The Importance of Small Structure in the CGM
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1 The Importance of Small Structure in the CGM Cameron Hummels NSF Postdoctoral Fellow California Institute of Technology Britton Smith Devin Silvia Bili Dong Lauren Corlies Britton Smith Devin Silvia Brian O Shea Jess Werk Molly Peeples Jason Tumlinson Lauren Corlies Nicolas Lehner Phil Hopkins Claude-Andre Faucher-Giguère Dusan Keres Norm Murray
2 A universal synthetic spectral utility Hummels, Smith, & Silvia 2017 Creates synthetic absorption spectra for any trajectory through simulated volume Reproduces different spectrographs (COS) Operates across UV, optical, and IR with many lines Estimates the presence of ions absent from the simulation outputs using equilibrium modeling Post-processing to add QSO, MW, S/N, etc. Built on yt infrastructure (Turk et al. 2011) Supports all astrophysical hydro code formats Fully parallelized using MPI Open source, Python-based code hosted on Github
3 A universal synthetic spectral utility
4 Compound Sightline for Continuous Lightcones
5 The Importance of Small Structure in the CGM
6 The Importance of Small Structure in the CGM
7 The Importance of Small Structure in the CGM
8 FOGGIE/Tempest Simulations (grid-based) Strength: Resolution
9 FOGGIE/Tempest Simulations (grid-based) Strength: Resolution H I Natural Refinement
10 FOGGIE/Tempest Simulations (grid-based) Strength: Resolution Resolution Natural Refinement
11 FOGGIE/Tempest Simulations (grid-based) Strength: Resolution Resolution Natural Refinement Forced Refinement FOGGIE (Hummels+ in prep)
12 FOGGIE/Tempest Simulations (grid-based) Strength: Resolution H I Natural Refinement Forced Refinement FOGGIE (Hummels+ in prep)
13 FOGGIE/Tempest Simulations (grid-based) Strength: Resolution H I Natural Refinement Forced Refinement FOGGIE (Hummels+ in prep)
14 FOGGIE/Tempest Simulations (grid-based) Strength: Resolution H I Column Density (cm -2 ) H I Column Density (cm -2 ) Natural Refinement Forced Refinement FOGGIE (Hummels+ in prep)
15 FOGGIE/Tempest Simulations (grid-based) Strength: Resolution H I plls Covering Fraction Covering Fraction of plls Impact Parameter (kpc) FOGGIE (Hummels+ in prep)
16 FIRE Simulations (particle-based) Strength: Feedback
17 FIRE Simulations (particle-based) Strength: Feedback Density Temperature COS-FIRE (Hummels+ in prep)
18 FIRE Simulations (particle-based) Strength: Feedback H I O VI COS-FIRE (Hummels+ in prep)
19 FIRE Simulations (particle-based) Strength: Feedback H I O VI COS-FIRE (Hummels+ in prep)
20 FIRE Simulations (particle-based) Strength: Feedback COS-FIRE (Hummels+ in prep)
21 FIRE Simulations (particle-based) Strength: Feedback Best Fit Halo Sample COS-FIRE (Hummels+ in prep)
22 FIRE Simulations (particle-based) Strength: Feedback H I O VI COS-FIRE (Hummels+ in prep)
23 FIRE Simulations (particle-based) Strength: Feedback Column Density vs Resolution H I O VI Resolution COS-FIRE (Hummels+ in prep)
24 FIRE Simulations (particle-based) Strength: Feedback Column Density vs Halo Mass H I O VI Halo Mass COS-FIRE (Hummels+ in prep)
25 FIRE Simulations (particle-based) Strength: Feedback Best Fit Halo Sample COS-FIRE (Hummels+ in prep)
26 FIRE Simulations (particle-based) Strength: Feedback Column Density vs Halo Mass Halo Mass Oppenheimer+ 2016
27 FIRE Simulations (particle-based) Strength: Feedback Column Density vs Inclusion of MHD H I O VI COS-FIRE (Hummels+ in prep)
28 FIRE Simulations (particle-based) Strength: Feedback Column Density vs Environment H I O VI COS-FIRE (Hummels+ in prep)
29 Conclusions Use Trident suite to post-process simulation data as synth observations ( Current cosmological hydro simulations do not well reproduce CGM New Tempest/FOGGIE runs better resolve halo (<1 kpc) and thermal instability increasing CGM column densities and kinematic structure Simulated FIRE CGM sensitive to halo resolution, halo mass Simulated FIRE CGM insensitive to galactic environment, B-fields Simulated FIRE sample reproduces COS-Halos oxygen without tuning
30 FIRE Simulations (particle-based) Strength: Feedback Column Density vs Resolution H I O VI Resolution COS-FIRE (Hummels+ in prep)
31 FIRE Simulations (particle-based) Strength: Feedback Physical Properties vs Resolution Temperature Oxygen Resolution COS-FIRE (Hummels+ in prep)
32 FIRE Simulations (particle-based) Strength: Feedback COS-FIRE (Hummels+ in prep)
33 Precipitation Simulation (grid-based) Strength: Resolution Silvia+ in prep FOGGIE z<2 (Hummels+ in prep)
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Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 9 September 2014 (MN LATEX style file v2.2) arxiv:1409.1919v1 [astro-ph.ga] 5 Sep 2014 Neutral hydrogen in galaxy halos at the peak of the cosmic star
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