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

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
Science with NeXT
High-energy universe
Global view of dynamical processes in the universe
Doppler spectroscopy Microcalorimeter
Gas motion, Shocks
Hard X-ray image Supermirror imaging detector
Gas heating
Particle acceleration
g-ray spectrum Compton telescope
Spectroscopy Microcalorimeter
Cosmic rays
3
Emission lines and Doppler spectroscopy
12 eV

• Energy resolution of SXS DE7 eV (or better)
• Fe-K line complex resolved into resonance,
  intercombination, forbidden lines
• Gas motion with v 100 km s-1 resolved

4
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
Cluster radio halos and relics
A3667 Radio relic
Dn3 GHz
Feretti astro-ph/0406090
7
Expected hard X-ray luminosity
Microwave background

• Observed data ? LRadio1041-42 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 (_at_ 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
MS0735.67421 (z0.22)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 gtgt u(magnetic field
  electrons)
• Large variation of k
• All protons or extremely hot gas?

k/f
HCG62
Dunn et al. 05
10
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 simulationKlypin 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
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

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 gt100
  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