Dust characterization of the HD 163296 disk with high-resolution multi-wavelength ALMA observations
Abstract
Context. Planets form through the growth and accumulation of dust grains in protoplanetary disks. Characterizing dust properties such as size, surface density, and temperature is key to understanding planet formation. Aims. We characterize the dust properties of the protoplanetary disk around HD 163296 by performing spectral energy distribution (SED) fitting of multi-wavelength high-resolution observations. Methods. We present new high-resolution ALMA Band 9 (0.45 mm) observations, which are sensitive to the temperature. We performed SED fitting at a common resolution of 0.066 arcsec using these new Band 9 observations along with archival ALMA Band 3, 4, 6, and 7 observations. We compared the fitted results with VLA observations and explored multiple dust models with different optical constants and porosities. Results. The Band 9 image shows the central disk, two rings at 0.67 and 1.00 arcsec, and outer extended emission previously seen at other wavelengths. At higher frequencies, the rings appear wider, the gaps appear shallower, and the extended emission appears brighter, which can be explained by optical-depth effects and/or size segregation. We characterized the dust properties, including temperature, surface density, and dust size, for each dust model. However, the inferred dust properties are dependent on the dust model, and the ALMA data alone do not allow us to determine which dust model is preferred. We identified the DSHARP Zubko (porous) model as the preferred model based on VLA profiles and physical and observational constraints. The outer ring temperature is lower than predicted by a passively irradiated disk model, suggesting shadowing by the inner ring. Although the surface density and dust size depend on the dust model, the preferred model indicates that the central disk, both rings, and the extended disk each contain more than a few Earth masses of dust.
Related
- The ALMA Survey of Gas Evolution of PROtoplanetary disks (AGE-PRO): Evolution of dust properties from multi-wavelength observations
- The ALMA Survey of Gas Evolution of PROtoplanetary disks (AGE-PRO): Evolution of dust properties from multi-wavelength observations
- The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems IX: A Multi-Wavelength Framework for Source Characterization in JWST Coronagraphic Imaging of the HIP 65426 System
- Multi-wavelength Constraints on Dust Dynamics and Size Evolution in Protoplanetary Disk Rings. II. Observational Implications
- Dust-induced reversal of the optical wavelength dependence of spiral-arm pitch angles
BibTeX
@misc{doi2026dust,
title = {{Dust characterization of the HD 163296 disk with high-resolution multi-wavelength ALMA observations}},
author = {Kiyoaki Doi and Myriam Benisty and Akimasa Kataoka and Haochang Jiang and Francesco Zagaria and Hauyu Baobab Liu and Carsten Dominik and Ryo Tazaki and Takahiro Ueda and Tomohiro C. Yoshida and Takashi Tsukagoshi and Yoshihide Yamato and Ryuta Orihara},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2607.22169},
eprint = {2607.22169},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2607.22169},
}
RIS
TY - UNPB
TI - Dust characterization of the HD 163296 disk with high-resolution multi-wavelength ALMA observations
AU - Kiyoaki Doi
AU - Myriam Benisty
AU - Akimasa Kataoka
AU - Haochang Jiang
AU - Francesco Zagaria
AU - Hauyu Baobab Liu
AU - Carsten Dominik
AU - Ryo Tazaki
AU - Takahiro Ueda
AU - Tomohiro C. Yoshida
AU - Takashi Tsukagoshi
AU - Yoshihide Yamato
AU - Ryuta Orihara
PY - 2026
DA - 2026/09/01
PB - arXiv
DO - 10.48550/arxiv.2607.22169
UR - https://arxiv.org/abs/2607.22169
AB - Context. Planets form through the growth and accumulation of dust grains in protoplanetary disks. Characterizing dust properties such as size, surface density, and temperature is key to understanding planet formation. Aims. We characterize the dust properties of the protoplanetary disk around HD 163296 by performing spectral energy distribution (SED) fitting of multi-wavelength high-resolution observations. Methods. We present new high-resolution ALMA Band 9 (0.45 mm) observations, which are sensitive to the temperature. We performed SED fitting at a common resolution of 0.066 arcsec using these new Band 9 observations along with archival ALMA Band 3, 4, 6, and 7 observations. We compared the fitted results with VLA observations and explored multiple dust models with different optical constants and porosities. Results. The Band 9 image shows the central disk, two rings at 0.67 and 1.00 arcsec, and outer extended emission previously seen at other wavelengths. At higher frequencies, the rings appear wider, the gaps appear shallower, and the extended emission appears brighter, which can be explained by optical-depth effects and/or size segregation. We characterized the dust properties, including temperature, surface density, and dust size, for each dust model. However, the inferred dust properties are dependent on the dust model, and the ALMA data alone do not allow us to determine which dust model is preferred. We identified the DSHARP Zubko (porous) model as the preferred model based on VLA profiles and physical and observational constraints. The outer ring temperature is lower than predicted by a passively irradiated disk model, suggesting shadowing by the inner ring. Although the surface density and dust size depend on the dust model, the preferred model indicates that the central disk, both rings, and the extended disk each contain more than a few Earth masses of dust.
ER -