J/A+A/686/A42 Improving the open cluster census. III. (Hunt+, 2024)
Improving the open cluster census. III. Using cluster masses, radii, and
dynamics to create a cleaned open cluster catalogue.
Hunt E.L., Reffert S.
<Astron. Astrophys. 686, A42 (2024)>
=2024A&A...686A..42H 2024A&A...686A..42H (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Surveys ; Clusters, open ; Positional data ; Optical
Keywords: methods: data analysis - catalogs - astrometry -
open clusters and associations: general
Abstract:
The census of open clusters has exploded in size thanks to data from
the Gaia satellite. However, it is likely that many of these reported
clusters are not gravitationally bound, making the open cluster census
impractical for many scientific applications. We aim to test different
physically motivated methods for distinguishing between bound and
unbound clusters, using them to create a cleaned star cluster
catalogue. We derived completeness-corrected photometric masses for
6957 clusters from our earlier work. Then, we used these masses to
compute the size of the Roche surface of these clusters (their Jacobi
radius) and distinguish between bound and unbound clusters. We find
that only 5648 (79%) of the clusters from our previous catalogue are
compatible with bound open clusters, dropping to just 11% of clusters
within 250pc. Our catalogue contains 3530 open clusters in a more
strongly cut high-quality sample of objects. The moving groups in our
sample show different trends in their size as a function of age and
mass, suggesting that they are unbound and undergoing different
dynamical processes. Our cluster mass measurements constitute the
largest catalogue of Milky Way cluster masses to date, which we also
use for further science. Firstly, we inferred the mass- dependent
completeness limit of the open cluster census, showing that the census
is complete within 1.8∼kpc only for objects heavier than 230 MSun.
Next, we derived a completeness-corrected age and mass function for
our open cluster catalogue, including estimating that the Milky Way
contains a total of 1.3*105 open clusters, only ∼4% of which are
currently known. Finally, we show that most open clusters have mass
functions compatible with the Kroupa initial mass function. We
demonstrate Jacobi radii for distinguishing between bound and unbound
star clusters, and publish an updated star cluster catalogue with
masses and improved cluster classifications.
Description:
We propose three tables. Clusters: the main catalogue (Table 1).
Members: members of clusters in the main catalogue (Table 2).
Crossmatches: a table of all clusters crossmatched against with IDs
corresponding to clusters in the main catalogue.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
clusters.dat 1131 7167 Main catalogue (table 1)
members.dat 1197 1291929 Member stars of clusters (table 2)
crossma.dat 207 29956 All (non-)xmatched clusters
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
J/A+A/646/A104 : Improving the open cluster census. I. (Hunt+, 2021)
J/A+A/673/A114 : Improving the open cluster census. II. (Hunt+, 2023)
Byte-by-byte Description of file: clusters.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 20 A20 --- Name Main accepted cluster name
22- 25 I4 --- ID Internal cluster ID
27- 279 A253 --- AllNames Comma separated list of all cluster names
this object crossmatched against and all
name variants
281 A1 --- Type [omgdr] Estimated type of object (1)
283- 293 F11.8 --- CST [3/99] Astrometric SNR
(cluster significance test) (2)
295- 300 I6 --- N [10/153797] Number of member stars
302- 312 F11.8 --- CSTt [2.9/99] Astrometric SNR within
tidal radius
314- 318 I5 --- Nt [10/53464] Number of stars within
tidal radius
320- 331 F12.8 deg RAdeg Right ascension of densest point
(ICRS) at Ep=2016.0
333- 344 F12.8 deg DEdeg Declination of densest point
(ICRS) at Ep=2016.0
346- 357 F12.8 deg GLON Galactic longitude
359- 369 E11.4 deg GLAT Galactic latitude
371- 381 F11.8 deg r50 Radius containing 50% of members
within the tidal radius
383- 393 F11.8 deg rc Core radius (approximate estimate)
395- 405 F11.8 deg rt Tidal radius (approximate estimate)
407- 417 F11.8 deg rtot Total radius
(including tidal tails, coma, etc)
419- 431 F13.8 pc r50pc Radius containing 50% of members
in parsecs
433- 445 F13.8 pc rcpc Core radius in parsecs
447- 459 F13.8 pc rtpc Tidal radius in parsecs
461- 473 F13.8 pc rtotpc Total radius in parsecs
475- 487 F13.8 mas/yr pmRA Mean proper motion in right ascension
