simulations of the merging galaxy cluster abell...
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Simulations of the merginggalaxy cluster Abell 3376
Rubens Machado, IAG/USPGastão Lima Neto, IAG/USP
USP Conference: Cosmology, Large Scale Structure and First Objects, 05/02/2013
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Summary
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 2 / 30
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Cluster mergers
Cluster mergers are the mechanismsby which clusters assemble
Mvir ∼ 1014 M�
Rvir ∼ 1 Mpc
b ∼ 100 kpcv ∼ 1000 km/s∆t ∼ 1 Gyr
Mach ∼ 1− 3Egrav ∼ 1063 erg
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 3 / 30
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Simulations of cluster mergers: examples
transient structures, Poole et al. (2006)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 4 / 30
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Simulations of cluster mergers: examples
gas sloshing and cold frontsAscasibar & Markevitch (2006)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 4 / 30
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Simulations of cluster mergers: examples
gas sloshing and cooling flows, ZuHone et al. (2010)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 4 / 30
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Simulations of cluster mergers: examples
parameter space exploration of mergers to study entropyZuHone (2011)
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Simulations of cluster mergers: examples
radio relics, van Weeren et al. (2011)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 4 / 30
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Simulations of cluster mergers: examples
triple merger, Brüggen et al. (2012)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 4 / 30
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Simulations of cluster mergers: examples
the Bullet Cluster:Springel & Farrar (2007), Mastropietro & Burkert (2007)Takizawa (2005, 2006), Milosavljevic et al. (2007)
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Cluster mergers
clusters in which gashas become dissociatedfrom dark matter
1) 1E 0657-56 (Clowe et al. 2006), “Bullet Cluster”2) MACS J0025.4-1222 (Bradac et al. 2008)3) Abell 520 (Mahdavi et al. 2007), “Train Wreck”4) Abell 2744 (Merten et al. 2011), “Pandora’s Cluster”5) Abell 2163 (Okabe et al. 2011)6) Abell 1758 (Ragozzine et al. 2011)7) DLSCL J0916.2+2951 (Dawson 2012), “Musket Ball Cluster”
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Abell 3376
Mvir = 5.2 × 1014 M�
z = 0.0456
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Abell 3376: a nearby merging cluster
X-ray emission
XMM-Newton
radio relics
ROSAT (X-ray) + VLA (radio)Bagchi, Durret, Lima Neto & Paul (2006)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 7 / 30
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Abell 3376: a nearby merging cluster
X-ray emission
XMM-Newton
radio relics
ROSAT (X-ray) + VLA (radio)Bagchi, Durret, Lima Neto & Paul (2006)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 7 / 30
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Abell 3376: a nearby merging cluster
X-ray emission
XMM-Newton
radio relics
ROSAT (X-ray) + VLA (radio)Bagchi, Durret, Lima Neto & Paul (2006)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 7 / 30
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Abell 3376: radio
giant (2 Mpc) radio lobes around clusterno associated jetsmagnetic field ∼ 1µG
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Abell 3376: brightest cluster galaxies
optical (galaxies)
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Abell 3376: brightest cluster galaxies
optical (galaxies)
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Abell 3376: brightest cluster galaxies
X-ray (intracluster gas)
second BCG coincides with X-ray peak; BCG does not
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Abell 3376: brightest cluster galaxies
X-ray (intracluster gas)
second BCG coincides with X-ray peak; BCG does notseparation: 970 kpc
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Numerical simulations: initial conditions
initial parameters:
• DM density profile • mass ratio• gas density profile • gas fraction• initial relative velocity • impact parameter
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Numerical simulations: initial conditions
initial parameters:
• DM density profile • mass ratio• gas density profile • gas fraction• initial relative velocity • impact parameter
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 10 / 30
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Numerical simulations: initial conditions
initial parameters:
• DM density profile • mass ratio• gas density profile • gas fraction• initial relative velocity • impact parameter
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 10 / 30
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Numerical simulations: initial conditions
initial parameters:
• DM density profile • mass ratio• gas density profile • gas fraction• initial relative velocity • impact parameter
a posteriori :
• time after central passage• projection angles
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Numerical simulations: alphacrucis, 2304 cores
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Numerical simulations: evolution
X-ray surface brightness
emission-weighted temperature
time
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Numerical simulations: evolution
