A search for TeV gamma-ray emission from SNRs, pulsars and unidentified GeV sources in the Galactic plane in the longitude range between 2 and 85°

被引：44

作者：

Aharonian, FA

Akhperjanian, AG

Beilicke, M

Bernlöhr, K

Bojahr, H

Bolz, O

Börst, H

Coarasa, T

Contreras, JL

Cortina, J

Denninghoff, S

Fonseca, V

Girma, M

Götting, N

Heinzelmann, G

Hermann, G

Heusler, A

Hofmann, W

Horns, D

Jung, I

Kankanyan, R

Kestel, M

Kettler, J

Kohnle, A

Konopelko, A

Kornmeyer, H

Kranich, D

Krawczynski, H

Lampeitl, H

Lopez, M

Lorenz, E

Lucarelli, F

Mang, O

Meyer, H

Mirzoyan, R

Moralejo, A

Ona, E

Panter, M

Plyasheshnikov, A

Pühlhofer, G

Rauteberg, G

Reyes, R

Rhode, W

Ripken, J

Röhring, A

Rowell, GP

Sahakian, V

Samorski, M

Schilling, M

Siems, M

机构：

[1] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany

[2] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[3] Univ Complutense, Fac Ciencias Fis, E-28040 Madrid, Spain

[4] Univ Hamburg, Inst Phys Expt, D-22761 Hamburg, Germany

[5] Univ Kiel, Inst Expt & Angew Phys, D-24118 Kiel, Germany

[6] Univ Wuppertal, Fachbereich Phys, D-42097 Wuppertal, Germany

[7] Yerevan Phys Inst, Yerevan 375036, Armenia

来源：

ASTRONOMY & ASTROPHYSICS | 2002年 / 395卷 / 03期

关键词：

gamma rays : observations; ISM : cosmic rays; stars : pulsars : general; ISM : supernova remnants;

D O I：

10.1051/0004-6361:20021347

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using the HEGRA system of imaging atmospheric Cherenkov telescopes, one quarter of the Galactic plane (-2degrees < l < 85degrees) was surveyed for TeV gamma-ray emission from point sources and moderately extended sources (O less than or equal to 0.8degrees). The region covered includes 86 known pulsars (PSR), 63 known supernova remnants (SNR) and nine GeV sources, representing a significant fraction of the known populations. No evidence for emission of TeV gamma radiation was detected, and upper limits range from 0.15 Crab units up to several Crab units, depending on the observation time and zenith angles covered. The ensemble sums over selected SNR and pulsar subsamples and over the GeV-sources yield no indication of emission from these potential sources. The upper limit for the SNR population is 6.7% of the Crab flux and for the pulsar ensemble is 3.6% of the Crab flux.

引用

页码：803 / 811

页数：9

共 42 条

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