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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 1.

Integrated intensity map of the ATCA and Parkes H I (Kim et al. 2003, colored image) overlaid with the Mopra 12CO(J = 1–0) integrated intensity (black dashed contours), Chandra X-ray boundary of N132D (Borkowski et al. 2007, black solid contour), and the H.E.S.S. teraelectronvolt gamma-ray excess counts (H.E.S.S. Collaboration et al. 2015, white solid contours). The CO data have been spatially smoothed to match the FWHM of H I (∼﹩60^{\prime\prime} ﹩). The integration velocity ranges of CO and H I are from 240 to 290 km s−1, which cover 74% of the total integrated intensity of H I. The lowest contour level and intervals of CO are 6.3 K km s−1 (∼9σ) and 2.1 K km s−1 (∼3σ), respectively. The contour level of the X-ray boundary is ﹩0.3\times {10}^{-6}﹩ counts pixel−1 s−1. The contour levels of teraelectronvolt gamma rays are 10, 14, and 18 excess counts. The dashed white rectangles indicate the observed areas of CO. The FWHM beam size of CO/H I and the PSF of the teraelectronvolt gamma rays are also shown in the top right corner.

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