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Numerical simulations: parameter space sample
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Numerical simulations: parameter space of IC
initial parameters:
• DM density profile
: Hernquist (similar to NFW)
• gas density profile
: Dehnen γ=0 (similar to β-model)
• initial relative velocity• mass ratio• gas fraction
: fgas = 0.18
• impact parameter
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Numerical simulations: parameter space of IC
initial parameters:
• DM density profile : Hernquist (similar to NFW)• gas density profile
: Dehnen γ=0 (similar to β-model)
• initial relative velocity• mass ratio• gas fraction
: fgas = 0.18
• impact parameter
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 15 / 30
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Numerical simulations: parameter space of IC
initial parameters:
• DM density profile : Hernquist (similar to NFW)• gas density profile : Dehnen γ=0 (similar to β-model)• initial relative velocity• mass ratio• gas fraction
: fgas = 0.18
• impact parameter
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 15 / 30
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Numerical simulations: parameter space of IC
initial parameters:
• DM density profile : Hernquist (similar to NFW)• gas density profile : Dehnen γ=0 (similar to β-model)• initial relative velocity• mass ratio• gas fraction : fgas = 0.18• impact parameter
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 15 / 30
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Numerical simulations: parameter space of IC
initial parameters:
• DM density profile : Hernquist (similar to NFW)• gas density profile : Dehnen γ=0 (similar to β-model)• initial relative velocity• mass ratio• gas fraction : fgas = 0.18• impact parameter• temperature profile : from hydrostatic equilibrium
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 15 / 30
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Numerical simulations: parameter space of IC
initial parameters:
• DM density profile : Hernquist (similar to NFW)• gas density profile : Dehnen γ=0 (similar to β-model)• initial relative velocity• mass ratio• gas fraction : fgas = 0.18• impact parameter• temperature profile : from hydrostatic equilibrium
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 15 / 30
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Numerical simulations: mass ratio
MBMA
= 1/2 1/4 1/6 1/8
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Numerical simulations: impact parameter
b = 0 150 kpc 350 kpc 500 kpc
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Numerical simulations: initial relative velocity
vo = 500 km/s 1000 km/s 1500 km/s 2000 km/s
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Numerical simulations: relative gas concentration
• central gas density of the minor cluster
ρBρA
= 1 2 4 6
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Numerical simulations: inclination
i = 0◦ 30◦ 40◦ 60◦
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Comparison to observations
observed simulated
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Mach number
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Mach number: Rankine-Hugoniot jump conditions
emissionmap
temperaturemap
temperature
density
pressure
entropy
streaminggas velocity
T2
T1=
5M4 + 14M2 − 3
16M2
n2
n1=
4M2
M2 + 3
P2
P1=
5M2 − 1
4
S2
S1=
(5M2 − 1
4
)(4M2
M2 + 3
)−5/3
(vx,2 − vx,1
)= (vs − u)
(3M2 − 3
4M2
)
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Mach number: inclination
i = 0◦
M = 3.9
i = 40◦
M = 2.9
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Mach number: inclination
i = 0◦
M = 3.9
i = 40◦
M = 2.9
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Dark matter
How is the dark matter distributed?
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 25 / 30
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Dark matter
projected mass (total)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 26 / 30
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BCG separation and dark matter
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Summary
reproduced featuresvirial massintegrated X-ray fluxapproximate X-ray morphologytemperature range(proxy of) BCG separation
approximate constraintscollision axis inclined by i=40◦ wrt plane of the skyobserved ∼0.5 Gyr after central passagemass ratio 1/6 – 1/8Mach ∼3–4small impact parameter (b<150 kpc), if any
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 28 / 30
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Summary
We have proposed a specific scenario of a dynamical history for themerging event of Abell 3376.
We have offered a possible combination of parameters that accountsfor several of its features.
Machado & Lima Neto (2013)
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 29 / 30
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Perspectives
• Distribution of dark matter:• Mass maps from gravitational weak lensing• either corroborate this scenario or necessitate its improvement
acknowledgement:
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 30 / 30
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Perspectives
• Distribution of dark matter:• Mass maps from gravitational weak lensing• either corroborate this scenario or necessitate its improvement
+ “All models are wrong; some models are useful.”Box & Draper (1987)
acknowledgement:
Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 30 / 30