J/ApJ/903/55 APOGEE parameters through 83 open clusters (Poovelil+, 2020)
Open Cluster Chemical Homogeneity throughout the Milky Way.
Poovelil, Poovelil V.J., Zasowski G., Hasselquist S., Seth A., Donor J.,
Beaton R.L., Cunha K., Frinchaboy P.M., Garcia-Hernandez D.A., Hawkins K.,
Kratter K.M., Lane R.R., Nitschelm C.
<Astrophys. J., 903, 55 (2020)>
=2020ApJ...903...55P 2020ApJ...903...55P
ADC_Keywords: Milky Way; Clusters, open; Spectra, infrared; Proper motions;
Radial velocities; Stars, ages
Keywords: Chemical enrichment ; Chemical abundances ; Star clusters ;
Milky Way evolution
Abstract:
The chemical homogeneity of surviving stellar clusters contains
important clues about interstellar medium (ISM) mixing efficiency,
star formation, and the enrichment history of the Galaxy. Existing
measurements in a handful of open clusters suggest homogeneity in
several elements at the 0.03dex level. Here we present (I) a new
cluster member catalog based only on APOGEE radial velocities and
Gaia-DR2 proper motions, (II) improved abundance uncertainties for
APOGEE cluster members, and (III) the dependence of cluster
homogeneity on Galactic and cluster properties, using abundances of
eight elements from the APOGEE survey for 10 high-quality clusters. We
find that cluster homogeneity is uncorrelated with Galactocentric
distance, |Z|, age, and metallicity. However, velocity dispersion,
which is a proxy for cluster mass, is positively correlated with
intrinsic scatter at relatively high levels of significance for
[Ca/Fe] and [Mg/Fe]. We also see a possible positive correlation at a
low level of significance for [Ni/Fe], [Si/Fe], [Al/Fe], and [Fe/H],
while [Cr/Fe] and [Mn/Fe] are uncorrelated. The elements that show a
correlation with velocity dispersion are those that are predominantly
produced by core-collapse supernovae (CCSNe). However, the small
sample size and relatively low correlation significance highlight the
need for follow-up studies. If borne out by future studies, these
findings would suggest a quantitative difference between the
correlation lengths of elements produced predominantly by Type Ia SNe
versus CCSNe, which would have implications for Galactic chemical
evolution models and the feasibility of chemical tagging.
Description:
We adopted stellar parameters, chemical abundances, and radial
velocities from the Apache Point Observatory Galactic Evolution
Experiment (APOGEE). APOGEE, one of the component surveys of the Sloan
Digital Sky Survey IV (SDSS-IV), is a high-resolution, near-infrared
spectroscopic survey of ∼500000 stars across the Milky Way.
Observations are taken with two custom-built, 300 fiber spectrographs,
one at the 2.5m Sloan Telescope at the Apache Point Observatory and
one at the 2.5m du Pont Telescope at Las Campanas Observatory. We use
data from the 16th SDSS data release.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 77 12296 Table of cluster members selected using our
membership selection
table2.dat 204 83 *Catalog clusters
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Note on table2.dat: Position, radius, age taken from
Kharchenko+, 2013, J/A+A/558/A53.
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/A+A/438/1163 : Catalogue of Open Cluster Data (COCD) (Kharchenko+, 2005)
J/MNRAS/374/399 : Infrared star clusters with |b|<20° (Froebrich+, 2007)
J/AJ/136/118 : Open clusters as galactic disk tracers. I. (Frinchaboy+, 2008)
J/AJ/138/159 : NGC 6819 stellar radial-velocity and photometry (Hole+, 2009)
J/MNRAS/415/563 : Elemental abundances in Hyades supercluster (De Silva+, 2011)
J/AJ/141/58 : NGC 2204 and NGC 2243 red giant abundances (Jacobson+, 2011)
J/AJ/142/59 : Chemical abundance in 10 open clusters (Jacobson+, 2011)
J/A+A/558/A53 : Milky Way global survey star clusters. II. (Kharchenko+, 2013)
J/AJ/146/133 : Stellar parameters from SDSS-III APOGEE DR10 (Meszaros+, 2013)
J/AJ/146/43 : WIYN open cluster study. LV. NGC 6819 (Platais+, 2013)
J/AJ/149/121 : WOCS. LXV. Abundances in NGC 6819 (Lee-Brown+, 2015)
J/AJ/151/144 : ASPCAP weights for 15 APOGEE chemical elements (Garcia+, 2016)
J/A+A/594/A43 : APOGEE/Kepler sample stars abundances (Hawkins+, 2016)
