  Gravity modes in the Sun have been long searched during the past decades.
Using their asymptotic properties Garcia et al. (2007) found the signature of
the dipole g modes analyzing an spectral window between 25 and 140 muHz of
velocity power spectrum obtained from the GOLF/SoHO instrument. Using this
result it has been possible to check some properties of the structure of the
solar interior (Garcia, Mathur & Ballot 2008) as well as some indications on
the dynamics of the core. However, the individual detection of such modes
remains evasive and they are needed to really improve our knowledge of the
deepest layers in the Sun (Mathur et al. 2008). In this work we study the
signal at 220.7 muHz which is present in most of the helioseismic instruments
during the last 10 years. This signal has been previously identified as part of
a g-mode candidate in the GOLF data (Turck-Chieze et al. 2004; Mathur et al.
2007) and in SPM/VIRGO (Garcia et al. 2008) with more than 90% confidence
level. It could be labelled as the l=2 n=-3 g mode as it is in the region were
this mode is expected.
  We have checked the possibility that the 220.7 muHz signal could have an
instrumental origin without success by analysing all the available housekeeping
data as well as the information on the roll, pith and yaw of the SoHO
spacecraft. In consequence, we are confident that this signal has a solar
origin.
