J/A+A/638/A85 3D view of Taurus with Gaia and Herschel (Roccatagliata+, 2020)
A 3D view of the Taurus star-forming region by Gaia and Herschel:
multiple populations related to the filamentary molecular cloud.
Roccatagliata V., Franciosini E., Sacco, G.G., Randich S.,
Sicilia-Aguilar A.
<Astron. Astrophys. 638, A85 (2020)>
=2020A&A...638A..85R 2020A&A...638A..85R (SIMBAD/NED BibCode)
ADC_Keywords: Associations, stellar ; Stars, pre-main sequence ;
Parallaxes, trigonometric ; Proper motions ; Radial velocities
Keywords: stars: pre-main sequence -
open clusters and associations: individual: Taurus - parallaxes -
proper motions - radio continuum: ISM
Abstract:
Taurus represents an ideal region to study the three-dimensional
distribution of the young stellar population and relate it to the
associated molecular cloud.
The second Gaia data release (DR2) enables us to investigate the
Taurus complex in three dimensions, starting from a previously defined
robust membership. The molecular cloud structured in filaments can be
traced in emission using the public far-infrared maps from Herschel.
From a compiled catalog of spectroscopically confirmed members, we
analyze the 283 sources with reliable parallax and proper motions in
the Gaia DR2 archive. We fit the distribution of parallaxes and proper
motions with multiple populations described by multivariate Gaussians.
We compute the cartesian Galactic coordinates (X,Y,Z) and, for the
populations associated with the main cloud, also the galactic space
velocity (U,V,W). We discuss the spatial distribution of the
populations in relation to the structure of the filamentary molecular
cloud traced by Herschel.
We discover the presence of six populations which are all well defined
in parallax and proper motions, with the only exception being Taurus
D. The derived distances range between ∼130 and ∼160pc. We do not
find a unique relation between stellar population and the associated
molecular cloud: while the stellar population seems to be on the cloud
surface, both lying at similar distances, this is not the case when
the molecular cloud is structured in filaments. Taurus B is probably
moving in the direction of Taurus A, while Taurus E appears to be
moving towards them.
The Taurus region is the result of a complex star formation history
which most probably occurred in clumpy and filamentary structures that
are evolving independently.
Description:
Table A.1 lists the properties of the 283 Taurus stars analysed in the
paper. The stars were selected from the catalogue of spectroscopically
confirmed members by Esplin & Luhman (2019, J/AJ/158/54), retaining
only those with a counterpart in the Gaia DR2 catalogue (I/345) and
reliable astrometry (RUWE<1.4). The table includes the 2MASS and
Gaia DR2 identifiers, the Gaia DR2 data used for the analysis
(positions, parallaxes, proper motions, correlation parameters, RUWE
parameter), the derived membership probabilities for each of the six
populations described in the paper, and the corresponding membership
information by Luhman (2018, J/AJ/156/271) and Galli et al. (2019,
J/A+A/630/A137).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 287 283 Membership results for 283 Taurus stars
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See also:
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/AJ/158/54 : New Taurus members from stellar to planetary masses
(Esplin+, 2019)
J/AJ/156/271 : The stellar membership of the Taurus SFR (Luhman, 2018)
J/A+A/630/A137 : Structure and kinematics of the Taurus region (Galli+, 2019)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- 2MASS 2MASS Point Source Catalog name
(JHHMMSSss+DDMMSSs)
20- 38 I19 --- GaiaDR2 Gaia DR2 identifier
40- 62 A23 --- Name Other source name
64- 68 A5 --- SpType Spectral type from Esplin & Luhman
(2019, J/AJ/158/54)
70- 75 F6.1 yr RefEp [2015.5] Reference epoch from Gaia DR2
77- 85 F9.6 deg RAdeg Right Ascension (ICRS) at Ep=2015.5
from Gaia DR2
87- 94 F8.6 deg e_RAdeg Error on Right Ascension
96-104 F9.6 deg DEdeg Declination (ICRS) at Ep=2015.5
from Gaia DR2
106-113 F8.6 deg e_DEdeg Error on Declination
115-123 F9.6 mas Plx Parallax from Gaia DR2
125-132 F8.6 mas e_Plx Error in Plx
134-142 F9.6 mas/yr pmRA* Proper motion in RA, pmRA*cosDE
from Gaia DR2
144-151 F8.6 mas/yr e_pmRA* Error in pmRA
153-162 F10.6 mas/yr pmDE Proper motion in DEC from Gaia DR2
164-171 F8.6 mas/yr e_pmDE Error in pmDE
173-181 F9.6 --- plxpmRAcor Correlation between parallax and
proper motion in RA
183-191 F9.6 --- plxpmDEcor Correlation between parallax and
proper motion in DEC
193-201 F9.6 --- pmRApmDEcor Correlation between proper motions in
RA and in DEC
203-212 F10.6 deg GLON Galactic longitude
214-223 F10.6 deg GLAT Galactic latitude
225-229 F5.3 --- RUWE Renormalized Unit Weight Factor
from Gaia DR2
231-235 F5.3 --- pA [0/1] Probability of membership to Taurus A
237-241 F5.3 --- pB [0/1] Probability of membership to Taurus B
243-247 F5.3 --- pC [0/1] Probability of membership to Taurus C
249-253 F5.3 --- pD [0/1] Probability of membership to Taurus D
255-259 F5.3 --- pE [0/1] Probability of membership to Taurus E
261-265 F5.3 --- pF [0/1] Probability of membership to Taurus F
267-274 F8.3 km/s RV ?=999.999 RV from Galli et al.
(2019, J/A+A/630/A137)
276-280 A5 --- PopL18 Population from Luhman
(2018, J/AJ/156/271) (1)
282-283 I2 --- ClustG19 [0/21] Cluster number from Galli et al.
(2019, J/A+A/630/A137)
285-287 I3 --- MemG19 [0/1] Membership status from Galli et al.
(2019, J/A+A/630/A137)
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Note (1): Color code for the kinematic populations in Figures 2-11 of
Galli et al., 2019A&A...630A.137G 2019A&A...630A.137G.
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Acknowledgements:
Veronica Roccatagliata, veronica.roccatagliata(at)unipi.it
(End) Veronica Roccatagliata [UNIPI, Italy], Patricia Vannier [CDS] 13-May-2020