multiplied by cos(dec)
489- 499 F11.8 mas/yr s_pmRA Standard deviation of pmra
501- 510 F10.8 mas/yr e_pmRA Standard error of pmra
512- 523 F12.8 mas/yr pmDE Mean proper motion in declination
525- 535 F11.8 mas/yr s_pmDE Standard deviation of pmdec
537- 546 F10.8 mas/yr e_pmDE Standard error of pmdec
548- 559 F12.8 mas Plx Mean parallax
561- 571 F11.8 mas s_Plx Standard deviation of parallax
573- 582 F10.8 mas e_Plx Standard error of parallax
584- 598 F15.8 pc dist16 16th percentile of maximum likelihood
distance
600- 614 F15.8 pc dist50 50th percentile of maximum likelihood
distance
616- 631 F16.8 pc dist84 84th percentile of maximum likelihood
distance
633- 637 I5 --- Ndist Number of stars used for distance
calculation
639 I1 --- globalPlx [0/1] Flag indicating clusters for which
a star-by-star parallax offset correction
was not possible during distance
calculation
641- 656 F16.8 pc X X coordinate in heliocentric galactic
coordinates
658- 673 F16.8 pc Y Y coordinate in heliocentric galactic
coordinates
675- 690 F16.8 pc Z Z coordinate in heliocentric galactic
coordinates
692- 704 F13.8 km/s RV ? Mean Gaia DR3 radial velocity
706- 718 F13.8 km/s s_RV ? Standard deviation of radial velocity
720- 732 F13.8 km/s e_RV ? Standard error of radial velocity
734- 737 I4 --- n_RV Number of member stars with a radial
velocity
739- 747 E9.4 --- CMDCl2.5 [0/1] 2.5th percentile of CMD class
749- 757 E9.4 --- CMDCl16 [0/1] 16th percentile of CMD class
759- 768 F10.8 --- CMDCl50 [0/1] 50th percentile of CMD class
770- 779 F10.8 --- CMDCl84 [0/1] 84th percentile of CMD class
781- 790 F10.8 --- CMDCl97.5 [0/1] 97.5th percentile of CMD class
792- 794 A3 --- CMDClHuman Human-assigned CMD class
(where available) (3)
796- 806 F11.8 [yr] logAge16 ? 16th percentile of logarithm of
cluster age
808- 818 F11.8 [yr] logAge50 ? 50th percentile of logarithm of
cluster age
820- 831 F12.8 [yr] logAge84 ? 84th percentile of logarithm of
cluster age
833- 841 E9.4 mag AV16 ? 16th percentile of V-band
cluster extinction
843- 853 F11.8 mag AV50 ? 50th percentile of V-band
cluster extinction
855- 865 F11.8 mag AV84 ? 84th percentile of V-band
cluster extinction
867- 875 E9.4 mag diffAV16 ? 16th percentile of approximate V-band
differential extinction
877- 887 F11.8 mag diffAV50 ? 50th percentile of approximate V-band
differential extinction
889- 899 F11.8 mag diffAV84 ? 84th percentile of approximate V-band
differential extinction
901- 912 F12.8 mag MOD16 ? 16th percentile of photometrically
estimated distance modulus
914- 925 F12.8 mag MOD50 ? 50th percentile of photometrically
estimated distance modulus
927- 938 F12.8 mag MOD84 ? 84th percentile of photometrically
estimated distance modulus
940- 950 F11.8 deg r50J ? Radius containing 50% of members within
the best fitting Jacobi radius
952- 963 F12.8 deg rJ ? Best fitting Jacobi radius - still
defined even for clusters with low
Jacobi radius probability
965- 976 F12.8 pc r50Jpc ? Radius containing 50% of members within
the Jacobi radius in parsecs
978- 990 F13.8 pc rJpc ? Jacobi radius in parsecs
992-1001 E10.4 --- probJ ? Probability of the cluster having
a valid Jacobi radius
1003-1006 I4 --- NJ [9/4171]?=-1 Number of stars within
best-fit Jacobi radius
1008-1022 F15.8 Msun MassJ ? Cluster mass within the Jacobi radius
1024-1038 F15.8 Msun e_MassJ ? Error on cluster mass within the
Jacobi radius
1040-1054 F15.8 Msun MassTot ? Total observed cluster mass
1056-1070 F15.8 Msun e_MassTot ? Error on total observed cluster mass
1072-1073 I2 --- minClSize [-1/80] HDBSCAN parameter used to
construct cluster membership list
(-1 for membership lists not made with
HDBSCAN)
1075 I1 --- isMerged [0/1] Flag indicating manually merged
cluster membership list
1077 I1 --- isGMMMemb [0/1] Flag indicating cluster membership
list constructed using additional
Gaussian mixture model post-processing
step
1079-1080 I2 --- NXmatches [0/24] Number of unique crossmatches to
this cluster
1082-1097 A16 --- XmatchType Type of crossmatch (4)
1099-1131 A33 --- Note Reason why cluster was rejected
--------------------------------------------------------------------------------
Note (1): Estimated type of object as follows:
o = open cluster
m = moving group
g = globular cluster
d = too distant to classify
r = rejected - see Note column
Note (2): Set to 99 for clusters with an SNR greater than approximately 38
(due to numerical precision limit in our pipeline/scipy)
Note (3): Human-assigned CMD class as follows:
FP = false positive
FP? = false positive ?
