J/AJ/164/25 Velocity data for 148590 stars in the Kepler field (Angus+, 2022)
The 3D Galactocentric Velocities of Kepler Stars; Marginalizing Over Missing
Radial Velocities.
Angus R., Price-Whelan A.M., Zinn J.C., Bedell M., Lu Y., Foreman-Mackey D.
<Astron. J., 164, 25 (2022)>
=2022AJ....164...25A 2022AJ....164...25A
ADC_Keywords: Milky Way; Stars, late-type; Proper motions; Radial velocities
Parallaxes, trigonometric; Optical
Keywords: Milky Way dynamics ; Late-type stars ; Solar neighborhood ;
Stellar properties ; Stellar ages
Abstract:
Precise Gaia measurements of positions, parallaxes, and proper motions
provide an opportunity to calculate 3D positions and 2D velocities
(i.e., 5D phase-space) of Milky Way stars. Where available,
spectroscopic radial velocity (RVel) measurements provide full 6D
phase-space information, however there are now and will remain many
stars without RV measurements. Without an RVel it is not possible to
directly calculate 3D stellar velocities; however, one can infer 3D
stellar velocities by marginalizing over the missing RV dimension. In
this paper, we infer the 3D velocities of stars in the Kepler field in
Cartesian Galactocentric coordinates (vx, vy, vz). We directly
calculate velocities for around a quarter of all Kepler targets, using
RV measurements available from the Gaia, LAMOST, and APOGEE
spectroscopic surveys. Using the velocity distributions of these stars
as our prior, we infer velocities for the remaining three quarters of
the sample by marginalizing over the RV dimension. The median
uncertainties on our inferred vx, vy, and vz velocities are around 4,
18, and 4km/s, respectively. We provide 3D velocities for a total of
148590 stars in the Kepler field. These 3D velocities could enable
kinematic age-dating, Milky Way stellar population studies, and other
scientific studies using the benchmark sample of well-studied Kepler
stars. Although the methodology used here is broadly applicable to
targets across the sky, our prior is specifically constructed from and
for the Kepler field. Care should be taken to use a suitable prior
when extending this method to other parts of the Galaxy.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 272 148590 Velocities and kinematic information for stars in
the Kepler field
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See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
I/352 : Distances to 1.47 billion stars in Gaia EDR3 (Bailer-Jones+, 2021)
V/117 : Geneva-Copenhagen Survey of Solar neighbourhood (Holmberg+, 2007)
V/130 : Geneva-Copenhagen Survey of Solar neighbourhood III (Holmberg+, 2009)
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJ/687/1264 : Age estimation for solar-type dwarfs (Mamajek+, 2008)
J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)
J/ApJ/821/93 : Rotation & Galactic kinematics of mid M dwarfs (Newton+, 2016)
J/AJ/153/257 : Comoving stars in Gaia DR1 (Oh+, 2017)
J/AJ/158/190 : Main sequence hot Jupiter hosts good astrometry (Hamer+, 2019)
J/AJ/157/231 : MLSDSS-GaiaDR2 sample of M and L dwarfs (Kiman+, 2019)
J/ApJ/878/21 : Vertical motions APOGEE & Gaia red clump stars (Ting+, 2019)
J/ApJS/245/34 : Abundances for 6 million stars from LAMOST DR5 (Xiang+, 2019)
J/AJ/160/90 : Stellar parameters for 13196 Kepler dwarfs (Angus+, 2020)
J/ApJ/888/43 : APOGEE-Kepler Cool Dwarf star ages (Claytor+, 2020)
J/ApJ/904/140 : Ruprecht 147 members & rot. for 5 other cl. (Curtis+, 2020)
J/AJ/161/189 : Gyro-kinematic ages for ∼30000 Kepler stars (Lu+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- Seq [0/148589] Sequential number identifier
8- 15 I8 --- KIC Kepler Input catalog identifier
17- 35 I19 --- Gaia Gaia EDR3 identifier
37- 43 F7.3 deg RAdeg [279/302] Gaia EDR3 right ascension (ICRS)
45- 49 F5.3 arcsec e_RAdeg [0.006/0.1] Uncertainty in RAdeg
51- 56 F6.3 deg DEdeg [36/53] Gaia EDR3 declination (ICRS)
58- 62 F5.3 arcsec e_DEdeg [0.007/0.1] Uncertainty in DEdeg
64- 69 F6.3 mas plx [0.09/18.6] Gaia EDR3 parallax
71- 75 F5.3 mas e_plx [0.007/0.1] Uncertainty in plx
77- 83 F7.1 pc Dist [53/18256]? Distance;
Bailer-Jones+, 2021, I/352
85- 91 F7.1 pc b_Dist [53/14207]? Lower bound on Dist
93- 99 F7.1 pc B_Dist [53/23570]? Upper bound on Dist
101-107 F7.3 mas/yr pmRA [-37.7/40.3] Gaia EDR3 proper motion in RA
109-115 F7.3 mas/yr e_pmRA [-38/41] Uncertainty in pmRA
117-123 F7.3 mas/yr pmDE [-39.2/38.7] Gaia EDR3 proper motion in DE
125-131 F7.3 mas/yr e_pmDE [-40/39] Uncertainty in pmDE
133-138 F6.1 km/s RVel-DR2 [-393/107]? Gaia DR2 radial velocity
140-143 F4.1 km/s e_RVel-DR2 [0.1/20]? Uncertainty in RVel-DR2
145-153 F9.4 km/s RVel-apo [-589/71]? APOGEE DR16 radial velocity
155-160 F6.4 km/s e_RVel-apo [0.0005/2]? Uncertainty in RVel-apo
162-169 F8.3 km/s RVel-lam [-403.0/94.0]? LAMOST DR5 radial velocity
171-174 F4.1 km/s e_RVel-lam [1/89]? Uncertainty in RVel-lam
176-182 F7.2 km/s vx-calc [-838/1421]? vx velocity calculated using RVel
184-189 F6.1 km/s vx-inf [-307/387] vx velocity sample, inferred
without RVel
191-194 F4.1 km/s e_vx-inf [2/18] Standard deviation of vx
196-202 F7.2 km/s vy-calc [-312/621]? vy velocity calculated using RVel
204-208 F5.1 km/s vy-inf [115/289] vy velocity sample, inferred without
RVel
210-213 F4.1 km/s e_vy-inf [20/26] Standard deviation of vy
215-221 F7.2 km/s vz-calc [-714/1090]? zx velocity calculated using RVel
223-228 F6.1 km/s vz-inf [-192/194] vz velocity sample, inferred
without RVel
230-233 F4.1 km/s e_vz-inf [2/11] Standard deviation of vz
235-240 F6.2 --- vxvy [28/225] covariance between vx and vy samples
242-247 F6.2 --- vxvz [-25/97] covariance between vx and vz samples
249-253 F5.2 --- vxlnd [-0.6/2] covariance between vx and
ln(distance) samples
255-260 F6.2 --- vyvz [54.3/206] covariance between vy & vz samples
262-266 F5.2 --- vylnd [-0.35/0.16] covariance between vy and
ln(distance) samples
268-272 F5.2 --- vzlnd [-0.38/0.35] covariance between vz and
ln(distance) samples
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 21-Oct-2022