}

Kawachi, A. ^{[6
]}

Mizumoto, Y. ^{[7
]}

Naito, T. ^{[5
]}

Nishijima, K. ^{[6
]}

Tanimori, T. ^{[8
]}

Thornton, G. J. ^{[9
]}

Yoshida, T. ^{[10
]}

机构：

[1] Univ Tokyo, Inst Cosm Ray Res, Chiba 2778582, Japan

[2] CSIRO, Australia Telescope Natl Facil, Narrabri Observ, Narrabri, NSW 2390, Australia

[3] Yamagata Univ, Dept Phys, Yamagata 9908560, Japan

[4] Ibaraki Prefectural Univ Hlth Sci, Ami, Ibaraki 3000394, Japan

[5] Yamanashi Gakuin Univ, Fac Management Informat, Yamanashi 4008575, Japan

[6] Tokai Univ, Dept Phys, Kanagawa 2591292, Japan

[7] Natl Astron Observ Japan, Tokyo 1818588, Japan

[8] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan

[9] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

[10] Ibaraki Univ, Fac Sci, Mito, Ibaraki 3108512, Japan

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 702卷 / 01期

关键词：

gamma rays: observations; methods: data analysis; pulsars: individual (PSR B1706-44; Vela pulsar); supernova remnants; supernovae: individual (SN 1006); TEV GAMMA-RAYS; CRAB-NEBULA; PULSAR; HESS; SEARCH; AUSTRALIA; DISCOVERY; ASTRONOMY; EMISSION; PLERIONS;

D O I：

10.1088/0004-637X/702/1/631

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have reanalyzed data from observations of PSR B1706-44, SN 1006, and the Vela pulsar region made with the CANGAROO 3.8 m Imaging Atmospheric Cherenkov Telescope between 1993 and 1998 in response to the results reported for these sources by the H. E. S. S. Collaboration. Although detections of TeV gamma-ray emission from these sources were claimed by CANGAROO more than 10 years ago, upper limits to the TeV gamma-ray signals from PSR B1706-44 and SN 1006 derived by H. E. S. S. are about an order of magnitude lower. The H. E. S. S. group detected strong diffuse TeV gamma-ray emission from Vela but with a morphology differing from the CANGAROO result. In our reanalysis, in which gamma-ray selection criteria have been determined exclusively using gamma-ray simulations and off-source data as background samples, no significant TeV gamma-ray signals have been detected from compact regions around PSR B1706-44 or within the northeast rim of SN 1006. The upper limits to the integral gamma-ray fluxes at the 95% confidence level have been estimated for the 1993 data of PSR B1706-44 to be F(> 3.2 +/- 1.6 TeV) < 8.03 x 10(-13) photons cm(-2) s(-1), for the 1996 and 1997 data of SN 1006 to be F(> 3.0 +/- 1.5 TeV) < 1.20 x 10(-12) photons cm(-2) s(-1) and F(> 1.8 +/- 0.9 TeV) < 1.96 x 10(-12) photons cm(-2) s(-1), respectively. We discuss reasons why the original analyses gave the source detections. The reanalysis did result in a TeV gamma-ray signal from the Vela pulsar region at the 4.5 sigma level using 1993, 1994, and 1995 data. The excess was located at the same position, 0 degrees.13 to the southeast of the Vela pulsar, as that reported in the original analysis. We have investigated the effect of the acceptance distribution in the field of view of the 3.8 m telescope, which rapidly decreases toward the edge of the field of the camera, on the detected gamma-ray morphology. The expected excess distribution for the 3.8 m telescope has been obtained by reweighting the distribution of HESS J0835-455 measured by H. E. S. S. with the acceptance of the 3.8 m telescope. The result is morphologically comparable to the CANGAROO excess distribution, although the profile of the acceptance-reweighted H. E. S. S. distribution is more diffuse than that of CANGAROO. The integral gamma-ray flux from HESS J0835-455 has been estimated for the same region as defined by H. E. S. S. from the 1993-1995 data of CANGAROO to be F(> 4.0 +/- 1.6 TeV) = ( 3.28 +/- 0.92) x 10(-12) photons cm(-2) s(-1), which is statistically consistent with the integral flux obtained by H. E. S.

引用

页码：631 / 648

页数：18