A Joint Approach of HSC WL and Astro-H (SXS/SXI/HXI)

to Cluster Sciences

Nobuhiro Okabe (Kavli IPMU)

2014

2015

2016

2017

2018

2019

2020

2021

HSC SXS SXI HXIAstro-H eROSITA XMM

~3-4yrs

2-4ksec~4yrs

survey pointing

~3yrs

ACT-pol deep field.

data release

VERY X-ray luminous clusters.

main role

pointing observations Stacked X+WL

X+SZ+WL

pointing

24 MCXC clusters (~60000 counts)

proposal??

LSS/XXL field

proposal

X+WL+SZ

X+WL+SZ

HSC clusters X+WL

HSC cluster catalog

eROSITA cluster catalog

?

current cluster catalog

new cluster catalog

HSC clusters X+WL(+SZ)

from Peter Predehl’s file (X-ray Universe 2014)

eROSITA (HSC survey region= 2-4ksec = 4-8ksec of XMM) is too shallow for cluster sciences

full sky

stacked X+WL analysisin eROSITA/HSC era

XMM (deep)+ HSC WL analysis

at early phase of eROSITA

Astro-H/SXS = very bright clusters

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)

Targets : 1 Cool-core of very luminous clusters 2 Merging/Cold-front clusters 3 Systematic Study (e.g. MCXC clusters in HSC survey region)

non-thermal pressure WL mass

hydrostatic equilibrium mass (X-ray)

Astro-H/SXS

XMM/Chandra

HSC

is one of outstanding problems in both cluster physics and cluster cosmology.

? @ central regions

SXS : cool-core in X-ray luminous clusters

Blue : X-rayRed : Radio

Hydra A SXS FoV*sound wave/ bulk motions ?

~3x3 arcmin^2

* gravity wave dominated ?Mach < 0.25

0.5 < Mach < 1

weak-limit of lensing signal is breakdown

in r<1 arcmin of clusters @ z>0.2

~ 500 km/s is detectable.gas motion with

SL+WL (A1689)

Broadhusrt,Takada,Umetsu+05 Newman+11

SL+WL+BCG Kinematics (A383)

External Data is essential to measure mass profile around cool - cores at the SXS’s accuracy level.

SL+WL vs X-ray masses (A1689:Kawaharada,Okabe,Umetsu+10)

SXS

non-thermal pressure or lensing bias ?

Hydra A : WL+BCG Kinematics (Okabe+ in prep)z~0.05

HSC(+Kinematics +SL) vs AstroH+XMM/Chandra would be powerful.

figure removed

SXS : cold front cluster (e.g. A2034)

Okabe+Umetsu08

Cold front (=contact discontinuity ) is formed by a moving dark matter clump.moving gas

cold front

Waked velocity field is calculated by linear perturbation theory for a moving point source (Mwl) in the gas.

z~0.09

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 lensing-detected clusters.

Watanabe+11

z~0.4z~0.4

z~0.2

z~0.2

z~0.2+z~0.1

2 : cluster outskirts.

Kawaharada+10

virial radius

unobservable before Suzaku

Sato+12

Unexpected feature of hot gas in cluster outskirts.

Temperature Entropy

Walker+12

* heating inefficiency (T: Lapi+10)? * gas clumsiness (n : Nagai+11) ?

flatness

flatness of entropy

Correlation between the outskirts temperature (or density) and surrounding large scale structure is

found in a few clusters.

kBT

could be replaced by HSC data

Kawaharada,Okabe+10

Galaxy distribution (SDSS)

Photometric data is important to determine X-ray pointings.

Entropy profile normalized by WL M200c and r200c

shock heating model

Entropy flattens at > ~ 0.5 r500

•Thermalization mechanism over the entire cluster region is controlled by the gravity.

•Heating efficiency in cluster outskirts needs to be modified from the standard law.

self-similar profile

Okabe+14

Joint Suzaku X-ray + Subaru WL analysis •developed a

simultaneous fitting method considering mass-observable scaling relation and radial profile.

Caused by the steeping T profile, rather than the flattening n profile.

Joint fit to Density and Temperature Profilesslightly shallower steeply drops

Considered error covariance matrix and intrinsic scatter.

Systematic study of SXI + HSC WL+photometric data on 24 MCXC clusters should be conducted.

HXI : 1: hard X-ray imager 2: one-order lower background

Targets: radio halo/relic clusters

Radio Halo Radio Relic

bullet

Govoni+04CIZA

J2242.8+5301

Stroe+12shock

to detect inverse Compton X-ray emission of Cosmic-ray electrons and constrain magnetic strength.

WL analysis : CIZA J2242.8+5301 (Okabe+ in prep) WL constrains Mass ratio, Merger time-scale, and so on.

X-ray structure is destroyedDM structure survives

figure removed

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)3 : SXI : cluster outskirts.

5 : HXI : Radio Relic clusters :

Chandra/XMM SXS

4 : SXI : follow-up observations for HSC-discovered clusters.

?

HSC photometric data : X-ray pointings/ anisotropic T/n distributionjoint fit with HSC WL + SXI observables

HSC WL is powerful to constrain Cluster Dynamics