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H I Shells and Supershells in the I-GALFA H I 21 cm Line Survey. I. Fast-expanding H I Shells Associated with Supernova Remnants

  • Authors: G. Park, B.-C. Koo, S. J. Gibson, J.-h. Kang, D. C. Lane, K. A. Douglas, J. E. G. Peek, E. J. Korpela, C. Heiles, and J. H. Newton

Park et al. 2013 The Astrophysical Journal 777 14.

  • Provider: AAS Journals

Caption: Figure 4.

Channel maps of HV H i gas associated with the SNR W44 at negative (left) and positive (right) velocities in the I-GALFA H i data. The central LSR velocity of each panel is written at the upper right corner in km s −1. The velocity width of one displayed channel is 3.68 km s −1; this is binned by a factor of 20 from the raw data and has a measured rms noise of 0.07 K. The H i brightness temperature in each gray scale ranges from 0 K (white) to the value (black) at the lower left corner of each panel in kelvins. Radio continuum emission at 21 cm is shown by red contours as in Figure 3. The blue arrows in the first two panels indicate an emission feature described in Section 3.1.2.

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