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We present a sample of $\sim$ 140,000 primary red clump (RC) stars ofspectral signal-to-noise ratios higher than 20 from the LAMOST Galacticspectroscopic surveys, selected based on their positions in themetallicity-dependent effective temperature--surface gravity andcolor--metallicity diagrams, supervised by high-quality $Kepler$asteroseismology data. The stellar masses and ages of those stars are furtherdetermined from the LAMOST spectra, using the Kernel Principal ComponentAnalysis method, trained with thousands of RCs in the LAMOST-$Kepler$ fieldswith accurate asteroseismic mass measurements. The purity and completeness ofour primary RC sample are generally higher than 80 per cent. For the mass andage, a variety of tests show typical uncertainties of 15 and 30 per cent,respectively. Using over ten thousand primary RCs with accurate distancemeasurements 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 themetallicity and age dependencies. With the the new calibration, distances arederived 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 starsbeyond 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 elementalabundances derived from the LAMOST spectra and proper motions of Gaia DR2 arealso provided for the sample stars. Finally, the selection function of thesample is carefully evaluated in the color-magnitude plane for different skyareas. The sample is publicly available.

the astrophysical journal. supplement series/astrophysical journal. supplement series

Mapping the Galactic disk with the LAMOST and Gaia Red clump sample: I:  precise distances, masses, ages and 3D velocities of $\sim$ 140000 red clump  stars