1. No category

A Joint Approach of
HSC WL and Astro-H (SXS/SXI/HXI)
to Cluster Sciences
Nobuhiro Okabe
(Kavli IPMU)
current
cluster
catalog
HSC
2014
Astro-H
eROSITA
XMM
SXS SXI HXI survey pointing pointing
~3-4yrs
2015
2016
2017
2018
2019
2020
2021
X+WL+SZ
~4yrs
proposal
2-4ksec
?
HSC
cluster
catalog
LSS/XXL field
pointing observations
Stacked X+WL
data release
main role
eROSITA
cluster
catalog
new
cluster VERY X-ray luminous clusters.
catalog
24 MCXC clusters
(~60000 counts)
X+WL+SZ
HSC clusters
X+WL(+SZ)
~3yrs
proposal??
ACT-pol deep field.
X+SZ+WL
HSC clusters X+WL
eROSITA (HSC survey region= 2-4ksec = 4-8ksec of XMM)
is too shallow for cluster sciences
Astro-H/SXS = very bright clusters
full sky
XMM (deep)+ HSC
WL analysis
at early phase of
eROSITA
stacked X+WL analysis
in eROSITA/HSC era
from Peter Predehl’s file (X-ray Universe 2014)
Definition of X-ray luminous clusters is
important for both Astro-H and XMM/eROSITA
24 MCXC clusters (we are preparing XMM proposal)
MCXC clusters
SXS : direct measurement of gas motions
(e.g. turbulence,bulk motions)
is one of outstanding problems in both cluster
physics and cluster cosmology.
?
@ central regions
non-thermal pressure
Astro-H/SXS
WL mass
HSC
hydrostatic equilibrium mass (X-ray)
XMM/Chandra
Targets : 1 Cool-core of very luminous clusters
2 Merging/Cold-front clusters
3 Systematic Study (e.g. MCXC clusters in HSC survey region)
SXS : cool-core in X-ray luminous clusters
Hydra A
SXS FoV
~3x3 arcmin^2
* gravity wave dominated ?
Mach < 0.25
*sound wave/
bulk motions ?
0.5 < Mach < 1
gas motion with
~ 500 km/s is detectable.
Blue : X-ray
Red : Radio
weak-limit of lensing
signal is breakdown
in r<1 arcmin of
clusters @ z>0.2
External Data is essential to measure mass profile
around cool - cores at the SXS’s accuracy level.
SL+WL (A1689)
SL+WL+BCG Kinematics (A383)
Broadhusrt,Takada,Umetsu+05
Newman+11
SL+WL vs X-ray masses
(A1689:Kawaharada,Okabe,Umetsu+10)
non-thermal pressure
or lensing bias ?
SXS
Hydra A : WL+BCG Kinematics (Okabe+ in prep)
z~0.05
figure removed
HSC(+Kinematics +SL) vs AstroH+XMM/Chandra
would be powerful.
SXS : cold front cluster (e.g. A2034)
cold front
Cold front (=contact
discontinuity )
is formed by a moving dark
matter clump.
moving gas
Okabe+Umetsu08
z~0.09
Waked velocity field is
calculated by linear perturbation
theory for a moving point source
(Mwl) in the gas.
SXI : 1 spatial resolution ~ 1 arcmin
2 powerful to detect faint X-ray emission
3 similar to Suzaku’s instrument.
Targets : 1 massive clusters discovered by HSC survey
( a few x 10 ksec; or XMM/Chandra) .
2 Cluster Outskirts (after SXS: 200-300 ksec)
1 : follow-up Suzaku obs for
2 : cluster outskirts.
lensing-detected clusters.
z~0.4
virial radius
z~0.4
unobservable
z~0.2
before
Suzaku
z~0.2
z~0.2+z~0.1
Watanabe+11
Kawaharada+10
Unexpected feature of hot gas in cluster outskirts.
Temperature
Entropy
flatness
Sato+12
Walker+12
flatness of entropy
* heating inefficiency (T: Lapi+10)?
* gas clumsiness (n : Nagai+11) ?
Correlation between the outskirts temperature (or
density) and surrounding large scale structure is
found in a few clusters.
Kawaharada,Okabe+10
kBT
Galaxy distribution
(SDSS)
could be
replaced by
HSC data
Photometric data is important to determine X-ray pointings.
Joint Suzaku X-ray + Subaru WL analysis
Entropy profile normalized by
WL M200c and r200c
•developed a
simultaneous fitting
method considering
Entropy flattens mass-observable
at > ~ 0.5 r500
scaling relation and
radial profile.
•Thermalization
mechanism over the
entire cluster region is
controlled by the gravity.
shock
heating
model
self-similar profile
Okabe+14
•Heating efficiency in
cluster outskirts needs
to be modified from the
standard law.
Joint fit to Density and Temperature Profiles
slightly shallower
steeply drops
Considered error
covariance matrix
and intrinsic
scatter.
Caused by the
steeping T profile,
rather than the
flattening n profile.
Systematic study of SXI + HSC WL+photometric data on 24 MCXC
clusters should be conducted.
1: hard X-ray imager
HXI : 2: one-order lower background
Targets: radio halo/relic clusters
to detect inverse Compton X-ray emission of Cosmic-ray
electrons and constrain magnetic strength.
Radio Halo
bullet
Radio Relic
Stroe+12
shock
Govoni+04
CIZA
J2242.8+5301
WL analysis : CIZA J2242.8+5301 (Okabe+ in prep)
WL constrains Mass ratio, Merger time-scale, and so on.
figure removed
DM structure survives
X-ray structure is destroyed
Systematic Joint Astro-H and HSC SSP Survey Study is
definitely powerful for cluster sciences.
1 : Definition of the Sample is important because only X-ray
luminous clusters can be observed.
(e.g. MCXC clusters in XMM proposal).
2 : SXS : direct probe of gas motion.
?
HSC WL + (SL+ Kinematics) Chandra/XMM SXS
3 : SXI : cluster outskirts.
joint fit with HSC WL + SXI observables
HSC photometric data : X-ray pointings/ anisotropic T/n distribution
4 : SXI : follow-up observations for HSC-discovered clusters.
5 : HXI : Radio Relic clusters :
HSC WL is powerful to constrain Cluster Dynamics