~1 million RGB and RC stars masses and ages

The RGBs, primary RCs, and secondary RCs are identified with the large frequency spacing ({DELTA}{nu}) and period spacing ({DELTA}P), estimated from the LAMOST spectra with spectral SNRs>10 by the neural network method supervised with the seismologic information from LAMOST-Kepler sample stars.

The purity and completeness of both RGB and RC samples are better than 95% and 90%, respectively. The mass and age of RGBs and RCs are determined again with the neural network method by taking the LAMOST-Kepler giant stars as the training set. The typical uncertainties of stellar mass and age are, respectively, 10% and 30% for the RGB stellar sample.