exoALMA. II. Data calibration and imaging pipeline

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

doi:10.3847/2041-8213/adc43a

exoALMA. II. Data calibration and imaging pipeline

Ryan A. Loomis^*, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario FlockMisato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida

^*Corresponding author for this work

School of Physics and Astronomy

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

Abstract

The exoALMA Large Program was designed to search for subtle kinematic deviations from Keplerian motion, indicative of embedded planets, in high-angular-resolution and high-spectral-resolution Band 7 observations of ¹²CO, ¹³CO, and CS emission from protoplanetary disks. This Letter summarizes the calibration and imaging pipelines used by the exoALMA collaboration. With sources ranging in diameter from 2.″4 to 13.″8 when probed by ¹²CO, multiple antennae configurations were required to maximally recover all spatial information (including Atacama Compact Array data for seven sources). Combining these data sets warranted particular care in their alignment during calibration and prior to imaging so as not to introduce spurious features that might resemble the kinematic deviations being investigated. Phase decoherence was found in several data sets, which was corrected by an iterative self-calibration procedure, and we explored the effects of the order of operations of spatial alignment, flux scaling, and self-calibration. A number of different imaging sets were produced for the continuum and line emission, employing an iterative masking procedure that minimizes bias due to non-Keplerian motions in the disk.

Original language	English
Article number	L7
Number of pages	20
Journal	Astrophysical Journal Letters
Volume	984
Issue number	1
Early online date	28 Apr 2025
DOIs	https://doi.org/10.3847/2041-8213/adc43a
Publication status	Published - 1 May 2025

Keywords

Protoplanetary disks
Radio interferometry
Observational astronomy
Calibration
Astronomical techniques

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7 Article

exoALMA. I. Science goals, project design, and data products
Teague, R., Benisty, M., Facchini, S., Fukagawa, M., Pinte, C., Andrews, S. M., Bae, J., Barraza-Alfaro, M., Cataldi, G., Cuello, N., Curone, P., Czekala, I., Fasano, D., Flock, M., Galloway-Sprietsma, M., Garg, H., Hall, C., Hammond, I., Hilder, T. & Huang, J. & 21 others, Ilee, J. D., Izquierdo, A. F., Kanagawa, K., Lesur, G., Lodato, G., Longarini, C., Loomis, R. A., Masset, F., Menard, F., Orihara, R., Price, D. J., Rosotti, G., Stadler, J., Testi, L., Yen, H.-W., Wafflard-Fernandez, G., Wilner, D. J., Winter, A. J., Wölfer, L., Yoshida, T. C. & Zawadzki, B., 1 May 2025, In: Astrophysical Journal Letters. 984, 1, 15 p., L6.
Research output: Contribution to journal › Article › peer-review

Open Access
File
exoALMA. III. Line-intensity modeling and system property extraction from protoplanetary disks
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. & Garg, H. & 20 others, Hall, C., Hammond, I., Hilder, T., Huang, J., Ilee, J. D., Isella, A., Kanagawa, K., Lesur, G., Lodato, G., Loomis, R. A., Orihara, R., Price, D. J., Rosotti, G., Testi, L., Yen, H.-W., Wafflard-Fernandez, G., Wilner, D. J., Winter, A. J., Yoshida, T. C. & Zawadzki, B., 1 May 2025, In: Astrophysical Journal Letters. 984, 1, 17 p., L8.
Research output: Contribution to journal › Article › peer-review

Open Access
File
exoALMA. IV. Substructures, asymmetries, and the faint outer disk in continuum emission
Curone, P., Facchini, S., Andrews, S. M., Testi, L., Benisty, M., Czekala, I., Huang, J., Ilee, J. D., Isella, A., Lodato, G., Loomis, R. A., Stadler, J., Winter, A. J., Bae, J., Barraza-Alfaro, M., Cataldi, G., Cuello, N., Fasano, D., Flock, M. & Fukagawa, M. & 19 others, Galloway-Sprietsma, M., Garg, H., Hall, C., Izquierdo, A. F., Kanagawa, K., Lesur, G., Longarini, C., Menard, F., Orihara, R., Pinte, C., Price, D. J., Rosotti, G., Teague, R., Wafflard-Fernandez, G., Wilner, D. J., Wölfer, L., Yen, H.-W., Yoshida, T. C. & Zawadzki, B., 1 May 2025, In: Astrophysical Journal Letters. 984, 1, 36 p., L9.
Research output: Contribution to journal › Article › peer-review

