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