Central Velocity Dispersion being the Primary Driver of Abundance Patterns in Quenched Galaxies
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866912247489495040 |
|---|---|
| author | Li, Haixin Wang, Enci Lyu, Cheqiu Chen, Yangyao Wang, Huiyuan Chen, Zeyu Yu, Haoran Jia, Cheng Ma, Chengyu |
| author_facet | Li, Haixin Wang, Enci Lyu, Cheqiu Chen, Yangyao Wang, Huiyuan Chen, Zeyu Yu, Haoran Jia, Cheng Ma, Chengyu |
| contents | The element abundances of galaxies provide crucial insights into their formation and evolution. Using high-resolution IFU data from the MaNGA survey, we analyze the central spectra (0-0.5 $R_{\rm e}$) of 1,185 quenched galaxies ($z = 0.012-0.15$) to study their element abundances and stellar populations. We employ the full-spectrum fitting code {\tt alf} to derive stellar ages and element abundances from synthetic spectra and empirical libraries. Our key findings are: (1) Central velocity dispersion ($σ_*$) is the most effective parameter correlating with (relative) element abundances, especially [Na/Fe], [Mg/Fe], [C/Fe], and [N/Fe], outperforming $M_\ast$ and $M_\ast/R_{\rm e}$. (2) When binned by $σ_*$, the relative abundances of Na, Mg, C, and N remain stable across different formation times ($T_{\rm form}$), suggesting these elements are primarily influenced by the burstiness of star formation (traced by $σ_*$) rather than prolonged evolutionary processes. (3) Fe and Ca show little variation with $σ_*$, indicating weaker sensitivity to $σ_*$-driven processes. However, $T_{\rm form}$ has a global influence on all elements, contributing to their overall chemical evolution, albeit secondary to $σ_*$ for most elements. These results support the primary role of $σ_*$ in shaping the abundance patterns, likely stemming from the connection between central massive black holes and possibly dark matter halos, which influences the burstiness of star formation histories. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2502_18785 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Central Velocity Dispersion being the Primary Driver of Abundance Patterns in Quenched Galaxies Li, Haixin Wang, Enci Lyu, Cheqiu Chen, Yangyao Wang, Huiyuan Chen, Zeyu Yu, Haoran Jia, Cheng Ma, Chengyu Astrophysics of Galaxies The element abundances of galaxies provide crucial insights into their formation and evolution. Using high-resolution IFU data from the MaNGA survey, we analyze the central spectra (0-0.5 $R_{\rm e}$) of 1,185 quenched galaxies ($z = 0.012-0.15$) to study their element abundances and stellar populations. We employ the full-spectrum fitting code {\tt alf} to derive stellar ages and element abundances from synthetic spectra and empirical libraries. Our key findings are: (1) Central velocity dispersion ($σ_*$) is the most effective parameter correlating with (relative) element abundances, especially [Na/Fe], [Mg/Fe], [C/Fe], and [N/Fe], outperforming $M_\ast$ and $M_\ast/R_{\rm e}$. (2) When binned by $σ_*$, the relative abundances of Na, Mg, C, and N remain stable across different formation times ($T_{\rm form}$), suggesting these elements are primarily influenced by the burstiness of star formation (traced by $σ_*$) rather than prolonged evolutionary processes. (3) Fe and Ca show little variation with $σ_*$, indicating weaker sensitivity to $σ_*$-driven processes. However, $T_{\rm form}$ has a global influence on all elements, contributing to their overall chemical evolution, albeit secondary to $σ_*$ for most elements. These results support the primary role of $σ_*$ in shaping the abundance patterns, likely stemming from the connection between central massive black holes and possibly dark matter halos, which influences the burstiness of star formation histories. |
| title | Central Velocity Dispersion being the Primary Driver of Abundance Patterns in Quenched Galaxies |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2502.18785 |