Artículos de revistas
Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au
Fecha
2021Registro en:
The Astrophysical Journal Supplement Series, 257:15 (18pp), 2021 November
10.3847/1538-4365/ac1433
Autor
Bosman, Arthur D.
Bergin, Edwin A.
Loomis, Ryan A.
Andrews, Sean M.
Van't Hoff, Merel L. R.
Teague, Richard
Oberg, Karin
Guzmán, Viviana V.
Walsh, Catherine
Aikawa, Yuri
Alarcón, Felipe
Bae, Jaehan
Bergner, Jennifer B.
Booth, Alice S.
Cataldi, Gianni
Cleeves, L. Ilsedore
Czekala, Ian
Huang, Jane
Ilee, John D.
Law, Charles J.
Le Gal, Romane
Liu, Yao
Long, Feng
Menard, Francois
Nomura, Hideko
Pérez Muñoz, Laura
Qi, Chunhua
Schwarz, Kamber R.
Sierra, Aníbal
Tsukagoshi, Takashi
Yamato, Yoshihide
Wilner, David J.
Zhang, Ke
Institución
Resumen
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.