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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 2.

(a) RGB X-ray image of N132D obtained with Chandra (e.g., Borkowski et al. 2007; Xiao & Chen 2008; Sharda et al. 2020). The red, green, and blue colors represent the energy bands 0.5–1.2 keV, 1.2–2.0 keV, and 2.0–7.0 keV, respectively. (b) Intensity map of 12CO(J = 3–2) obtained with ASTE overlaid with the Chandra X-ray contours. The integration velocity range is from 256.8 km s−1 to 271.2 km s−1. The black contours represent the X-ray intensities: 0.3, 0.6, 1.8, 3.6, 7.2, and ﹩14.4\times {10}^{-6}﹩ counts pixel−1 s−1. (c) Intensity map of H I obtained with ATCA and Parkes (Kim et al. 2003) overlaid with the Chandra X-ray contours. The integration velocity range and contour levels are the same as in Figure 2(b). The beam size and scale bar are also shown.

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