CLASH SZE Observations and CollaborationsCLASH SZE Observations and Collaborations

Keiichi Umetsu, Keiichi Umetsu,

Academia Sinica IAcademia Sinica IAAAA (ASIAA (ASIAA), Taiwan ), Taiwan (September 20, 2010)(September 20, 2010)

ContentsContents

1)1) Thermal Sunyaev-Zel’dovich Effect (tSZE)Thermal Sunyaev-Zel’dovich Effect (tSZE)2)2) SZE Importance in Cluster ScienceSZE Importance in Cluster Science3)3) Ground-based SZE InstrumentsGround-based SZE Instruments4)4) ““CLASH SZE” CollaborationsCLASH SZE” Collaborations5)5) Weak lensing distortion (shear) + depletion Weak lensing distortion (shear) + depletion

(magnification bias) with Subaru (magnification bias) with Subaru

CLASH-SZE wikiCLASH-SZE wiki https://sites.google.com/site/clashsze/

1. Thermal Sunyaev-Zel’dovich Effect (tSZE)1. Thermal Sunyaev-Zel’dovich Effect (tSZE)

Zel’dovich & Sunyaev (1969); Sunyaev & Zel’dovich (1972)

ObserverCMB Last Scattering surface (z~1100)

Hot gasHot gas with the electron temperature Te>>TCMB(z)

Degree of Comptonization: y = (optical depth of gas) x (gain per scattering)

= (thermal electron pressure) x (dlos)

ygT/T )(CMB g=-2 (=0), gn<0 (<~220GHz),

g=0 (~220GHz), g>0 (>~220GHz)Te-dependent relativistic correction needed for hot clusters (>5% at 90GHz for >8keV clusters)

Energy transfer by IC scattering

10^-4 10^-2 10^-2

SZE Frequency Spectrum: Theory vs. MeasurementsSZE Frequency Spectrum: Theory vs. Measurements

Nord et al. 2009, A&A, 506, 623

Abell 2163 (z=0.201)Abell 2163 (z=0.201)

SZE

Brig

htne

ss

Relativistic correction: Te=14, 12, 10, 8keV from top to bottom

SZE ImportanceSZE Importance

42 )1()/( zDD LA

① ① Independent of D(z) Independent of D(z)

i.e., free from cosmological i.e., free from cosmological brightness dimming,brightness dimming,

Power of tSZE:Power of tSZE:tSZE brightness istSZE brightness is

② ② A measure of projected A measure of projected thermal electron pressurethermal electron pressure

Complementary to X-rayComplementary to X-ray

dlPdlTnI

zdlTnI

eeeSZE

eeX4)1(2/12

Bremsstrahlung

Inverse Compton (no redshift dimming)

AMiBA-7 SZE images (Wu et al. 2009, ApJ, 694, 1619)

2. Science with SZE+2. Science with SZE+

• CosmologyCosmology– Cluster counts and evolution, N(z) – SZE power spectrum (8)– Hubble diagram by SZE+X (0.18<z<0.9)

• Cluster PhysicsCluster Physics– Total thermal energy

• Gas mass fractions, fgas(r), from lensing+X+SZE• Thermal pressure, Pgas(r): universal? equilibrium?• Entropy profile shapes (Tozzi & Norman ’01; Cavaliere+05)• Mass proxy: Y-M and deviations

– IC gas structure• Merger shocks and substructure

– Greater frequency of violent activities at z> (m/DE)^(1/3w)-1 ~ 0.4• Gas clumpiness• Accretion shocks in cluster outskirts (ALMA)

– Gas radial velocities (w.r.t. CMB) by kinematic SZE • Sensitive multifrequency SZE, including 220GHz needed (Planck)

Hig

her r

esol

ution

, sen

sitiv

ityH

ighe

r res

oluti

on, s

ensi

tivity

Science Highlight (I): Baryon FractionsScience Highlight (I): Baryon Fractions

Umetsu, Birkinshaw, Liu et al. 2009, ApJ, 694, 1643 (arXiv:0810.969)

Komatsu et al. 2010, WMAP-7yr

WMAP7 tSZE and X-ray constraintsAMiBA-7 tSZE + WL + X-ray

Large-scale fgas constraints (~0.8rvir, <z>=0.2) from tSZE+WL+X, independent of dynamical state and level of hydrostatic equilibrium

Vikhlinin+2009

Science Highlight (2): Level of H.E.Science Highlight (2): Level of H.E.Level of Hydrostatic Equilibrium (H.E.) in relaxed clustersLevel of Hydrostatic Equilibrium (H.E.) in relaxed clusters: Thermal (hot gas) to equilibrium (lensing) pressure ratio in clusters?

