J/A+A/695/A13 SUCANES data base substellar candidates (Perez-Garcia+, 2025)
Substellar candidates at the earliest stages: The SUCANES database.
Perez-Garcia A.M., Huelamo N., Garcia Lopez A., Perez-Martinez R.,
Verdugo E., Palau A., de Gregorio-Monsalvo I., Morata O., Barrado D.,
Morales-Calderon M., Mas-Hesse M., Bayo A., Mauco K., Bouy H.
<Astron. Astrophys. 695, A13 (2025)>
=2025A&A...695A..13P 2025A&A...695A..13P (SIMBAD/NED BibCode)
ADC_Keywords: Stars, brown dwarf ; Stars, distances
Keywords: astronomical data bases - brown dwarfs - stars: low-mass -
stars: protostars
Abstract:
Brown dwarfs are the bridge between low-mass stars and giant planets.
One way of shedding light on their dominant formation mechanism is to
study them at the earliest stages of their evolution, when they are
deeply embedded in their parental clouds. Several works have
identified pre- and proto-brown dwarf candidates using different
observational approaches.
The aim of this work is to create a database of all the objects
classified as very young substellar candidates in the literature in
order to study them homogeneously.
We gathered all the information about very young substellar candidates
available in the literature until 2020. We retrieved their published
photometry from the optical to the centimetre regime, and we wrote our
own codes to derive their bolometric temperatures and luminosities,
and their internal luminosities. We also populated the database with
other parameters extracted from the literature, such as the envelope
masses, their detection in some molecular species, and the presence of
outflows.
The result of our search is the SUbstellar CANdidates at the Earliest
Stages (SUCANES) database, containing 174 objects classified as
potential very young substellar candidates in the literature. We
present an analysis of the main properties of the retrieved objects.
Since we updated the distances to several star forming regions, we
were able to reject some candidates based on their internal
luminosities. We also discuss the derived physical parameters and
envelope masses for the best substellar candidates isolated in
SUCANES. As an example of a scientific exploitation of this database,
we present a feasibility study for the detection of radio jets with
upcoming facilities: the next generation Very Large Array and the
Square Kilometer Array interferometers. The SUCANES database is
accessible through a graphical user interface, and it is open to any
potential user.
Description:
TableB1 includes all the objects identified as very young substellar
candidates in the literature that are contained in the SUCANES data
base. In this table, we provide their meain properties, and the
bibliographic references from which the information has been
extracted. An analysis of the data base has also allowed us to discard
some of the previous identified objects as substellar candidates,
mainly based on updated distances to the objects.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 122 174 The targets included in the SUCANES data base
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 25 A25 --- Name Target Name
27- 28 I2 h RAh Right Ascension (J2000)
30- 31 I2 min RAm Right Ascension (J2000)
33- 37 F5.2 s RAs Right Ascension (J2000)
39 A1 --- DE- Declination sign (J2000)
40- 41 I2 deg DEd Declination (J2000)
43- 44 I2 arcmin DEm Declination (J2000)
46- 50 F5.2 arcsec DEs Declination (J2000)
52- 56 F5.1 pc Dist Distance (1)
58- 62 F5.1 pc e_Dist Distance uncertainty
64- 77 A14 --- Region Star forming Region the object belongs to
79- 93 A15 --- Type Classification of the object in the
literature (2)
95- 98 A4 --- Class Evolutionary Class of the object
as found in the literature
100-118 A19 --- Refs References from which all the information
from previous columns has been extracted (3)
120-122 I3 --- ObjID Object Identification Number in SUCANES
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Note (1): Some objects show updated distances, as explained in in the paper.
Note (2): Objects with '/D' after the Type are discarded as
substellar candidates in SUCANES.
