New model explains why galaxies' high-speed winds are harder to spot than expected
Researchers have cracked a decades-old puzzle about why certain signatures of galactic winds are rarely observed, despite being theoretically abundant. The discovery could transform how scientists map gas flows around galaxies—critical for understanding galaxy evolution, star formation, and the mechanisms that regulate cosmic structure.
Originaltitel: Modelling emission-line surface brightness in a multiphase galactic wind: an O <scp>vi</scp> case study
ABSTRACT We present a fast and robust analytic framework for predicting surface brightness (SB) of emission lines in galactic winds as a function of radius up to $\sim 100$ kpc out in the circum-galactic medium. We model multiphase structure in galactic winds by capturing emission from both the volume-filling hot phase (T $\sim 10^{6-7}$ K) and turbulent radiative mixing layers that host intermediate temperature gas at the boundaries of cold clouds (T $\sim 10^4$ K). Our multiphase framework makes significantly different predictions of emission signatures compared to traditional single-phase models and explains the paucity of O vi SB measurements in the literature. After accounting for ram pressure equilibrium between the cold clouds and hot wind in supersonic outflows, non-equilibrium ionization effects, and energy budgets other than mechanical energy from core-collapse supernovae, our O vi SB predictions qualitatively match observational results. Our framework provides constraints on the optimal galactic wind properties that facilitate O vi emission observations, including star formation rate surface density, hot phase mass loading factor, and thermalization efficiency factor. These constraints are consistent with existing observations and can help inform future target selections.