J/other/Nat/631.49 Nearby young star clusters (Swiggum+, 2024)
Most nearby young star clusters formed in three massive complexes.
Swiggum C., Alves J., Benjamin R., Ratzenbock S., Miret-Roig N.,
Grossschedl J., Meingast S., Goodman A., Konietzka R., Zucker C.,
Hunt E.L., Reffert S.
<Nature, 631, 49 (2024)>
=2024Natur.631...49S 2024Natur.631...49S (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Optical ; Morphology ;
Space velocities
Abstract:
Efforts to unveil the structure of the local interstellar medium and
its recent star-formation history have spanned the past 70 years.
Recent studies using precise data from space astrometry missions have
revealed nearby, newly formed star clusters with connected origins.
Nonetheless, mapping young clusters across the entire sky back to
their natal regions has been hindered by a lack of clusters with
precise radial-velocity data. Here we show that 155 out of 272 (57%)
high-quality young clusters within 1 kiloparsec of the Sun arise from
three distinct spatial volumes. This conclusion is based on the
analysis of data from the third Gaia release and other large-scale
spectroscopic surveys. At present, dispersed throughout the solar
neighbourhood, their past positions more than 30 million years ago
reveal that these families of clusters each formed in one of three
compact, massive star-forming complexes. One of these families
includes all of the young clusters near the Sun - the Taurus and
Scorpius-Centaurus star-forming complexes. We estimate that more than
200 supernovae were produced from these families and argue that these
clustered supernovae produced both the Local Bubble18 and the largest
nearby supershell GSH 238+00+09, both of which are clearly visible in
modern three-dimensional dust maps.
Description:
We have used a recently published star cluster catalogue (Hunt &
Reffert, 2023A&A...673A.114H 2023A&A...673A.114H, Cat. J/A+A/673/A114) to create a sample
of 254 high-quality, young (<70Myr old) clusters within approximately
1kpc of the Sun, supplemented with a further set of 18 young local
associations (Gagne et al. 2018ApJ...856...23G 2018ApJ...856...23G, Cat. J/ApJ/856/23)
(YLAs), which are low-mass, comoving associations of stars located
within 200 parsec (pc) of the Sun.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 1675 272 *Table of 272 clusters constructed and
analysed in this work
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Note on table.dat: 64 first parameters (Name to XmatchType) from Hunt & Reffert
(2023A&A...673A.114H 2023A&A...673A.114H, Cat. J/A+A/673/A114).
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See also:
J/ApJ/856/23 : BANYAN. XI. The BANYAN Σ algorithm (Gagne+, 2018)
J/A+A/673/A114 : Improving the open cluster census. II. (Hunt+, 2023)
Byte-by-byte Description of file: table.dat
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Bytes Format Units Label Explanations
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1- 22 A22 --- Name Main accepted cluster name
24- 29 F6.1 --- ID ? Internal cluster ID
31- 155 A125 --- AllNames Comma separated list of all crossmatched
cluster names
157- 159 A3 --- Type [omg ] Type of object (o open cluster,
m moving group, g: globular cluster)
161- 179 F19.16 --- CST ? Astrometric SNR
(cluster significance test) (1)
181- 184 I4 --- N Number of member stars
186- 203 F18.15 --- CSTt ? Astrometric SNR within
tidal radius (1)
205- 209 F5.1 --- Nt ? Number of stars within
tidal radius
211- 230 F20.16 deg RAdeg ? Right ascension of densest point
(ICRS) at Ep=2016.0
232- 251 F20.16 deg DEdeg ? Declination of densest point
(ICRS) at Ep=2016.0
253- 272 F20.16 deg GLON ? Galactic longitude
274- 293 F20.16 deg GLAT ? Galactic latitude
295- 313 F19.16 deg r50 ? Radius containing 50% of members within
the tidal radius
315- 333 F19.16 deg rc ? Core radius (approximate estimate)
335- 353 F19.16 deg rt ? Tidal radius (approximate estimate)
355- 373 F19.16 deg rtot ? Total radius
(including tidal tails, coma, etc)
375- 393 F19.16 pc r50pc ? Radius containing 50% of members
395- 413 F19.16 pc rcpc ? Core radius in parsecs
415- 433 F19.16 pc rtpc ? Tidal radius in parsecs
435- 454 F20.16 pc rtotpc ? Total radius in parsecs
456- 475 F20.16 mas/yr pmRA ? Mean proper motion in right ascension
multiplied by cos(dec)
477- 494 F18.16 mas/yr s_pmRA ? Standard deviation of pmRA
496- 513 F18.16 mas/yr e_pmRA ? Standard error of pmRA
515- 534 F20.16 mas/yr pmDE ? Mean proper motion in declination
536- 553 F18.16 mas/yr s_pmDE ? Standard deviation of pmDE
555- 572 F18.16 mas/yr e_pmDE ? Standard error of pmDE
574- 592 F19.16 mas Plx ? Mean parallax
594- 611 F18.16 mas s_Plx ? Standard deviation of parallax
613- 630 F18.16 mas e_Plx ? Standard error of parallax
632- 650 F19.14 pc dist16 ? 16th percentile of maximum likelihood
