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Modeling Cosmic Reionization (Leave No Photon Behind) Nick Gnedin.

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Presentation on theme: "Modeling Cosmic Reionization (Leave No Photon Behind) Nick Gnedin."— Presentation transcript:

1 Modeling Cosmic Reionization (Leave No Photon Behind) Nick Gnedin

2 Co-starring Gayler Harford

3 Balancing the Books (Bunker et al. 2004) Low High

4 Simulations Mass Space 8 chimp 400 pc @z=6 3x10 6 M  Low res, large box High res, small box

5 Numerical Challenges Enough resolution to do reionization right (resolving Lyman-limit systems) Enough volume to model observable (i.e. bright enough) galaxies L ObservationSimulation Limited box sizeLimiting flux Bigger simulationDeeper observation Lyman-Limit systems

6 We Do Not Know Everything M N(<M) Free parameter: Star Formation Efficiency M N(<M) z = 4z = 6 The real test for a simulation is to fit two luminosity functions at two different redshifts simultaneously!

7 Reionization? Low SFR High SFR High res, small box

8 Luminosity Functions z = 4 High SFR Low SFR z = 6

9 Balancing the Books (Bunker et al. 2004) Low High Uncorrected Corrected

10 Conclusions Simulations of reionization are consistent with the “high” value of SFR at z~6 (~0.02 M  /Mpc 3 /yr). Simulations are not consistent with the “low” value (~0.005 M  /Mpc 3 /yr). Our simulations have barely enough resolution to make this claim. They need to be confirmed by better ones.

11 The End

12 Title


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