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| Main Authors: | , , , , , , , , , , , , , |
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| Format: | Preprint |
| Published: |
2025
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2505.04534 |
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| _version_ | 1866913825627832320 |
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| author | Zheng, Yun Yang, Yujiao Zhang, Yong-kun Zheng, Zheng Wang, Jing Staveley-Smith, Lister Tsai, Chao-Wei Li, Di Liu, Chao Hu, Jingjing Chen, Huaxi Quan, Donghui Zheng, Yinghui Li, Hangyuan |
| author_facet | Zheng, Yun Yang, Yujiao Zhang, Yong-kun Zheng, Zheng Wang, Jing Staveley-Smith, Lister Tsai, Chao-Wei Li, Di Liu, Chao Hu, Jingjing Chen, Huaxi Quan, Donghui Zheng, Yinghui Li, Hangyuan |
| contents | Stellar populations serve as a fossil record of galaxy formation and evolution, providing crucial information about the history of star formation and galaxy evolution. The color-magnitude diagram (CMD) stands out as the most accurate tool currently available for inferring the star formation histories (SFHs) of nearby galaxies with stellar-resolved multiband data. The launch of new space telescopes, including JWST, EUCLID, and the upcoming CSST and Roman, will significantly increase the number of stellar-resolved galaxies over the next decade. A user-friendly and customizable CMD fitting package would be valuable for galaxy evolution studies with these data. We develop an open-source Python-based package named \textsc{pancake}, which is fast and accurate in determining SFHs and stellar population parameters in nearby galaxies. We have validated our method via a series of comprehensive tests. First, \textsc{pancake} performs well on mock data, meanwhile the random and systematic uncertainties are quantified. Second, \textsc{pancake} performs well on observational data containing a star cluster and 38 dwarf galaxies (50 fields). Third, the star formation rate (SFR) from \textsc{pancake} is consistent with the SFR from FUV photometry. To ensure compatibility and accuracy, we have included isochrone libraries generated using PARSEC for most of the optical and near-infrared filters used in space telescopes such as HST, JWST, and the upcoming CSST. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_04534 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | PANCAKE: Python bAsed Numerical Color-magnitude-diagram Analysis pacKagE Zheng, Yun Yang, Yujiao Zhang, Yong-kun Zheng, Zheng Wang, Jing Staveley-Smith, Lister Tsai, Chao-Wei Li, Di Liu, Chao Hu, Jingjing Chen, Huaxi Quan, Donghui Zheng, Yinghui Li, Hangyuan Astrophysics of Galaxies Stellar populations serve as a fossil record of galaxy formation and evolution, providing crucial information about the history of star formation and galaxy evolution. The color-magnitude diagram (CMD) stands out as the most accurate tool currently available for inferring the star formation histories (SFHs) of nearby galaxies with stellar-resolved multiband data. The launch of new space telescopes, including JWST, EUCLID, and the upcoming CSST and Roman, will significantly increase the number of stellar-resolved galaxies over the next decade. A user-friendly and customizable CMD fitting package would be valuable for galaxy evolution studies with these data. We develop an open-source Python-based package named \textsc{pancake}, which is fast and accurate in determining SFHs and stellar population parameters in nearby galaxies. We have validated our method via a series of comprehensive tests. First, \textsc{pancake} performs well on mock data, meanwhile the random and systematic uncertainties are quantified. Second, \textsc{pancake} performs well on observational data containing a star cluster and 38 dwarf galaxies (50 fields). Third, the star formation rate (SFR) from \textsc{pancake} is consistent with the SFR from FUV photometry. To ensure compatibility and accuracy, we have included isochrone libraries generated using PARSEC for most of the optical and near-infrared filters used in space telescopes such as HST, JWST, and the upcoming CSST. |
| title | PANCAKE: Python bAsed Numerical Color-magnitude-diagram Analysis pacKagE |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2505.04534 |