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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 2.

Cartoon line-of-sight reddening profile assuming a model with a single velocity slice v1 (where the cloud can be described by a single distance component d1). Such a reddening profile is defined by the free parameters dfore (foreground cloud distance), Efore (foreground cloud reddening), d1 (distance modulus to single velocity slice), and c1 (gas-to-dust conversion coefficient in single velocity slice). The quantity Ij,1 constitutes the CO emission for star i lying in pixel j in the single velocity slice v1. The reddening profile is overlaid on an idealized joint posterior on distance and reddening (grayscale ellipsoid) for individual star i lying in CO pixel j. The star’s likelihood is simply the integral over μ following the reddening profile (solid red line); the dashed red lines are excluded from the integration. In Section 6 the likelihood from this star would be multiplied together with the likelihoods of thousands of other stars to get the total likelihood contribution (see Equation (4)).

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