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.<br> 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. <br> The purity and completeness of our primary RC sample are generally higher than 80\,per cent.<br> For the mass and age, a variety of tests show typical uncertainties of 15 and 30\,per cent, respectively.<br> 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.<br> 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.<br> The sample covers a significant volume of the Galactic disk of $4\,\leq\,R\,\leq\,16$\,kpc, $|Z|\,\leq\,5$\,kpc, and $-20\,\leq\,\phi\,\leq\,50^{\circ}$.<br> 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.<br> 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)<br> DEC: Declination (degrees)<br> GLON: Galactic longitude l (degrees)<br> GLAT: Galactic latitude b (degrees)<br> RV: Line-of-sight velocity (km/s)<br> ERR_RV: Uncertainty of line-of-sight velocity (km/s)<br> TEFF: Effective temperature (K)<br> ERR_TEFF: Uncertainty of effective temperature (K)<br> LOGG: Surface gravity<br> ERR_LOGG: Uncertainty of surface gravity<br> FEH: Metallicity<br> ERR_FEH: Uncertainty of metallicity<br> AFE: Alpha-to-iron abundance<br> ERR_AFE: Uncertainty of apha-to-iron abundance<br> AGE: Stellar age (Gyr)<br> ERR_AGE: Uncertainty of stellar age (Gyr)<br> MASS: Stellar mass (solar mass)<br> ERR_MASS: Uncertainty of stellar mass (solar mass)<br> J: 2MASS J band magnitude<br> ERR_J: Uncertainty of 2MASS J band magnitude<br> H: 2MASS H band magnitude<br> ERR_H: Uncertainty of 2MASS H band magnitude<br> KS: 2MASS Ks band magnitude<br> ERR_KS: Uncertainty of 2MASS Ks band magnitude<br> G: Gaia DR2 G band magnitude<br> ERR_G: Uncertainty of Gaia DR2 G band magnitude<br> BP: Gaia DR2 BP band magnitude<br> ERR_BP: Uncertainty of Gaia DR2 BP band magnitude<br> RP: Gaia DR2 RP band magnitude<br> ERR_RP: Uncertainty of Gaia DR2 RP band magnitude<br> EBV: E (B - V) (mag)<br> MKS: Absolute magnitude in Ks band<br> DISTANCE: distance (kpc)<br> ERR_DISTANCE: Uncertainty of distance (kpc)<br> PARALLAX: Gaia DR2 parallax (mas)<br> ERR_PARALLAX: Uncertainty of Gaia DR2 parallax (mas)<br> PMRA: Proper motion in R.A. (mas/yr)<br> ERR_PMRA: Uncertainty of proper motion in R.A. (mas/yr)<br> PMDEC: Proper motion in Dec. (mas/yr)<br> ERR_PMDEC: Uncertainty of proper motion in Dec. (mas/yr)<br> F_CMD: Selection fraction in color-magnitude diagram