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The Javalambre-Physics of the Accelerating Universe Astrophysical Survey(J-PAS) is expected to map thousands of square degrees of the northern sky with56 narrowband filters in the upcoming years. This will make J-PAS a verycompetitive and unbiased emission line survey compared to spectroscopic ornarrowband surveys with fewer filters. The miniJPAS survey covered 1 deg$^2$,and it used the same photometric system as J-PAS, but the observations werecarried out with the pathfinder J-PAS camera. In this work, we identify andcharacterize the sample of emission line galaxies (ELGs) from miniJPAS with aredshift lower than $0.35$. Using a method based on artificial neural networks,we detect the ELG population and measure the equivalent width and flux of the$H\alpha$, $H\beta$, [OIII], and [NII] emission lines. We explore theionization mechanism using the diagrams [OIII]/H$\beta$ versus [NII]/H$\alpha$(BPT) and EW(H$\alpha$) versus [NII]/H$\alpha$ (WHAN). We identify 1787 ELGs($83$%) from the parent sample (2154 galaxies) in the AEGIS field. For thegalaxies with reliable EW values that can be placed in the WHAN diagram (2000galaxies in total), we obtained that $72.8 \pm 0.4$%, $17.7 \pm 0.4$% , and$9.4 \pm 0.2$% are star-forming (SF), active galactic nucleus (Seyfert), andquiescent galaxies, respectively. Based on the flux of $H\alpha$ we find thatthe star formation main sequence is described as $\log$ SFR $[M_\mathrm{\odot}\mathrm{yr}^{-1}] = 0.90^{+ 0.02}_{-0.02} \log M_{\star} [M_\mathrm{\odot}]-8.85^{+ 0.19}_{-0.20}$ and has an intrinsic scatter of $0.20^{+0.01}_{-0.01}$. The cosmic evolution of the SFR density ($\rho_{\text{SFR}}$)is derived at three redshift bins: $0 < z \leq 0.15$, $0.15 < z \leq 0.25$, and$0.25 < z \leq 0.35$, which agrees with previous results that were based onmeasurements of the $H\alpha$ emission line.

The miniJPAS survey: Identification and characterization of the emission line galaxies down to $z < 0.35$ in the AEGIS field