J/A+A/671/A1 cosmic DANCe of Perseus (Olivares+, 2023)
The cosmic DANCe of Perseus.
I. Membership, phase-space structure, mass, and energy distributions.
Olivares J., Bouy H., Miret-Roig N., Galli P.A.B., Sarro L.M., Moraux E.,
Berihuete A.
<Astron. Astrophys. 671, A1 (2023)>
=2023A&A...671A...1O 2023A&A...671A...1O (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Space velocities ; Extinction ; Optical ;
Stars, masses
Keywords: open clusters and associations: individual: Perseus -
stars: luminosity function, mass function - proper motions -
stars: kinematics and dynamics - methods: statistical - astrometry -
Abstract:
Star-forming regions are excellent benchmarks for testing and
validating theories of star formation and stellar evolution. The
Perseus star-forming region, being one of the youngest (<10Myr),
closest (280-320pc), and most studied in the literature, is a
fundamental benchmark.
We aim to study the membership, phase-space structure, mass, and
energy (kinetic plus potential) distribution of the Perseus
star-forming region using public catalogues (Gaia, APOGEE, 2MASS, and
Pan-STARRS).
We used Bayesian methodologies that account for extinction to identify
the Perseus physical groups in the phase-space, retrieve their
candidate members, derive their properties (age, mass, 3D positions,
3D velocities, and energy), and attempt to reconstruct their origin.
Results. We identify 1052 candidate members in seven physical groups
(one of them new) with ages between 3 and 10Myr, dynamical
super-virial states, and large fractions of energetically unbounded
stars. Their mass distributions are broadly compatible with that of
Chabrier for masses ≳0.1M☉ and do not show hints of
over-abundance of low-mass stars in NGC1333 with respect to IC348.
These groups' ages, spatial structure, and kinematics are compatible
with at least three generations of stars. Future work is still needed
to clarify if the formation of the youngest was triggered by the
oldest.
The exquisite Gaia data complemented with public archives and mined
with comprehensive Bayesian methodologies allow us to identify 31%
more members than previous studies, discover a new physical group
(Gorgophone: 7Myr, 191 members, and 145M☉), and confirm that the
spatial, kinematic, and energy distributions of these groups support
the hierarchical star formation scenario.
Description:
Table containing the properties of the 1052 Perseus candidate members.
It comprises the parent group of the candidate member, its Gaia DR3
source identifier, right ascension, and declination, both from Gaia
DR3. The remaining properties were inferred using Markov chain Monte
Carlo methods and the statistics of the resulting samples are provided
as mean values and standard deviations or percentiles and
maximum-a-posteriori (i.e. the mode of the posterior distribution).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 283 1052 Properties of the 1052 candidate members
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Group Parent statistical group
(statistical_group) (1)
17- 34 I18 --- GaiaDR3 ? Gaia DR3 source_id (source_id)
36- 53 F18.15 deg RAdeg [51.23/59.0] Right ascension (ICRS)
at Ep=2016.0 (from Gaia DR3) (ra)
55- 72 F18.15 deg DEdeg [30.0/33.0] Declination (ICRS)
at Ep=2016.0 (from Gaia DR3) (dec)
74- 80 F7.3 pc meanX [111.98/202.89] Mean value of the
Cartesian X position (mean_X)
82- 87 F6.3 pc e_meanX [0.49/10.95] Standard deviation of the
Cartesian X position (sd_X)
89- 95 F7.3 pc meanY [174.0/307.1] Mean value of the
Cartesian Y position (mean_Y)
97-102 F6.3 pc e_meanY [0.72/16.32] Standard deviation of the
Cartesian Y position (sd_Y)
104-110 F7.3 pc meanZ [125.39/217.24] Mean value of the
Cartesian Z position (mean_Z)
112-117 F6.3 pc e_meanZ [0.55/11.22] Standard deviation of the
Cartesian Z position (sd_Z)
119-124 F6.3 km/s meanU [-1.28/9.53] Mean value of the
Cartesian U velocity (mean_U)
126-130 F5.3 km/s e_meanU [0.05/1.65] Standard deviation of the
Cartesian U velocity (sd_U)
132-137 F6.3 km/s meanV [15.47/25.3] Mean value of the
Cartesian V velocity (mean_V)
139-143 F5.3 km/s e_meanV [0.05/2.25] Standard deviation of the
Cartesian V velocity (sd_V)
145-150 F6.3 km/s meanW [-8.04/4.66] Mean value of the
Cartesian W velocity (mean_W)
152-156 F5.3 km/s e_meanW [0.05/1.63] Standard deviation of the
Cartesian W velocity (sd_W)
158-178 F21.18 Msun b_mapmass [0.02/17.55] Percentile 2.5 of the
system mass (lower_mass)
180-200 F21.18 Msun mapmass [0.02/17.87] Maximum-a-posteriori of the
system mass (map_mass)
202-222 F21.18 Msun B_mapmass [0.03/17.96] Percentile 97.5 of the
system mass (upper_mass)
224-243 F20.18 mag b_mapAv [0.03/9.12] Percentile 2.5 of the
Av extinction (lower_Av)
245-264 F20.18 mag mapAv [0.0/9.99] Maximum-a-posteriori of the
Av extinction (map_Av)
266-283 F18.16 mag B_mapAv [0.31/9.9] Percentile 97.5 of the
Av extinction (upper_Av)
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Note (1): Parent statistical group are Alcaeus, Autochthe, Gorgophone_core,
Gorgophone_halo, Heleus, IC348_core, IC348_halo and NGC1333.
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Acknowledgements:
Javier Olivares, jolivares at dia.uned.es
(End) Patricia Vannier [CDS] 10-Jan-2023