Constraining the Nature of the PDS 70 Protoplanets with VLTI/GRAVITY

Creators: Wang, J. J.; Vigan, A.; Lacour, S.; Nowak, M.; Stolker, T.; De Rosa, R. J.; Ginzburg, S.; Gao, P.; Abuter, R.; Amorim, A.; Asensio-Torres, R.; Bauböck, M.; Benisty, M.; Berger, J. P.; Beust, H.; Beuzit, J.-L.; Blunt, S.; Boccaletti, A.; Bohn, A.; Bonnefoy, M.; Bonnet, H.; Brandner, W.; Cantalloube, F.; Caselli, P.; Charnay, B.; Chauvin, G.; Choquet, E.; Christiaens, V.; Clénet, Y.; Coudé du Foresto, V.; Cridland, A.; de Zeeuw, P. T.; Dembet, R.; Dexter, J.; Drescher, A.; Duvert, G.; Eckart, A.; Eisenhauer, F.; Facchini, S.; Gao, F.; Garcia, P.; Garcia Lopez, R.; Gardner, T.; Gendron, E; Genzel, R.; Gillessen, S.; Girard, J.; Haubois, X.; Heißel, G.; Henning, T.; Hinkley, S.; Hippler, S.; Horrobin, M.; Houllé, M.; Hubert, Z.; Jiménez-Rosales, A.; Jocou, L.; Kammerer, J.; Keppler, M.; Kervella, P.; Meyer, M.; Kreidberg, L.; Lagrange, A.-M.; Lapeyrère, V.; Le Bouquin, J.-B.; Léna, P.; Lutz, D.; Maire, A.-L.; Ménard, F.; Mérand, A.; Mollière, P.; Monnier, J. D.; Mouillet, D; Müller, A.; Nasedkin, E.; Ott, T.; Otten, G. P. P. L.; Paladini, C.; Paumard, T.; Perraut, K.; Perrin, G.; Pfuhl, O.; Pueyo, L.; Rameau, J.; Rodet, L.; Rodríguez-Coira, G.; Rousset, G.; Scheithauer, S.; Shangguan, J.; Shimizu, T.; Stadler, J.; Straub, O.; Straubmeier, C.; Sturm, E.; Tacconi, L. J.; van Dishoeck, E. F.; Vincent, F.; von Fellenberg, S. D.; Ward-Duong, K.; Widmann, F.; Wieprecht, E.; Wiezorrek, E.; Woillez, J.; GRAVITY Collaboration

Abstract

We present K-band interferometric observations of the PDS 70 protoplanets along with their host star using VLTI/GRAVITY. We obtained K-band spectra and 100 μas precision astrometry of both PDS 70 b and c in two epochs, as well as spatially resolving the hot inner disk around the star. Rejecting unstable orbits, we found a nonzero eccentricity for PDS 70 b of 0.17 ± 0.06, a near-circular orbit for PDS 70 c, and an orbital configuration that is consistent with the planets migrating into a 2:1 mean motion resonance. Enforcing dynamical stability, we obtained a 95% upper limit on the mass of PDS 70 b of 10 M_(Jup), while the mass of PDS 70 c was unconstrained. The GRAVITY K-band spectra rules out pure blackbody models for the photospheres of both planets. Instead, the models with the most support from the data are planetary atmospheres that are dusty, but the nature of the dust is unclear. Any circumplanetary dust around these planets is not well constrained by the planets' 1–5 μm spectral energy distributions (SEDs) and requires longer wavelength data to probe with SED analysis. However with VLTI/GRAVITY, we made the first observations of a circumplanetary environment with sub-astronomical-unit spatial resolution, placing an upper limit of 0.3 au on the size of a bright disk around PDS 70 b.

Additional Information

© 2021 The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2020 October 19; revised 2021 January 8; accepted 2021 January 11; published 2021 February 25. Based on observations collected at the European Southern Observatory under ESO programmes 0101.C-0281(B), 1103.B-0626(A), 2103.C-5018(A), and 1104.C-0651(A). We thank Dino Mesa and Michael Liu for helpful discussions. This research has made use of the Jean-Marie Mariotti Center Aspro service. J.J.W., S.G., P.G., and S.B. acknowledge support from the Heising-Simons Foundation, including grant 2019-1698. A.V. acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 757561). T.H, P.M., and R.A.-T. acknowledge support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 83 24 28. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF—Osservatorio di Padova (Italy), Observatoire de Genève (Switzerland), ETH Zürich (Switzerland), NOVA (Netherlands), ONERA (France), and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland), and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004-2008), grant number 226604 for FP7 (2009-2012), and grant number 312430 for FP7 (2013-2016). R.G.L. has received funding from Science Foundation Ireland under grant No. 18/SIRG/5597. Facility: VLTI (GRAVITY). - Software: orbitize! (Blunt et al. 2020), pyKLIP (Wang et al. 2015), vlt-sphere (Vigan 2020), emcee (Foreman-Mackey et al. 2013), ptemcee (Vousden et al. 2016), pymultinest (Buchner et al. 2014), REBOUND (Rein & Liu 2012; Rein & Spiegel 2015), astropy (Astropy Collaboration et al. 2018).

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