A faint companion around CrA-9: protoplanet or obscured binary?. Issue 4 (22nd February 2021)

• Record Type: Journal Article
• Authors: Christiaens, V; Ubeira-Gabellini, M-G; Cánovas, H; Delorme, P; Pairet, B; Absil, O; Casassus, S; Girard, J H; Zurlo, A; Aoyama, Y; Marleau, G-D; Spina, L; van der Marel, N; Cieza, L; Lodato, G; Pérez, S; Pinte, C; Price, D J; Reggiani, M
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 502:Issue 4(2021)
• Page Start: 6117
• Page End: 6139
• Publication Date: 2021-02-22
• Subjects: techniques: image processing -- planets and satellites: formation -- planet–disc interactions -- protoplanetary discs; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab480
• Languages: English
• ISSNs: 0035-8711

Abstract

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- μ m 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.