Joint modeling of IGM attenuation and stellar populations

Derive a joint fit of the intergalactic-medium damping wing and the stellar-population properties of GN-z11 to separate IGM attenuation from the intrinsic strength of the N V stellar-wind absorption.

Background

The observed N V P-Cygni profile is affected by damping-wing absorption from neutral hydrogen in the intergalactic medium. The authors model a range of ionized-bubble sizes separately from the stellar continuum, showing that the inferred intrinsic N V profile and stellar-population properties depend on the assumed distance to the nearest neutral IGM. A simultaneous treatment is therefore needed to constrain both the reionization environment and the massive-star population consistently.

References

While a full, joint fit of the damping wing and stellar populations is left to future work, combining the N~V emission with the other stellar-wind features and the strength of Ly$\alpha$ emission should enable a more precise separation of the IGM attenuation and the intrinsic strength of N~V absorption.

— SPURS: Massive Stars, Dense Gas, and Ly$α$ Escape in GN-z11 at $z = 10.6$  (2608.12699 - Chen et al., 13 Aug 2026) in Section 6.3, Impact of IGM Damping Wing on N V