GA-NIFS: Dissecting The Alchemised: JWST reveals turbulent metal-poor gas fuelling a co-spatial starburst in a complex system at z = 10.17
Clicks: 3
ID: 321927
2026
Article Quality & Performance Metrics
Overall Quality
Not rated
Combines reader engagement with the AI quality analysis. This
article has not been analysed, so there is no overall score —
reader engagement is measured and shown alongside.
Reader Engagement
0.0
/100
3 views
0 readers
AI Quality Assessment
Not analyzed
Readership in this journal
Ranked #146 of 897 articles by views in monthly notices of the royal astronomical society
Most read
Least read
Bar heights use a square-root scale. Only the 120 most-read articles are drawn; the journal has 897 in total.
Mint this article as an NFT
Not yet mintedCreate a permanent, verifiable on-chain record of this article on the Scimatic Network. The NFT is held in your Journament account, and you can withdraw it to your own wallet at any time.
5
SUSD
one-off · no wallet required
Abstract
Abstract Recent observations revealed that distant galaxies have bursty star formation histories, regulated by stellar or active galactic nuclei (AGN) feedback and gas inflows. According to theoretical models, feedback preferentially removes metal-rich gas, while subsequent starbursts are triggered by mergers and newly accreted gas that is generally less enriched than the galaxy’s interstellar medium (ISM). Therefore, gas-phase metallicity provides key insights into the baryonic processes shaping early galaxies. We present the first NIRSpec/IFU study of spatially resolved ISM properties in the MACS0647-JD system (z = 10.17). The system consists of two stellar components detected in NIRSpec/IFU and NIRCam photometry. The main component (log (M*/M⊙) = 7.77 ± 0.09; $12+\log \left(\rm O/H\right)=7.89 \pm 0.16$) is more massive and significantly more metal-rich compared to its companion (log (M*/M⊙) = 7.42 ± 0.07; $12+\log \left(\rm O/H\right)=7.47 \pm 0.20$), suggesting an older stellar population and a prolonged chemical enrichment history. We find that the Hγ line emission centroid is spatially offset by ~0.1″ (150 pc in the source plane) from the stellar continuum centroid; the latter coincides with the location of the main stellar component. This offset provides possible evidence of a merger-driven starburst in this system. By comparing the spatial distributions of the metallicity, velocity dispersion, and the burstiness of star formation history, we infer the presence of turbulent, metal-poor gas outside the stellar components. This metal-poor, dynamically unstable gas is likely responsible for the enhanced recent star formation in the north-east region of the system.
| Reference Key |
openalex_W7169858023
Use this key to autocite in the manuscript while using
SciMatic Manuscript Manager or Thesis Manager
|
|---|---|
| Authors | Robert G. Pascalau, F D’Eugenio, Roberto Maiolino, Qiao Duan, Yuki Isobe, Santiago Arribas, Andrew J. Bunker, S. Charlot, M Perna, Bruno Rodríguez Del Pino, H Übler, E. Bertola, Torsten Böker, S Carniani, Dan Coe, G Cresci, Mirko Curti, Tiger Y Y Hsiao, Lucy R. Ivey, Gareth C. Jones, Isabella Lamperti, Eleonora Parlanti, Jan Scholtz, Sandro Tacchella, L. Ulivi, Giacomo Venturi, Joris Witstok, Sandra Zamora |
| Journal | monthly notices of the royal astronomical society |
| Year | 2026 |
| DOI |
10.1093/mnras/stag1369
|
| URL | |
| Keywords | Keywords not found |
Citations
No citations found. To add a citation, contact the admin at info@scimatic.org
Comments
No comments yet. Be the first to comment on this article.