Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au

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

doi:10.3847/1538-4365/ac1433

Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au

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

^*Corresponding author for this work

School of Physics and Astronomy

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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.

Original language	English
Article number	15
Number of pages	18
Journal	Astrophysical Journal Supplement Series
Volume	257
Issue number	1
Early online date	3 Nov 2021
DOIs	https://doi.org/10.3847/1538-4365/ac1433
Publication status	Published - Nov 2021

Keywords

Millimeter astronomy
Protoplanetary disks
Planet formation

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Bosman_2021_ApJS_257_15
Copyright © 2021. The American Astronomical Society. All rights reserved. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.3847/1538-4365/ac1433.
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Bosman, A. D., Bergin, E. A., Loomis, R. A., Andrews, S. M., van't Hoff, M. L. R., Teague, R., Öberg, K. I., Guzmán, V. V., Walsh, C., Aikawa, Y., Alarcón, F., Bae, J., Bergner, J. B., Booth, A. S., Cataldi, G., Cleeves, L. I., Czekala, I., Huang, J., Ilee, J. D., ... Zhang, K. (2021). Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au. Astrophysical Journal Supplement Series, 257(1), Article 15. https://doi.org/10.3847/1538-4365/ac1433

@article{9325a7cd2eb648d58d6ea367d5f12362,

title = "Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au",

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.",

keywords = "Millimeter astronomy, Protoplanetary disks, Planet formation",

author = "Bosman, {Arthur D.} and Bergin, {Edwin A.} and Loomis, {Ryan A.} and Andrews, {Sean M.} and {van't Hoff}, {Merel L. R.} and Richard Teague and {\"O}berg, {Karin I.} and Guzm{\'a}n, {Viviana V.} and Catherine Walsh and Yuri Aikawa and Felipe Alarc{\'o}n and Jaehan Bae and Bergner, {Jennifer B.} and Booth, {Alice S.} and Gianni Cataldi and Cleeves, {L. Ilsedore} and Ian Czekala and Jane Huang and Ilee, {John D.} and Law, {Charles J.} and {Le Gal}, Romane and Yao Liu and Feng Long and Fran{\c c}ois M{\'e}nard and Hideko Nomura and P{\'e}rez, {Laura M.} and Chunhua Qi and Schwarz, {Kamber R.} and Anibal Sierra and Takashi Tsukagoshi and Yoshihide Yamato and Wilner, {David J.} and Ke Zhang",

note = "Funding: J.B., J.B.B., I.C., J.H., K. R.S., and K.Z. acknowledge support by NASA through the NASA Hubble Fellowship grant Nos. HST-HF2-51427.001-A, HST-HF2- 51429.001-A, HST-HF2-51405.001-A, HST-HF2-51460.001-A, HST-HF2-51419.001, and HST-HF2-51401.001, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. C.W. acknowledges financial support from the University of Leeds and from the Science and Technology Facilities Council (grant Nos. ST/R000549/1 and ST/T000287/1). A.S.B acknowledges the studentship funded by the Science and Technology Facilities Council of the United Kingdom (STFC). J.D.I. acknowledges support from the Science and Technology Facilities Council of the United Kingdom (STFC) under ST/T000287/1.",

year = "2021",

month = nov,

doi = "10.3847/1538-4365/ac1433",

language = "English",

volume = "257",

journal = "Astrophysical Journal Supplement Series",

issn = "0067-0049",

publisher = "American Astronomical Society",

number = "1",

}

Bosman, AD, Bergin, EA, Loomis, RA, Andrews, SM, van't Hoff, MLR, Teague, R, Öberg, KI, Guzmán, VV, Walsh, C, Aikawa, Y, Alarcón, F, Bae, J, Bergner, JB, Booth, AS, Cataldi, G, Cleeves, LI, Czekala, I, Huang, J, Ilee, JD, Law, CJ, Le Gal, R, Liu, Y, Long, F, Ménard, F, Nomura, H, Pérez, LM, Qi, C, Schwarz, KR, Sierra, A, Tsukagoshi, T, Yamato, Y, Wilner, DJ & Zhang, K 2021, 'Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au', Astrophysical Journal Supplement Series, vol. 257, no. 1, 15. https://doi.org/10.3847/1538-4365/ac1433

TY - JOUR

T1 - Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au

AU - Bosman, Arthur D.

AU - Bergin, Edwin A.

AU - Loomis, Ryan A.

AU - Andrews, Sean M.

AU - van't Hoff, Merel L. R.

AU - Teague, Richard

AU - Öberg, Karin I.

AU - Guzmán, Viviana V.

AU - Walsh, Catherine

AU - Aikawa, Yuri

AU - Alarcón, Felipe

AU - Bae, Jaehan

AU - Bergner, Jennifer B.

AU - Booth, Alice S.

AU - Cataldi, Gianni

AU - Cleeves, L. Ilsedore

AU - Czekala, Ian

AU - Huang, Jane

AU - Ilee, John D.

AU - Law, Charles J.

AU - Le Gal, Romane

AU - Liu, Yao

AU - Long, Feng

AU - Ménard, François

AU - Nomura, Hideko

AU - Pérez, Laura M.

AU - Qi, Chunhua

AU - Schwarz, Kamber R.

AU - Sierra, Anibal

AU - Tsukagoshi, Takashi

AU - Yamato, Yoshihide

AU - Wilner, David J.

AU - Zhang, Ke

N1 - Funding: J.B., J.B.B., I.C., J.H., K. R.S., and K.Z. acknowledge support by NASA through the NASA Hubble Fellowship grant Nos. HST-HF2-51427.001-A, HST-HF2- 51429.001-A, HST-HF2-51405.001-A, HST-HF2-51460.001-A, HST-HF2-51419.001, and HST-HF2-51401.001, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. C.W. acknowledges financial support from the University of Leeds and from the Science and Technology Facilities Council (grant Nos. ST/R000549/1 and ST/T000287/1). A.S.B acknowledges the studentship funded by the Science and Technology Facilities Council of the United Kingdom (STFC). J.D.I. acknowledges support from the Science and Technology Facilities Council of the United Kingdom (STFC) under ST/T000287/1.

PY - 2021/11

Y1 - 2021/11

N2 - 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.

AB - 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.

KW - Millimeter astronomy

KW - Protoplanetary disks

KW - Planet formation

U2 - 10.3847/1538-4365/ac1433

DO - 10.3847/1538-4365/ac1433

M3 - Article

SN - 0067-0049

VL - 257

JO - Astrophysical Journal Supplement Series

JF - Astrophysical Journal Supplement Series

IS - 1

M1 - 15

ER -

Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au

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