Contributors: Institute of Astronomy Leuven; Catholic University of Leuven = Katholieke Universiteit Leuven (KU Leuven); Space Sciences, Technologies and Astrophysics Research Institute (STAR); Université de Liège; Max-Planck-Institut für Astronomie (MPIA); Max-Planck-Gesellschaft; Kapteyn Astronomical Institute Groningen; University of Groningen Groningen; Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA); Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris; Université Paris Sciences et Lettres (PSL)-Université Paris Sciences et Lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité); Institut d'astrophysique spatiale (IAS); Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales Paris (CNES); Universität Duisburg-Essen = University of Duisburg-Essen Essen; Institut für Astronomie und Astrophysik Tübingen (IAAT); Eberhard Karls Universität Tübingen = University of Tübingen; Physikalisches Institut Bern; Universität Bern = University of Bern = Université de Berne (UNIBE); Universiteit Leiden = Leiden University; Max-Planck-Institut für Extraterrestrische Physik (MPE); Institut für Astrophysik Wien; Universität Wien = University of Vienna; Institute for Particle Physics and Astrophysics ETH Zürich (IPA); Department of Physics = Departement Physik ETH Zürich (D-PHYS); Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology Zürich (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology Zürich (ETH Zürich); Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)); Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité); Centro de Astrobiologia Madrid (CAB); Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Cientificas España = Spanish National Research Council Spain (CSIC); INAF - Osservatorio Astronomico di Capodimonte (OAC); Istituto Nazionale di Astrofisica (INAF); Dublin Institute for Advanced Studies (DIAS); Stockholm University; Department of Astrophysics Nijmegen; Institute for Mathematics, Astrophysics and Particle Physics (IMAPP); Radboud University Nijmegen -Radboud University Nijmegen; SRON Netherlands Institute for Space Research (SRON); Institut für Weltraumforschung = Space Research institute Graz (IWF); Osterreichische Akademie der Wissenschaften (ÖAW); Graz University of Technology Graz (TU Graz); We thank Jason Wang for sharing atmospheric models and GRAVITY spectra of the protoplanets. We also thank Yuhiko Aoyama, Faustine Cantalloube and Julien Girard for useful discussions. VC and OA thank the Belgian F.R.S.-FNRS, and the Belgian Federal Science Policy Office (BELSPO) for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contract number 4000142531. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 819155), and from the Wallonia–Brussels Federation (grant for Concerted Research Actions). G-DM acknowledges thesupport of the DFG priority program SPP 1992 “Exploring the Diversity of Extrasolar Planets” (MA 9185/1) and from the Swiss National Science Foundation under grant 200021_204847 “PlanetsInTime”. Parts of this work have been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. TPR acknowledges support from the ERC under grant 743029 (EASY). This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work benefited from the 2022 Exoplanet Summer Program in the Other Worlds Laboratory (OWL) at the University of California, Santa Cruz, a program funded by the Heising-Simons Foundation.; European Project: 819155,EPIC; European Project: 743029,EASY
نبذة مختصرة : International audience ; Context. Two protoplanets have recently been discovered within the PDS 70 protoplanetary disk. JWST/NIRCam offers a unique opportunity to characterize them and their birth environment at wavelengths that are difficult to access from the ground. Aims. We image the circumstellar environment of PDS 70 at 1.87 μm and 4.83 μm, assess the presence of Pa- α emission due to accretion onto the protoplanets, and probe any IR excess indicative of heated circumplanetary material. Methods. We obtained noncoronagraphic JWST/NIRCam images of PDS 70 within the MIRI mid-INfrared Disk Survey (MINDS) program. We leveraged the Vortex Image Processing (VIP) package for data reduction, and we developed dedicated routines for optimal stellar point spread function subtraction, unbiased imaging of the disk, and protoplanet flux measurement in this type of dataset. A radiative transfer model of the disk was used to separate the contributions from the disk and the protoplanets. Results. We redetect both protoplanets and identify extended emission after subtracting a disk model, including a large-scale spiral-like feature. We interpret its signal in the direct vicinity of planet c as tracing the accretion stream that feeds its circumplanetary disk, while the outer part of the feature may rather reflect asymmetric illumination of the outer disk. We also report a bright signal that is consistent with a previously proposed protoplanet candidate enshrouded in dust near the 1:2:4 mean-motion resonance with planets b and c . The 1.87 μm flux of planet b is consistent with atmospheric model predictions, but the flux of planet c is not. We discuss potential origins for this discrepancy, including significant Pa- α line emission. The 4.83 μm fluxes of planets b and c suggest enshrouding dust or heated CO emission from their circumplanetary environment. Conclusions. The use of image-processing methods that are optimized for extended disk signals on high-sensitivity and high-stability from JWST can uniquely identify ...
Processing Request
No Comments.