Mapping Jet-Gas Coupling and energetic ionized outflows in High-Redshift Radio Galaxies with JWST/NIRSpec
Fuente:
arXiv
Gespeichert in:
| Hauptverfasser: | , , |
|---|---|
| Format: | Preprint |
| Veröffentlicht: |
2025
|
| Schlagworte: | |
| Online-Zugang: | |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| _version_ | 1866913982641602560 |
|---|---|
| author | Roy, Namrata Heckman, Timothy Henry, Alaina |
| author_facet | Roy, Namrata Heckman, Timothy Henry, Alaina |
| contents | We present spatially resolved maps of morphology, kinematics, and energetics of warm ionized gas in six powerful radio galaxies at z=3.5-4, using JWST/NIRSpec IFU to quantify jet-driven feedback in the early universe. All sources exhibit broad [OIII] emission-line profiles with W80 (line width) values of 950-2500 km/s across $\sim$10s of kpc, signifying large-scale outflows. The outflowing nebulae are preferentially aligned with the radio jet axis, suggesting jet-driven origin. On average, the regions with the broadest lines and highest velocities are co-spatial with radio lobes or cores, and exhibit the strongest kinetic power. Ionized gas masses associated with the outflows span 1 to 8 $\times 10^{9} \ M_\odot$, with total mass outflow rates of 80-950 Msun/yr and kinetic powers between 10^{43.2} and 10^{45.0} erg/s. The outflow kinetic power corresponds to 0.15%-2% of the AGN bolometric luminosity, sufficient to impact galaxy evolution. However, only $\lesssim 1$\% of the jet mechanical energy couples to the warm ionized gas via outflows, consistent with predictions from hydrodynamic simulations. A large fraction of the jet energy may instead reside in shock-heated hot gas, supported by X-ray detection, or used to thermalize the gas and produce the observed emission-line nebulae. Our results demonstrate that radio jets in massive, gas-rich systems at high-redshift can inject significant kinetic and thermal energy to the surroundings, providing direct evidence for jet-driven feedback operating during the peak epoch of galaxy formation. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_06707 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Mapping Jet-Gas Coupling and energetic ionized outflows in High-Redshift Radio Galaxies with JWST/NIRSpec Roy, Namrata Heckman, Timothy Henry, Alaina Astrophysics of Galaxies We present spatially resolved maps of morphology, kinematics, and energetics of warm ionized gas in six powerful radio galaxies at z=3.5-4, using JWST/NIRSpec IFU to quantify jet-driven feedback in the early universe. All sources exhibit broad [OIII] emission-line profiles with W80 (line width) values of 950-2500 km/s across $\sim$10s of kpc, signifying large-scale outflows. The outflowing nebulae are preferentially aligned with the radio jet axis, suggesting jet-driven origin. On average, the regions with the broadest lines and highest velocities are co-spatial with radio lobes or cores, and exhibit the strongest kinetic power. Ionized gas masses associated with the outflows span 1 to 8 $\times 10^{9} \ M_\odot$, with total mass outflow rates of 80-950 Msun/yr and kinetic powers between 10^{43.2} and 10^{45.0} erg/s. The outflow kinetic power corresponds to 0.15%-2% of the AGN bolometric luminosity, sufficient to impact galaxy evolution. However, only $\lesssim 1$\% of the jet mechanical energy couples to the warm ionized gas via outflows, consistent with predictions from hydrodynamic simulations. A large fraction of the jet energy may instead reside in shock-heated hot gas, supported by X-ray detection, or used to thermalize the gas and produce the observed emission-line nebulae. Our results demonstrate that radio jets in massive, gas-rich systems at high-redshift can inject significant kinetic and thermal energy to the surroundings, providing direct evidence for jet-driven feedback operating during the peak epoch of galaxy formation. |
| title | Mapping Jet-Gas Coupling and energetic ionized outflows in High-Redshift Radio Galaxies with JWST/NIRSpec |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2508.06707 |