  We present an analysis of the first connection mosaic made by the SPICE
instrument on board of the ESA / NASA Solar Orbiter mission on March 2nd, 2022.
The data will be used to map coronal composition that will be compared with
in-situ measurements taken by SWA/HIS to establish the coronal origin of the
solar wind plasma observed at Solar Orbiter. The SPICE spectral lines were
chosen to have varying sensitivity to the First Ionization Potential (FIP)
effect, and therefore the radiances of the spectral lines will vary
significantly depending on whether the elemental composition is coronal or
photospheric. We investigate the link between the behavior of sulfur with the
hypothesis that Alfv\'en waves drive FIP fractionation above the chromosphere.
We perform temperature diagnostics using line ratios and Emission Measure (EM)
loci, and compute relative FIP biases using three different approaches (two
line ratio (2LR), ratios of linear combinations of spectral lines (LCR), and
differential emission measure (DEM) inversion) to perform composition
diagnostics in the corona. We then compare the SPICE composition analysis and
EUI data of the potential solar wind source regions to the SWA / HIS data
products. Radiance maps are extracted from SPICE spectral data cubes, with
values matching previous observations. We find isothermal plasma of around LogT
= 5.8 for the active region loops targeted, and that higher FIP-bias values are
present at the footpoints of the coronal loops associated with two active
regions. Comparing the results with the SWA/HIS data products encourages us to
think that Solar Orbiter was connected to a source of slow solar wind during
this observation campaign. We demonstrate FIP fractionation in observations of
the upper chromosphere and transition region, emphasized by the behavior of the
intermediate-FIP element sulfur.
