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ALMA Observations of Supernova Remnant N49 in the Large Magellanic Cloud. II. Non-LTE Analysis of Shock-heated Molecular Clouds

  • Authors: H. Sano, Y. Yamane, J. Th. van Loon, K. Furuya, Y. Fukui, R. Z. E. Alsaberi, A. Bamba, R. Enokiya, M. D. Filipović, R. Indebetouw, T. Inoue, A. Kawamura, M. Lakićević, C. J. Law, N. Mizuno, T. Murase, T. Onishi, S. Park, P. P. Plucinsky, J. Rho, A. M. S. Richards, G. Rowell, M. Sasaki, J. Seok, P. Sharda, L. Staveley-Smith, H. Suzuki, T. Temim, K. Tokuda, K. Tsuge, K. Tachihara

H. Sano et al 2023 The Astrophysical Journal 958 .

  • Provider: AAS Journals

Caption: Figure 1.

Peak intensity maps of (a) 12CO(J = 1–0), (b) 12CO(J = 2–1), (c) 13CO(J = 2–1), and (d) 12CO(J = 3–2). (e) Intensity ratio map of 12CO(J = 2–1)/12CO(J = 1–0) (hereafter R 2−1/1−0). The velocity range of CO is from 285.5 to 287.8 km s−1. Superposed contours represent Chandra X-ray intensity in the energy band of 0.5–7.0 keV. The lowest contour level and the contour intervals are 5 × 10−7 and 3 × 10−6 photons pixel−1 s−1, respectively. The regions enclosed by dashed lines indicate the observed areas using ALMA. The CO peaks K, L, N, O–R, and T defined by Paper I are also indicated in (c). When we take the intensity ratio of R 2−1/1−0, the 12CO(J = 2–1) data were smoothed with a two-dimensional Gaussian kernel to match the effective beam size of the 12CO(J = 1–0) data. The gray shaded area in (e) represents the 12CO(J = 1–0) and/or 12CO(J = 2–1) data showing significance lower than ∼10σ.

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