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<supportEmail caption="Support">icrc2007@icrc2007.unam.mx</supportEmail>
<title>30th International Cosmic Ray Conference</title>
<description>The 30th International Cosmic Ray Conference will be held from July 3, 2007 to July 11, 2007 in Merida, Yucatan, Mexico.</description>
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<closed>True</closed>
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 <name>Merida, Mexico</name>
 <address></address>
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<startDate>2007-07-03T08:00:00</startDate>
<endDate>2007-07-11T19:00:00</endDate>
<creationDate>2005-09-26T05:04:53</creationDate>
<modificationDate>2024-04-12T17:46:55</modificationDate>
<timezone>Mexico/General</timezone>
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 <track>OG.2.2</track>
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 <title>Observations of extended VHE gamma-ray emission from MSH 15-52 with CANGAROO-III</title>
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   <organization>Australian National University</organization>
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   <name first="Takanori" middle="" last="Yoshikoshi"></name>
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   <organization>Konan University</organization>
   <emailHash>d41d8cd98f00b204e9800998ecf8427e</emailHash>
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 </coAuthors>
 <location>
  <name>Merida, Mexico</name>
  <address></address>
  <room>Uxmal + Tulum (Holiday Inn)</room>
 </location>
 <startDate>2007-07-04T12:41:00</startDate>
 <endDate>2007-07-04T12:53:00</endDate>
 <duration>00:12</duration>
 <abstract>The gamma-ray pulsar PSR B1509-58, surrounded by the supernova remnant 
MSH15-
52, was expected to be a Very High Energy gamma-ray source. CANGAROO-I 3.8
m telescope reported a marginal detection of VHE gamma-rays above 1.9 TeV 
and
recently H.E.S.S. detected an extended signal along with the pulsar jets, from
sub-TeV to tens of TeV.

 We observed MSH15-52 using CANGAROO-III imaging atmospheric Cherenkov
telescope array located in South Australia, from April to June in 2006. We
also detected gamma-rays above 860GeV with more than 5 sigma level during 
an
effective exposure of 48.4 hours. Obtained differential flux of VHE gamma-ray
is consistent with that of H.E.S.S., and its morphology shows an extended
emission compared to our PSF.</abstract>
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