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ALMA CO Observations of Gamma-Ray Supernova Remnant N132D in the Large Magellanic Cloud: Possible Evidence for Shocked Molecular Clouds Illuminated by Cosmic-Ray Protons

  • Authors: H. Sano, P. P. Plucinsky, A. Bamba, P. Sharda, M. D. Filipović, C. J. Law, R. Z. E. Alsaberi, Y. Yamane, K. Tokuda, F. Acero, M. Sasaki, J. Vink, T. Inoue, S. Inutsuka, J. Shimoda, K. Tsuge, K. Fujii, F. Voisin, N. Maxted, G. Rowell, T. Onishi, A. Kawamura, N. Mizuno, H. Yamamoto, K. Tachihara, and Y. Fukui

2020 The Astrophysical Journal 902 53.

  • Provider: AAS Journals

Caption: Figure 3.

Position–velocity diagram of H I. Superposed white solid contours indicate 12CO(J = 3–2) intensity. The integration range in R.A. is from ﹩{05}^{{\rm{h}}}{24}^{{\rm{m}}}{57}^{{\rm{s}}}﹩ to ﹩{05}^{{\rm{h}}}{25}^{{\rm{m}}}{09}^{{\rm{s}}}﹩. The lowest contour and contour intervals of CO are 0.003 K degree and 0.005 K degree, respectively. The dashed white line delineates an H I cavity with the H I intensity of 0.3 K degree. The beam size and velocity resolution are also shown in the bottom right corner. Horizontal dashed lines represent observed boundaries of CO.

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