J/A+A/695/A48 Young stellar pop. in Carina nebula and Car OB1 (Goeppl+, 2025)
Spatial distribution and clustering properties of the young stellar populations
in the Carina Nebula complex and Car OB1.
Goeppl C., Preibisch T.
<Astron. Astrophys. 695, A48 (2025)>
=2025A&A...695A..48G 2025A&A...695A..48G (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Associations, stellar ; Stars, O ; Stars, B-type
Keywords: stars: formation - stars: kinematics and dynamics -
stars: pre-main sequence
Abstract:
We use Gaia DR3 astrometry and photometry to analyze the spatial
distribution of the young stellar populations and stellar clusters,
and to search for new OB star candidates in the Carina Nebula Complex
and the full extent (∼5°, corresponding to ∼200pc) of the Car OB1
association.
First, we perform a new census of high-mass stars in Car OB1 and
compile a comprehensive catalog of 517 stars with known spectral types
(128 O-type, WR, and supergiant stars, and 389 B-type stars) which
have Gaia DR3 parallaxes consistent with membership in the
association. We apply the clustering algorithm DBSCAN on the Gaia DR3
data of the region to find stellar clusters, determine their distances
and kinematics, and estimate ages. We also use Gaia astrometry and the
additional astrophysical_parameterstable to perform a spatially
unbiased search for further high-mass members of Car OB1 over the full
area of the association.
Our DBSCAN analysis finds 15 stellar clusters and groups in Car OB1,
four of which were not known before. Most clusters (80%) show signs of
expansion/contraction, four of them with >2σ significance. We
find a global expansion of the Car OB1 association with a velocity of
vout=5.25±0.02km/s. A kinematic traceback of the high-mass
stars shows that the spatial extent of the association was at a
minimum 3-4 Myr ago. Using astrophysical parameters by Gaia DR3, we
identify 15 new O-type and 589 new B-type star candidates in Car OB1.
The majority (>54%) of the high-mass stars constitutes a
non-clustered, distributed stellar population. Based on our sample of
high-mass stars we estimate a total stellar population of at least
∼8*104stars in Car OB1.
Our study is the first systematic astrometric analysis that covers the
full spatial extent of the Car OB1 association, and therefore
substantially increases the knowledge of the distributed stellar
population and spatial evolution of the whole association. It suggests
Car OB1 to be the most massive known star-forming complex in our
Galaxy.
Description:
Table B1 contains the mean astrometric parameters for all clusters
found with DBSCAN.
Table B2 contains the astrometric parameters, spectral type, effective
temperature, to which population (clustered or distributed) a star
belongs, and how the star was selected, for all Car OB1 high-mass
stars and OB candidates.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 242 462 Mean astrometric parameters for all clusters
found with DBSCAN
tableb2.dat 205 1374 Astrometric parameters, spectral type, effective
temperature, to which population (clustered or
distributed) a star belongs, and how the star
was selected, for all Car OB1 high-mass stars
and OB candidates
--------------------------------------------------------------------------------
See also:
I/355 : Gaia DR3 (Gaia Collaboration, 2022)
Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Seq Cluster number
5- 7 I3 --- NMem Number of cluster members
9- 26 F18.14 deg RAdeg Weighted mean of right ascension (ICRS)
at Ep=2016.0
28- 46 F19.15 deg DEdeg Weighted mean of declination (ICRS)
at Ep=2016.0
