MINDS: JWST/NIRCam imaging of the protoplanetary disk PDS 70

Autor(en): V. Christiaens, M. Samland, Th Henning, B. Portilla-Revelo, G. Perotti, E. Matthews, O. Absil, L. Decin, I. Kamp, A. Boccaletti, B. Tabone, G. D. Marleau, E. F. van Dishoeck, M. Güdel, P. O. Lagage, D. Barrado, A. Caratti o Garatti, A. M. Glauser, G. Olofsson, T. P. Ray, S. Scheithauer, B. Vandenbussche, L. B.F.M. Waters, A. M. Arabhavi, S. L. Grant, H. Jang, J. Kanwar, J. Schreiber, K. Schwarz, M. Temmink, G. Östlin
Abstrakt: 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 signatures of planet–disk interactions and enable accurate photometry of protoplanets at wavelengths that are difficult to probe from the ground. Our results indicate that more protoplanets can be identified and characterized in other JWST datasets.
Organisation(en): Institut für Astrophysik
Externe Organisation(en): Katholieke Universiteit Leuven, Université de Liège, Max-Planck-Institut für Astronomie, University of Groningen, Université de recherche Paris Sciences et Lettres, Université Paris XI - Paris-Sud, Universität Duisburg-Essen, Eberhard Karls Universität Tübingen, Universität Bern, Leiden University, Max-Planck-Institut für extraterrestrische Physik, Eidgenössische Technische Hochschule Zürich, Université Paris Saclay, European Space Astronomy Centre (ESA), INAF-Osservatorio Astronomico di Capodimonte, Dublin Institute for Advanced Studies, AlbaNova University Centre, Radboud University, SRON Netherlands Institute for Space Research , Österreichische Akademie der Wissenschaften (ÖAW), Technische Universität Graz
Journal: Astronomy and Astrophysics
Band: 685
Anzahl der Seiten: 18
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/202349089
Publikationsdatum: 05-2024
Peer-reviewed: Ja
ÖFOS 2012: 103003 Astronomie, 103004 Astrophysik
Schlagwörter
ASJC Scopus Sachgebiete: Astronomy and Astrophysics, Space and Planetary Science
Link zum Portal: https://ucrisportal.univie.ac.at/de/publications/4a2f4c8c-bc3c-4c0c-a07d-7b031d6fd3d5

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