TP = true positive
TP? = true positive ?
Note (4): Type of crossmatch as follows:
1:1 = one to one
1:m = one to many
m:1 = many to one
m:m = many to many
blank for new object
Names updated from Paper 1 are marked with +name_updated.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: members.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 I7 --- Seq Sequential number
9- 28 A20 --- Name Main accepted cluster name
30- 33 I4 --- ID Internal cluster ID
35- 53 I19 --- GaiaDR3 Gaia DR3 source ID
55 I1 --- inrj [0/1] Flag indicating if cluster is
within Jacobi radius (i.e. true tidal
radius from cluster mass)
57 I1 --- inrt [0/1] Flag indicating if cluster is
within estimated King
(1962AJ.....67..471K 1962AJ.....67..471K) tidal radius
based on cluster profile
59- 78 F20.18 --- Prob [0/1] Membership probability
80- 103 F24.20 deg RAdeg Right ascension of star (ICRS)
at Ep=2016.0
105- 125 F21.19 mas e_RAdeg Standard error on ra
127- 148 E22.16 deg DEdeg Declination of star (ICRS) at Ep=2016.0
150- 170 F21.19 mas e_DEdeg Standard error on dec
172- 195 F24.20 deg GLON Galactic longitude
197- 219 E23.17 deg GLAT Galactic latitude
221- 243 E23.17 mas/yr pmRA Mean proper motion in right ascension
multiplied by cos(dec)
245- 265 F21.19 mas/yr e_pmRA Standard error of pmRA
267- 289 E23.17 mas/yr pmDE Mean proper motion in declination
291- 310 F20.18 mas/yr e_pmDE Standard error of pmDE
312- 334 E23.17 mas Plx Mean parallax
336- 355 F20.18 mas e_Plx Standard error of parallax
357- 374 F18.16 um-1 pscol ? Estimated pseudocolour
376- 396 F21.19 um-1 e_pscol ? Standard error on pseudocolor
398- 420 E23.17 --- PlxpmRACor Correlation between parallax and pmra
422- 444 E23.17 --- PlxpmDECor Correlation between parallax and pmdec
446- 468 E23.17 --- pmRApmDECor Correlation between pmra and pmdec
470- 492 E23.17 --- PlxpscolCor ? Correlation between parallax and
pseudocolour
494- 516 E23.17 --- pmRApscolCor ? Correlation between pmra and
pseudocolour
518- 540 E23.17 --- pmDEpscolCor ? Correlation between pmdec and
pseudocolour
542- 543 I2 --- Solved [31/95] Gaia DR3 flag indicating which
parameters solved for
545- 568 F24.20 deg ELAT Ecliptic latitude
570- 587 F18.16 um-1 nueff ? Effective wavenumber of source used
in astrometric solution
589- 607 F19.16 --- RUWE Renormalised unit weight error
609- 626 F18.16 --- FidelityV1 Rybizki et al. (2022MNRAS.510.2597R 2022MNRAS.510.2597R)
V1 fidelity parameter
628- 652 F25.14 e-/s FG Mean G-band flux
654- 678 F25.17 e-/s e_FG Error on mean G-band flux
680- 705 F26.16 e-/s FBP Mean BP-band flux
707- 733 F27.18 e-/s e_FBP Error on mean BP- band flux
735- 759 F25.15 e-/s FRP Mean RP-band flux
761- 787 F27.18 e-/s e_FRP Error on mean RP- band flux
789- 807 F19.16 mag Gmag Mean G-band magnitude
809- 827 F19.16 mag BPmag Mean BP-band magnitude
829- 847 F19.16 mag RPmag Mean RP-band magnitude
849- 871 E23.17 mag BP-RP BP-RP colour
873- 895 E23.17 mag BP-G BP-G colour
897- 919 E23.17 mag G-RP G-RP colour
921- 942 E22.16 km/s RV ? Mean Gaia DR3 radial velocity
944- 963 F20.17 km/s e_RV ? Standard error of radial velocity