48- 66 F19.16 mas/yr pmRA Weighted mean of proper motion in
right ascension
68- 85 F18.16 mas/yr pmDE Weighted mean of proper motion in
declination
87-105 F19.17 mas plx Weighted parallax mean
107-127 F21.19 mas e_plx Standard deviation of weighted
parallax mean
129-132 I4 kpc Dist ? Kalkayotl mean distance
134-137 I4 kpc b_Dist ? 16th percentile Kalkayotl distance
confidence interval
139-142 I4 kpc B_Dist ? 84th percentile Kalkayotl distance
confidence interval
144-201 A58 --- OName Cluster counterpart in literature
203-220 A18 --- Ref ? Reference for counterpart (1)
222 A1 --- CarOB1 [Y/N] Cluster part of Car OB1
224-242 A19 --- subclusters Subcluster associated with each other
reference
--------------------------------------------------------------------------------
Note (1): References as follows:
B19 = Bica et al., 2019AJ....157...12B 2019AJ....157...12B, Cat. J/AJ/157/12
C18 = Cantat-Gaudin et al., 2018A&A...618A..93C 2018A&A...618A..93C, Cat. J/A+A/618/A93
C20 = Cantat-Gaudin et al., 2020A&A...640A...1C 2020A&A...640A...1C, Cat. J/A+A/640/A1
CJ20 = Castro-Ginard et al., 2020A&A...635A..45C 2020A&A...635A..45C. Cat. J/A+A/635/A45
C22 = Castro-Ginard et al., 2022A&A...661A.118C 2022A&A...661A.118C. Cat. J/A+A/661/A118
D03 = Dutra et al., 2003A&A...400..533D 2003A&A...400..533D, Cat. J/A+A/400/533
D14 = Dias et al., 2014A&A...564A..79D 2014A&A...564A..79D, Cat. J/A+A/564/A79
F11 = Feigelson et al., 2011ApJS..194....9F 2011ApJS..194....9F, Cat. J/ApJS/194/9
H22 = Hao et al., 2022A&A...660A...4H 2022A&A...660A...4H, J/A+A/660/A4
H23 = Hunt & Reffert, 2023A&A...673A.114H 2023A&A...673A.114H, Cat. J/A+A/673/A114
K05 = Kharchenko et al., 2005A&A...440..403K 2005A&A...440..403K, Cat. J/A+A/440/403
K06 = Kronberger et al., 2006A&A...447..921K 2006A&A...447..921K, Cat. J/A+A/447/921
K13 = Kharchenko et al., 2013A&A...558A..53K 2013A&A...558A..53K, Cat. J/A+A/558/A53
K14 = Kuhn et al., 2014ApJ...787..107K 2014ApJ...787..107K, Cat. J/ApJ/787/107
O18 = Oliveira et al., 2018MNRAS.476..842O 2018MNRAS.476..842O
P11 = Preibisch et al., 2011A&A...530A..34P 2011A&A...530A..34P
S10 = Smith et al., 2010MNRAS.406..952S 2010MNRAS.406..952S
T21 = Tarricq et al., 2021A&A...647A..19T 2021A&A...647A..19T, Cat. J/A+A/647/A19
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- --- [Gaia DR3]
10- 28 I19 --- GaiaDR3 ? Gaia DR3 Designation
30- 59 A30 --- Name Star Name
61- 78 F18.14 deg RAdeg Gaia DR3 Right Ascension (ICRS)
at Ep=2016.0 (1)
80- 98 F19.15 deg DEdeg Gaia DR3 Declination (ICRS) at Ep=2016.0 (1)
100-120 F21.18 mas plx ? Offset corrected Gaia DR3 parallax (2)
122-141 F20.18 mas e_plx ? Gaia DR3 parallax error
143-158 F16.10 K Teff-esphs ? Gaia DR3 effective temperature, teff_esphs
160-180 A21 --- SpType ? Spectral type
182-200 A19 --- r_SpType Reference for spectral type
202 A1 --- Pop [C/D] Star part of clustered (C) or
distributed (D) population
204-205 A2 --- Selection High-mass star selection criteria (3)
--------------------------------------------------------------------------------
Note (1): Star [AHP2016] OBc 59 has no Gaia DR3 counterpart, the right ascension
and declination are taken from Alexander et al. (2016AJ....152..190A 2016AJ....152..190A).
Note (2): The parallax offset was calculated with the algorithm provided by
Lindegren et al. (2021A&A...649A...4L 2021A&A...649A...4L).
Note (3): Selection criteria code as follows:
L = literature
TD = temperature plus DBSCAN
T = temperature
--------------------------------------------------------------------------------
Acknowledgements:
Christiane Goeppl, cgoeppl(at)usm.uni-muenchen.de
(End) Patricia Vannier [CDS] 23-Jan-2025