Molecular mapping of the PDS70 system

Context. Determining the chemical properties of atmosphere young forming gas giants might shed light on location their formation occurred and mechanisms involved. Aims. Our aim was to detect molecules in companion PDS70 b by searching for atmospheric absorption features typical substellar objects. Methods. We obtained medium-resolution ( R ≈ 5075) spectra planetary system with SINFONI integral field spectrograph at Very Large Telescope. applied molecular mapping, based cross-correlation synthetic spectra, identify signatures species planet. Results. Although planet emission is clearly detected when resampling data lower resolution, no could be identified technique. estimated upper limits abundances H 2 O, CO, CH 4 (log( X mol ) < −4.0, − 4.1, 4.9, respectively) assuming a clear atmosphere, we explored impact clouds, which increase factor up 0.7 dex. Assuming that observations directly probe planet’s found lack compared other imaged companions or Under assumption presents similar characteristics planets, conclude dusty environment surrounds planet, effectively obscuring any feature generated its atmosphere. quantify extinction necessary impede detection A V 16−17 mag), pointing possibility higher optical thickness than previously from studies. Finally, non-detection conflicts models proposed describe Conclusions. To reveal how giant planets form comprehensive approach includes constraints multiple techniques needs undertaken. Molecular mapping emerges as an alternative more classical like SED fitting. Specifically tuned are likely required faithfully atmospheres protoplanets, spectral resolution may lines despite enshrouding b.