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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 3.

(a) Radial profile of the normalized X-ray intensity, centered at (α J2000, δ J2000) = (05h25m59.ˢ57, ﹩-66^\circ 04^{\prime} 56\buildrel{\rm{s}}\over{.} 4﹩) as the geometric center of the SNR. The steps with filled circles indicate averaged values of normalized X-ray intensity at each annulus. The green line indicates the three-dimensional Gaussian distribution, and the orange line represents its projected distribution given by the least-squares fitting (see the text). (b) Scatter plot of kinetic temperature T kin for each cloud as a function of the projected radial distance. The dashed horizontal line represents T kin=10 K, corresponding to the typical temperature of quiescent molecular clouds. The red and green symbols represent high- and moderate-temperature clouds, respectively.

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