Saved in:
| Main Authors: | , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | https://arxiv.org/abs/2411.04741 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866929612736430080 |
|---|---|
| author | Martinien, Laurine Ménard, François Duchêne, Gaspard Tazaki, Ryo Perrin, Marshall D. Stapelfeldt, Karl R. Pinte, Christophe Wolff, Schuyler G. Grady, Carol Dominik, Carsten Roumesy, Maxime Ma, Jie Ginski, Christian Hines, Dean C. Schneider, Glenn |
| author_facet | Martinien, Laurine Ménard, François Duchêne, Gaspard Tazaki, Ryo Perrin, Marshall D. Stapelfeldt, Karl R. Pinte, Christophe Wolff, Schuyler G. Grady, Carol Dominik, Carsten Roumesy, Maxime Ma, Jie Ginski, Christian Hines, Dean C. Schneider, Glenn |
| contents | PDS 453 is a rare highly inclined disk where the stellar photosphere is seen at grazing incidence on the disk surface. Our goal is take advantage of this geometry to constrain the structure and composition of this disk, in particular the fact that it shows a 3.1 $μ$m water ice band in absorption that can be related uniquely to the disk. We observed the system in polarized intensity with the VLT/SPHERE instrument, as well as in polarized light and total intensity using the HST/NICMOS camera. Infrared archival photometry and a spectrum showing the water ice band are used to model the spectral energy distribution under Mie scattering theory. Based on these data, we fit a model using the radiative transfer code MCFOST to retrieve the geometry and dust and ice content of the disk. PDS 453 has the typical morphology of a highly inclined system with two reflection nebulae where the disk partially attenuates the stellar light. The upper nebula is brighter than the lower nebula and shows a curved surface brightness profile in polarized intensity, indicating a ring-like structure. With an inclination of 80° estimated from models, the line-of-sight crosses the disk surface and a combination of absorption and scattering by ice-rich dust grains produces the water ice band. PDS 453 is seen highly inclined and is composed of a mixture of silicate dust and water ice. The radial structure of the disk includes a significant jump in density and scale height at a radius of 70 au in order to produce a ring-like image. The depth of the 3.1 $μ$m water ice band depends on the amount of water ice, until it saturates when the optical thickness along the line-of-sight becomes too large. Therefore, quantifying the exact amount of water from absorption bands in edge-on disks requires a detailed analysis of the disk structure and tailored radiative transfer modeling. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2411_04741 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The grazing angle icy protoplanetary disk PDS 453 Martinien, Laurine Ménard, François Duchêne, Gaspard Tazaki, Ryo Perrin, Marshall D. Stapelfeldt, Karl R. Pinte, Christophe Wolff, Schuyler G. Grady, Carol Dominik, Carsten Roumesy, Maxime Ma, Jie Ginski, Christian Hines, Dean C. Schneider, Glenn Solar and Stellar Astrophysics PDS 453 is a rare highly inclined disk where the stellar photosphere is seen at grazing incidence on the disk surface. Our goal is take advantage of this geometry to constrain the structure and composition of this disk, in particular the fact that it shows a 3.1 $μ$m water ice band in absorption that can be related uniquely to the disk. We observed the system in polarized intensity with the VLT/SPHERE instrument, as well as in polarized light and total intensity using the HST/NICMOS camera. Infrared archival photometry and a spectrum showing the water ice band are used to model the spectral energy distribution under Mie scattering theory. Based on these data, we fit a model using the radiative transfer code MCFOST to retrieve the geometry and dust and ice content of the disk. PDS 453 has the typical morphology of a highly inclined system with two reflection nebulae where the disk partially attenuates the stellar light. The upper nebula is brighter than the lower nebula and shows a curved surface brightness profile in polarized intensity, indicating a ring-like structure. With an inclination of 80° estimated from models, the line-of-sight crosses the disk surface and a combination of absorption and scattering by ice-rich dust grains produces the water ice band. PDS 453 is seen highly inclined and is composed of a mixture of silicate dust and water ice. The radial structure of the disk includes a significant jump in density and scale height at a radius of 70 au in order to produce a ring-like image. The depth of the 3.1 $μ$m water ice band depends on the amount of water ice, until it saturates when the optical thickness along the line-of-sight becomes too large. Therefore, quantifying the exact amount of water from absorption bands in edge-on disks requires a detailed analysis of the disk structure and tailored radiative transfer modeling. |
| title | The grazing angle icy protoplanetary disk PDS 453 |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2411.04741 |