CLASH SZE Observations and Collaborations

1. CLASH SZE Observations and Collaborations Keiichi Umetsu, Academia Sinica IAA (ASIAA), Taiwan (September 20, 2010)

2. Contents • Thermal Sunyaev-Zel’dovich Effect (tSZE) • SZE Importance in Cluster Science • Ground-based SZE Instruments • “CLASH SZE” Collaborations • Weak lensing distortion (shear) + depletion (magnification bias) with Subaru CLASH-SZE wikihttps://sites.google.com/site/clashsze/

3. 1. Thermal Sunyaev-Zel’dovich Effect (tSZE) Zel’dovich & Sunyaev (1969); Sunyaev & Zel’dovich (1972) Energy transfer by IC scattering Observer CMB Last Scattering surface (z~1100) Hot gas with the electron temperature Te>>TCMB(z) gn=-2 (n=0), gn<0 (n<~220GHz), gn=0 (n~220GHz), gn>0 (n>~220GHz) Te-dependent relativistic correction needed for hot clusters (>5% at 90GHz for >8keV clusters) 10^-4 10^-2 10^-2 Degree of Comptonization: y = (optical depth of gas) x (gain per scattering) = (thermal electron pressure) x (dlos)

4. SZE Frequency Spectrum: Theory vs. Measurements Abell 2163 (z=0.201) SZE Brightness Relativistic correction: Te=14, 12, 10, 8keV from top to bottom Nord et al. 2009, A&A, 506, 623

5. SZE Importance AMiBA-7 SZE images (Wu et al. 2009, ApJ, 694, 1619) Power of tSZE: tSZE brightness is ① Independent of D(z) i.e., free from cosmological brightness dimming, ② A measure of projected thermal electron pressure Complementary to X-ray Bremsstrahlung Inverse Compton (no redshift dimming)

6. Higher resolution, sensitivity 2. Science with SZE+ • Cosmology • Cluster counts and evolution, N(z) • SZE power spectrum (s8) • Hubble diagram by SZE+X (0.18<z<0.9) • Cluster 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> (Wm/WDE)^(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)

7. Science Highlight (I): Baryon Fractions Large-scale fgas constraints (~0.8rvir, <z>=0.2) from tSZE+WL+X, independent of dynamical state and level of hydrostatic equilibrium AMiBA-7 tSZE + WL + X-ray WMAP7 tSZE and X-ray constraints Vikhlinin+2009 Komatsu et al. 2010, WMAP-7yr Umetsu, Birkinshaw, Liu et al. 2009, ApJ, 694, 1643 (arXiv:0810.969)

8. Science Highlight (2): Level of H.E. Level of Hydrostatic Equilibrium (H.E.) in relaxed clusters: Thermal (hot gas) to equilibrium (lensing) pressure ratio in clusters? Theory: Molnar, Chiu, Umetsu+10 Observations: Kawaharada, Okabe, Umetsu+10 M>1e15 Msun AMR1: relaxed AMR2: relaxed AMR3: disturbed Suzaku-Xray on A1689 Thermal to equilibrium pressure ratio • 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%

9. Methodology: (X+SZE) + Lensing • Detailed X+SZE modeling of (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 parameters 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) (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 mass • Free from any equilibrium assumption (Umetsu+09; Zhang+10)

10. Non-Parametric X+SZE Deprojetion A2163 (z=0.21): Nord et al. (2009) Color-coded: APEX-SZ (150GHz) Contours: XMM-Newton Joint Abel deprojection (Silk & White 1978)

11. 3. Ground-based SZE Instruments 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 purposes - 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

12. SZE Frequency Coverage Red: Interferometer Blue: Multi-pixel bolometer • Relative SZE strength w.r.t. primary CMB and foreground emission 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. SZA(BIMA,CBI,VSA) SPT ACT APEXBolocam AMI AMiBA [SZA] SPT, GBT/Mustang SPT ACT APEX Figure from Zhang+02

13. 4. CLASH-SZE Collaborations CLASH-SZE • Collaboration between CLASH and several groups observing the SZ effect (Bolocam, Mustang, AMiBA, SZA) • CLASH-SZE wiki has been set up thanks to Dan https://sites.google.com/site/clashsze/ Rationale: SZE counter part of “ACS+Subaru” multiscale lensing collaboration • Large 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 SZE(10”-1’) • GBT/Mustang@90GHz (40”x40” FoV, 9” res) • SZA@90GHz (4’ FoV, 20” res) Two-types of collaboration involved: • CLASH lensing+SZE+ collaboration (involving CLASH data) • Multiscale SZE collaboration (pure SZE collaboration)

14. (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!! • Bolocam SZE observations in October 8-21 (Observers: K. Umetsu, P. Koch, S. Molnar, K.-Y. Lin, J. Sayers, N. Czakon) • Status 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+

15. (2) CLASH-Mustang Collaboration B. Mason et al. 2010 • Status 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

16. (3) AMiBA and SZA Interferometers Ho, P.T.P.+2009, ApJ AMiBA-7 (2006-2008) AMiBA-13 (2010-) Sunyaev Zeldovich Array Muchovej, S. et al. 2007, ApJ

17. Summary • 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 Mason et al.

18. Distortion vs. Magnification-Bias (Counts) Profiles Count depletion of red background galaxies being consistent with the tangential distortion!!!

19. 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 Preliminary results (Umetsu+2010, in prep) Model independent constraints on the density slope, dS/dr

20. Sample of Cluster Mass Profiles Distortion + Magnification Umetsu+2010 in prep

21. Fin

22. Appendix: Foreground Contaminations Typical SEDs of Galaxies – most radio point sources have negative spectral index Synchrotron Dust CMB interferometers: CBI (@30GHz) AMI (@15GHz) SZA (@30/90GHz)

23. Appendix: SZE with ALMA