J/MNRAS/463/696 : M67 solar twins chemical compositions (Liu+, 2016)
J/A+A/618/A93 : Gaia DR2 open clusters in the Milky Way (Cantat-Gaudin+, 2018)
J/AJ/156/142 : Precision cluster abund. APOGEE using SDSS DR14 (Donor+, 2018)
J/AJ/156/126 : Stellar parameters & abund. BACCHUS analysis (Jonsson+, 2018)
J/A+A/629/A34 : APOGEE stars members of 35 star clusters (Garcia-Dias+, 2019)
J/AJ/158/122 : Local structure & star formation history of MW (Kounkel+, 2019)
J/A+A/628/A54 : Fe, Mg, Ti in Galactic clusters (Kovalev+, 2019)
J/AJ/159/199 : OCCAM. IV. Open cluster abundances APOGEE DR16 (Donor+, 2020)
J/A+A/638/A76 : StarHorse data for 5 surveys (Queiroz+, 2020)
J/AJ/159/19 : SOAR TESS survey. I. (Ziegler+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Cluster Name of cluster
19- 36 A18 --- APOGEE APOGEE identifier
38- 47 F10.6 deg RAdeg [0.002/360] Right Ascension of star (J2000)
49- 58 F10.6 deg DEdeg [-63.7/86.4] Declination of star (J2000)
60- 64 F5.2 --- NRV [0/38.6]? Number of σ, Radial Velocity (1)
66- 70 F5.2 --- NPM [0.01/38.6]? Number of σ, Proper Motion (1)
72- 77 F6.2 arcmin Dist [0.15/371.84] Distance to cluster center
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Note (1): Number of σ from the cluster membership distribution function
in radial velocity or proper motion.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Cluster Name of cluster
19- 28 F10.6 deg RAdeg [6.41/360] Right Ascension, cluster center
(J2000)
30- 39 F10.6 deg DEdeg [-63.5/85.3] Declination, cluster center
(J2000)
41- 46 F6.2 arcmin Radius [3.6/186.0] Adopted cluster radius
48- 51 F4.2 kpc Dist [0.17/8.63] Median spectrophotometric distance
(1)
53- 56 F4.2 kpc e_Dist [0/2.7] Dispersion of distance
58- 62 F5.3 [yr] Age [6/9.7] Log(age) of cluster
64- 68 F5.3 [yr] e_Age [0/0.2] Uncertainty in log(age) of cluster
70- 75 F6.3 [-] [M/H] [-0.47/0.35] Mean [M/H] of cluster members
77- 81 F5.3 [-] e_[M/H] [0/0.47] Standard deviation of [M/H]
83- 88 F6.2 km/s RVel [-97.8/92.1] Mean of best-fit Gaussian to RVs
90- 93 F4.2 km/s e_RVel [0.2/6] Standard deviation of RVel
95- 98 F4.2 km/s ARVel [0.01/0.22] Amplitude of best-fit Gaussian to
Radial velocities
100-105 F6.2 mas/yr pmRA [-10.98/4.29] Mean proper motion in RA of
best-fit Gaussian to pmRA*pmDE
107-111 F5.2 mas/yr pmDE [-8.76/5.5] Mean proper motion in DE of
best-fit Gaussian to pmRA*pmDE
113-117 F5.2 mas/yr e_pmRA [-0.7/4.4] Standard deviation in pmRA
119-123 F5.2 mas/yr e_pmDE [-0.7/5.9] Standard deviation in pmDE
125-129 F5.2 --- Apm [-0.05/0.25] Amplitude of best-fit Gaussian to
pmRA*pmDE
131-136 F6.2 rad Rpm [-24.7/17.4] Rotation angle of Gaussian fit to
pmRA*pmDE
138-143 F6.3 --- Spm [-0.14/1.46] Scale of annular PM distribution
145-150 F6.2 --- ARV/e [9.6/210]? RVel Amplitude over residual
(σresidual)
152-154 I3 --- Nmem [4/381] Number of selected cluster members
156-159 A4 --- Flag Validation flag for the cluster (2)
161-166 F6.3 [-] [Mg/Fe] [-0.12/0.2] Mean [Mg/Fe] of cluster members
168-172 F5.3 [-] e_[Mg/Fe] [0/0.3] Standard deviation of [Mg/Fe]
174-178 F5.3 kpc Z [0.003/1.34] Vertical distance from the
Milky Way disc
180-184 F5.2 kpc Rgc [1.39/13.4] Galactocentric distance of cluster
186-190 F5.2 kpc e_Rgc [-1.8/1.3] Uncertainty in R GC
192-197 F6.3 kpc 3Dvel [0.64/50.1] 3D velocity dispersion
199-204 F6.3 kpc e_3Dvel [0.03/13] Uncertainty in 3Dvel
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Note (1): Median spectrophotometric distance of cluster members from
Rojas-Arriagada+, 2017A&A...601A.140R 2017A&A...601A.140R.
Note (2): Flags as follows:
GOOD = Clusters that have distinct kinematics (ARV/σresid>9.5;
Section 3.1.2) and metallicity dispersion less than 0.13 dex.
(34 occurrences)
INSU = (Insufficient data) Clusters that have distinct kinematics
(ARV/σresid>9.5; Section 3.1.2) but fewer than 5 cluster
members, making it difficult to interpret the diagnostic CMD and MDF
distributions (11 occurrences)
WARN = Clusters that have distinct kinematics (ARV/σresid>9.5;
Section 3.1.2) and metallicity dispersion greater than 0.13dex.
(38 occurrences)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 31-Jan-2022