Figure 5 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 5.

RGB image of N132D obtained with the HST Hα (red), ALMA ¹²CO(J = 1–0) (green), and Chandra X-rays in the energy band 0.5–7.0 keV (blue). The integration velocity range is from 262.0 km s⁻¹ to 268.4 km s⁻¹. The contours represent the integrated intensity of CO, whose levels are 1.2 (﹩\sim 3\sigma ﹩), 1.5, 2.0, 3.0, 4.0, 6.0, 9.0, 13.0, 18.0, and 24.0 K km s⁻¹. The region enclosed by the dashed line indicates the area observed with ALMA. The CO clouds, named A to I, discussed in Section 4.3 are indicated.

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