exoALMA. III. Line-intensity modeling and system property extraction from protoplanetary disks

Andrés F. Izquierdo; Jochen Stadler; Maria Galloway-Sprietsma; Myriam Benisty; Christophe Pinte; Jaehan Bae; Richard Teague; Stefano Facchini; Lisa Wölfer; Cristiano Longarini; Pietro Curone; Sean M. Andrews; Marcelo Barraza-Alfaro; Gianni Cataldi; Nicolás Cuello; Ian Czekala; Daniele Fasano; Mario Flock; Misato Fukagawa; Himanshi Garg; Cassandra Hall; Iain Hammond; Thomas Hilder; Jane Huang; John D. Ilee; Andrea Isella; Kazuhiro Kanagawa; Geoffroy Lesur; Giuseppe Lodato; Ryan A. Loomis; Ryuta Orihara; Daniel J. Price; Giovanni Rosotti; Leonardo Testi; Hsi-Wei Yen; Gaylor Wafflard-Fernandez; David J. Wilner; Andrew J. Winter; Tomohiro C. Yoshida; Brianna Zawadzki

doi:10.3847/2041-8213/adc439

exoALMA. III. Line-intensity modeling and system property extraction from protoplanetary disks

Andrés F. Izquierdo^*, Jochen Stadler, Maria Galloway-Sprietsma, Myriam Benisty, Christophe Pinte, Jaehan Bae, Richard Teague, Stefano Facchini, Lisa Wölfer, Cristiano Longarini, Pietro Curone, Sean M. Andrews, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Ian Czekala, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi GargCassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Ryan A. Loomis, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Tomohiro C. Yoshida, Brianna Zawadzki

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

The ALMA large program exoALMA offers a unique window into the three-dimensional physical and dynamical properties of 15 circumstellar disks where planets may be actively forming. Here, we present an analysis methodology to map the gas disk structure and substructure encoded in ¹²CO, ¹³CO, and CS line emission from our targets. To model and characterize the disk structure probed by optically thin species, such as CS and, in some cases, ¹³CO, we introduce a composite line profile kernel that accounts for increased intensities caused by the projected overlap between the disk’s front and back side emission. Our workflow, built on the discminer modeling framework, incorporates an improved iterative two-component fitting method for inclined sources (i > 40°) to mitigate the impact of the disk back side on the extraction of velocity maps. Also, we report best-fit parameters for the Keplerian stellar masses, as well as inclinations, position angles, systemic velocities, rotation direction, and emission surfaces of the disks in our sample.

Original language	English
Article number	L8
Number of pages	17
Journal	Astrophysical Journal Letters
Volume	984
Issue number	1
Early online date	28 Apr 2025
DOIs	https://doi.org/10.3847/2041-8213/adc439
Publication status	Published - 1 May 2025

Keywords

Protoplanetary disks
Exoplanets
Planet formation

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Izquierdo, A. F., Stadler, J., Galloway-Sprietsma, M., Benisty, M., Pinte, C., Bae, J., Teague, R., Facchini, S., Wölfer, L., Longarini, C., Curone, P., Andrews, S. M., Barraza-Alfaro, M., Cataldi, G., Cuello, N., Czekala, I., Fasano, D., Flock, M., Fukagawa, M., ... Zawadzki, B. (2025). exoALMA. III. Line-intensity modeling and system property extraction from protoplanetary disks. Astrophysical Journal Letters, 984(1), Article L8. https://doi.org/10.3847/2041-8213/adc439

@article{1a2e279f153445e8875bf7aeea71e0a8,

title = "exoALMA. III. Line-intensity modeling and system property extraction from protoplanetary disks",

abstract = "The ALMA large program exoALMA offers a unique window into the three-dimensional physical and dynamical properties of 15 circumstellar disks where planets may be actively forming. Here, we present an analysis methodology to map the gas disk structure and substructure encoded in 12CO, 13CO, and CS line emission from our targets. To model and characterize the disk structure probed by optically thin species, such as CS and, in some cases, 13CO, we introduce a composite line profile kernel that accounts for increased intensities caused by the projected overlap between the disk{\textquoteright}s front and back side emission. Our workflow, built on the discminer modeling framework, incorporates an improved iterative two-component fitting method for inclined sources (i > 40°) to mitigate the impact of the disk back side on the extraction of velocity maps. Also, we report best-fit parameters for the Keplerian stellar masses, as well as inclinations, position angles, systemic velocities, rotation direction, and emission surfaces of the disks in our sample.",

