Searching for intergalactic star forming regions in Stephan's Quintet
  with SITELLE: II. Physical properties and metallicity
  Based on SITELLE spectroscopy, we studied the ionised gas emission for the
175 H$\alpha$ emission regions in the Stephan's Quintet (SQ). A detailed
analysis is performed of the star formation rate (SFR), oxygen abundance (O/H),
and nitrogen-to-oxygen abundance ratio (N/O) of the SQ regions, to explore the
provenance and evolution of this complex structure. According to the BPT
diagram, we found 91 HII, 17 composite, and 7 active galactic nucleus-like
regions in SQ. Several regions are compatible with fast shocks models without a
precursor for solar metallicity and low density (n=0.1 cm$^{-3}$), with
velocities between 175 - 300 km s$^{-1}$. We derived the total SFR in SQ
(log(SFR/M$_\odot\,yr^{-1}$=0.496); starburst A and B provide 28% and 9% of the
total SFR, and 45% comes from the regions with a radial velocity lower than
6160 km s$^{-1}$. For this reason, we assume that the material prior to the
collision with the new intruder (NI) does not show a high SFR, and therefore SQ
was apparently quenched. When considering the integrated SFR for the whole SQ
and the NI, we found that both zones have a SFR consistent with those obtained
in the SDSS star-forming galaxies. At least two chemically different gas
components cohabit in SQ where, on average, the regions with high radial
velocities (v$>$6160 km s$^{-1}$) have lower values of O/H and N/O than those
with low radial velocities (v$\leq$6160 km s$^{-1}$). The values found for the
line ratios, O/H, and N/O for the southern debris region and the northernmost
tidal tail, are compatible with regions belonging to the outer part of the
galaxies. We highlight the presence of inner-outer variation for O/H and some
emission line ratios along the NI strands and the young tidal tail south
strand. Finally, the SQ H$\alpha$ regions are outside the galaxies because the
interactions have dispersed the gas to the peripheral zones.
