Journal
ASTROPHYSICAL JOURNAL
Volume 865, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/1538-4357/aada49
Keywords
astrometry; radiation mechanisms: non-thermal; radio continuum: stars; stars: individual (IC 348, NGC 1333); techniques: interferometric
Categories
Funding
- von Humboldt Stiftung
- Sao Paulo Research Foundation (FAPESP) [2013/04934-8, 2015/14696-2]
- DGAPA, UNAM [IN112417]
- CONACyT, Mexico
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
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We derive the distance and structure of the Perseus molecular cloud by combining trigonometric parallaxes from Very Long Baseline Array (VLBA) observations, taken as part of the GOBELINS survey and Gaia Data Release 2. Based on our VLBA astrometry, we obtain a distance of 321 +/- 10 pc for IC 348. This is fully consistent with the mean distance of 320 +/- 26 measured by Gaia. The VLBA observations toward NGC 1333 are insufficient to claim a successful distance measurement to this cluster. Gaia parallaxes, on the other hand, yield a mean distance of 293 +/- 22 pc. Hence, the distance along the line of sight between the eastern and western edges of the cloud is similar to 30 pc, which is significantly smaller than previously inferred. We use Gaia proper motions and published radial velocities to derive the spatial velocities of a selected sample of stars. The average velocity vectors with respect to the LSR are ((u) over bar, (v) over bar, (w) over bar) = (-6.1 +/- 1.6, 6.8 +/- 1.1, -0.9 +/- 1.2) and (-6.4 +/- 1.0, 2.1 +/- 1.4, -2.4 +/- 1.0) km s(-1) for IC. 348 and NGC 1333, respectively. Finally, our analysis of the kinematics of the stars has shown that there is no clear evidence of expansion, contraction, or rotational motions within the clusters.
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