PEACHES IV: Tracing the Formation & Evolution of C$_2$H in Perseus Low-Mass Protostars
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arXiv
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| Autori principali: | , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866911093664776192 |
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| author | Anderson, Jack G. Bergner, Jennifer B. Yang, Yao-Lun Zhang, Yichen Sakai, Nami |
| author_facet | Anderson, Jack G. Bergner, Jennifer B. Yang, Yao-Lun Zhang, Yichen Sakai, Nami |
| contents | The radical hydrocarbon molecule C$_2$H is widely detected in various stages of star and planet formation, and has emerged as a useful tracer of high-C/O gas within the photochemically active surface layers of mature (Class II) protoplanetary disks. However, the chemistry and evolution of C$_2$H within younger (Class 0/I) protostars remains much more poorly understood. Here, using data observed as part of the PEACHES survey along with new ALMA ACA observations, we investigate the C$_2$H emission towards an unbiased sample of 35 Class 0/I low-mass protostars in Perseus. With this large sample, we identify a clear association between C$_2$H emission and the protostellar outflow cavity walls, and a consistent spatial anti-correlation between C$_2$H and SO emission. Together, these trends confirm that C$_2$H is tracing photochemically active, O-poor gas in these younger sources. We fitted the C$_2$H spectra with a simple LTE model to yield column density maps, and find values ranging from 10$^{14}$ -- 10$^{15}$ cm$^{-2}$ in these sources. We also looked for trends in the C$_2$H emission morphology as a function of various protostellar evolutionary metrics, but find no clear patterns: the C$_2$H emission remains spatially extended in most sources, independent of age. This indicates that the transition to the compact C$_2$H emission observed on the surface of Class II disks must happen rapidly, sometime just after the embedded stage. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_03918 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | PEACHES IV: Tracing the Formation & Evolution of C$_2$H in Perseus Low-Mass Protostars Anderson, Jack G. Bergner, Jennifer B. Yang, Yao-Lun Zhang, Yichen Sakai, Nami Astrophysics of Galaxies Solar and Stellar Astrophysics The radical hydrocarbon molecule C$_2$H is widely detected in various stages of star and planet formation, and has emerged as a useful tracer of high-C/O gas within the photochemically active surface layers of mature (Class II) protoplanetary disks. However, the chemistry and evolution of C$_2$H within younger (Class 0/I) protostars remains much more poorly understood. Here, using data observed as part of the PEACHES survey along with new ALMA ACA observations, we investigate the C$_2$H emission towards an unbiased sample of 35 Class 0/I low-mass protostars in Perseus. With this large sample, we identify a clear association between C$_2$H emission and the protostellar outflow cavity walls, and a consistent spatial anti-correlation between C$_2$H and SO emission. Together, these trends confirm that C$_2$H is tracing photochemically active, O-poor gas in these younger sources. We fitted the C$_2$H spectra with a simple LTE model to yield column density maps, and find values ranging from 10$^{14}$ -- 10$^{15}$ cm$^{-2}$ in these sources. We also looked for trends in the C$_2$H emission morphology as a function of various protostellar evolutionary metrics, but find no clear patterns: the C$_2$H emission remains spatially extended in most sources, independent of age. This indicates that the transition to the compact C$_2$H emission observed on the surface of Class II disks must happen rapidly, sometime just after the embedded stage. |
| title | PEACHES IV: Tracing the Formation & Evolution of C$_2$H in Perseus Low-Mass Protostars |
| topic | Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2508.03918 |