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Dense CO in Mrk 71-A: Superwind Suppressed in a Young Super Star Cluster

  • Authors: M. S. Oey, C. N. Herrera, Sergiy Silich, Megan Reiter, Bethan L. James, A. E. Jaskot, and Genoveva Micheva

2017 The Astrophysical Journal Letters 849 L1.

  • Provider: AAS Journals

Caption: Figure 3.

Panel (a) (left) shows the CO(2–1) line profile for Mrk 71-A, extracted from an area of ﹩0\buildrel{\prime\prime}\over{.} 68﹩ size, defined as the emission ﹩\gt 2\sigma ﹩ in the map integrated over 72–88 ﹩\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩. The two fitted Gaussian components are shown with dashed blue and red lines, and the single fitted Gaussian is shown with the solid green line. Panel (b) (right) shows the spatial distribution of the two components in blue and red contours, corresponding to the respective kinematic components in the left panel. The continuum flux is indicated by the color scale bar. The contours for the continuum correspond to 2σ, 3σ, 4σ, and 5σ with rms 0.075 mJy/beam. The contours for the blue and red components are integrated over 72.4–77.6 ﹩\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩ and 82.8–88.0 ﹩\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩, respectively, both showing contours starting at ﹩2\sigma ﹩ in integer σ intervals. For the blue and red components, ﹩1\sigma =12.9﹩ and 13.7 mJy/beam km s−1, respectively. The rectangle indicates the region from which the PV diagram in Figure 4 is calculated. The NOEMA beam is also shown in the lower left.

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