We attempt to make high resolution spectroscopic
  observations of  chromospherically active stars.
  The aim of the project is the confirmation of the
  presence of photospheric emission lines from Mg I
  and chromospheric emission lines from H I(7-6), both
  in the wavelength range around 12 microns. These
  lines have been observed previously in the Sun.
  They show a strengthen towards the solar limb and
  the Mg I lines also show a large Zeeman sensitivity
  compared with transitions in the optical (5-10
  times). These lines should appear enhanced in very
  active stars. The proposed observations will provide
  important diagnostics of stellar magnetic fields. We
  will obtain simultaneous spectra  at shorter wavelenghts,
  for the Pfund(beta), Brackett(alpha) and Brackett(beta)
  at 4.625, 4.051 and 2.625  microns, respectively,
  with lower resolution, in order to compare with other
  chromospheric lines which have been observed previously
  by us in other spectral ranges.