exoALMA XV: Interpreting the height of CO emission layer
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arXiv
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| author | Rosotti, Giovanni P. Longarini, Cristiano Paneque-Carreño, Teresa Cataldi, Gianni Galloway-Sprietsma, Maria Andrews, Sean M. Bae, Jaehan Barraza-Alfaro, Marcelo Benisty, Myriam Curone, Pietro Czekala, Ian Facchini, Stefano Fasano, Daniele Flock, Mario Fukagawa, Misato Garg, Himanshi Hall, Cassandra Huang, Jane Ilee, John D. Izquierdo, Andrés F. Kanagawa, Kazuhiro Lesur, Geoffroy Lodato, Giuseppe Loomis, Ryan A. Orihara, Ryuta Pinte, Christophe Price, Daniel J. Stadler, Jochen Teague, Richard Wafflard-Fernandez, Gaylor Winter, Andrew J. Wölfer, Lisa Yen, Hsi-Wei Yoshida, Tomohiro C. Zawadzki, Brianna |
| author_facet | Rosotti, Giovanni P. Longarini, Cristiano Paneque-Carreño, Teresa Cataldi, Gianni Galloway-Sprietsma, Maria Andrews, Sean M. Bae, Jaehan Barraza-Alfaro, Marcelo Benisty, Myriam Curone, Pietro Czekala, Ian Facchini, Stefano Fasano, Daniele Flock, Mario Fukagawa, Misato Garg, Himanshi Hall, Cassandra Huang, Jane Ilee, John D. Izquierdo, Andrés F. Kanagawa, Kazuhiro Lesur, Geoffroy Lodato, Giuseppe Loomis, Ryan A. Orihara, Ryuta Pinte, Christophe Price, Daniel J. Stadler, Jochen Teague, Richard Wafflard-Fernandez, Gaylor Winter, Andrew J. Wölfer, Lisa Yen, Hsi-Wei Yoshida, Tomohiro C. Zawadzki, Brianna |
| contents | The availability of exquisite data and the development of new analysis techniques have enabled the study of emitting heights in proto-planetary disks. In this paper we introduce a simple model linking the emitting height of CO to the disk surface density and temperature structure. We then apply the model to measurements of the emitting height and disk temperature conducted as part of exoALMA, integrated with additional legacy measurements from the MAPS Large Programme, to derive CO column densities and surface density profiles (assuming a CO abundance) for a total of 14 disks. A unique feature of the method we introduce to measure surface densities is that it can be applied to optically thick observations, rather than optically thin as conventionally done. While we use our method on a sample of well studied disks where temperature structures have been derived using two emission lines, we show that reasonably accurate estimates can be obtained also when only one molecular transition is available. With our method we obtain independent constraints from $^{12}$CO and $^{13}$CO and we find they are in general good agreement using the standard $^{12}$C/$^{13}$C isotopic ratio. The masses derived from our method are systematically lower compared with the values derived dynamically from the rotation curve if using an ISM CO abundance, implying that CO is depleted by a median factor $\sim$20 with respect to the ISM value, in line with other works that find that CO is depleted in proto-planetary disks. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2504_20012 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | exoALMA XV: Interpreting the height of CO emission layer Rosotti, Giovanni P. Longarini, Cristiano Paneque-Carreño, Teresa Cataldi, Gianni Galloway-Sprietsma, Maria Andrews, Sean M. Bae, Jaehan Barraza-Alfaro, Marcelo Benisty, Myriam Curone, Pietro Czekala, Ian Facchini, Stefano Fasano, Daniele Flock, Mario Fukagawa, Misato Garg, Himanshi Hall, Cassandra Huang, Jane Ilee, John D. Izquierdo, Andrés F. Kanagawa, Kazuhiro Lesur, Geoffroy Lodato, Giuseppe Loomis, Ryan A. Orihara, Ryuta Pinte, Christophe Price, Daniel J. Stadler, Jochen Teague, Richard Wafflard-Fernandez, Gaylor Winter, Andrew J. Wölfer, Lisa Yen, Hsi-Wei Yoshida, Tomohiro C. Zawadzki, Brianna Earth and Planetary Astrophysics Astrophysics of Galaxies Solar and Stellar Astrophysics The availability of exquisite data and the development of new analysis techniques have enabled the study of emitting heights in proto-planetary disks. In this paper we introduce a simple model linking the emitting height of CO to the disk surface density and temperature structure. We then apply the model to measurements of the emitting height and disk temperature conducted as part of exoALMA, integrated with additional legacy measurements from the MAPS Large Programme, to derive CO column densities and surface density profiles (assuming a CO abundance) for a total of 14 disks. A unique feature of the method we introduce to measure surface densities is that it can be applied to optically thick observations, rather than optically thin as conventionally done. While we use our method on a sample of well studied disks where temperature structures have been derived using two emission lines, we show that reasonably accurate estimates can be obtained also when only one molecular transition is available. With our method we obtain independent constraints from $^{12}$CO and $^{13}$CO and we find they are in general good agreement using the standard $^{12}$C/$^{13}$C isotopic ratio. The masses derived from our method are systematically lower compared with the values derived dynamically from the rotation curve if using an ISM CO abundance, implying that CO is depleted by a median factor $\sim$20 with respect to the ISM value, in line with other works that find that CO is depleted in proto-planetary disks. |
| title | exoALMA XV: Interpreting the height of CO emission layer |
| topic | Earth and Planetary Astrophysics Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2504.20012 |