keywords = "Protoplanetary disks, Exoplanets, Planet formation",

author = "Izquierdo, \{Andr{\'e}s F.\} and Jochen Stadler and Maria Galloway-Sprietsma and Myriam Benisty and Christophe Pinte and Jaehan Bae and Richard Teague and Stefano Facchini and Lisa W{\"o}lfer and Cristiano Longarini and Pietro Curone and Andrews, \{Sean M.\} and Marcelo Barraza-Alfaro and Gianni Cataldi and Nicol{\'a}s Cuello and Ian Czekala and Daniele Fasano and Mario Flock and Misato Fukagawa and Himanshi Garg and Cassandra Hall and Iain Hammond and Thomas Hilder and Jane Huang and Ilee, \{John D.\} and Andrea Isella and Kazuhiro Kanagawa and Geoffroy Lesur and Giuseppe Lodato and Loomis, \{Ryan A.\} and Ryuta Orihara and Price, \{Daniel J.\} and Giovanni Rosotti and Leonardo Testi and Hsi-Wei Yen and Gaylor Wafflard-Fernandez and Wilner, \{David J.\} and Winter, \{Andrew J.\} and Yoshida, \{Tomohiro C.\} and Brianna Zawadzki",

note = "Funding: Support for AFI was provided by NASA through the NASA Hubble Fellowship grant No. HST-HF2-51532.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. J.S., M.B., D.F. have received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation program (PROTOPLANETS, grant agreement No. 101002188). C.P. acknowledges Australian Research Council funding via FT170100040, DP18010423, DP220103767, and DP240103290. J.B. acknowledges support from NASA XRP grant No. 80NSSC23K1312. S.F. is funded by the European Union (ERC, UNVEIL, 101076613), and acknowledges financial contribution from PRIN-MUR 2022YP5ACE. C.L. has received funding from the European Union{\textquoteright}s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 823823 (DUSTBUSTERS) and by the UK Science and Technology research Council (STFC) via the consolidated grant ST/W000997/1. P.C. and L.T. acknowledge support by the Italian Ministero dell{\textquoteright}Istruzione, Universit{\`a} e Ricerca through the grant Progetti Premiali 2012—iALMA (CUP C52I13000140001) and by the ANID BASAL project FB210003. N.C. has received funding from the European Research Council (ERC) under the European Union Horizon Europe research and innovation program (grant agreement No. 101042275, project Stellar-MADE). M.F. has received funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (grant agreement No. 757957). M.F. is supported by a Grant-in-Aid from the Japan Society for the Promotion of Science (KAKENHI: No. JP22H01274). C.H. acknowledges support from NSF AAG grant No. 2407679. I.H. and T.H. are supported by an Australian Government Research Training Program (RTP) Scholarship. J.D.I. acknowledges support from an STFC Ernest Rutherford Fellowship (ST/W004119/1) and a University Academic Fellowship from the University of Leeds. A.I. acknowledges support from the National Aeronautics and Space Administration under grant No. 80NSSC18K0828. G.L. has received funding from the European Union{\textquoteright}s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 823823 (DUSTBUSTERS). D.P. acknowledges Australian Research Council funding via DP18010423, DP220103767, and DP240103290. G.R. acknowledges funding from the Fondazione Cariplo, grant No. 2022-1217, and the European Research Council (ERC) under the European Union{\textquoteright}s Horizon Europe Research \& Innovation Programme under grant agreement No. 101039651 (DiscEvol). H.-W.Y. acknowledges support from National Science and Technology Council (NSTC) in Taiwan through grant NSTC 113-2112-M-001-035- and from the Academia Sinica Career Development Award (AS-CDA-111-M03). G.W.F. acknowledges support from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 815559 (MHDiscs)). G.W.F. was granted access to the HPC resources of IDRIS under the allocation A0120402231 made by GENCI. A.J.W. has received funding from the European Union{\textquoteright}s Horizon 2020 research and innovation program under the Marie Sk{\l}odowska-Curie grant agreement No. 101104656. T.C.Y. acknowledges support by Grant-in-Aid for JSPS Fellows JP23KJ1008. Support for B.Z. was provided by The Brinson Foundation. This work was partly supported by the Deutsche Forschungsgemein- schaft (DFG, German Research Foundation)—Ref no. 325594231 FOR 2634/2 TE 1024/2-1, and by the DFG Cluster of Excellence Origins (www.origins-cluster.de). This project has received funding from the European Research Council (ERC) via the ERC Synergy Grant ECOGAL (grant 855130).",

