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Dynamical Properties of Galaxies with Different Morphological
Types
Adelheid Teklu(አደልሀይድ ተክሉ )
USM/Excellence Cluster
Supervisors: RheaSilvia Remus, Klaus Dolagand the Magneticum Pathfinder Team
The Interplay between Local and Global Processes in Galaxies, Cozumel
13/04/2016
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The Magneticum Pathfinder Simulationsdifferent galaxy types
Relation toRelation to dark matter dark matter dynamics dynamics
68.5 Mpc
seesee poster poster byby K. DolagK. Dolag
100 kpc
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The Magneticum Pathfinder Simulations
Romanowsky & Fall 2012
68.5 Mpc
100 kpc
different galaxy types
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The Magneticum Pathfinder Simulations
68.5 Mpc
100 kpc
different galaxy types
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Classification
(e.g. Scannapieco et al. 2008)
ε = 0 → dispersion dominated
ε = 1 → rotation dominated
13/04/2016 Teklu et al. 2015
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Classification
(e.g. Scannapieco et al. 2008)
Criteria at z=0.1:
ε = 0 → dispersion dominated
ε = 1 → rotation dominated
f(ε≥0.7)≥0.4 and Mcoldgas
/Mstar
≥0.215
→ Disk
f(|ε|≤0.4)⩾0.6 and Mcoldgas
/Mstar
≤0.065
→ Speroid
13/04/2016 Teklu et al. 2015
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Comparison to Observations
Simulation Observation
13/04/2016 Teklu et al. 2015
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Spin Parameter of Host Halo
Splitup into spheroids and disks!
(Peebles 1969/71,Mo et al. 1998)
(including all components DM, gas & stars)
13/04/2016 Teklu et al. 2015
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Spin Parameter of Host Halo
Splitup into spheroids and disks!
(Peebles 1969/71,Mo et al. 1998)
(including all components DM, gas & stars)
Already present at z = 2 !
13/04/2016 Teklu et al. 2015
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Spin Parameter of the DMcomponent
Implications: interplay between baryons and DM
or due to different formation histories
(Bullock et al. 2001,van den Bosch et al. 2002)
Modified Spin Parameter:
13/04/2016 Teklu et al. 2015
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DMonly run
CrossMatching Halos DMonly vs. HydroHydro run
λ classification
Criteria: d < 200kpc mass difference < 30%
Crossmatched:575/622
13/04/2016 Teklu et al. 2015
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Spin Parameter of DMonly Halos
Even here is a splitup of different galaxy types → morphology a result of formation history/environment?
13/04/2016 Teklu et al. 2015
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Summary and Conclusion
● Our simulated disks and spheroids populate different regions in the M
starj
starplane, in
agreement with observations
● Disks have higher median spin parameter compared to spheroids
● There are also spheroids with high λ (for detailed study see Schulze et al., in prep.)
● Even in DMonly a splitup of λdistribution
→ Formation history and environment shape simultaneously galaxy type and halo
13/04/2016 Teklu et al. 2015
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Alignment Angles
In the hydro run DM components (inner part with total halo) are better aligned than in DMonly run influence of baryons on DM →
13/04/2016 Teklu et al. 2015
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Spin Parameter of Different Components
Splitup of:
hothot and coldcold gasstarsstars,, DM and gasgas
13/04/2016 Teklu et al. 2015
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how disk components (stars and gas) trace, how halo and disk (dm and gas) trace...
13/04/2016 Teklu et al. 2015
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The Dependence of the bvalue on Radius
For spheroidal galaxies the measurment of the bvalue is strongly radiusdependend
13/04/2016 Teklu et al. 2015
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Threshold for epsilonClassification
13/04/2016 Teklu et al. 2015
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Gas Fractions
13/04/2016 Teklu et al. 2015
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Stellar Mass Functions
13/04/2016 Teklu et al. 2015
Remus et al. 2015