Note (3): References as follows:
A99 = Andre et al., 1999ApJ...513L..57A 1999ApJ...513L..57A
A05 = Apai et al., 2005A&A...433L..33A 2005A&A...433L..33A
A12 = Andre et al., 2012Sci...337...69A 2012Sci...337...69A
B06 = Belloche et al., 2006A&A...454L..51B 2006A&A...454L..51B
B09 = Barrado et al., 2009A&A...508..859B 2009A&A...508..859B
B14 = Bulger et al., 2014A&A...570A..29B 2014A&A...570A..29B, Cat. J/A+A/570/A29
B20 = Busch et al., 2020A&A...633A.126B 2020A&A...633A.126B, Cat. J/A+a/633/A126
C10 = Chen et al., 2010ApJ...715.1344C 2010ApJ...715.1344C
C16 = Carney et al., 2016A&A...586A..44C 2016A&A...586A..44C
C18 = Clemens et al., 2018ApJ...867...79C 2018ApJ...867...79C, cat. J/ApJ/867/79
D08 = Dunham et al., 2008ApJS..179..249D 2008ApJS..179..249D, Cat. J/ApJS/179/249
D15 = Dunham et al., 2015ApJS..220...11D 2015ApJS..220...11D, Cat. J/ApJS/220/11
DD16 = Dang-Duc et al., 2016A&A...588L...2D 2016A&A...588L...2D
E06 = Enoch et al., 2006ApJ...638..293E 2006ApJ...638..293E, Cat. J/ApJ/638/293
E10 = Enoch et al., 2010ApJ...722L..33E 2010ApJ...722L..33E
F06 = Furuya et al., 2006ApJ...653.1369F 2006ApJ...653.1369F
F09 = Forbrich et al., 2009ApJ...704..292F 2009ApJ...704..292F
dG16 = de Gregorio-Monsalvo et al., 2016A&A...590A..79D 2016A&A...590A..79D
G17 = Gerin et al., 2017A&A...606A..35G 2017A&A...606A..35G , Cat. J/A+A/606/A35
H06 = Huard et al., 2006ApJ...640..391H 2006ApJ...640..391H
H14 = Hirano & Liu, 2014ApJ...789...50H 2014ApJ...789...50H
H16 = Hsieh et al., 2016ApJ...826...68H 2016ApJ...826...68H
H17 = Huelamo et al., 2017A&A...597A..17H 2017A&A...597A..17H
H19 = Hirano, 2019asrc.confE..90H
K08 = Kauffmann et al., 2008A&A...487..993K 2008A&A...487..993K, Cat. J/A+A/487/993
K16 = Kim et al., 2016ApJS..225...26K 2016ApJS..225...26K, Cat. J/ApJS/225/26
K17 = Kirk et al., 2017ApJ...838..114K 2017ApJ...838..114K
K18 = Kawabe et al., 2018ApJ...866..141K 2018ApJ...866..141K
K19 = Kim et al., 2019ApJS..240...18K 2019ApJS..240...18K
L10 = Lee et al., 2010ApJ...709L..74L 2010ApJ...709L..74L
L13 = Lee et al., 2013ApJ...777...50L 2013ApJ...777...50L
L16 = Liu et al., 2016ApJS..222....7L 2016ApJS..222....7L
L18 = Lee et al., 2018ApJ...865..131L 2018ApJ...865..131L
M15 = Morata et al., 2015ApJ...807...55M 2015ApJ...807...55M
M17 = Mowat et al., 2017MNRAS.467..812M 2017MNRAS.467..812M
M20 = Maureira et al., 2020MNRAS.499.4394M 2020MNRAS.499.4394M
O14 = Oya et al., 2014ApJ...795..152O 2014ApJ...795..152O
P11 = Pineda et al., 2011ApJ...743..201P 2011ApJ...743..201P
P12 = Palau et al., 2012MNRAS.424.2778P 2012MNRAS.424.2778P
P14 = Palau et al., 2014MNRAS.444..833P 2014MNRAS.444..833P
R15 = Riaz et al., 2015MNRAS.446.2550R 2015MNRAS.446.2550R
R16 = Riaz et al., 2016ApJ...831..189R 2016ApJ...831..189R
R18 = Riaz et al., 2018MNRAS.481.4662R 2018MNRAS.481.4662R
RB21 = Riaz & Bally, 2021MNRAS.501.3781R 2021MNRAS.501.3781R
RM21 = Riaz & Machida, 2021MNRAS.504.6049R 2021MNRAS.504.6049R
SM21 = Santamaria-Miranda et al., 2021A&A...646A..10S 2021A&A...646A..10S
T13 = Tsitali et al., 2013A&A...557A..98T 2013A&A...557A..98T
T16 = Tobin et al., 2016ApJ...818...73T 2016ApJ...818...73T, Cat. J/ApJ/818/73
W04 = White & Hillenbrand, 2004ApJ...616..998W 2004ApJ...616..998W
W07 = Dunham et al., 2007AJ....133.1560W 2007AJ....133.1560W, Cat. J/AJ/133/1560
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Acknowledgements:
A.M. Perez-Garcia, amperez(at)isdefe.es
(End) Patricia Vannier [CDS] 21-Feb-2025