Figure 6 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 6.

Intensity ratio map of ¹²CO(J = 3–2)/¹²CO(J = 1–0) using ASTE and ALMA. The ALMA data were smoothed to match the effective beam size of the ASTE data (an effective beam size of ﹩23^{\prime\prime} ﹩). The beam size and scale bar are also shown in the top right corner. The velocity range is the same as in Figure 5. White dashed contours represent the X-ray intensity, whose contour levels are the same as in Figure 2(b). The gray areas represent that the ¹²CO(J = 1–0) or ¹²(J = 3–2) data show a low significance of ∼8σ or lower.

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