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

T. Ohashi (Tokyo Metropolitan U) 1. Instrumentation for dynamics 2. Cluster hard X-rays3. X-ray cavities4. 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, intercombinatio

n, forbidden lines Gas motion with v ~ 100 km s-1 resolved

2-order increase in hard-X sensitivity

Suzaku

NeXT

10 keV 100 keV

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)

Cluster hard X-rays

Nevalainen et al. 04

Hard X-rays from 14 clusters

Thermal

Cluster radio halos and relics

A3667: Radio relic

1045 1046Lx

(h=0.5)

Ensslin and Roettgering 02

1042

1041

LRadio

(erg/s)

Feretti astro-ph/0406090

=3 GHz

Expected hard X-ray luminosity

Observed data → LRadio~1041-42 erg s-1

if B = 3 G, 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)

ph

B

IC

syn

u

u

L

L

L

L

X-Hard

RadioMicrowave background

X-ray CavitiesHCG62 (Chandra):Morita et al. 06

“Ghost cavity”

MS0735.6+7421 (z=0.22)McNamara et al. 05

Hot gas displaced by radio lobesGhost cavities are X-ray cavities without radio lobes nor radio galaxy

deviation

Non-thermal pressure

HCG62k/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

Gas Dark 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 = 100-1000 km s-1

Motion of dark matter blobs

1E0657-56: 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

Darkmatt

er

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

y1024

1 9coll

2

acc

tVc

t

(V = 2000 km s-1, tcoll = 100 kpc/c = 1013 s)

Dark Matterblob

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, G

alactic 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. 03

5 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 decadeLow 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