Missing Thermal Energy of the Universe Niayesh Afshordi

Missing Thermal Energy of the Universe Niayesh Afshordi Institute for Theory and Computation Harvard College Observatory 1 August 1, 2006 Modern Cosmology, Inflation, CMB and LSS Benasque workshop, August 2006

My Collaborators Yen-Ting Lin University of Illinois Urbana-Champaign Princeton Daisuke Nagai Cal. Tech Alastair Sanderson University of Illinois Urbana-Champaign University of Birmingham Afshordi, Lin, & Sanderson 2005 (1 st yr) Afshordi, Lin, Sanderson, & Nagai 2006 (3 yrs) in preparation 2 August 1, 2006 Missing Thermal Energy of the Universe

Thermal Sunyaev-Zel’dovich (SZ) Effect and Intra-Cluster Medium (ICM) l Probes thermal energy distribution of electrons in the Intra. Cluster Medium l Dominates CMB at angles < 0. 1 o l Generates an anti-correlation between WMAP and galaxy/cluster distribution WMAP sees here 3 August 1, 2006 Missing Thermal Energy of the Universe

Thermal Sunyaev-Zel’dovich (SZ) Effect and the CMB Can VSA and SZA confirm this? Tension with new low WMAP 8 ? ! 4 August 1, 2006 Readhead et al. 2004 Missing Thermal Energy of the Universe

Can SZ surveys sustain the CMB dominance? l SZ clusters can be Detected up to high redshifts l Their number counts probe Dark Energy/Cosmology l Many SZ surveys are underway: APEX, SZA, ACT, SPT, Planck, … l Can they deliver? Calibration of SZ-Mass relation, Gastrophysics, … Courtesy of John Carlstrom 5 August 1, 2006 Missing Thermal Energy of the Universe

In the mean time … While Raul is happily paragliding … … Gastrophysics is waiting with a vengeance! 6 August 1, 2006 Missing Thermal Energy of the Universe

SZ detections in Cross-Correlation with Galaxy/Cluster Surveys l l 7 Bennett et al. 2003 (XBAC’s clusters; 2. 5 ) Fosalba, Gaztanaga, & Castander 2003; Fosalba & Gaztanaga 2004 (SDSS, APM; 2. 7 ) Myers et al. 2004 (APM+ACO; ~2 ) Afshordi, Loh, & Strauss 2004 (2 MASS; 3. 7 ) August 1, 2006 Missing Thermal Energy of the Universe

t. SZ in 2 MASSx. WMAP Correlation Afshordi, Loh, & Strauss 2004 (2 MASS Deepest magnitude bin): l data best fit model ISW SZ Point Sources 8 • Cluster physics is mixed with cosmology, and non-linear bias Missing Thermal Energy of the • Does not employ the 1, non-Gaussianity of the signal August 2006 Universe

SZ detection based on SZ templates made out of Galaxy/Cluster Surveys l l Hernandez-Monteagudo & Rubino-Martin 2004 (BCS, NORAS, etc; 2 -5 ) Hernandez-Monteagudo et al. 2004, 2006 (2 MASSx. WMAP+Archeops; 5 ) • Does employ the non-Gaussianity of the signal • Cluster physics is mixed with template making procedure in a non-trivial manner 9 August 1, 2006 Missing Thermal Energy of the Universe

How to get the most physics out? l l 10 Most Galaxies are NOT in clusters Most SZ signal comes from clusters thus… The SZ detection is more significant if we just look around clusters Make an SZ template The S/N is maximized if the template matches the actual SZ profile Constraint on the SZ profile Observed Sky Template August 1, 2006 Missing Thermal Energy of the Universe

WMAP SZ clusters … l Three close-by clusters in the 3 yr cleaned map (Tegmark et al) Abell 2319 11 Abell 1656 August 1, 2006 Abell 133 Missing Thermal Energy of the Universe

Filter-matched SZ detection in WMAP 3 yr maps l WMAP 3 years – – l 417 clusters – 12 Temperature: Q, V, W Nres = 9 (pixel size ' 0. 1 deg) meaured X-ray temperature August 1, 2006 Missing Thermal Energy of the Universe

Methodology l l l 13 Find R 200 for each cluster using M 200 -TX relation Constrain pressure within spherical radial bins centered at: 0. 25, 0. 5, 1, 2, 4, 8 x R 200 + a central radio source : Only consider pixels close to each cluster, with resolution degrading with distance Makes covariance matrix tractable August 2006 Degraded Abell 23191, in Q-band Missing Thermal Energy of the Universe Abell 2319 in Q-band

Universal Pressure Profile TX > 3 ke. V; 193 Clusters __ CDM/ crit __ Hydro-Simulations __ WMAP Random Realization l WMAP best fit Prior: gas > 0 First direct measurement of ICM pressure profile 2 ' 50 for the simulated profiles 7 detection 14 August 1, 2006 Missing Thermal Energy of the Universe

Hydro-Simulations Total ICM gas fraction __ __ WMAP Random Realization l WMAP best fit 9 model independent measurement of SZ l X-ray and SZ observations are both missing ~30% of baryons l Simulations are also missing the same fraction in cold gas 15 August 1, 2006 Missing Thermal Energy of the Universe

32 ± 10% of Baryons are missing from the ICM! l Where are the rest of baryons? – – – 16 stars are < 10% Intracluster stars (how do they get there? ) warm gas: 105 -106 K (why doesn’t it cool? ) cold starless clouds thermal evaporation from the cluster (Loeb 06) August 1, 2006 Missing Thermal Energy of the Universe

Systematic Trends l l No significant dependence on TX Cool-core clusters seem to have – – 17 Simulations Larger gas fraction Flatter inner pressure profile ? ? August 1, 2006 Missing Thermal Energy of the Universe

Conclusions l l 18 A model-independent analysis of 3 year WMAP data with 193 massive clusters yields: The first model independent universal pressure profile, closely follows dark matter Prefers simulation results to null at » 7 30% of Intracluster medium is consistently missing in SZ and X-ray, as well as simulations, and is nowhere to be found! August 1, 2006 Missing Thermal Energy of the Universe

The Moral l l 19 In the run-up to high resolution SZ surveys, there is much more that can and should be learnt about ICM Higher Resolution CMB/SZ surveys (Planck, SZA, APEX, SPT, …) will be able to significantly lower their effective cluster detection mass threshold thru combination with wide-angle Xray cluster surveys (e. g. , DUO) X-ray and SZ surveys must be combined to provide reliable tests for models of Dark Energy or Cluster Physics Beware of the Alligator … August 1, 2006 Missing Thermal Energy of the Universe