J/ApJ/929/33 Chemical & kinematic data of giants from APOGEE & Gaia (Hu+, 2022)
Quantifying chemical and kinematical properties of Galactic disks.
Hu G., Shao Z.
<Astrophys. J., 929, 33 (2022)>
=2022ApJ...929...33H 2022ApJ...929...33H
ADC_Keywords: Milky Way; Stars, giant; Stars, halo; Abundances;
Radial velocities; Space velocities
Keywords: Milky Way Galaxy ; Milky Way disk ; Milky Way evolution ;
Milky Way formation ; Milky Way dynamics ; Galaxy structure ;
Galaxy kinematics ; Astronomy data analysis ; Stellar abundances
Abstract:
We aim to quantify the chemical and kinematical properties of Galactic
disks with a sample of 119,558 giant stars having abundances and 3D
velocities taken or derived from the APOGEE DR17 and Gaia EDR3
catalogs. A Gaussian mixture model is employed to distinguish the
high-α and low-α sequences along the metallicity by
simultaneously using chemical and kinematical data. Four disk
components are identified and quantified; they are named the
hαmp, hαmr, lαmp, and lαmr disks and
correspond to the high-α or low-α, and metal-poor or
metal-rich properties. Combined with the spatial and stellar-age
information, we confirm that they are well interpreted by the
two-infall formation model. The first infall of turbulent gas quickly
forms the hot and thick hαmp disk with consequent thinner
hαmr and lαmr disks. Then the second gas accretion forms a
thinner and outermost lαmp disk. We find that the inside-out and
upside-down scenario does not only satisfy the overall Galactic disk
formation of these two major episodes but is also presented in the
formation sequence of the three inner disks. Importantly, we reveal
the inverse age-[M/H] trend of the lαmr disk, which means its
younger stars are more metal-poor, indicating that the rejuvenated gas
from the second accretion gradually dominates later star formation.
Meanwhile, the recently formed stars converge to [M/H]~-0.1dex,
demonstrating a sufficient mixture of gas from two infalls.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 81 119558 Chemical and kinematical data and membership
probability of sample stars
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See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
V/154 : Sloan Digital Sky Surveys (SDSS), Release 16 (DR16) (Ahumada+, 2020)
I/352 : Distances to 1.47 billion stars in Gaia EDR3 (Bailer-Jones+, 2021)
III/286 : APOGEE-2 DR17 final allStar catalog (Abdurro'uf+, 2022)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
J/A+A/410/527 : Abundances in the Galactic disk (Bensby+, 2003)
J/A+A/438/139 : Abundances in Milky Way's disk (Soubiran+, 2005)
J/MNRAS/367/1329 : Elemental abundances for 176 stars (Reddy+, 2006)
J/ApJS/168/297 : Stellar parameters of nearby cool stars (Takeda+, 2007)
J/A+A/511/L10 : Abundances and space velocities of 94 stars (Nissen+, 2010)
J/A+A/525/A90 : Thick disc vertical properties (Katz+, 2011)
J/A+A/535/A107 : Spectroscopic survey of thick disc stars (Kordopatis+, 2011)
J/A+A/562/A71 : Abundances of solar neighbourhood dwarfs (Bensby+, 2014)
J/MNRAS/476/5216 : Thick disc probability of GALAH stars (Duong+, 2018)
J/ApJS/239/32 : APOKASC-2 cat. of Kepler evolved stars (Pinsonneault+, 2018)
J/MNRAS/489/2079 : Calibration of distances with deep learning (Leung+, 2019)
J/MNRAS/489/176 : Dynamical heating across the MW disc (Mackereth+, 2019)
J/A+A/643/A106 : 55 close-in (P<100days) small planets list (Bashi+, 2020)
J/A+A/645/A85 : Age dissection of the Milky Way discs (Miglio+, 2021)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- APOGEE APOGEE DR17 object name
21- 39 I19 --- Gaia Gaia EDR3 source identifier
41- 46 F6.3 [-] [a/M] [-0.22/0.5] APOGEE DR17 α abundance,
[α/M]
48- 53 F6.3 [-] [M/H] [-2.25/0.54] APOGEE DR17 metal abundance
to hydrogen
55- 60 F6.1 km/s VR [-444.5/373.5] Radial velocity component, VR
62- 67 F6.1 km/s VT [-299.2/344.8] Tangential velocity component,
Vφ
69- 74 F6.1 km/s VZ [-352.7/286.8] Azimuthal velocity component, VZ
76- 76 I1 --- K [1/2] Number of Gaussian components
78- 81 F4.2 --- phia [0/1]? Probability, high-α sequence;
section 4.3.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 05-Mar-2024