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Chemistry of the High-mass Protostellar Molecular Clump IRAS 16562–3959

  • Authors: Andrés E. Guzmán, Viviana V. Guzmán, Guido Garay, Leonardo Bronfman, and Federico Hechenleitner

2018 The Astrophysical Journal Supplement Series 236 45.

  • Provider: AAS Journals

Caption: Figure 7.

Panels (a) and (b) show zero-moment maps of the CH3OH (E1) ﹩{2}_{\mathrm{1,1}}\to {1}_{\mathrm{1,0}}﹩ (Eup = 21.6 K) and the HC15N ﹩1\to 0﹩ (Eup = 4.1 K) transitions, respectively. Red crosses mark the continuum sources identified at 3 mm in Paper I. Green crosses show the position of the CH3OH, (E2) ﹩{5}_{-\mathrm{1,0}}\to {4}_{\mathrm{0,0}}﹩ maser spots. Black crosses mark the DR(a), (b), and (c) positions in the Diffuse Ridge, the NEC-wall (a) and (b) positions, and the NW cloud (a) position (Section 4.2). Black dashed ellipses mark the CC core, the N-red cloud, and the NW cloud. To the left and on top of panel (a) we show R.A.−velocity and decl.−velocity PV diagrams, respectively. In the top R.A.−velocity PV diagram, we mark the N-red cloud with a dashed circle, and two arrows indicate the sources that compose the blended CC core emission in the CH3OH zero-moment map. PV diagrams of the HC15N emission are shown to the right and on top of panel (b).

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