year = "2025",

month = may,

day = "1",

doi = "10.3847/2041-8213/adc439",

language = "English",

volume = "984",

journal = "Astrophysical Journal Letters",

issn = "2041-8205",

publisher = "American Astronomical Society",

number = "1",

}

Izquierdo, AF, Stadler, J, Galloway-Sprietsma, M, Benisty, M, Pinte, C, Bae, J, Teague, R, Facchini, S, Wölfer, L, Longarini, C, Curone, P, Andrews, SM, Barraza-Alfaro, M, Cataldi, G, Cuello, N, Czekala, I, Fasano, D, Flock, M, Fukagawa, M, Garg, H, Hall, C, Hammond, I, Hilder, T, Huang, J, Ilee, JD, Isella, A, Kanagawa, K, Lesur, G, Lodato, G, Loomis, RA, Orihara, R, Price, DJ, Rosotti, G, Testi, L, Yen, H-W, Wafflard-Fernandez, G, Wilner, DJ, Winter, AJ, Yoshida, TC & Zawadzki, B 2025, 'exoALMA. III. Line-intensity modeling and system property extraction from protoplanetary disks', Astrophysical Journal Letters, vol. 984, no. 1, L8. https://doi.org/10.3847/2041-8213/adc439

TY - JOUR

T1 - exoALMA. III. Line-intensity modeling and system property extraction from protoplanetary disks

AU - Izquierdo, Andrés F.

AU - Stadler, Jochen

AU - Galloway-Sprietsma, Maria

AU - Benisty, Myriam

AU - Pinte, Christophe

AU - Bae, Jaehan

AU - Teague, Richard

AU - Facchini, Stefano

AU - Wölfer, Lisa

AU - Longarini, Cristiano

AU - Curone, Pietro

AU - Andrews, Sean M.

AU - Barraza-Alfaro, Marcelo

AU - Cataldi, Gianni

AU - Cuello, Nicolás

AU - Czekala, Ian

AU - Fasano, Daniele

AU - Flock, Mario

AU - Fukagawa, Misato

AU - Garg, Himanshi

AU - Hall, Cassandra

AU - Hammond, Iain

AU - Hilder, Thomas

AU - Huang, Jane

AU - Ilee, John D.

AU - Isella, Andrea

AU - Kanagawa, Kazuhiro

AU - Lesur, Geoffroy

AU - Lodato, Giuseppe

AU - Loomis, Ryan A.

AU - Orihara, Ryuta

AU - Price, Daniel J.

AU - Rosotti, Giovanni

AU - Testi, Leonardo

AU - Yen, Hsi-Wei

AU - Wafflard-Fernandez, Gaylor

AU - Wilner, David J.

AU - Winter, Andrew J.

AU - Yoshida, Tomohiro C.

