Coordinated multi‑wavelength campaigns will allow us to (stars, gas, dust) and measure feedback signatures (outflows, ionizing photon leakage) in a single, well‑characterized galaxy at a pivotal epoch.
| Facility | Observation | Goal | |---|---|---| | (R ≈ 2700) | Rest‑frame optical emission lines (Hα, [O III], Hβ). | Precise metallicity, ionization parameter, and dynamical mass. | | ALMA (Band 8) | CO(6‑5) or CO(7‑6) detection. | Direct molecular gas mass, excitation ladder, and gas kinematics. | | VLT/MUSE (deep IFU) | Lyα line profile and extended halo. | Lyα escape fraction, IGM transmission, and CGM mapping. | | Roman Space Telescope (wide‑field NIR imaging) | Search for satellite companions within 100 kpc. | Assess environment and potential proto‑cluster. | FSDSS-281