A faint companion around CrA-9: protoplanet or obscured binary?
Lodato, G.; Pinte, C.; Casassus, S.; Absil, O.; Cánovas, H.; Spina, L.; van der Marel, N.; Zurlo, A.; Delorme, P.; Girard, J. H.; Reggiani, M.; Price, D. J.; Cieza, L.; Christiaens, V.; Marleau, G. -D.; Pérez, S.; Pairet, B.; Ubeira-Gabellini, M. -G.; Aoyama, Y.
Australia, Italy, Spain, France, Belgium, Chile, United States, China, Germany, Switzerland, Canada
Abstract
Understanding how giant planets form requires observational input from directly imaged protoplanets. We used VLT/NACO and VLT/SPHERE to search for companions in the transition disc of 2MASS J19005804-3645048 (hereafter CrA-9), an accreting M0.75 dwarf with an estimated age of 1-2 Myr. We found a faint point source at ∼0.7-arcsec separation from CrA-9 (∼108 au projected separation). Our 3-epoch astrometry rejects a fixed background star with a 5σ significance. The near-IR absolute magnitudes of the object point towards a planetary-mass companion. However, our analysis of the 1.0-3.8 $\,\mu$ m spectrum extracted for the companion suggests it is a young M5.5 dwarf, based on both the 1.13-μm Na index and comparison with templates of the Montreal Spectral Library. The observed spectrum is best reproduced with high effective temperature ( $3057^{+119}_{-36}$ K) BT-DUSTY and BT-SETTL models, but the corresponding photometric radius required to match the measured flux is only $0.60^{+0.01}_{-0.04}$ Jovian radius. We discuss possible explanations to reconcile our measurements, including an M-dwarf companion obscured by an edge-on circum-secondary disc or the shock-heated part of the photosphere of an accreting protoplanet. Follow-up observations covering a larger wavelength range and/or at finer spectral resolution are required to discriminate these two scenarios.