Figure 10 from 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

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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 10.

RGB X-ray image toward the center of N132D. The red, green, and blue colors represent the energy bands 0.35–0.85 keV, 0.85–1.6 keV, and 1.6–6.0 keV, respectively. Superposed contours indicate boundaries of ALMA CO clouds B to I as shown in Figure 5, whose contour levels are 1.2 K km s⁻¹. Note that cloud A is located outside the field of view. The dashed line indicates the X-ray filament, discussed in Section 5.1.

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