Dynamical Properties of Galaxies with Different ... · Dynamical Properties of Galaxies with...
Transcript of Dynamical Properties of Galaxies with Different ... · Dynamical Properties of Galaxies with...
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
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
The Magneticum Pathfinder Simulations
Romanowsky & Fall 2012
68.5 Mpc
100 kpc
different galaxy types
The Magneticum Pathfinder Simulations
68.5 Mpc
100 kpc
different galaxy types
Classification
(e.g. Scannapieco et al. 2008)
ε = 0 → dispersion dominated
ε = 1 → rotation dominated
13/04/2016 Teklu et al. 2015
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
Comparison to Observations
Simulation Observation
13/04/2016 Teklu et al. 2015
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
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
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
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
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
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
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
Spin Parameter of Different Components
Splitup of:
hothot and coldcold gasstarsstars,, DM and gasgas
13/04/2016 Teklu et al. 2015
how disk components (stars and gas) trace, how halo and disk (dm and gas) trace...
13/04/2016 Teklu et al. 2015
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
Threshold for epsilonClassification
13/04/2016 Teklu et al. 2015
Gas Fractions
13/04/2016 Teklu et al. 2015
Stellar Mass Functions
13/04/2016 Teklu et al. 2015
Remus et al. 2015