Saved in:
| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | https://arxiv.org/abs/2508.10759 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866917058963308544 |
|---|---|
| author | Dutkowska, Katarzyna M. Vermariën, Gijs Viti, Serena Jiménez-Serra, Izaskun Colzi, Laura Busch, Laura A. Rivilla, Víctor M. Mills, Elisabeth A. C. Martín, Sergio Henkel, Christian García, Pablo Lu, Xing Santa-Maria, Miriam G. Armijos-Abendaño, Jairo Hu, Yue Ott, Jürgen Smith, Kai Xu, Fengwei Zeng, Shaoshan Sánchez-Monge, Álvaro Schmiedeke, Anika Pineda, Jaime E. Longmore, Steven N. Lamberts, Thanja |
| author_facet | Dutkowska, Katarzyna M. Vermariën, Gijs Viti, Serena Jiménez-Serra, Izaskun Colzi, Laura Busch, Laura A. Rivilla, Víctor M. Mills, Elisabeth A. C. Martín, Sergio Henkel, Christian García, Pablo Lu, Xing Santa-Maria, Miriam G. Armijos-Abendaño, Jairo Hu, Yue Ott, Jürgen Smith, Kai Xu, Fengwei Zeng, Shaoshan Sánchez-Monge, Álvaro Schmiedeke, Anika Pineda, Jaime E. Longmore, Steven N. Lamberts, Thanja |
| contents | (Abridged) The Central Molecular Zone (CMZ) of the Milky Way exhibits extreme conditions, including high gas densities, elevated temperatures, enhanced cosmic-ray ionization rates, and large-scale dynamics. Large-scale molecular surveys reveal increasing chemical and physical complexity in the CMZ. A key step to interpreting the molecular richness found in the CMZ is to build chemical templates tailored to its diverse conditions. The combined impact of high ionization, elevated temperatures, and dense gas remains insufficiently explored for observable tracers. In this study, we utilized UCLCHEM, a gas-grain time-dependent chemical model, to link physical conditions with their corresponding molecular signatures and identify key tracers of temperature, density, ionization, and shock activity. We ran a grid of models of shocks and protostellar objects representative of typical CMZ conditions, focusing on twenty-four species, including complex organic molecules. Shocked and protostellar environments show distinct evolutionary timescales ($\lesssim 10^4$ vs. $\gtrsim 10^4$ years), with 300 K emerging as a key temperature threshold for chemical differentiation. We find that cosmic-ray ionization and temperature are the main drivers of chemical trends. HCO$^+$, H$_2$CO, and CH$_3$SH trace ionization, while HCO, HCO$^+$, CH$_3$SH, CH$_3$NCO, and HCOOCH$_3$ show consistent abundance contrasts between shocks and protostellar regions over similar temperature ranges. While our models underpredict some complex organics in shocks, they reproduce observed trends for most species, supporting scenarios involving recurring shocks in Galactic Center clouds and enhanced ionization towards Sgr B2(N2). Future work should assess the role of shock recurrence and metallicity in shaping chemistry. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_10759 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Chemical templates of the Central Molecular Zone. Shock and protostellar object signatures under Galactic Center conditions Dutkowska, Katarzyna M. Vermariën, Gijs Viti, Serena Jiménez-Serra, Izaskun Colzi, Laura Busch, Laura A. Rivilla, Víctor M. Mills, Elisabeth A. C. Martín, Sergio Henkel, Christian García, Pablo Lu, Xing Santa-Maria, Miriam G. Armijos-Abendaño, Jairo Hu, Yue Ott, Jürgen Smith, Kai Xu, Fengwei Zeng, Shaoshan Sánchez-Monge, Álvaro Schmiedeke, Anika Pineda, Jaime E. Longmore, Steven N. Lamberts, Thanja Astrophysics of Galaxies (Abridged) The Central Molecular Zone (CMZ) of the Milky Way exhibits extreme conditions, including high gas densities, elevated temperatures, enhanced cosmic-ray ionization rates, and large-scale dynamics. Large-scale molecular surveys reveal increasing chemical and physical complexity in the CMZ. A key step to interpreting the molecular richness found in the CMZ is to build chemical templates tailored to its diverse conditions. The combined impact of high ionization, elevated temperatures, and dense gas remains insufficiently explored for observable tracers. In this study, we utilized UCLCHEM, a gas-grain time-dependent chemical model, to link physical conditions with their corresponding molecular signatures and identify key tracers of temperature, density, ionization, and shock activity. We ran a grid of models of shocks and protostellar objects representative of typical CMZ conditions, focusing on twenty-four species, including complex organic molecules. Shocked and protostellar environments show distinct evolutionary timescales ($\lesssim 10^4$ vs. $\gtrsim 10^4$ years), with 300 K emerging as a key temperature threshold for chemical differentiation. We find that cosmic-ray ionization and temperature are the main drivers of chemical trends. HCO$^+$, H$_2$CO, and CH$_3$SH trace ionization, while HCO, HCO$^+$, CH$_3$SH, CH$_3$NCO, and HCOOCH$_3$ show consistent abundance contrasts between shocks and protostellar regions over similar temperature ranges. While our models underpredict some complex organics in shocks, they reproduce observed trends for most species, supporting scenarios involving recurring shocks in Galactic Center clouds and enhanced ionization towards Sgr B2(N2). Future work should assess the role of shock recurrence and metallicity in shaping chemistry. |
| title | Chemical templates of the Central Molecular Zone. Shock and protostellar object signatures under Galactic Center conditions |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2508.10759 |