The ALPINE-ALMA [CII] survey: A self-consistent model linking [CII] line emission to nebular lines in ALPINE galaxies

In this poster I present a new physically motivated model able to link the [CII] emission from photodissociation regions (PDRs), to the optical and UV lines tracing ionized gas phase in high-z galaxies extracted from the ALPINE sample. The model combines a set of tailored CLOUDY photoionization simulations with an analytical approach able to link the HII region and PDRs physical conditions to the impinging radiation from star formation traced by UV and IR continuum. In particular, the model takes into account three physical properties characterising the gas: the hydrogen number density (n), the ionization parameter (U) and the gas metallicity (Z). I will show that the slope of the correlation between UV and optical emission lines (i.e. CIII], [OIII], [NII], Ha) and the star formation rate (SFR) is a valuable tool to get information on the ISM physical parameters. Finally, I will focus on the strong impact of UV binaries, and highlight how their presence can balance the effect of star formation quenching in the predictions.