High-Redshift Circumgalactic Medium in FIRE Simulations (work in - - PowerPoint PPT Presentation

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high redshift circumgalactic medium in fire simulations
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High-Redshift Circumgalactic Medium in FIRE Simulations (work in - - PowerPoint PPT Presentation

Jul 21, 2023 199 likes •365 views

High-Redshift Circumgalactic Medium in FIRE Simulations (work in progress) Bili Dong UC San Diego with advisor Dusan Keres & FIRE collaboration August 24, 2017 - GalFRESCA Circumgalactic Medium (CGM) background source down the barrel

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SLIDE 1

High-Redshift Circumgalactic Medium in FIRE Simulations

(work in progress)

Bili Dong UC San Diego

with advisor Dusan Keres & FIRE collaboration

August 24, 2017 - GalFRESCA

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SLIDE 2

Circumgalactic Medium (CGM)

background source transverse absorption-line down the barrel

Empirical definition: gas surrounding galaxies within virial radii

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SLIDE 3

CGM Distribution from Observations

increasing ionization potential increasing ionization potential

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SLIDE 4

COS-Burst

  • 17 low-redshift starburst galaxies vs control sample
  • Starbursts could influence CGM distribution and kinematics

Lya SiIII OVI CIV

Heckman et al. 2017

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SLIDE 5

Cosmic Star-Formation History

  • SFR peaks at 1 < z < 3 (cosmic noon)
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SLIDE 6

http://fire.northwestern.edu/ FIRE-2, Hopkins et al. 2017 FIRE-1, Hopkins et al. 2014

  • Images are logarithmically-weighted surface-density

projections, showing hot (> 106K), warm ionized (~ 104 - 105K), and cool neutral (< 8000K) gas

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SLIDE 7

Galactic Winds in FIRE

  • utflow

inflow SFR×10

Muratov et al. 2015

  • High-redshift galaxies undergo bursty star formation followed

by high mass-loading outflows suppressing inflows and SFR

  • How do inflow & outflow shape CGM?
  • utflow

inflow

  • utflow
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SLIDE 8

Halo Sample

  • FIRE-1 feedback
  • Halo mass range:

11.7 - 12.4

  • Redshift range:

2 - 4

MFz2_A1 z2h506 z2h400 z2h830 log M = 12.38 log M = 12.08 log M = 11.90 log M = 11.73 snapshots at z = 2

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SLIDE 9

Radial-Temporal Profiles

  • Ion fields added using Trident (Hummels et al. 2016)
  • Correlation between CGM distribution and inflow/outflow
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SLIDE 10

Keck Baryonic Structure Survey (KBSS)

Rudie et al. 2012 Steidel et al. 2014 Turner et al. 2014

  • EW converted to N assuming linear curve-of-growth regime
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SLIDE 11

Simulation vs Observation

  • Averaged over 2 < z < 3
  • Is there a halo mass trend?

decreasing halo mass

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SLIDE 12

Bonus: the Demeshening in yt

  • ctree method

particle method

A work by Nathan Goldbaum, Meagan Lang and Matthew Turk to remove the global octree mesh for particle data Goldbaum & Lang, SciPy 2017 https://doi.org/10.6084/m9.figshare.5203801.v1

  • Does octree method converge to particle method?
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SLIDE 13

Octree vs Particle

converge

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SLIDE 14

Octree vs Particle

converge

Can we describe this distribution analytically?

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SLIDE 15

Summary

  • Preliminary results

○ Correlation between CGM distribution and inflow/outflow ○ CGM distribution in FIRE matches high-redshift observation ○ Potential halo mass trend in CGM distribution

  • Numerical tests on yt demeshening

○ Octree method converges to particle method

  • Future work

○ Physical explanation (phase structure? metallicity?) ○ Upgrade to FIRE-2 for better numerics and physics ○ Larger sample for better statistics ○ Mock spectra for fairer comparisons with observations (using Trident)

Thank you!

Bili Dong