Calibration of mid- to far-infrared spectral lines in galaxies

Mid- to far-infrared (IR) lines are suited study dust obscured regions in galaxies, because IR spectroscopy allows us explore the most hidden where heavily star formation as well accretion onto supermassive black-holes occur. This is mostly important at redshifts of 1<z<3, when baryonic mass galaxies has been assembled. We provide reliable calibrations mid- far-IR ionic fine structure lines, brightest H2 pure rotational and Polycyclic Aromatic Hydrocarbons (PAHs) features, that will be used analyse current future observations mm/submm range from ground, mid-IR upcoming James Webb Space Telescope. use three samples observed local Universe: forming AGN low-metallicity dwarf galaxies. For each population we derive different line luminosities versus total luminosities. spectroscopic measurements SFR BHAR using PAH features. robust star-formation tracers based on [CII]158 $\mu$m line; sum [OI]63$\mu$m [OIII]88$\mu$m lines; a combination neon sulfur bright features 6.2 11.3 $\mu$m, 9.7, 12.3 17 $\mu$m. propose [CII]158$\mu$m line, two and, for solar-like metallicity may harbor an AGN, PAH11.3$\mu$m feature best tracers. A measure can obtained [OIV]25.9 [NeV]14.3 24.3 lines. commonly fine-structure compare our calibration with existing ALMA high redshift finding overall good agreement results.