AU - Zawadzki, Brianna

N1 - Funding: Support for AFI was provided by NASA through the NASA Hubble Fellowship grant No. HST-HF2-51532.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. J.S., M.B., D.F. have received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (PROTOPLANETS, grant agreement No. 101002188). C.P. acknowledges Australian Research Council funding via FT170100040, DP18010423, DP220103767, and DP240103290. J.B. acknowledges support from NASA XRP grant No. 80NSSC23K1312. S.F. is funded by the European Union (ERC, UNVEIL, 101076613), and acknowledges financial contribution from PRIN-MUR 2022YP5ACE. C.L. has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 823823 (DUSTBUSTERS) and by the UK Science and Technology research Council (STFC) via the consolidated grant ST/W000997/1. P.C. and L.T. acknowledge support by the Italian Ministero dell’Istruzione, Università e Ricerca through the grant Progetti Premiali 2012—iALMA (CUP C52I13000140001) and by the ANID BASAL project FB210003. N.C. has received funding from the European Research Council (ERC) under the European Union Horizon Europe research and innovation program (grant agreement No. 101042275, project Stellar-MADE). M.F. has received funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (grant agreement No. 757957). M.F. is supported by a Grant-in-Aid from the Japan Society for the Promotion of Science (KAKENHI: No. JP22H01274). C.H. acknowledges support from NSF AAG grant No. 2407679. I.H. and T.H. are supported by an Australian Government Research Training Program (RTP) Scholarship. J.D.I. acknowledges support from an STFC Ernest Rutherford Fellowship (ST/W004119/1) and a University Academic Fellowship from the University of Leeds. A.I. acknowledges support from the National Aeronautics and Space Administration under grant No. 80NSSC18K0828. G.L. has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 823823 (DUSTBUSTERS). D.P. acknowledges Australian Research Council funding via DP18010423, DP220103767, and DP240103290. G.R. acknowledges funding from the Fondazione Cariplo, grant No. 2022-1217, and the European Research Council (ERC) under the European Union’s Horizon Europe Research & Innovation Programme under grant agreement No. 101039651 (DiscEvol). H.-W.Y. acknowledges support from National Science and Technology Council (NSTC) in Taiwan through grant NSTC 113-2112-M-001-035- and from the Academia Sinica Career Development Award (AS-CDA-111-M03). G.W.F. acknowledges support from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 815559 (MHDiscs)). G.W.F. was granted access to the HPC resources of IDRIS under the allocation A0120402231 made by GENCI. A.J.W. has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101104656. T.C.Y. acknowledges support by Grant-in-Aid for JSPS Fellows JP23KJ1008. Support for B.Z. was provided by The Brinson Foundation. This work was partly supported by the Deutsche Forschungsgemein- schaft (DFG, German Research Foundation)—Ref no. 325594231 FOR 2634/2 TE 1024/2-1, and by the DFG Cluster of Excellence Origins (www.origins-cluster.de). This project has received funding from the European Research Council (ERC) via the ERC Synergy Grant ECOGAL (grant 855130).

PY - 2025/5/1

Y1 - 2025/5/1

N2 - The ALMA large program exoALMA offers a unique window into the three-dimensional physical and dynamical properties of 15 circumstellar disks where planets may be actively forming. Here, we present an analysis methodology to map the gas disk structure and substructure encoded in 12CO, 13CO, and CS line emission from our targets. To model and characterize the disk structure probed by optically thin species, such as CS and, in some cases, 13CO, we introduce a composite line profile kernel that accounts for increased intensities caused by the projected overlap between the disk’s front and back side emission. Our workflow, built on the discminer modeling framework, incorporates an improved iterative two-component fitting method for inclined sources (i > 40°) to mitigate the impact of the disk back side on the extraction of velocity maps. Also, we report best-fit parameters for the Keplerian stellar masses, as well as inclinations, position angles, systemic velocities, rotation direction, and emission surfaces of the disks in our sample.

AB - The ALMA large program exoALMA offers a unique window into the three-dimensional physical and dynamical properties of 15 circumstellar disks where planets may be actively forming. Here, we present an analysis methodology to map the gas disk structure and substructure encoded in 12CO, 13CO, and CS line emission from our targets. To model and characterize the disk structure probed by optically thin species, such as CS and, in some cases, 13CO, we introduce a composite line profile kernel that accounts for increased intensities caused by the projected overlap between the disk’s front and back side emission. Our workflow, built on the discminer modeling framework, incorporates an improved iterative two-component fitting method for inclined sources (i > 40°) to mitigate the impact of the disk back side on the extraction of velocity maps. Also, we report best-fit parameters for the Keplerian stellar masses, as well as inclinations, position angles, systemic velocities, rotation direction, and emission surfaces of the disks in our sample.

KW - Protoplanetary disks

KW - Exoplanets

KW - Planet formation

UR - https://www.scopus.com/pages/publications/105003961803

U2 - 10.3847/2041-8213/adc439

DO - 10.3847/2041-8213/adc439

M3 - Article

AN - SCOPUS:105003961803

SN - 2041-8205

VL - 984

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 1

M1 - L8

ER -

exoALMA. III. Line-intensity modeling and system property extraction from protoplanetary disks

Abstract

Keywords

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exoALMA. I. Science goals, project design, and data products

exoALMA. II. Data calibration and imaging pipeline

exoALMA. IV. Substructures, asymmetries, and the faint outer disk in continuum emission

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