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First Results from a 1.3 cm Expanded Very Large Array Survey of Massive Protostellar Objects: G35.03+0.35

  • Authors: C. L. Brogan, T. R. Hunter, C. J. Cyganowski, R. K. Friesen, C. J. Chandler, and R. Indebetouw

Brogan et al. 2011 The Astrophysical Journal Letters 739 L16.

  • Provider: AAS Journals

Caption: Figure 3.

(a) Color scale of the NH 3 kinetic temperature using fitting method (1): gray areas indicate where the assumptions for this technique are invalid. The blue, red, and white contours show the lowest 3.6 cm contour from Figure 2, highest (3,3) contour from Figure 2(c), and highest (1,1) contour from Figure 1(a), respectively. The locations of the profiles shown in (b), for the non-thermal NH 3 emission (18 h54 m01 fs119, +02°01′14 farcs08), and (c) the stronger 25 GHz CH 3OH maser (18 h54 m01 fs076, +02°01′16 farcs47) are indicated along with other positions fitted with method (2) and presented in Table 2. In (b) and (c), the vertical dotted line marks the local standard of rest (LSR) velocity of +53.1 km s −1.

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