FERMI LARGE AREA TELESCOPE DISCOVERY OF GeV GAMMA-RAY EMISSION FROM THE VICINITY OF SNR W44
FERMI LARGE AREA TELESCOPE DISCOVERY OF GeV GAMMA-RAY EMISSION FROM THE VICINITY OF SNR W44
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DOI：
10.1088/2041-8205/749/2/l35
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发表时间：
2012-03
期刊：
影响因子：
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通讯作者：
Y. Uchiyama;S. Funk;H. Katagiri;J. Katsuta;M. Lemoine-Goumard;H. Tajima;Takaaki Tanaka;D. Torres
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文献类型：
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作者：
Y. Uchiyama;S. Funk;H. Katagiri;J. Katsuta;M. Lemoine-Goumard;H. Tajima;Takaaki Tanaka;D. Torres
我们报道了费米星上的大口径望远镜对超新星遗迹W 44周围分子云复合体的GeV γ射线辐射的探测。虽然先前报告的SNR W 44的γ射线发射可能来自残骸内密集的无线电发射细丝，但似乎来自周围分子云复合体的γ射线发射可以归因于从W 44逃逸的宇宙射线（CR）。没有探测到与分子云复合体相关的同步辐射，这表明强子碰撞中产生的π0介子衰变是γ射线发射机制。逃逸的CRs的总动能估计为Wesc（0.3-3）× 1050 erg，这与SNRs是银河系CRs主要来源的猜想大致一致。
We report the detection of GeV γ-ray emission from the molecular cloud complex that surrounds the supernova remnant (SNR) W44 using the Large Area Telescope on board Fermi. While the previously reported γ-ray emission from SNR W44 is likely to arise from the dense radio-emitting filaments within the remnant, the γ-ray emission that appears to come from the surrounding molecular cloud complex can be ascribed to the cosmic rays (CRs) that have escaped from W44. The non-detection of synchrotron radio emission associated with the molecular cloud complex suggests the decay of π0 mesons produced in hadronic collisions as the γ-ray emission mechanism. The total kinetic energy channeled into the escaping CRs is estimated to be Wesc ∼ (0.3–3) × 1050 erg, in broad agreement with the conjecture that SNRs are the main sources of Galactic CRs.