PART II Simulations of Shocks in Clusters of
- Slides: 20
PART II Simulations of Shocks in Clusters of Galaxies ALMA Users Workshop 8 February, 2010 Sándor M. Molnár, Patrick Koch Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan
Collaborators for FLASH Simulations: Nathan Hearn (Univ. of Chicago) Joachim Stadel (Univ. of Zurich)
Outline I. Shocks in Clusters of Galaxies: Observations II. Shocks in Clusters of Galaxies: FLASH 3 D Simulations III. Applications to ALMA: work in progress IV. Summary
I. Shocks in Clusters of Galaxies: Observations
Coma Cluster of Galaxies (z=0. 025, 2 x 1015 M⦿); optical image (Kitt Peak National Observatory).
Coma Cluster of Galaxies: X-ray image (XMM-Newton).
The bullet cluster: 1 E 0657 -56: Mach ~ 3; Markevitch & vikhlinin (2007); Clowe et al. (2006).
The bullet cluster: Bradac et al. (2006)
II. Shocks in Clusters of Galaxies: FLASH 3 D Simulations
Shocks in Clusters of Galaxies Rankine-Hugoniot jump conditions ρ2 / ρ1 = (γ+1) M 12 / ((γ-1) M 1 2 +2) P 2 / P 1 = 1 + 2 γ (M 12 -1)/ (γ+1) T 2 / T 1 = (1+γ (2 M 12 -1))(2+(γ-1) M 12)/((γ+1)2 M 12) M 1 = ( 2 r / (γ + 1 – r (γ-1) )-1 Compression: r = ρ2 / ρ1
FLASH Simulations of clusters of galaxies total mass: 1014 M⦿ - 1015 M⦿ dark matter NFW from Navarro at el. (1997): ρgas ~ ( r/rs )-1 (1 + r/rs)-2 R < Rcut σr from Lokas & Gamon (2001) ICG model density: β model: ρ ~ (1 + r 2/r 2 core)-3β/2 R < Rcut temperature: from hydrostatic equilibrium previous simulations: GADGET 2 (SPH): Springel & Farrar (2007); GASOLINE (SPH): Mastropietro & Burkert (2008); FLASH 2 D: Milosavljevic et al. (2007) FLASH 3 D: Zu. Hone et al. (2009 a, b)
FLASH 3 D simulations: line of sight collision
FLASH Simulations of clusters of galaxies Simulations for high resolution SZ-X-ray observations: RXJ 1347
High-resolution multi-wavelength observations of RXJ 1347 (Mason et al. 2010; submitted to Ap. J. )
FLASH 3 D simulations for RXJ 1347 (Molnar et al. 2010; in prep. )
III. Applications to ALMA
Why arc second resolution? – – To understand the physics of the cluster gas: • • • The role of transport proceses Thermal viscosity Conduction Turbulence Magnetic fields Can we model clusters well enough to do precision cosmology? Example: arc second resolution in X-ray: – – Turbulent intra-cluster gas with disturbed struct. shock physics: below the Coulomb mean free path Arc sec SZ (ALMA) – Accurate pressure distribution: same as X-ray resol.
Work in progress – Accretion shocks in clusters of galaxies: hard to observe but important (Molnar et al 2009) – Merger shocks in clusters of galaxies: CASA simulations based on images from FLASH 3 D simulations
IV. Summary • Arc minute scale: Clusters of galaxies for cosmology – – • numbers counts scaling relations (e. g. , AMi. BA) Few arc second to (sub)arc second: Cluster physics – – 10 arc second: shock features appear (e. g. , Mustang) 1 arc second: detailed maps comparable to Xray (ALMA)
THE END
- How does aunt alexandra treat calpurnia
- Fsae shocks
- Shift in sras curve
- World history simulations
- Baton simulations
- Clinical simulations in nursing education
- Simulations for solid state physics
- Chris harding simulations
- Www.irs.gov/app/understanding taxes/student/simulations.jsp
- Tcad simulations
- Key tenets of ippd
- Don't gamble with physical properties for simulations
- Technical description meaning
- Brainpop ratios
- Front bar parts
- Addition symbol
- The phase of the moon you see depends on ______.
- Part to part ratio definition
- Part to part variation
- Regents
- Galaxy clusters