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The Simulated Circumgalactic Medium at z∼2 Molly S. Peeples (CGE Fellow; UCLA) with Ben Oppenheimer, Romeel Davé , Amanda Ford, Sean Fillingham , Juna Kollmeier The Dynamic Nature of Baryons; Leiden, August 2012. - PowerPoint PPT Presentation
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Density and temperature conspire to have higher ionization
species peak at higher radii (below); this qualitative behavior is seen for
all feedback models and mass rangesdetails will depend on UV
background
The Simulated Circumgalactic Medium at z 2∼Molly S. Peeples (CGE Fellow; UCLA)
with Ben Oppenheimer, Romeel Davé,Amanda Ford, Sean Fillingham, Juna Kollmeier
The Dynamic Nature of Baryons; Leiden, August 2012
Stay tuned to an arXiv near you for upcoming papers…
Wind Model Wind velocity vw Mass-loading factor ηw
Fiducial:momentum-driven scaling vw = [150 km/s] / σgal ηw σ∝ gal
-1
Mixed: v-2 energy-driven scaling for dwarfs vw = [150 km/s] / σgal
σgal > 75 km/s: ηw σ∝ gal-1
σgal < 75 km/s: ηw σ∝ gal-2
constant wind vw = 680 km/s ηw = 2
€
ηwind ≡˙ M wind˙ M SFR
The Simulations 32 h-1 Mpc comoving cosmological 5123 particle SPH simulations evolved with Gadget-2 Updated versions from Oppenheimer et al. (2010) Wiersma et al. (2009) cooling; Haardt & Madau UV background Compare effects of three star-formation driven wind scalings Everything shown here is at z=2.2
z=2.2 star formation rate – stellar mass relation
z=2.2 mass-metallicity relation
❷ The z=2.2 circumgalactic medium: physical properties
❶ Bulk galaxy properties Steeper wind scaling ➜ shallower low-
end mass function (left), steeper mass-metallicity relation (right); very little effect on star formation rates at fixed stellar mass (middle)
Simulated star formation rates (middle) still well below those inferred from observations; see Davé (2008), Narayanan & Davé (2012) for more thorough discussions
Feedback efficiency affects metal content of the ISM (right); is the metal content of the CGM another observable consequence?
How do different models of star-formation driven winds affect the circumgalactic medium at z 2?∼❶ Bulk galaxy properties ❷ The physical circumgalactic medium ❸ The observable circumgalactic medium
❸ The observable z=2.2 circumgalactic mediumMost absorption is saturated even out to large impact parameters (e.g.,
left, for OVI absorption around a M★~1010 galaxy in the fiducial simulation).Stacking over multiple sightlines (below) leads to ① broader profiles
than typically seen in individual spectra and ② not-as-black spectra. These effects will both be compounded with observation noise + resolution added.
Comparing at fixed stellar mass (right) allows for fairer comparison to observations: model galaxies will have made roughly the same amount of
metals, so testing density of halos they live in, and where they have distributed their metals.
log M★=10 1 Mpc/h comoving ~ 446 kpc physical300 km/s deep projections
Tran
smitt
ed O
VI fl
ux
z=2.2 halo mass – stellar mass relation
Feedback processes affect densities, temperatures, and metallicities. Left: mean stacks of 50 matched galaxies with Mhalo = 1011M
☀3-d profiles show detailed differences (middle); fast winds ➜ higher temperatures; metallicity profiles show strong slope differences
Fidu
cial
Cons
tant
Mixe
d
Do column density profiles measured from spectra (left) agree with
the intrinsic column density profiles (right)?