distance
652- 670 F19.14 pc dist50 ? 50th percentile of maximum likelihood
distance
672- 690 F19.14 pc dist84 ? 84th percentile of maximum likelihood
distance
692- 696 F5.1 --- Ndist ? Number of stars used for distance
calculation
698- 704 A7 --- globalPlx Flag indicating clusters for which a
star-by-star parallax offset correction
was not possible during distance
calculation
706- 724 F19.13 pc X ? X coordinate in galactocentric galactic
coordinates
726- 746 F21.16 pc Y ? Y coordinate in galactocentric galactic
coordinates
748- 768 F21.16 pc Z ? Z coordinate in galactocentric galactic
coordinates
770- 789 F20.16 km/s RV ? Mean Gaia DR3 radial velocity
791- 810 F20.16 km/s s_RV ? Standard deviation of radial velocity
812- 830 F19.16 km/s e_RV ? Standard error of radial velocity
832- 836 F5.1 --- n_RV ? Number of member stars with a
radial velocity
838- 855 F18.16 --- CMDCl2.5 [0/1]? 2.5th percentile of CMD class
857- 874 F18.16 --- CMDCl16 [0/1]? 16th percentile of CMD class
876- 893 F18.16 --- CMDCl50 [0/1]? 50th percentile of CMD class
895- 912 F18.16 --- CMDCl84 [0/1]? 84th percentile of CMD class
914- 931 F18.16 --- CMDCl97.5 [0/1]? 97.5th percentile of CMD class
933- 936 A4 --- CMDClHuman Human-assigned CMD class
(where available) (2)
938- 955 F18.16 [yr] logAge16 ? 16th percentile of logarithm of
cluster age
957- 974 F18.16 [yr] logAge50 ? 50th percentile of logarithm of
cluster age
976- 993 F18.16 [yr] logAge84 ? 84th percentile of logarithm of
cluster age
995-1016 E22.17 mag AV16 ? 16th percentile of V-band cluster
extinction
1018-1035 F18.16 mag AV50 ? 50th percentile of V-band cluster
extinction
1037-1054 F18.16 mag AV84 ? 84th percentile of V-band cluster
extinction
1056-1077 E22.17 mag diffAV16 ? 16th percentile of approximate V-band
differential extinction
1079-1096 F18.16 mag diffAV50 ? 50th percentile of approximate V-band
differential extinction
1098-1115 F18.16 mag diffAV84 ? 84th percentile of approximate V-band
differential extinction
1117-1135 F19.16 mag MOD16 ? 16th percentile of photometrically
estimated distance modulus
1137-1155 F19.16 mag MOD50 ? 50th percentile of photometrically
estimated distance modulus
1157-1175 F19.16 mag MOD84 ? 84th percentile of photometrically
estimated distance modulus
1177-1180 F4.1 --- minClSize ? HDBSCAN parameter used to construct
cluster membership list
(-1 for membership lists not made with
HDBSCAN)
1182-1188 A7 --- isMerged Flag indicating manually merged
cluster membership list
1190-1196 A7 --- isGMMMemb Flag indicating cluster membership list
constructed using additional Gaussian
mixture model post-processing step
1198-1200 F3.1 --- NXmatches ? Number of unique crossmatches to
this cluster
1202-1206 A5 --- XmatchType Type of crossmatch (3)
1208-1214 A7 --- dataSource Indicates original catalog source
1216-1230 A15 ---- Family Assigned cluster family
1232-1250 F19.16 Myr Age Age of cluster
1252-1271 F20.16 km/s RVcomb ? Median cluster RV from gaia/apogee/galah
1273-1293 F21.16 pc Xhelio Heliocentric x position
1295-1315 F21.16 pc Yhelio Heliocentric y position
1317-1337 F21.16 pc Zhelio Heliocentric z position
1339-1358 F20.16 km/s U Heliocentric U velocity
1360-1380 F21.16 km/s V Heliocentric V velocity
1382-1401 F20.16 km/s W Heliocentric W velocity
1403-1421 F19.16 pc e_Xhelio Error in x_helio
1423-1443 E21.17 pc e_Yhelio Error in y_helio
1445-1463 F19.16 pc e_Zhelio Error in z_helio
1465-1482 F18.16 km/s e_U Error in U
1484-1501 F18.16 km/s e_V Error in V
1503-1520 F18.16 km/s e_W Error in W
1522-1526 F5.1 --- nRVcomb ? number of RVs
1528-1547 F20.15 Msun Mass16 ? 16th percentile cluster mass estimate
1549-1568 F20.15 Msun Mass50 ? 50th percentile cluster mass estimate
1570-1589 F20.15 Msun Mass84 ? 84th percentile cluster mass estimate
1591-1594 F4.1 --- nSNe16 ? 16th percentile number of SNe
1596-1599 F4.1 --- nSNe50 ? 50th percentile number of SNe
1601-1604 F4.1 --- nSNe84 ? 84th percentile number of SNe
1606-1609 F4.1 --- nsg8M16 ? 16th percentile number of stars
greater than 8Msun
1611-1614 F4.1 --- nsg8M50 ? 50th percentile number of stars
greater than 8Msun
1616-1619 F4.1 --- nsg8M84 ? 84th percentile number of stars
greater than 8Msun
1621-1638 F18.16 --- Weightsc Average weight score assigned to cluster
1640-1675 A36 --- NameBoth Names of clusters; separated by
a / if two names are given
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Note (1): set to 99 for clusters with an SNR greater than approximately 38
(due to numerical precision limit in our pipeline/scipy).
Note (2): Human-assigned CMD class as follows:
FP = false positive
FP? = false positive ?
TP = true positive
TP? = true positive ?
Note (3): 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
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Aug-2024