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Mapping Distances across the Perseus Molecular Cloud Using CO Observations, Stellar Photometry, and Gaia DR2 Parallax Measurements

• Authors: Catherine Zucker, Edward F. Schlafly, Joshua S. Speagle, Gregory M. Green, Stephen K. N. Portillo, Douglas P. Finkbeiner, and Alyssa A. Goodman

2018 The Astrophysical Journal 869 83.

• Provider: AAS Journals

Caption: Figure 4.

Monte Carlo realizations of the average reddening-weighted distance to each cloud as described at the beginning of Section 7. Each “count” is a reddening-weighted average distance computed using Equation (7). From top to bottom, the panels are sorted in order of increasing R.A. We report the mean of the distribution in each panel (vertical blue lines) as the final overall average distance to each star-forming region in Table 3. Likewise, the uncertainty we report in Table 3 is the standard deviation of each distribution. An average distance and distance uncertainty for the Perseus complex as a whole (bottom panel) is computed by stacking the average distances to individual regions in the first six panels.