Summary(3) -- Dynamics in the universe -- T. Ohashi (Tokyo Metropolitan U) 1.Instrumentation for dynamics 2.Cluster hard X-rays 3.X-ray cavities 4.Dark matter dynamics 5.Large-scale features

Science with NeXT Strong gravity(BH, Darkmatter) Collision, Explosion, Jets, Magnetic fields etc Gas motion, Shocks Particle acceleration Spectroscopy Microcalorimeter Hard X-ray image Supermirror + imaging detector  -ray spectrum Compton telescope Gas heating High-energy universe X-rays  -rays Doppler spectroscopy Microcalorimeter Cosmic rays Global view of dynamical processes in the universe

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

2-order increase in hard-X sensitivity Suzak u NeXT 10 keV100 keV

L Hard ~ 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) Cluster hard X-rays Nevalainen et al. 04 Hard X-rays from 14 clusters Thermal

Cluster radio halos and relics A3667: Radio relic L x (h=0.5) Ensslin and Roettgering L Radio (erg/s ) Feretti astro-ph/  =3 GHz

Expected hard X-ray luminosity Observed data → L Radio ~ erg s -1 if B = 3  G, then u B ~ u ph ~ 0.3 eV cm -3 → sensitivity of L Hard ~ 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 erg s -1 ) Microwave background

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

Non-thermal pressure HCG62 k/f 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? Dunn et al. 05 Pressure to match gas pressure

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

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

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

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

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

Warm-hot intergalactic medium Yoshikawa et al degree = 75 Mpc Expectation from DIOS

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

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