965- 967 F3.1 --- n_RV ? Method used to obtain the RV
969- 973 F5.1 --- o_RV ? Number of transits used to compute
the RV
975- 978 F4.1 --- o_RVd ? Number of transits that underwent
deblending
980- 998 F19.16 mag GRVSmag ? Mean Grvs magnitude
1000-1020 F21.19 mag e_GRVSmag ? Error on mean Grvs magnitude
1022-1026 F5.1 --- o_GRVSmag ? Number of transits used to construct
Grvs magnitude
1028-1047 F20.16 km/s Vbroad ? Spectral line broadening parameter
1049-1069 F21.17 km/s e_Vbroad ? Error on the spectral line broadening
1071-1074 F4.1 --- o_Vbroad ? Number of transits used to compute
vbroad
1076-1088 A13 --- VarFlag Gaia DR3 photometric variability flag
1090 I1 --- NSS [0/6] Flag indicating source has
additional information in the Gaia DR3
non single star tables
1092 I1 --- RVS [0/1] Flag indicating the availability
of mean RVS spectrum for this source
1094-1113 F20.17 Msun Mass2.5 ? 2.5th percentile of stellar mass for
this star, assuming star is single
1115-1134 F20.17 Msun Mass16 ? 16th percentile of stellar mass for
this star, assuming star is single
1136-1155 F20.17 Msun Mass50 ? 50th percentile of stellar mass for
this star, assuming star is single
1157-1176 F20.17 Msun Mass84 ? 84th percentile of stellar mass for
this star, assuming star is single
1178-1197 F20.17 Msun Mass97.5 ? 97.5th percentile of stellar mass for
this star, assuming star is single
--------------------------------------------------------------------------------
Byte-by-byte Description of file: crossma.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- ID ? Internal cluster ID (blank if object has
no crossmatched cluster in our work)
6- 26 A21 --- NameLit Name in literature catalogue
28- 43 A16 --- SourceCat Source catalogue reference (1)
45- 72 A28 --- TypeSourceCat Comma separated list of all source
catalogue crossmatch types for this
crossmatch
74- 83 E10.4 deg Sep [0/2]? Separation between cluster centres
85- 95 F11.8 --- SepTidal [0/0.94]? Separation in terms of largest
tidal radius
97-107 F11.8 --- SepTidalLit [0/1]? Separation in terms of literature
tidal radius
109-119 F11.8 --- SepTidalData [0/1]? Separation in terms of tidal radius
in this work
121-130 E10.4 mas/yr pmRASep [0/17.41]? Separation in pmRA times
cos(DE) between this work and literature
132-142 F11.8 --- pmRASigma ? pmRA separation in terms of uncertainty
on pmRA in this work and literature added
in quadrature
144-153 E10.4 mas/yr pmDESep [0/11.24]? Separation in pmDE between this
work and literature
155-164 E10.4 --- pmDESigma ? pmDE separation in terms of uncertainty
on pmRA in this work and literature
added in quadrature
166-175 E10.4 mas PlxSep [0/2.8]? Separation in parallax between
this work and literature
177-186 E10.4 --- PlxSigma ? Parallax separation in terms of
uncertainty on pmRA in this work and
literature added in quadrature
188-196 E9.3 --- maxSigma ? Maximum value of pmRASepSigma,
pmDESepSigma, and PlxSepSigma (must be
less than 2.0 for a valid astrometric
match)
198-207 E10.4 --- meanSigma ? Mean value of pmRASepSigma,
pmDESepSigma, and PlxSepSigma
