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We present a 24 um-selected spectroscopic sample z > 0.13 (median z = 0.41)in the Lockman Hole field, consisting of 4035 spectra. Our aim is to identifyAGNs and determine their fraction in this mid-infrared selected sample. In thiswork, we use the [Ne V]3426 emission line to spectroscopically identify AGNs.Combined with broad-line Type I AGNs selected in our previous study, our sampleconsists of 887 (22%) spectroscopically confirmed AGNs. We perform a stackinganalysis on the remaining spectra, and find that in various MIR-wedge-selectedAGN candidates, the stacked spectra still show significant [Ne V]3426 emission,In contrast, no clear [Ne V]3426 signal is detected in non-AGN candidatesfalling outside the wedges. Assuming a range of AGN mid-IR SED slope of 0.3<alpha <0.7, and an average star-forming relation derived from 65 star-formingtemplates, we develop a robust method to separate the AGN and star-formingcontributions to the mid-IR SEDs using the rest-frame L12 /L1.6 vs L4.5 /L1.6diagram. We separate the objects into bins of L12 , and find that AGN fractionincreases with increasing L12. We also find that the stacked [Ne V]3426strength scales with L12 . The pure AGN luminosity at 12 um exhibits a positivecorrelation with the star formation rates, indicating possible co-evolution andcommon gas supply between the AGN and their host galaxies. Varying populationproperties across the redshift range explored contribute to the observedcorrelation.

Active Galactic Nuclei in a Mid-Infrared Selected Galaxy Sample at z>0.13: [Ne V]3426 Line Emission as a Benchmark