What matters around galaxies during the epoch of reionization Sarah - - PowerPoint PPT Presentation
What matters around galaxies during the epoch of reionization Sarah Bosman Harley Katz Laura Keating Martin Haehnelt Can trace the CGM to z~6-7 talk by Laura Keating OI courtesy Rapid evolution of OI at z>5.7 CGM appears to
Sarah Bosman Harley Katz Laura Keating
courtesy George Becker Berlin 2016
OI Ø Can trace the CGM to z~6-7 àtalk by Laura Keating Ø Rapid evolution of OI at z>5.7 à CGM appears to become more neutral at z>5 Ø Will affect escape of ionizing photons, evolution
Carefully calibratted with Lyα forest data RAMSES post-processed with ATON
Fully coupled radiative transfer with RAMSES-RT
z=6 z=7
HII HI H2 Γ
young stars
intermediate
contours:NHI This is rather sensitive to the implementation of stellar feedback in the simulation But simulating the local radiation is crucial for modeling ionization states.
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.
Ledd ( log Mbh =6)
L
no AGN Ledd ( log Mbh =7)
Presence of AGN in dense regions removes the offset between OIII and CII.