--------------------------------------------------------------------------------
Note (1): References as follows:
Anders+22 = Anders et al., 2021A&A...645L...2A 2021A&A...645L...2A
Bastian+19 = Bastian et al., 2019MNRAS.489L..80B 2019MNRAS.489L..80B
Bica+08 = Bica et al., 2008MNRAS.389..678B 2008MNRAS.389..678B, Cat. J/MNRAS/389/678
Bica+18 = Bica et al., 2018
Cantat-Gaudin+20 = Cantat-Gaudin et al., 2020A&A...640A...1C 2020A&A...640A...1C,
Cat. J/A+A/640/A1
Casado+21 = Casado et al., 2021RAA....21..117C 2021RAA....21..117C
Casado+23 = Casado et al., 2023MNRAS.521.1399C 2023MNRAS.521.1399C
Castro-Ginard+20 = Castro-Ginard et al., 2020A&A...635A..45C 2020A&A...635A..45C,
Cat. J/A+A/635/A45
Castro-Ginard+22 = Castro-Ginard et al., 2022A&A...661A.118C 2022A&A...661A.118C,
Cat. J/A+A/661/A118
Chi+22 = Chi et al, 2022
Chi+23 = Chi et al, 2023ApJS..265...20C 2023ApJS..265...20C, Cat. J/ApJS/265/20
Dias+02 = Dias et al., 2002A&A...389..871D 2002A&A...389..871D, Cat. B/ocl
Ferreira+19 = Ferrrira et al., 2019MNRAS.483.5508F 2019MNRAS.483.5508F,
Cat. J/MNRAS/483/5508
Ferreira+20 = Ferreira et al., 2020MNRAS.496.2021F 2020MNRAS.496.2021F,
Cat. J/MNRAS/496/2021
Ferreira+21 = Ferreira et al., 2021MNRAS.502L..90F 2021MNRAS.502L..90F,
Cat. J/MNRAS/502/L90
Hao+20 = Hao et al., 2020PASP..132c4502H 2020PASP..132c4502H
Hao+22 = Hao et al., 2022A&A...660A...4H 2022A&A...660A...4H, Cat. J/A+A/660/A4
He+21 = He et al., 2021RAA....21...93H 2021RAA....21...93H, Cat. J/other/RAA/21.93
He+22a = He et al., 2022ApJS..260....8H 2022ApJS..260....8H, Cat. J/ApJS/260/8
He+22b = He et al., 2022ApJS..262....7H 2022ApJS..262....7H
He+22c = He et al., 2022MNRAS.517.5496Y 2022MNRAS.517.5496Y
Hunt+21 = Hunt et al., 2021A&A...646A.104H 2021A&A...646A.104H, Cat. J/A+A/646/A104
Jaehnig+21 = Jaehnig et al., 2021ApJ...923..129J 2021ApJ...923..129J, Cat. J/ApJ/923/129
Kharchenko+13 = Kharchenko et al., 2013A&A...558A..53K 2013A&A...558A..53K,
Cat. J/A+A/558/A53
Kounkel+20 = Kounkel et al., 2020
Kronberger+06 = Kronberger et al., 2020AJ....160..279K 2020AJ....160..279K, Cat. J/AJ/159/279
Li+22 = Li et al., 2022A&A...668A..13H 2022A&A...668A..13H, Cat. J/A+A/668/A13
Li+23 = Lui et al., 2023MNRAS.526.1075P 2023MNRAS.526.1075P
Liu+19 = Liu et al., 2019ApJS..245...32L 2019ApJS..245...32L, Cat. J/ApJS/245/32
Qin+20 = Qin et al., 2020
Qin+23 = Qin et al., 2023ApJS..265...12Q 2023ApJS..265...12Q, Cat. J/ApJS/265/12
Santos-Silva+21 = Santos-Silva et al., 2021MNRAS.508.1033S 2021MNRAS.508.1033S
Sim+19 = Sim et al., 2019JKAS...52...145S
Tian+20 = Tian et al., 2020ApJ...904..196T 2020ApJ...904..196T
Vasiliev+21 = Vasiliev et al., 2021MNRAS.505.5978V 2021MNRAS.505.5978V,
Cat. J/MNRAS/505/5978
Zari+18 = Zari et al., 2018A&A...620A.172Z 2018A&A...620A.172Z, Cat. J/A+a/620/A172
--------------------------------------------------------------------------------
Acknowledgements:
Emily Hunt, ehunt(at)lsw.uni-heidelberg.de
References:
Hunt & Reffert, Paper I 2021A&A...646A.104H 2021A&A...646A.104H, Cat. J/A+A/646/A104
Hunt & Reffert, Paper II 2023A&A...673A.114H 2023A&A...673A.114H, Cat. J/A+A/673/A114
(End) Patricia Vannier [CDS] 08-Mar-2024