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Precise distances, masses, ages and 3D velocities of ~140000 red clump stars

We present a sample of $\sim$\,140,000 primary red clump (RC) stars of spectral signal-to-noise ratios higher than 20 from the LAMOST Galactic spectroscopic surveys, selected based on their positions in the metallicity-dependent effective temperature--surface gravity and color--metallicity diagrams, supervised by high-quality $Kepler$ asteroseismology data. The stellar masses and ages of those stars are further determined from the LAMOST spectra, using the Kernel Principal Component Analysis method, trained with thousands of RCs in the  LAMOST-$Kepler$ fields with accurate asteroseismic mass measurements.   The purity and completeness of our primary RC sample are generally higher than 80\,per cent. For the mass and age, a variety of tests show typical uncertainties of 15 and 30\,per cent, respectively. Using over ten thousand primary RCs with accurate distance measurements from the parallaxes of Gaia\,DR2, we re-calibrate the $K_{\rm s}$ absolute magnitudes of primary RCs by, for the first time, considering both the metallicity and age dependencies. With the the new calibration, distances are derived for all the primary RCs, with a typical uncertainty of 5--10\,per cent,  even better than the values yielded by the Gaia parallax measurements for stars beyond 3--4\,kpc. The sample covers a significant volume of the Galactic disk of $4\,\leq\,R\,\leq\,16$\,kpc, $|Z|\,\leq\,5$\,kpc, and $-20\,\leq\,\phi\,\leq\,50^{\circ}$. Stellar atmospheric parameters, line-of-sight velocities and elemental abundances derived from the LAMOST spectra and proper motions of Gaia\,DR2 are also provided for the sample stars. Finally, the selection function of the sample is carefully evaluated in the color-magnitude plane for different sky areas. Details about the table:   RA: Right ascension (degrees)   DEC: Declination (degrees)   GLON: Galactic longitude l (degrees)   GLAT: Galactic latitude b (degrees)   RV: Line-of-sight velocity (km/s)   ERR_RV: Uncertainty of line-of-sight velocity (km/s)   TEFF: Effective temperature (K)   ERR_TEFF: Uncertainty of effective temperature (K)    LOGG: Surface gravity    ERR_LOGG: Uncertainty of surface gravity    FEH: Metallicity    ERR_FEH: Uncertainty of metallicity    AFE: Alpha-to-iron abundance    ERR_AFE: Uncertainty of apha-to-iron abundance    AGE: Stellar age (Gyr)    ERR_AGE: Uncertainty of stellar age (Gyr)    MASS: Stellar mass (solar mass)    ERR_MASS: Uncertainty of stellar mass (solar mass)    J: 2MASS J band magnitude    ERR_J: Uncertainty of 2MASS J band magnitude    H: 2MASS H band magnitude    ERR_H: Uncertainty of 2MASS H band magnitude    KS: 2MASS Ks band magnitude    ERR_KS: Uncertainty of 2MASS Ks band magnitude    G: Gaia DR2 G band magnitude    ERR_G: Uncertainty of Gaia DR2 G band magnitude    BP: Gaia DR2 BP band magnitude    ERR_BP: Uncertainty of Gaia DR2 BP band magnitude    RP: Gaia DR2 RP band magnitude    ERR_RP: Uncertainty of Gaia DR2 RP band magnitude    EBV: E (B - V) (mag)    MKS: Absolute magnitude in Ks band    DISTANCE: distance (kpc)    ERR_DISTANCE: Uncertainty of distance (kpc)    PARALLAX: Gaia DR2 parallax (mas)    ERR_PARALLAX: Uncertainty of Gaia DR2 parallax (mas)    PMRA: Proper motion in R.A. (mas/yr)    ERR_PMRA: Uncertainty of proper motion in R.A. (mas/yr)    PMDEC: Proper motion in Dec. (mas/yr)    ERR_PMDEC: Uncertainty of proper motion in Dec. (mas/yr)    F_CMD: Selection fraction in color-magnitude diagram

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28/100

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These five areas show where the dataset supports — or may limit — practical reuse.

Stewardship: 4
Harmonization: 4
Access: 16
Reuse readiness: 0
Engagement: 4