Very high energy gamma rays from the Vela pulsar direction

被引：70

作者：

Yoshikoshi, T

Kifune, T

Dazeley, SA

Edwards, PG

Hara, T

Hayami, Y

Kakimoto, F

Konishi, T

Masaike, A

Matsubara, Y

Matsuoka, T

Mizumoto, Y

Mori, M

Muraishi, H

Muraki, Y

Naito, T

Nishijima, K

Oda, S

Ogio, S

Ohsaki, T

Patterson, JR

Roberts, MD

Rowell, GP

Sako, T

Sakurazawa, K

Susukita, R

Suzuki, A

Tamura, T

Tanimori, T

Thornton, GJ

Yanagita, S

Yoshida, T

机构：

[1] UNIV TOKYO,INST COSM RAY RES,TANASHI,TOKYO 188,JAPAN

[2] UNIV ADELAIDE,DEPT PHYS & MATH PHYS,ADELAIDE,SA 5005,AUSTRALIA

[3] INST SPACE & ASTRONAUT SCI,SAGAMIHARA,KANAGAWA 229,JAPAN

[4] YAMANASHI GAKUIN UNIV,FAC MANAGEMENT INFORMAT,KOFU,YAMANASHI 400,JAPAN

[5] KOBE UNIV,DEPT PHYS,KOBE,HYOGO 637,JAPAN

[6] KYOTO UNIV,DEPT PHYS,KYOTO 606,JAPAN

[7] NATL ASTRON OBSERV,MITAKA,TOKYO 181,JAPAN

[8] MIYAGI UNIV EDUC,DEPT PHYS,SENDAI,MIYAGI 980,JAPAN

[9] IBARAKI UNIV,FAC SCI,MITO,IBARAKI 310,JAPAN

[10] UNIV TOKYO,DEPT EARTH & PLANETARY PHYS,TOKYO 113,JAPAN

[11] TOKAI UNIV,DEPT PHYS,HIRATSUKA,KANAGAWA 259,JAPAN

[12] INST PHYS & CHEM RES,WAKO,SAITAMA 35101,JAPAN

[13] KANAGAWA UNIV,FAC ENGN,YOKOHAMA,KANAGAWA 221,JAPAN

来源：

ASTROPHYSICAL JOURNAL | 1997年 / 487卷 / 01期

基金：

澳大利亚研究理事会;

关键词：

gamma rays; observations; ISM; individual (Vela supernova remnant); magnetic fields; pulsars; individual (Vela pulsar); supernova remnants;

D O I：

10.1086/310874

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cerenkov telescope near Woomera, South Australia between 1993 January and 1995 March. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 sigma level. The detected gamma-ray flux is (2.9 +/- 0.5 +/- 0.4) x 10(-12) photons cm(-2) s(-1) above 2.5 +/- 1.0 TeV, and the signal is consistent with steady emission over the 2 years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0 degrees.13. No pulsed emission modulated with the pulsar period has been detected, and the 95% confidence flux upper limit to the pulse demission from the pulsar is (3.7 +/- 0.7) x 10(-13) photons cm(-2) s(-1) above 2.5 +/- 1.0 TeV.

引用

页码：L65 / L68

页数：4

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