TheoryTheory: Molnar, Chiu, Umetsu+10

AMR1: relaxedAMR2: relaxedAMR3: disturbed

• Nonthermal pressure contribution in relaxed (high-mass) clusters takes a minimum of ~15% at 0.1Rvir, growing to >30% at r=Rvir. (cf. Lau, Kravtsov, Nagai 09).

• Subsonic random gas motions at r<0.1Rvir contributes by 15%-40%

M>1e15 Msun

ObservationsObservations: Kawaharada, Okabe, Umetsu+10

Suzaku-Xray on A1689

Thermal to equilibrium pressure ratio

Methodology: Methodology: (X+SZE) + Lensing(X+SZE) + Lensing

• Detailed X+SZE modeling of Detailed X+SZE modeling of (n, T)(n, T) (e.g., Molnar, Umetsu, Birkinshaw+10, ApJ, arXiv:1009.1943)

– Calibrated by high-resolution cosmological simulations– High-resolution X-ay data to constrain the central structure parame

ters of (n, T) typically at r<r500

– Large-scale SZE (e.g., AMiBA) to constrain the normalization and outer scale of P(r) typically at r~r200

• Simultaneous X+SZE deprojection of (n, T)Simultaneous X+SZE deprojection of (n, T) (e.g., Ameglio+07, MNRAS, 382, 397; Nord+09, A&A, 506, 623)

– Non-parametric – Spherical symmetry assumed– Without using spectroscopic X-ray temperature (cf. Mazzotta+04)

• Lensing data to constrain the total massLensing data to constrain the total mass– Free from any equilibrium assumption (Umetsu+09; Zhang+10)

Non-Parametric X+SZE DeprojetionNon-Parametric X+SZE Deprojetion

Joint Abel deprojectionJoint Abel deprojection (Silk & White 1978)

Color-coded:

APEX-SZ APEX-SZ (150GHz)

Contours: XMXMM-NewtonM-Newton

A2163 (z=0.21): Nord et al. (2009)

SZE-dedicated SZE-dedicated

- Bolometers: ACT (145,225,265 GHz), APEX-SZ (150,217 GHz), SPT (95,150,225 GHz)

- Interferometers: AMI (15GHz), AMiBA (90GHz), SZA (30,90GHz)

General purposeGeneral purposess

- Bolometers: GBT/MUSTANG @90GHz, Bolocam @150GHz

- Interferometers: CARMA-SZA @30,90GHz

- Single dish radiometer: OCRA @30GHz

Blue: multi-pixel bolometer array

Red: interferometer array

Green: single dish radiometer

3. Ground-based SZE Instruments3. Ground-based SZE Instruments

SZE Frequency CoverageSZE Frequency Coverage

SPT ACT APEX Bolocam

SZA (BIMA,CBI,VSA)

Red: Interferometer

Blue: Multi-pixel bolometer

– Relative SZE strength w.r.t. priprimary mary CMBCMB and foreground foreground emissionemission is maximized at 90-100GHz.

– CMB/SZE interferometers based on HEMT (<100GHz).

– Except CSO/Bolocam (+19.8d) and GBT/Mustang (+38.4d), SZE bolometers are mostly sited in the southern hemisphere.

