tokens: We are thankful to the helpful comments about star formation rate estimation and the implications of MIR neon emission lines from an anonymous referee on this paper. This work is supported by the National Natural Science Foundation of China (NSFC-11573024, 11903029, 11473025, 11421303) and the National Basic Research Program of China (2013CB834905). W.L. acknowledges supports from the Natural Science Foundation of China grant (NSFC-11703079) and the 'Light of West China' Program of Chinese Academy of Sciences (CAS). P.J. is supported by the National Natural Science Foundation of China (NSFC-11973037), and H.W. is supported by the Natural Science Foundation of China (NSFC-11890693). We acknowledge the use of the Hale 200-inch Telescope at Palomar Observatory through the Telescope Access Program (TAP), as well as the archival data from the SDSS, 2MASS, and WISE surveys. TAP is funded by the Strategic Priority Research Program, the Emergence of Cosmological Structures (XDB09000000), National Astronomical Observatories, Chinese Academy of Sciences, and the Special Fund for Astronomy from the Ministry of Finance. Observations obtained with the Hale Telescope at Palomar Observatory were obtained as part of an agreement between the National Astronomical Observatories, Chinese Academy of Sciences, and the California Institute of Technology. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/ .
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