  High resolution precision spectroscopy provides a multitude of robust
techniques for probing exoplanetary atmospheres. We present multiple
VLT/ESPRESSO transit observations of the hot-Jupiter exoplanet WASP-19b with
previously published but disputed atmospheric features from low resolution
studies. Through spectral synthesis and modeling of the Rossiter-McLaughlin
(RM) effect we calculate stellar, orbital and physical parameters for the
system. From narrow-band spectroscopy we do not detect any of H\,I, Fe\,I,
Mg\,I, Ca\,I, Na\,I and K\,I neutral species, placing upper limits on their
line contrasts. Through cross correlation analyses with atmospheric models, we
do not detect Fe\,I and place a 3$\sigma$ upper limit of
$\log\,(X_{\textrm{Fe}}/X_\odot) \approx -1.83\,\pm\,0.11$ on its mass
fraction, from injection and retrieval. We show the inability to detect the
presence of H$_2$O for known abundances, owing to lack of strong absorption
bands, as well as relatively low S/N ratio. We detect a barely significant peak
(3.02\,$\pm$\,0.15\,$\sigma$) in the cross correlation map for TiO, consistent
with the sub-solar abundance previously reported. This is merely a hint for the
presence of TiO and does \textit{not} constitute a confirmation. However, we do
confirm the presence of previously observed enhanced scattering towards blue
wavelengths, through chromatic RM measurements, pointing to a hazy atmosphere.
We finally present a reanalysis of low resolution transmission spectra of this
exoplanet, concluding that unocculted starspots alone cannot explain previously
detected features. Our reanalysis of the FORS2 spectra of WASP-19b finds a
$\sim$\,100$\times$ sub-solar TiO abundance, precisely constrained to
$\log\,X_{\textrm{TiO}} \approx -7.52 \pm 0.38$, consistent with the TiO hint
from ESPRESSO. We present plausible paths to reconciliation with other
seemingly contradicting results.