Open Access
File

Cite this

Loomis, R. A., Facchini, S., Benisty, M., Curone, P., Ilee, J. D., Cataldi, G., Yen, H.-W., Teague, R., Pinte, C., Huang, J., Garg, H., Orihara, R., Czekala, I., Zawadzki, B., Andrews, S. M., Wilner, D. J., Bae, J., Barraza-Alfaro, M., Fasano, D., ... Yoshida, T. C. (2025). exoALMA. II. Data calibration and imaging pipeline. Astrophysical Journal Letters, 984(1), Article L7. https://doi.org/10.3847/2041-8213/adc43a

@article{d59688600c8f48349a1efdc39d1c39fe,

title = "exoALMA. II. Data calibration and imaging pipeline",

abstract = "The exoALMA Large Program was designed to search for subtle kinematic deviations from Keplerian motion, indicative of embedded planets, in high-angular-resolution and high-spectral-resolution Band 7 observations of 12CO, 13CO, and CS emission from protoplanetary disks. This Letter summarizes the calibration and imaging pipelines used by the exoALMA collaboration. With sources ranging in diameter from 2.″4 to 13.″8 when probed by 12CO, multiple antennae configurations were required to maximally recover all spatial information (including Atacama Compact Array data for seven sources). Combining these data sets warranted particular care in their alignment during calibration and prior to imaging so as not to introduce spurious features that might resemble the kinematic deviations being investigated. Phase decoherence was found in several data sets, which was corrected by an iterative self-calibration procedure, and we explored the effects of the order of operations of spatial alignment, flux scaling, and self-calibration. A number of different imaging sets were produced for the continuum and line emission, employing an iterative masking procedure that minimizes bias due to non-Keplerian motions in the disk.",

keywords = "Protoplanetary disks, Radio interferometry, Observational astronomy, Calibration, Astronomical techniques",

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

note = "Funding: J.B. acknowledges support from NASA XRP grant No. 80NSSC23K1312. M.B., D.F., and J.S. 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). Computations by JS have been performed on the “Mesocentre SIGAMM” machine, hosted by Observatoire de la Cote d{\textquoteright}Azur. P.C. acknowledges 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. S.F. is funded by the European Union (ERC, UNVEIL, 101076613) and acknowledges financial contribution from PRIN-MUR 2022YP5ACE. M.F. is supported by a Grant-in-Aid from the Japan Society for the Promotion of Science (KAKENHI: No. JP22H01274). J.D.I. acknowledges support from an STFC Ernest Rutherford Fellowship (ST/W004119/1) and a University Academic Fellowship from the University of Leeds. 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. 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. C.P. acknowledges Australian Research Council funding via FT170100040, DP18010423, DP220103767, and DP240103290. 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). FMe received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon Europe research and innovation program (grant agreement No. 101053020, project Dust2Planets). H-W.Y. acknowledges support from the 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)). GWF was granted access to the HPC resources of IDRIS under the allocation A0120402231 made by GENCI. Support for BZ was provided by The Brinson Foundation. T.C.Y. acknowledges support by Grant-In-Aid for JSPS Fellows JP23KJ1008.",

year = "2025",

month = may,

day = "1",

doi = "10.3847/2041-8213/adc43a",

language = "English",

volume = "984",

journal = "Astrophysical Journal Letters",

issn = "2041-8205",

publisher = "American Astronomical Society",

number = "1",

}

Loomis, RA, Facchini, S, Benisty, M, Curone, P, Ilee, JD, Cataldi, G, Yen, H-W, Teague, R, Pinte, C, Huang, J, Garg, H, Orihara, R, Czekala, I, Zawadzki, B, Andrews, SM, Wilner, DJ, Bae, J, Barraza-Alfaro, M, Fasano, D, Flock, M, Fukagawa, M, Galloway-Sprietsma, M, Izquierdo, AF, Kanagawa, K, Lesur, G, Longarini, C, Menard, F, Price, DJ, Rosotti, G, Stadler, J, Wafflard-Fernandez, G, Wölfer, L & Yoshida, TC 2025, 'exoALMA. II. Data calibration and imaging pipeline', Astrophysical Journal Letters, vol. 984, no. 1, L7. https://doi.org/10.3847/2041-8213/adc43a

TY - JOUR

T1 - exoALMA. II. Data calibration and imaging pipeline

AU - Loomis, Ryan A.

AU - Facchini, Stefano

AU - Benisty, Myriam

AU - Curone, Pietro

AU - Ilee, John D.

AU - Cataldi, Gianni

AU - Yen, Hsi-Wei

AU - Teague, Richard

AU - Pinte, Christophe

AU - Huang, Jane

AU - Garg, Himanshi

AU - Orihara, Ryuta

AU - Czekala, Ian

AU - Zawadzki, Brianna

AU - Andrews, Sean M.

