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Structure and kinematics of the Taurus star-forming region from Gaia-DR2 and VLBI astrometry

hal.structure.identifierInstituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] [IAG]
dc.contributor.authorGALLI, P. A. B.
hal.structure.identifierCentro de Radioastronomia y Astrofisica [CRyA]
dc.contributor.authorLOINARD, L.
hal.structure.identifierM2A 2019
dc.contributor.authorBOUY, H.
hal.structure.identifierUniversidad Nacional de Educación a Distancia [UNED]
dc.contributor.authorSARRO, L. M.
dc.contributor.authorORTIZ-LEÓN, G. N.
dc.contributor.authorDZIB, S. A.
hal.structure.identifierM2A 2019
dc.contributor.authorOLIVARES, J.
dc.contributor.authorHEYER, M.
dc.contributor.authorHERNANDEZ, J.
dc.contributor.authorROMÁN-ZÚÑIGA, C.
dc.contributor.authorKOUNKEL, M.
dc.contributor.authorCOVEY, K.
dc.date.issued2019
dc.identifier.issn0004-6361
dc.description.abstractEnAims: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 $d=129.9^{+0.4}_{-0.3}$ 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. 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 $^{13}$CO molecular gas and report a mean difference of $0.04\pm0.12$ km/s (with r.m.s. of 0.63 km/s) confirming that the stars and the gas are tightly coupled.
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enStructure and kinematics of the Taurus star-forming region from Gaia-DR2 and VLBI astrometry
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201935928
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]
dc.identifier.arxiv1909.01118
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA137
bordeaux.volume630
bordeaux.peerReviewedoui
hal.identifierhal-02282391
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02282391v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2019&rft.volume=630&rft.spage=A137&rft.epage=A137&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=GALLI,%20P.%20A.%20B.&LOINARD,%20L.&BOUY,%20H.&SARRO,%20L.%20M.&ORTIZ-LE%C3%93N,%20G.%20N.&rft.genre=article


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