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Simulations of the Merging Galaxy Cluster Abell 3376 Simulations of the merging galaxy cluster Abell 3376 Rubens Machado, IAG/USP Gastão Lima Neto, IAG/USP USP Conference: Cosmology, Large Scale Structure and First Objects, 05/02/2013 Summary Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 2 / 30 Cluster mergers 14 Mvir ∼ 10 M Rvir ∼ 1 Mpc b ∼ 100 kpc v ∼ 1000 km/s ∆t ∼ 1 Gyr Mach ∼ 1 − 3 Cluster mergers are the mechanisms 63 by which clusters assemble Egrav ∼ 10 erg Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 3 / 30 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 Simulations of cluster mergers: examples gas sloshing and cold fronts Ascasibar & Markevitch (2006) Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 4 / 30 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 Simulations of cluster mergers: examples parameter space exploration of mergers to study entropy ZuHone (2011) Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 4 / 30 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 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 Simulations of cluster mergers: examples the Bullet Cluster: Springel & Farrar (2007), Mastropietro & Burkert (2007) Takizawa (2005, 2006), Milosavljevic´ et al. (2007) Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 4 / 30 Cluster mergers 1) 1E 0657-56 (Clowe et al. 2006), “Bullet Cluster” clusters in which gas 2) MACS J0025.4-1222 (Bradac et al. 2008) 3) Abell 520 (Mahdavi et al. 2007), “Train Wreck” has become dissociated 4) Abell 2744 (Merten et al. 2011), “Pandora’s Cluster” 5) Abell 2163 (Okabe et al. 2011) from dark matter 6) Abell 1758 (Ragozzine et al. 2011) 7) DLSCL J0916.2+2951 (Dawson 2012), “Musket Ball Cluster” Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 5 / 30 Abell 3376 14 Mvir = 5.2 × 10 M z = 0.0456 Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 6 / 30 radio relics ROSAT (X-ray) + VLA (radio) Bagchi, Durret, Lima Neto & Paul (2006) Abell 3376: a nearby merging cluster X-ray emission XMM-Newton Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 7 / 30 Abell 3376: a nearby merging cluster X-ray emission radio relics XMM-Newton 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 Abell 3376: a nearby merging cluster X-ray emission radio relics XMM-Newton 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 Abell 3376: radio giant (2 Mpc) radio lobes around cluster no associated jets magnetic field ∼ 1µG Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 8 / 30 Abell 3376: brightest cluster galaxies optical (galaxies) Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 9 / 30 Abell 3376: brightest cluster galaxies optical (galaxies) Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 9 / 30 Abell 3376: brightest cluster galaxies X-ray (intracluster gas) second BCG coincides with X-ray peak; BCG does not Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 9 / 30 Abell 3376: brightest cluster galaxies X-ray (intracluster gas) second BCG coincides with X-ray peak; BCG does not separation: 970 kpc Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 9 / 30 initial parameters: • DM density profile • mass ratio • gas density profile • gas fraction • initial relative velocity • impact parameter Numerical simulations: initial conditions Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 10 / 30 initial parameters: • DM density profile • mass ratio • gas density profile • gas fraction • initial relative velocity • impact parameter Numerical simulations: initial conditions Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 10 / 30 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 Numerical simulations: initial conditions initial parameters: a posteriori: • DM density profile • mass ratio • time after central passage • gas density profile • gas fraction • projection angles • initial relative velocity • impact parameter Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 10 / 30 Numerical simulations: alphacrucis, 2304 cores Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 11 / 30 Numerical simulations: evolution X-ray surface brightness emission-weighted temperature time Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 12 / 30 Numerical simulations: evolution Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 13 / 30 Numerical simulations: parameter space sample Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 14 / 30 : Hernquist (similar to NFW) : Dehnen γ=0 (similar to β-model) : fgas = 0:18 Numerical simulations: parameter space of IC initial parameters: • DM density profile • gas density profile • initial relative velocity • mass ratio • gas fraction • impact parameter Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 15 / 30 : Dehnen γ=0 (similar to β-model) : fgas = 0:18 Numerical simulations: parameter space of IC initial parameters: • DM density profile : Hernquist (similar to NFW) • gas density profile • initial relative velocity • mass ratio • gas fraction • impact parameter Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 15 / 30 : fgas = 0:18 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 • impact parameter Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 15 / 30 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 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 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 Numerical simulations: mass ratio MB = 1/2 1/4 1/6 1/8 MA Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 16 / 30 Numerical simulations: impact parameter b = 0 150 kpc 350 kpc 500 kpc Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 17 / 30 Numerical simulations: initial relative velocity vo = 500 km/s 1000 km/s 1500 km/s 2000 km/s Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 18 / 30 Numerical simulations: relative gas concentration • central gas density of the minor cluster ρB = 1 2 4 6 ρA Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 19 / 30 Numerical simulations: inclination i = 0◦ 30◦ 40◦ 60◦ Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 20 / 30 Comparison to observations observed simulated Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 21 / 30 Mach number Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 22 / 30 Mach number: Rankine-Hugoniot jump conditions emission map temperature map T 5M4 + 14M2 − 3 2 = T 16M2 temperature 1 n 4M2 2 = 2 density n1 M + 3 P 5M2 − 1 2 = pressure P1 4 ! !−5=3 S 5M2 − 1 4M2 2 = 2 entropy S1 4 M + 3 2 ! 3M − 3 vx;2 − vx;1 = (vs − u) streaming 4M2 gas velocity Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 23 / 30 i = 40◦ M = 2.9 Mach number: inclination i = 0◦ M = 3.9 Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 24 / 30 Mach number: inclination i = 0◦ i = 40◦ M = 3.9 M = 2.9 Rubens Machado (IAG/USP) Simulations of the merging galaxy cluster Abell 3376 24 / 30 Dark matter
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