2014MNRAS.437.3766M

Although gravitational collapse is supposed to play an essential role in the star formation process, infall motions have been always elusive to detect. So far, only a few observational signatures have been commonly used to claim for the presence of infall. Often these features consist in either `blue asymmetries' or absorption at redshifted velocities (e.g. inverse P Cygni profiles). Both signatures are based only on the shape of the line profile and they do not guarantee by themselves the presence of dominant infall motions. More robust `mapping signatures' can be obtained from images that angularly resolve the infalling gas. Here we present Very Large Array observations of the ammonia inversion transitions (2,2), (3,3), (4,4), (5,5) and (6,6) towards the hot molecular core (HMC) near G31.41+0.31 that show the signatures of protostellar infall theoretically predicted by Anglada et al. The intensity of the ammonia emission is compact and sharply increases towards the centre in the blueshifted velocity channel maps, while it shows a more flattened distribution in the redshifted velocity channels. Additionally, the emission becomes more compact with increasing (relative) velocity for both red- and blueshifted channels. We introduce a new infall signature, the `central blue spot', easily identifiable in the first-order moment maps. We show that rotation produces an additional, independent signature, making the distribution of the emission in the channel maps asymmetric with respect to the central position, but without masking the infall signatures. All these mapping signatures, which are identified here for the first time, are present in the observed ammonia transitions of G31 HMC.