AU - Wilner, David J.

AU - Bae, Jaehan

AU - Barraza-Alfaro, Marcelo

AU - Fasano, Daniele

AU - Flock, Mario

AU - Fukagawa, Misato

AU - Galloway-Sprietsma, Maria

AU - Izquierdo, Andrés F.

AU - Kanagawa, Kazuhiro

AU - Lesur, Geoffroy

AU - Longarini, Cristiano

AU - Menard, Francois

AU - Price, Daniel J.

AU - Rosotti, Giovanni

AU - Stadler, Jochen

AU - Wafflard-Fernandez, Gaylor

AU - Wölfer, Lisa

AU - Yoshida, Tomohiro C.

N1 - Funding: J.B. acknowledges support from NASA XRP grant No. 80NSSC23K1312. M.B., D.F., and J.S. 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). Computations by JS have been performed on the “Mesocentre SIGAMM” machine, hosted by Observatoire de la Cote d’Azur. P.C. acknowledges 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. S.F. is funded by the European Union (ERC, UNVEIL, 101076613) and acknowledges financial contribution from PRIN-MUR 2022YP5ACE. M.F. is supported by a Grant-in-Aid from the Japan Society for the Promotion of Science (KAKENHI: No. JP22H01274). J.D.I. acknowledges support from an STFC Ernest Rutherford Fellowship (ST/W004119/1) and a University Academic Fellowship from the University of Leeds. 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. 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. C.P. acknowledges Australian Research Council funding via FT170100040, DP18010423, DP220103767, and DP240103290. 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). FMe received funding from the European Research Council (ERC) under the European Union’s Horizon Europe research and innovation program (grant agreement No. 101053020, project Dust2Planets). H-W.Y. acknowledges support from the 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)). GWF was granted access to the HPC resources of IDRIS under the allocation A0120402231 made by GENCI. Support for BZ was provided by The Brinson Foundation. T.C.Y. acknowledges support by Grant-In-Aid for JSPS Fellows JP23KJ1008.

PY - 2025/5/1

Y1 - 2025/5/1

N2 - The exoALMA Large Program was designed to search for subtle kinematic deviations from Keplerian motion, indicative of embedded planets, in high-angular-resolution and high-spectral-resolution Band 7 observations of 12CO, 13CO, and CS emission from protoplanetary disks. This Letter summarizes the calibration and imaging pipelines used by the exoALMA collaboration. With sources ranging in diameter from 2.″4 to 13.″8 when probed by 12CO, multiple antennae configurations were required to maximally recover all spatial information (including Atacama Compact Array data for seven sources). Combining these data sets warranted particular care in their alignment during calibration and prior to imaging so as not to introduce spurious features that might resemble the kinematic deviations being investigated. Phase decoherence was found in several data sets, which was corrected by an iterative self-calibration procedure, and we explored the effects of the order of operations of spatial alignment, flux scaling, and self-calibration. A number of different imaging sets were produced for the continuum and line emission, employing an iterative masking procedure that minimizes bias due to non-Keplerian motions in the disk.

AB - The exoALMA Large Program was designed to search for subtle kinematic deviations from Keplerian motion, indicative of embedded planets, in high-angular-resolution and high-spectral-resolution Band 7 observations of 12CO, 13CO, and CS emission from protoplanetary disks. This Letter summarizes the calibration and imaging pipelines used by the exoALMA collaboration. With sources ranging in diameter from 2.″4 to 13.″8 when probed by 12CO, multiple antennae configurations were required to maximally recover all spatial information (including Atacama Compact Array data for seven sources). Combining these data sets warranted particular care in their alignment during calibration and prior to imaging so as not to introduce spurious features that might resemble the kinematic deviations being investigated. Phase decoherence was found in several data sets, which was corrected by an iterative self-calibration procedure, and we explored the effects of the order of operations of spatial alignment, flux scaling, and self-calibration. A number of different imaging sets were produced for the continuum and line emission, employing an iterative masking procedure that minimizes bias due to non-Keplerian motions in the disk.

KW - Protoplanetary disks

KW - Radio interferometry

KW - Observational astronomy

KW - Calibration

KW - Astronomical techniques

U2 - 10.3847/2041-8213/adc43a

DO - 10.3847/2041-8213/adc43a

M3 - Article

SN - 2041-8205

VL - 984

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 1

M1 - L7

ER -

exoALMA. II. Data calibration and imaging pipeline

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Keywords

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Research output

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

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

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

Cite this