Detection of TeV emission from the intriguing composite SNR G327.1-1.1

Details Detection of TeV emission from the intriguing composite SNR G327.1-1.1 Detection of TeV emission from the intriguing composite SNR G327.1-1.1

2012-01-02

arxiv.org/abs/1201.0481v1

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

Proceeding of the 32nd ICRC, August 11-18 2011, Beijing, China

Scientific paper

The shock wave of supernova remnants (SNRs) and the wind termination shock in pulsar wind nebula (PWNe) are considered as prime candidates to accelerate the bulk of Galactic cosmic ray (CR) ions and electrons. The SNRs hosting a PWN (known as composite SNRs) provide excellent laboratories to test these hypotheses. The SNR G327.1-1.1 belongs to this category and exhibits a shell and a bright central PWN, both seen in radio and X-rays. Interestingly, the radio observations of the PWN show an extended blob of emission and a curious narrow finger structure pointing towards the offset compact X-ray source indicating a possible fast moving pulsar in the SNR and/or an asymmetric passage of the reverse shock. We report here on the observations, for a total of 45 hours, of the SNR G327.1-1.1 with the H.E.S.S. telescope array which resulted in the detection of TeV gamma-ray emission in spatial coincidence with the PWN.

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