Chinese Physics C > 2014, Vol. 38 > Issue(8): 085001 DOI: 10.1088/1674-1137/38/8/085001

Multi-wavelength study of MGRO J2019+37

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Abstract：
MGRO J2019+37, within the Cygnus region, is a bright extended source revealed by Milagro at 12-35 TeV. This source is almost as bright as the Crab Nebula in the northern sky, but is not confirmed by ARGO-YBJ around the TeV scale. Up to now, no obvious counterpart at low energy wavelengths has been found. Hence, MGRO J2019+37 is a rather mysterious object and its VHEγ-ray emission mechanism is worth investigating. In this paper, a brief summary of the multi-wavelength observations from radio to γ-rays is presented. All the available data from XMM-Newton and INTEGRAL at X-ray, and Fermi-LAT atγ-ray bands, are used to get constraints on its emission flux at low energy wavelengths. Then, its possible counterparts and the VHE emission mechanism are discussed.

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HOU Chao, CHEN Song-Zhan, YUAN Qiang, CAO Zhen, HE Hui-Hai and SHENG Xiang-Dong. Multi-wavelength study of MGRO J2019+37[J]. Chinese Physics C, 2014, 38(8): 085001. doi: 10.1088/1674-1137/38/8/085001

HOU Chao, CHEN Song-Zhan, YUAN Qiang, CAO Zhen, HE Hui-Hai and SHENG Xiang-Dong. Multi-wavelength study of MGRO J2019+37[J]. Chinese Physics C, 2014, 38(8): 085001. doi:10.1088/1674-1137/38/8/085001 shu

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Received: 2014-03-11
Revised: 1900-01-01

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沈阳化工大学材料科学与工程学院沈阳 110142

Multi-wavelength study of MGRO J2019+37

Corresponding author:HOU Chao,

Received Date:2014-03-11
Accepted Date:1900-01-01
Available Online:2014-08-05

Abstract:MGRO J2019+37, within the Cygnus region, is a bright extended source revealed by Milagro at 12-35 TeV. This source is almost as bright as the Crab Nebula in the northern sky, but is not confirmed by ARGO-YBJ around the TeV scale. Up to now, no obvious counterpart at low energy wavelengths has been found. Hence, MGRO J2019+37 is a rather mysterious object and its VHEγ-ray emission mechanism is worth investigating. In this paper, a brief summary of the multi-wavelength observations from radio to γ-rays is presented. All the available data from XMM-Newton and INTEGRAL at X-ray, and Fermi-LAT atγ-ray bands, are used to get constraints on its emission flux at low energy wavelengths. Then, its possible counterparts and the VHE emission mechanism are discussed.