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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 2.

Top panels: large velocity gradient results on the number density of molecular hydrogen, n(H2), and the kinetic temperature, T kin, for the ambient cloud P, pre-shocked cloud R, and the post-shocked cloud L. The red lines and blue dashed-dotted lines indicate the intensity ratios of 12CO(J = 3–2)/12CO(J =2–1) and 13CO(J = 2–1)/12CO(J =3–2), respectively. The shaded areas surrounding the red and blue lines indicate the 1σ ranges of each intensity ratio. Yellow crosses represent the best-fit values of n(H2) and T kin for each cloud. The spatial positions and best-fit values for each cloud are shown in the top-right corners for each panel. Bottom panels: CO intensity profiles for clouds P, R, and L. The physical properties of each cloud are summarized in Table 1.

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