Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing Protoplanetary Disk Structure within 20 au - Archive ouverte HAL Access content directly
Journal Articles The Astrophysical Journal Supplement Series Year : 2021

Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing Protoplanetary Disk Structure within 20 au

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Arthur D. Bosman
  • Function : Author
Edwin A. Bergin
  • Function : Author
Ryan A. Loomis
  • Function : Author
Sean M. Andrews
  • Function : Author
Merel L. R. Van'T Hoff
  • Function : Author
Richard Teague
Karin I. Öberg
  • Function : Author
Viviana V. Guzmán
  • Function : Author
Catherine Walsh
  • Function : Author
Yuri Aikawa
Felipe Alarcón
  • Function : Author
Jaehan Bae
Jennifer B. Bergner
  • Function : Author
Alice S. Booth
  • Function : Author
Gianni Cataldi
  • Function : Author
L. Ilsedore Cleeves
  • Function : Author
Ian Czekala
  • Function : Author
Jane Huang
  • Function : Author
John D. Ilee
  • Function : Author
Charles J. Law
  • Function : Author
Yao Liu
  • Function : Author
Feng Long
  • Function : Author
Hideko Nomura
Laura M. Pérez
  • Function : Author
Chunhua Qi
Kamber R. Schwarz
  • Function : Author
Anibal Sierra
  • Function : Author
Takashi Tsukagoshi
Yoshihide Yamato
  • Function : Author
David J. Wilner
  • Function : Author
Ke Zhang
  • Function : Author

Abstract

Constraining the distribution of gas and dust in the inner 20 au of protoplanetary disks is difficult. At the same time, this region is thought to be responsible for most planet formation, especially around the water ice line at 3-10 au. Under the assumption that the gas is in a Keplerian disk, we use the exquisite sensitivity of the Molecules with ALMA at Planet-forming Scales (MAPS) ALMA large program to construct radial surface brightness profiles with a ~3 au effective resolution for the CO isotopologue J = 2-1 lines using the line velocity profile. IM Lup reveals a central depression in 13CO and C18O that is ascribed to a pileup of ~500 M of dust in the inner 20 au, leading to a gas-to-dust ratio of around <10. This pileup is consistent with an efficient drift of grains (≳100 M Myr-1) and a local gas-to-dust ratio that suggests that the streaming instability could be active. The CO isotopologue emission in the GM Aur disk is consistent with a small (~15 au), strongly depleted gas cavity within the ~40 au dust cavity. The radial surface brightness profiles for both the AS 209 and HD 163296 disks show a local minimum and maximum in the C18O emission at the location of a known dust ring (~14 au) and gap (~10 au), respectively. This indicates that the dust ring has a low gas-to-dust ratio (>10) and that the dust gap is gas-rich enough to have optically thick C18O. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.

Dates and versions

insu-03672366 , version 1 (19-05-2022)

Identifiers

Cite

Arthur D. Bosman, Edwin A. Bergin, Ryan A. Loomis, Sean M. Andrews, Merel L. R. Van'T Hoff, et al.. Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing Protoplanetary Disk Structure within 20 au. The Astrophysical Journal Supplement Series, 2021, 257, ⟨10.3847/1538-4365/ac1433⟩. ⟨insu-03672366⟩
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