CHIMPS2: $^{13}$CO $J = 3 \to 2$ emission in the Central Molecular Zone
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866909292985057280 |
|---|---|
| author | King, S. M. Moore, T. J. T. Henshaw, J. D. Longmore, S. N. Eden, D. J. Rigby, A. J. Rosolowsky, E. Tahani, K. Su, Y. Yiping, A. Tang, X. Ragan, S. Liu, T. Kuan, Y. -J. Rani, R. |
| author_facet | King, S. M. Moore, T. J. T. Henshaw, J. D. Longmore, S. N. Eden, D. J. Rigby, A. J. Rosolowsky, E. Tahani, K. Su, Y. Yiping, A. Tang, X. Ragan, S. Liu, T. Kuan, Y. -J. Rani, R. |
| contents | We present the initial data for the ($J = 3 \to 2$) transition of $^{13}$CO obtained from the Central Molecular Zone (CMZ) of the Milky Way as part of the CO Heterodyne Inner Milky Way Plane Survey 2 (CHIMPS2). Covering $359^\circ \leq l \leq 1^\circ$ and $|b| \leq 0.5^\circ$ with an angular resolution of 19 arcsec, velocity resolution of 1 km s$^{-1}$, and rms $T_A^* = 0.59$ K at these resolutions, our observations unveil the complex structure of the CMZ molecular gas in improved detail. Complemented by the $^{12}$CO CHIMPS2 data, we estimate a median optical depth of $τ_{13} = 0.087$. The preliminary analysis yields a median $^{13}$CO column density range equal to $N(^{13}\text{CO})= 2$--$5 \times 10^{18}$ cm$^{-2}$, median H$_2$ column density equal to $N(\text{H}_2)= 4 \times 10^{22}$ cm$^{-2}$ to $1 \times 10^{23}$ cm$^{-2}$.
We derive $N(\text{H}_2)$-based total mass estimates of $M(\text{H}_2)= 2$--$6 \times 10^7\, M_{\odot}$, in agreement with previous studies. We analyze the relationship between the integrated intensity of $^{13}$CO and the surface density of compact sources identified by Herschel Hi-GAL, and find that younger Hi-GAL sources detected at 500 $μ$m but not at 70 $μ$m follow the dense gas of the CMZ more closely than those that are bright at 70 $μ$m. The latter, actively star-forming sources, appear to be more associated with material in the foreground spiral arms. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_11548 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | CHIMPS2: $^{13}$CO $J = 3 \to 2$ emission in the Central Molecular Zone King, S. M. Moore, T. J. T. Henshaw, J. D. Longmore, S. N. Eden, D. J. Rigby, A. J. Rosolowsky, E. Tahani, K. Su, Y. Yiping, A. Tang, X. Ragan, S. Liu, T. Kuan, Y. -J. Rani, R. Astrophysics of Galaxies We present the initial data for the ($J = 3 \to 2$) transition of $^{13}$CO obtained from the Central Molecular Zone (CMZ) of the Milky Way as part of the CO Heterodyne Inner Milky Way Plane Survey 2 (CHIMPS2). Covering $359^\circ \leq l \leq 1^\circ$ and $|b| \leq 0.5^\circ$ with an angular resolution of 19 arcsec, velocity resolution of 1 km s$^{-1}$, and rms $T_A^* = 0.59$ K at these resolutions, our observations unveil the complex structure of the CMZ molecular gas in improved detail. Complemented by the $^{12}$CO CHIMPS2 data, we estimate a median optical depth of $τ_{13} = 0.087$. The preliminary analysis yields a median $^{13}$CO column density range equal to $N(^{13}\text{CO})= 2$--$5 \times 10^{18}$ cm$^{-2}$, median H$_2$ column density equal to $N(\text{H}_2)= 4 \times 10^{22}$ cm$^{-2}$ to $1 \times 10^{23}$ cm$^{-2}$. We derive $N(\text{H}_2)$-based total mass estimates of $M(\text{H}_2)= 2$--$6 \times 10^7\, M_{\odot}$, in agreement with previous studies. We analyze the relationship between the integrated intensity of $^{13}$CO and the surface density of compact sources identified by Herschel Hi-GAL, and find that younger Hi-GAL sources detected at 500 $μ$m but not at 70 $μ$m follow the dense gas of the CMZ more closely than those that are bright at 70 $μ$m. The latter, actively star-forming sources, appear to be more associated with material in the foreground spiral arms. |
| title | CHIMPS2: $^{13}$CO $J = 3 \to 2$ emission in the Central Molecular Zone |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2408.11548 |