  Our understanding of the formation and evolution of the corona and the
heliosphere is linked to our capability of properly interpreting the data from
remote sensing and in-situ observations. In this respect, being able to
correctly connect in-situ observations with their source regions on the Sun is
the key for solving this problem. In this work we aim at testing a diagnostics
method for this connectivity. This paper makes use of a coronal jet observed on
2010 August 2nd in active region 11092 as a test for our connectivity method.
This combines solar EUV and in-situ data together with magnetic field
extrapolation, large scale MHD modeling and FIP (First Ionization Potential)
bias modeling to provide a global picture from the source region of the jet to
its possible signatures at 1AU. Our data analysis reveals the presence of
outflow areas near the jet which are within open magnetic flux regions and
which present FIP bias consistent with the FIP model results. In our picture,
one of these open areas is the candidate jet source. Using a back-mapping
technique we identified the arrival time of this solar plasma at the ACE
spacecraft. The in-situ data show signatures of changes in the plasma and
magnetic field parameters, with FIP bias consistent with the possible passage
of the jet material. Our results highlight the importance of remote sensing and
in-situ coordinated observations as a key to solve the connectivity problem. We
discuss our results in view of the recent Solar Orbiter launch which is
currently providing such unique data.
