What matters around galaxies during the epoch of reionization Sarah Bosman Harley Katz Laura Keating Martin Haehnelt
Ø Can trace the CGM to z~6-7 à talk by Laura Keating OI courtesy Ø Rapid evolution of OI at z>5.7 à CGM appears to George Becker Berlin 2016 become more neutral at z>5 Ø Will affect escape of ionizing photons, evolution of Lyman-alpha emitters
RAMSES post-processed with ATON Carefully calibratted with Lyα forest data
Fully coupled radiative transfer with RAMSES-RT
HII HI H 2 z=7 z=6 Γ young stars intermediate old stars
CII OIII NII contours:N HI This is rather sensitive to the implementation of stellar feedback in the simulation But simulating the local radiation is crucial for modeling ionization states.
Spatial offset of CII and OIII with ALMA Carniani et al. 17 Katz et al. 17 Offsets of CII and OIII occur naturally as OIII traces is often produced by hot gas produced by SN feedback which is offset from the dense star forming regions. Obscuration by the (not yet modelled) dust can explain offset of Lyα +UV. What about AGN.
L L edd ( log M bh =6) L edd ( log M bh =7) no AGN Presence of AGN in dense regions removes the offset between OIII and CII.
Summary Ø Evidence is building for rather late reionization so study of CGM and ISM of galaxies during the epoch of reionization has become observationally possible and will really take of with JWST. Ø At z>5.7 the CGM is becoming rapidly more neutral. Ø Modelling of local radiation with full RT transfer simulation has become possible and is essential.
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