JWST Imaging of Edge-on Protoplanetary Disks. IV. Mid-infrared Dust Scattering in the HH 30 disk

We present near- and mid-infrared (IR) broadband imaging observations of the edge-on protoplanetary disk around HH 30 with the James Webb Space Telescope/Near Infrared Camera (NIRCam) and the Mid-Infrared Instrument (MIRI). We combine these observations with archival optical/near-IR scattered light...

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Bibliographic Details
Published in:arXiv.org 2024-12
Main Authors: Tazaki, Ryo, Ménard, François, Duchêne, Gaspard, Villenave, Marion, Ribas, Álvaro, Stapelfeldt, Karl R, Perrin, Marshall D, Pinte, Christophe, Wolff, Schuyler G, Padgett, Deborah L, Ma, Jie, Martinien, Laurine, Roumesy, Maxime
Format: Article
Language:English
Subjects:
Broadband
Dust
Inclination angle
Infrared cameras
Infrared imaging
Infrared instruments
Infrared telescopes
Motion perception
Near infrared radiation
Planet formation
Protoplanetary disks
Radiative transfer
Radio telescopes
Reflection nebulae
Scale height
Space telescopes
Spatial resolution
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Summary:We present near- and mid-infrared (IR) broadband imaging observations of the edge-on protoplanetary disk around HH 30 with the James Webb Space Telescope/Near Infrared Camera (NIRCam) and the Mid-Infrared Instrument (MIRI). We combine these observations with archival optical/near-IR scattered light images obtained with the Hubble Space Telescope (HST) and a millimeter-wavelength dust continuum image obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) with the highest spatial resolution ever obtained for this target. Our multiwavelength images clearly reveal the vertical and radial segregation of micron-sized and sub-mm-sized grains in the disk. In the near- and mid-IR, the images capture not only bi-reflection nebulae separated by a dark lane but also diverse dynamical processes occurring in the HH 30 disk, such as spiral- and tail-like structures, a conical outflow, and a collimated jet. In contrast, the ALMA image reveals a flat dust disk in the disk midplane. By performing radiative transfer simulations, we show that grains of about 3 \(\mu\)m in radius or larger are fully vertically mixed to explain the observed mid-IR scattered light flux and its morphology, whereas millimeter-sized grains are settled into a layer with a scale height of \(\gtrsim1\) au at \(100\) au from the central star. We also find a tension in the disk inclination angle inferred from optical/near-IR and mm observations with the latter being closer to an exactly edge-on. Finally, we report the first detection of the proper motion of an emission knot associated with the mid-IR collimated jet detected by combining two epochs of our MIRI 12.8-\(\mu\)m observations.
ISSN:2331-8422