Translators of Galaxy Morphology Indicators between Observation and Simulation
Based on the recent advancements in numerical simulations of galaxy formation, we anticipate the achievement of realistic models of galaxies in the near future. Morphology is the most basic and fundamental property of galaxies, yet observations and simulations still use different methods to determin...
| Main Authors: | , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/accd68 |
| _version_ | 1797694766753775616 |
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| author | J. K. Jang Sukyoung K. Yi Yohan Dubois Jinsu Rhee Christophe Pichon Taysun Kimm Julien Devriendt Marta Volonteri Sugata Kaviraj Sebastien Peirani Sree Oh Scott Croom |
| author_facet | J. K. Jang Sukyoung K. Yi Yohan Dubois Jinsu Rhee Christophe Pichon Taysun Kimm Julien Devriendt Marta Volonteri Sugata Kaviraj Sebastien Peirani Sree Oh Scott Croom |
| author_sort | J. K. Jang |
| collection | DOAJ |
| description | Based on the recent advancements in numerical simulations of galaxy formation, we anticipate the achievement of realistic models of galaxies in the near future. Morphology is the most basic and fundamental property of galaxies, yet observations and simulations still use different methods to determine galaxy morphology, making it difficult to compare them. We hereby perform a test on the recent NewHorizon simulation, which has spatial and mass resolutions that are remarkably high for a large-volume simulation, to resolve the situation. We generate mock images for the simulated galaxies using SKIRT, which calculates complex radiative transfer processes in each galaxy. We measure morphological and kinematic indicators using photometric and spectroscopic methods following observers’ techniques. We also measure the kinematic disk-to-total ratios using the Gaussian mixture model and assume that they represent the true structural composition of galaxies. We found that spectroscopic indicators such as V / σ and λ _R closely trace the kinematic disk-to-total ratios. In contrast, photometric disk-to-total ratios based on the radial profile fitting method often fail to recover the true kinematic structure of galaxies, especially small ones. We provide translating equations between various morphological indicators. |
| first_indexed | 2024-03-12T03:02:34Z |
| format | Article |
| id | doaj.art-e2876c6bc3234aa8ad0810c71d06b760 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:02:34Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-e2876c6bc3234aa8ad0810c71d06b7602023-09-03T14:38:33ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-019501410.3847/1538-4357/accd68Translators of Galaxy Morphology Indicators between Observation and SimulationJ. K. Jang0Sukyoung K. Yi1https://orcid.org/0000-0002-4556-2619Yohan Dubois2https://orcid.org/0000-0003-0225-6387Jinsu Rhee3https://orcid.org/0000-0002-0184-9589Christophe Pichon4https://orcid.org/0000-0003-0695-6735Taysun Kimm5https://orcid.org/0000-0002-3950-3997Julien Devriendt6https://orcid.org/0000-0002-8140-0422Marta Volonteri7https://orcid.org/0000-0002-3216-1322Sugata Kaviraj8Sebastien Peirani9Sree Oh10https://orcid.org/0000-0002-4731-9604Scott Croom11https://orcid.org/0000-0003-2880-9197Department of Astronomy and Yonsei University Observatory, Yonsei University , Seoul 03722, Republic of Korea ; yi@yonsei.ac.krDepartment of Astronomy and Yonsei University Observatory, Yonsei University , Seoul 03722, Republic of Korea ; yi@yonsei.ac.krInstitut d’Astrophysique de Paris, Sorbonne Université , CNRS, UMR 7095, 98 bis bd Arago, F-75014 Paris, FranceDepartment of Astronomy and Yonsei University Observatory, Yonsei University , Seoul 03722, Republic of Korea ; yi@yonsei.ac.krInstitut d’Astrophysique de Paris, Sorbonne Université , CNRS, UMR 7095, 98 bis bd Arago, F-75014 Paris, FranceDepartment of Astronomy and Yonsei University Observatory, Yonsei University , Seoul 03722, Republic of Korea ; yi@yonsei.ac.krDepartment of Physics, University of Oxford , Keble Road, Oxford OX1 3RH, UKInstitut d’Astrophysique de Paris, Sorbonne Université , CNRS, UMR 7095, 98 bis bd Arago, F-75014 Paris, FranceUniversity of Hertfordshire , Hatfield, Hertfordshire, UKUniversité Côte d’Azur , Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, FranceDepartment of Astronomy and Yonsei University Observatory, Yonsei University , Seoul 03722, Republic of Korea ; yi@yonsei.ac.kr; Research School of Astronomy and Astrophysics, Australian National University , Canberra, ACT 2611, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , AustraliaARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , Australia; Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney , NSW 2006, AustraliaBased on the recent advancements in numerical simulations of galaxy formation, we anticipate the achievement of realistic models of galaxies in the near future. Morphology is the most basic and fundamental property of galaxies, yet observations and simulations still use different methods to determine galaxy morphology, making it difficult to compare them. We hereby perform a test on the recent NewHorizon simulation, which has spatial and mass resolutions that are remarkably high for a large-volume simulation, to resolve the situation. We generate mock images for the simulated galaxies using SKIRT, which calculates complex radiative transfer processes in each galaxy. We measure morphological and kinematic indicators using photometric and spectroscopic methods following observers’ techniques. We also measure the kinematic disk-to-total ratios using the Gaussian mixture model and assume that they represent the true structural composition of galaxies. We found that spectroscopic indicators such as V / σ and λ _R closely trace the kinematic disk-to-total ratios. In contrast, photometric disk-to-total ratios based on the radial profile fitting method often fail to recover the true kinematic structure of galaxies, especially small ones. We provide translating equations between various morphological indicators.https://doi.org/10.3847/1538-4357/accd68Galaxy classification systemsGalaxy kinematicsGalaxy structure |
| spellingShingle | J. K. Jang Sukyoung K. Yi Yohan Dubois Jinsu Rhee Christophe Pichon Taysun Kimm Julien Devriendt Marta Volonteri Sugata Kaviraj Sebastien Peirani Sree Oh Scott Croom Translators of Galaxy Morphology Indicators between Observation and Simulation The Astrophysical Journal Galaxy classification systems Galaxy kinematics Galaxy structure |
| title | Translators of Galaxy Morphology Indicators between Observation and Simulation |
| title_full | Translators of Galaxy Morphology Indicators between Observation and Simulation |
| title_fullStr | Translators of Galaxy Morphology Indicators between Observation and Simulation |
| title_full_unstemmed | Translators of Galaxy Morphology Indicators between Observation and Simulation |
| title_short | Translators of Galaxy Morphology Indicators between Observation and Simulation |
| title_sort | translators of galaxy morphology indicators between observation and simulation |
| topic | Galaxy classification systems Galaxy kinematics Galaxy structure |
| url | https://doi.org/10.3847/1538-4357/accd68 |
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