Modelling line ratios and continuum SED of NGC4993 and other short GRB
  host galaxies
  We present a detailed spectral modelling of NGC4993 -- the host galaxy of
GW170817 -- and other SGRB host galaxies. In order to determine their physical
conditions and the element abundances, we have gathered spectroscopic and
photometric data from the literature. The observation data are sometimes
missing preventing us from fully constraining the model. However, for most of
the SGRB hosts the [OIII]5007/Hb and [NII]6548/Ha line ratios are reported. The
analysis of NGC4993 by a composite model (photoionization+shock) confirms that
an AGN, most probably a LINER or a LLAGN, is the gas photoionization source.
Shock velocities and preshock densities are similar to those found in the
narrow line region of AGN. O/H and N/H have solar values. For the other SGRB of
the sample we have found that O/H ratios are nearly solar, while N/H cover a
much larger range of values at redshifts close to 0.4. In NGC4993, the relative
contribution to the SED of an old stellar population, characterized by a black
body temperature of Tbb=4000K, with respect to Bremsstrahlung is higher by a
factor >100 than in most of the local AGN and SB galaxies. For the other SGRB
composing the sample, Tbb ranges between 2000K for SGRB100206A and 8000K for
SGRB111117A.
