Journal
ASTRONOMY & ASTROPHYSICS
Volume 630, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201935928
Keywords
open clusters and associations: individual: Taurus; stars: formation; stars: distances; methods: statistical
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Funding
- European Research Council (ERC) under the European Union [682903]
- Investments for the future Program, IdEx Bordeaux [ANR-10-IDEX-03-02]
- PAPIIT-UNAM [IN112417]
- CONACyT
- von Humboldt Stiftung
- European Research Council (ERC) [682903] Funding Source: European Research Council (ERC)
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Aims. We take advantage of the second data release of the Gaia space mission and the state-of-the-art astrometry delivered from very long baseline interferometry observations to revisit the structure and kinematics of the nearby Taurus star-forming region. Methods. We apply a hierarchical clustering algorithm for partitioning the stars in our sample into groups (i.e., clusters) that are associated with the various molecular clouds of the complex, and derive the distance and spatial velocity of individual stars and their corresponding molecular clouds. Results. We show that the molecular clouds are located at different distances and confirm the existence of important depth effects in this region reported in previous studies. For example, we find that the L 1495 molecular cloud is located at d = 129(-0.3)(+0.4) pc, while the filamentary structure connected to it (in the plane of the sky) is at d = 160.0(-1.2)(+1.2) pc. We report B 215 and L 1558 as the closest (d = 128.5(-1.6)(+1.6)pc) and most remote (d = 198.1(-2.5)(+2.5)pc) substructures of the complex, respectively. The median inter-cloud distance is 25 pc and the relative motion of the subgroups is on the order of a few km s(-1). We find no clear evidence for expansion (or contraction) of the Taurus complex, but signs of the potential effects of a global rotation. Finally, we compare the radial velocity of the stars with the velocity of the underlying (CO)-C-13 molecular gas and report a mean difference of 0.04 +/- 0.12 km s(-1) (with rms of 0.63 km s(-1)) confirming that the stars and the gas are tightly coupled.
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