SPT ACT APEX

AMiBA [SZA] SPT, GBT/Mustang

AMI

Figure from Zhang+02

)()(

CMB

tSZE)( fIfI

I fS

4. CLASH-SZE Collaborations4. CLASH-SZE CollaborationsCLASH-SZECLASH-SZE

– Collaboration between CLASH and several groups observing the SZ effect (Bolocam, Mustang, AMiBA, SZA)

– CLASH-SZE wikiCLASH-SZE wiki has been set up thanks to Danhttps://sites.google.com/site/clashsze/

Rationale: Rationale: SZE counter part of “ACS+Subaru” multiscale lensing collaboration– Large scale SZELarge scale SZE (1’-10’)

• Bolocam@150GHz (8’ FoV, 1’ res)• AMiBA-13@94GHz (11’ FoV, 2’ res) or (22’ FoV, 3’ res)• SZA@30GHz (11’ FoV, 1’ res)

– Small scale SZESmall scale SZE (10”-1’)• GBT/Mustang@90GHz (40”x40” FoV, 9” res)• SZA@90GHz (4’ FoV, 20” res)

Two-types of collaboration involvedTwo-types of collaboration involved:– CLASH lensing+SZE+ collaboration (involving CLASH data)– Multiscale SZE collaboration (pure SZE collaboration)

(1) CLASH-Bolocam SZE Collaboration(1) CLASH-Bolocam SZE Collaboration

12 nights proposed for 2010B in collaboration with the Bolocam team:

Umetsu/National, Golwala/Caltech, Moustakas/JPL 14 nights allocated!!14 nights allocated!!

Bolocam SZE observations in October 8-21 (ObserversObservers: K. Umetsu, P. Koch, S. Molnar, K.-Y. Lin, J. Sayers, N. Czakon)

Status SummaryStatus Summary:• 12/25 CLASH clusters observed with by the Bolocam team+

• 8 clusters TBO in 2010B+2011A with CLASH+Bolocam collaboration

• 5 clusters in accessible from MK

Figures by Sunil Golwala, Jack Sayers+

(2)(2) CLASH-Mustang Collaboration CLASH-Mustang Collaboration

B. Mason et al. 2010B. Mason et al. 2010

Status SummaryStatus Summary:• 3 CLASH targets observed (CLJ1226+33, MACSJ0744+39 , RXJ1347-11)

• 1 more in fall 2010 (MACSJ0717+37)

• Planning on joint Mustang proposal with CLASH

(3) AMiBA and SZA Interferometers(3) AMiBA and SZA InterferometersAMiBA-7 (2006-2008)AMiBA-13 (2010-)

Sunyaev Zeldovich Array

Ho, P.T.P.+2009, ApJ

Muchovej, S. et al. 2007, ApJ

SummarySummary• Mid-term

– The baseline of collaboration policies has been set up • For papers involving HST-CLASH data, we will invite all of the

CLASH core members (those 23 on the HST MCT proposal) to join as co-authors.

• Each of the SZE groups may have similar policies at their discretion. That is, whenever their data is used, they decide who on their team should be invited to join on the paper.

– Details to be discussed further (individually and collectively among the groups)

• Short-term– Upcoming Mustang proposal: coordination with Brian M

ason et al.

Distortion vs. Magnification-Bias (Counts) ProfilesDistortion vs. Magnification-Bias (Counts) Profiles

Count depletion of red background galaxies being consistent with the tangential distortion!!!

Bayesian mass profile reconstruction Bayesian mass profile reconstruction • Bayesian analysis of joint distortion and magnification (counts) profiles

• Model independent

• Mass-sheet (boundary condition) free

• Automatically account for the depth miss-match between the distortion (blue+red) and magnification (red) galaxy samples

Individual (lines) and stacked (red) surface mass density profiles of 5 massive clusters

Model independent constraints on the density slope, d/dr

Preliminary results (Umetsu+2010, in prep)

Sample of Cluster Mass ProfilesSample of Cluster Mass Profiles

Distortion + Magnification

Umetsu+2010 in prep

FinFin

Appendix: FAppendix: Foreground Contaminationsoreground Contaminations

Synchrotron Dust

Typical SEDs of Galaxies – most radio point sources have negative spectral index

CMB interferometers:

CBI (@30GHz)

AMI (@15GHz)

SZA (@30/90GHz)

Appendix: SZE with ALMAAppendix: SZE with ALMA