Hydrodynamical simulations of cosmic structures

Hydrodynamical simulations of cosmic structures
at INAF-OATs & dip. Fisica
Paramita Barai
Stefano Borgani
Emanuele Contini
Weiguang Cui
Gabriella De Lucia
Gianluigi Granato
Michaela Hirschmann
Madhura Killedar
Pierluigi Monaco
Emiliano Munari
Giuseppe Murante
Susana Planelles
Cinthia Ragone Figueroa
Luca Tornatore
Matteo Viel
Alvaro Villalobos
http://adlibitum.oats.inaf.it/cosmocomp

Members of the CosmoComp ITN:
An FP7 Initial Training Network for
Computational Cosmology
http://www.cosmocomp.dur.ac.uk/
CosmoComp fellows in Trieste:
Weiguang Cui, Madhura Killedar and Susana Planelles
CosmoComp Nodes: Durham (C. Baugh), CONICET (P. Tissera),
Leiden (J. Schaye), MPA (S. White), Nottingham (F. Pearce), Saclay
(R. Teyssier), Shanghai (Y.P. Jing), Sussex (P. Thomas), Trieste (S.
Borgani)
CosmoComp General Meeting (Trieste – September 4th-7th, 2012)
http://adlibitum.oats.inaf.it/meetings/COSMOCOMPTS/

GADGET-3 by V. Springel
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Tools
Tree code to solve gravity + PM at large scales
SPH hydro with energy and entropy conserving formulation
refined load balance to work for isolated objects
chemical evolution code
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enrichment of several chemical species by SNII, SNIa and AGB
metal cooling of gas by interpolating Cloudy tables
AGN feedback
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heating from accreting massive black holes
Energy-driven and momentum-driven winds
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standard and improved implementations
MUlti-Phase Particle Integrator
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star formation and SN feedback
Zoomed-in initial conditions generator
Molecular chemistry and cooling below 10 4 K
Magnetic fields in clusters
WISH LIST: autonomy on initial conditions, radiative transfer...

collapse
Cosmology (ΛCDM)
gravitational
Dark matter
Galaxies
astrophysics

The big questions
We use hydrodynamical codes and cosmological initial conditions
to simulate the formation of:
galaxy clusters and their intra-cluster medium,
the inter-galactic medium,
galaxies in various environments.
How do galaxy formation processes impact on observational
properties of clusters?
Can we produce realistic disc galaxies? can we produce realistic
galaxy populations?
Do we understand inflows and outflows of baryons?
Do simulations and semi-analytic models give a consistent picture
of galaxy formation?
How confident are we on the reliability of the adopted numerical
hydro schemes?

Simulating
galaxy clusters
zoomed-in initial conditions
Cluster astrophysics:
Thermo- and chemodynamical
properties of the ICM
Properties of cluster galaxies
Properties and detectability
of diffuse intra-cluster light
How do galaxy formation
processes impact on observational
properties of clusters?
Fabjan et al. (2010)

galaxy clusters
4
Simulating
Map of diffuse intra-cluster light
(Cui et al. in preparation)
Simulation of cluster
shocks with Eulierian code
(Planelles et al. submitted)
Maps of metal enrichment
for different baryon physics
(Fabjan et al. 2010)
-> observations
of clusters
(Tozzi's talk )
-> cluster
cosmology
(Viel's talk)

Simulating galaxy clusters
cosmological boxes
Role of feedback for:
• Physics of galaxy
formation
• IGM properties at
low and high-z
• Properties of the
ICM
Multi-million CPUh projects granted through DEISA, Gauss and
ISCRA, using SP6 and BlueGene/P (PIs: K. Dolag & S. Borgani)

Simulating galaxies
Galaxy astrophysics:
Sub-resolution
star formation and
SN feedback
Properties of
galaxies: size,
morphology, gas
fraction, bar, Tully-
Fisher, Schmidt-
Kennicutt
Baryon fraction
in DM halos
Can we produce
realistic spiral
galaxies?
Murante et al., in prep.

Scannapieco et al. (2012)

Zoom-in simulations of 45 individual halos (5e10-2e13M⊙)
Hirschmann et al. in preparation
Can we produce
realistic galaxy
populations?
Ongoing project: simulation of 36 Mpc/h box with 512 3 gas + 512 3 DM particles and
128 outputs, with several star formation & SN feedback models, granted by
CASPUR and proposed to CINECA (PI: Murante & Monaco)
-> chemical evolution (De Lucia's talk)
-> SED synthesis (De Lucia's talk)
-> observations of galaxies (Tozzi's talk)

Simulating the IGM
IGM astrophysics:
Statistics of Lyman-alpha
forest
Thermal and chemical
properties of the IGM
Role of galaxy outflows and
their detectability as metal
absorbers
-> IGM (D'Odorico's talk)
-> Cosmology with Lymanalpha
forest (Viel's talk)
Do we understand inflows
and outflows of baryons?

Log Temperature Projection of (200/h kpc)3 volume
around a massive group (3 x 10 12 M ) center (run RVWa, z = 1.98)
(Barai et al. in prep.)

Comparison with semi-analytic
models: cooling
Saro et al. (2010)
Viola et al. (2008)
-> SAM comparison
project (De Lucia)
Do simulations and semi-analytic models give
a consistent picture of galaxy formation?
Ongoing project: simulation of 36 Mpc/h box with 512 3 gas + 512 3 DM particles and
128 outputs, only cooling of primordial gas, to be compared with down-stripped
SAM predictions at the object-by-object level, granted by CINECA (PI: Monaco)

Extending SPH: Godunov-SPH
How confident are we on the reliability of
the adopted numerical hydro schemes?
Murante et al. (2011)

Computers
Supercomputing time obtained
through grants at CINECA
(ISCRA + UniTS), CASPUR,
PRACE...
In-house post-processing
analyses (with lapoderosa, 16-
processor shared memory
DELL machine with 128 Gb of
RAM)
Moving to the Blue Gene era...
Fermi Blue Gene/Q @ CINECA