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Vector magnetic fields of an active region filament in the photosphere andupper chromosphere are obtained from spectro-polarimetric observations recordedwith the Tenerife Infrared Polarimeter (TIP II) at the German Vacuum TowerTelescope (VTT). We apply Milne-Eddington inversions on full Stokes vectors ofthe photospheric Si I 1082.7 nm and the upper chromospheric He I triplet at1083.0 nm to obtain magnetic field vector and velocity maps in two atmospherelayers. We find that: (1)A complete filament was already present in H$\alpha$at the beginning of the TIP II data acquisition. Only a partially formed one,composed of multiple small threads, was present in He I. (2) The AR filamentcomprises two sections. One shows strong magnetic field intensities, about 600- 800 G in the upper chromosphere and 800 - 1000 G in the photosphere. Theother exhibits only comparatively weak magnetic field strengths in both layers.(3) The Stokes V signal is indicative of a dip in the magnetic field strengthclose to the chromospheric PIL. (3) In the chromosphere consistent upflows arefound along the PIL flanked by downflows. (4) The transversal magnetic field isnearly parallel to the PIL in the photosphere and inclined by 20 - 30 degree inthe chromosphere. (5) The chromospheric magnetic field around the filament isfound to be in normal configuration, while the photospheric field presents aconcave magnetic topology. The observations are consistent with the emergenceof a flux rope with a subsequent formation of a filament.

Magnetic fields of an active region filament from full Stokes analysis of Si I 1082.7 nm and He I 1083.0 nm