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Summary(3) -- Dynamics in the universe --

Summary(3) -- Dynamics in the universe --. T. Ohashi (Tokyo Metropolitan U) Instrumentation for dynamics Cluster hard X-rays X-ray cavities Dark matter dynamics Large-scale features. Strong gravity(BH, Darkmatter) Collision, Explosion, Jets, Magnetic fields etc. X-rays. g -rays.

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Summary(3) -- Dynamics in the universe --

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  1. Summary(3)-- Dynamics in the universe -- T. Ohashi (Tokyo Metropolitan U) Instrumentation for dynamics Cluster hard X-rays X-ray cavities Dark matter dynamics Large-scale features

  2. Strong gravity(BH, Darkmatter)Collision, Explosion, Jets, Magnetic fields etc X-rays g-rays Science with NeXT High-energy universe Global view of dynamical processes in the universe Doppler spectroscopyMicrocalorimeter Gas motion, Shocks Hard X-ray imageSupermirror + imaging detector Gas heating Particle acceleration g-ray spectrumCompton telescope SpectroscopyMicrocalorimeter Cosmic rays

  3. Emission lines and Doppler spectroscopy 12 eV • Energy resolution of SXS DE~7 eV (or better) • Fe-K line complex resolved into resonance, intercombination, forbidden lines • Gas motion with v ~ 100 km s-1 resolved

  4. 10 keV 100 keV Suzaku NeXT 2-order increase in hard-X sensitivity

  5. Cluster hard X-rays Hard X-rays from 14 clusters • LHard ~ 1043 erg s-1 is reported from about 10 clusters • Merger systems tend to show hard X-ray emission • The detection is still controversial.Coma cluster(Fusco-Femiano et al 04 ⇔ Rossetti and Molendi 04) Nevalainen et al. 04 Thermal

  6. LRadio(erg/s) Lx (h=0.5) 1045 1046 1042 1041 Ensslin and Roettgering 02 Cluster radio halos and relics A3667: Radio relic Dn=3 GHz Feretti astro-ph/0406090

  7. Expected hard X-ray luminosity Microwave background • Observed data → LRadio~1041-42 erg s-1 • if B = 3 mG, then uB ~ uph ~ 0.3 eV cm-3→ sensitivity of LHard ~ 1041-42 erg s-1 is necessary to explore inverse Compton emission • This is about 100 times higher sensitivity, achievable with the supermirror instrument • If protons carry 100 times more energy than electrons (@ magnetic energy density), then non-thermal energy is a large fraction in clusters (equivalent to 1043-44 erg s-1)

  8. X-ray Cavities HCG62 (Chandra):Morita et al. 06 MS0735.6+7421 (z=0.22)McNamara et al. 05 deviation “Ghost cavity” Hot gas displaced by radio lobes Ghost cavities are X-ray cavities without radio lobes nor radio galaxy

  9. Non-thermal pressure Pressure to match gas pressure • k = Ratio of proton/electron energy density • f = filling factor (~1) • Required energy density >> u(magnetic field + electrons) • Large variation of k • All protons or extremely hot gas? k/f HCG62 Dunn et al. 05

  10. (z=0) Gas Dark Matter Dark matter blobs Cluster simulation: Eke et al. 98 Simulation under CDM scenario • Dark matter blobs are produced • In local group, only ~1/10 are detected as satellite galaxies • Blob velocity (groups): v = 100-1000 km s-1 Galaxy group simulation:Klypin et al. 99

  11. Motion of dark matter blobs Weak lens mass (DM travels forward) • DM particles/blobs continue to move even after gas is relaxed • Dark matter blobs may carry significant fraction of energy Gas 1E0657-56: Markevitch et al. 04 Darkmatter Evrard 1990 (line = velocity)

  12. Particle collision with DM blobs can cause Statistical Fermi acceleration It is possible to accelerate particles within life of clusters DM blobs may contribute to acceleration Dark Matterblob Particle V (V = 2000 km s-1, tcoll = 100 kpc/c = 1013 s) Intracluster space

  13. Pointing vs survey • Narrow field, high sensitivity: NeXT, Con-X, Xeus • Wide field, survey: eROSITA, MAXI, DIOS • Only a few % of the whole sky covered with CCD resolution • Truly large scale structures: cosmic web, Galactic hot gas, cluster survey etc

  14. Spectroscopy with microcalorimeters NeXT SXS Large 12x12 pix, f.l. = 6m 32 pix, f.l. = 9m

  15. Warm-hot intergalactic medium Expectation from DIOS 5 degree = 75 Mpc Yoshikawa et al. 03

  16. Dynamics of galactic hot gas Dynamics of hot galactic ISM: Galactic fountain GSPC spectrum OVII ROSAT map Snowden et al. 95, ApJ 454, 643 Inoue et al. 79, ApJ 227, L85

  17. Suzaku to NeXT decade Suzaku • Low background and wide-band sensitivity • Detection of non-thermal emission from bright objects NeXT • First image of non-thermal emission with >100 times higher sensitivity • Gas dynamics through X-ray spectroscopy, with low background soft g-ray detectors • Science of on-thermal universe will be much advanced + Wide field mission for complementary science

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