  Hot giant planets like MASCARA-1 b are expected to have thermally inverted
atmospheres, that makes them perfect laboratory for the atmospheric
characterization through high-resolution spectroscopy. Nonetheless, previous
attempts of detecting the atmosphere of MASCARA-1 b in transmission have led to
negative results.
  In this paper we aim at the detection of the optical emission spectrum of
MASCARA-1 b.
  We used the high-resolution spectrograph PEPSI to observe MASCARA-1 (spectral
type A8) near the secondary eclipse of the planet. We cross-correlated the
spectra with synthetic templates computed for several atomic and molecular
species.
  We obtained the detection of FeI, CrI and TiI in the atmosphere of MASCARA-1
b with a S/N ~7, 4 and 5 respectively, and confirmed the expected systemic
velocity of ~13 km/s and the radial velocity semi-amplitude of MASCARA-1 b of
~200 km/s. The detection of Ti is of particular importance in the context of
the recently proposed Ti cold-trapping below a certain planetary equilibrium
temperature.
  We confirm the presence of an the atmosphere around MASCARA-1 b through
emission spectroscopy. We conclude that the atmospheric non detection in
transmission spectroscopy is due to the high gravity of the planet and/or to
the overlap between the planetary track and its Doppler shadow.
