J/A+A/681/A72 TAMC Gaia DR3 stars (Gomez de Castro+, 2024)
Uncovering a new group of T Tauri stars in the Taurus-Auriga molecular complex
from Gaia and GALEX data.
Gomez de Castro A.I., de la Fuente Marcos R., Canet A., Beitia-Antero L.,
Yanez-Gestoso J., Vallejo J.C.
<Astron. Astrophys. 681, A72 (2024)>
=2024A&A...681A..72G 2024A&A...681A..72G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Parallaxes, trigonometric ; Proper motions ;
Optical
Keywords: stars, variables: T Tauri, Herbig Ae/Be - Galaxy: stellar content -
surveys - stars: low-mass -
Abstract:
Determining a complete census of young stars in any star forming
region is a challenge even for the nearest and best-observed molecular
clouds, such as Taurus-Auriga (TAMC). Deep surveys at infrared (IR)
and X-ray wavelengths and astrometric surveys using Gaia DR2 and DR3
have been carried out to detect the sparse population and constrain
the low-mass end of the initial mass function. These compilations have
resulted in lists of more than 500 sources, including reliable members
of the association and candidates. The astrometric information
provided by the Gaia mission has proven to be of fundamental
importance in evaluating these candidates.
In the present work, we examine the list of 63 candidate T Tauri star
(TTS) in the TAMC identified by their ultraviolet (UV) and IR colours
measured from data obtained by the Galaxy Evolution Explorer all sky
survey (GALEX-AIS) and the Two Microns All Sky Survey (2MASS),
respectively. These sources have not been included in previous studies
and the objectives of this work are twofold: to evaluate whether or
not they are pre-main sequence (PMS) stars and to evaluate the true
potentials of the UV-IR colour-colour diagram to detect PMS stars in
wide fields.
We retrieved the kinematic properties and the parallax of these
sources from the Gaia DR3 catalogue and used them to evaluate their
membership probability. We tested several classification algorithms to
search for the kinematical groups, but made the final classification
with k-means++ algorithms. We evaluated membership probability by
applying logistic regression. In addition, we used spectroscopic
information available in the archive of the Large Sky Area Multi
Object Fiber Spectroscopic Telescope (LAMOST) to ascertain their PMS
nature when available.
About 20% of the candidates share the kinematics of the TAMC members.
Among them, HD 281691 is a G8-type field star located in front of the
cloud and HO Aur is likely a halo star given the very low metallicity
provided by Gaia. The remaining sources included three known PMS stars
(HD 30171, V600 Aur and J04590305+3003004), two previously unknown
accreting M-type stars (J04510713+1708468 and J05240794+2542438), and
five additional sources that are very likely PMS stars. Most of these
new sources are concentrated at low galactic latitudes over the
Auriga-Perseus region.
Description:
The Table is based on the catalog of T Tauri Stars in the
Taurus-Auriga Molecular Complex (TAMC) compiled by Joncour et al.
(2017A&A...599A..14J 2017A&A...599A..14J, Cat. J/A+A/599/A14).
Table 2 contains sources from this catalog that have Gaia DR3
counterparts, with high quality astrometric measurements (RUWE ≤1.4)
and Gaia parallax compatible with the distance to the TAMC.
The sources in this Table have been used as qualification sample for
the study of the kinematics of the young stellar population in the
TAMC.
All astrometric values have been extracted from the Gaia DR3 catalog.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 72 166 Sources from TAMC catalog that have Gaia DR3
counterparts
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
J/A+A/599/A14 : Taurus ultra-wide pairs (Joncour+, 2017)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 F11.7 deg GLON Galactic longitude
13- 25 F13.9 deg GLAT Galactic latitude
27- 32 F6.4 mas plx Parallax
34- 39 F6.4 mas e_plx Parallax error
41- 46 F6.3 mas/yr pmRA Proper motion in right ascension
48- 52 F5.3 mas/yr e_pmRA Error in proper motion in right ascension
54- 60 F7.3 mas/yr pmDE Proper motion in declination
62- 66 F5.3 mas/yr e_pmDE Error in proper motion in declination
68- 72 F5.3 --- RUWE Renormalised unit weight error
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Acknowledgements:
Ana Ines Gomez de Castro, aig(at)ucm.es
(End) Patricia Vannier [CDS] 25-Oct-2023