Multiwavelength Analysis of CLASH Clusters

Transcription

1 The Galaxy Cluster MACSJ From Umetsu et al ' N E Multiwavelength Analysis of CLASH Clusters Seth Siegel

2 Collaboration Bolocam Team: Sunil Golwala, Jack Sayers, Nicole Czakon, Tom Downes, Patrick Koch, Kai-Yang Lin, Sandor Molnar, Leonidas Moustakas, Tony Mroczkowski, Elena Pierpaoli, Jennifer Shitanishi JACO Software: Andisheh Mahdavi CLASH Team: Marc Postman (PI), Megan Donahue, Julian Merten, Adi Zitrin, Keiichi Umetsu, Massimo Meneghetti 2

3 Postman et al Cluster Lensing And Supernova survey with Hubble 25 galaxy clusters 20 selected based on X-ray data alone X-ray temperatures TX > 5 kev massive 3.45 Surface brightness maps have well defined peaks, nearly concentric isophotes dynamically relaxed 16 filter HST strong/weak lensing data 24/25 have weak lensing data from Suprime-Cam on Subaru 25/25 have Chandra (Avg. Exposure = 63 ks) 15/25 have XMM 25/25 have Bolocam SZ at 140 GHz Median peak S/N = 12 Postman et al Taken from the Archive of Chandra Cluster Entropy Profiles (ACCEPT) database 1 resolution out to 6-7 3

4 Multiwavelength Analysis Combine HST Strong Lensing HST + Subaru Weak Lensing Chandra + XMM X-ray Bolocam SZ Fit a parametric model for the distribution of dark and baryonic matter in the cluster to the combined data set. What can be gained from a joint analysis of the CLASH cluster sample over a lensing-only analysis? (1) Probe elongation of cluster along the line of sight, constrain full triaxial shape and orientation. (2) Probe the dynamical state of the ICM, constrain the level of non-thermal pressure support. 4

5 Triaxial Shape Numerical simulations indicate that dark matter halos are triaxial Intermediate-Major and Minor-Intermediate axis ratios ~0.8 on average Lensing sensitive to projected mass distribution Z = dz Deprojecting to recover 3-D structure of the cluster is under constrained problem X-ray and SZ observables have different dependencies on projected properties of the ICM Z SZ: T CMB / P e dz where P e = n e k B T e X-ray: S X / Combined data set sensitive to elongation of the ICM along the LOS Making weak assumptions about cluster geometry (ICM and DM are coaligned), full 3-D shape and orientation can be constrained Meneghetti et al Z n 2 e T 1/2 e dz Measure the bias in the lensing-only derived mass profiles due to triaxial shape and orientation 5

6 Non-thermal Pressure Support At the cluster outskirts, this is sourced by incomplete thermalization resulting in bulk and turbulent flow of the accreted gas. Few observational measurements Expected that P nt P tot & 0.30 at cluster outskirts, based on hydrodynamical simulations SL + WL constrain total mass density. This constrains total pressure of the ICM through the generalized equation of hydrostatic equilibrium rp tot = gas r P tot = P th + P nt X-ray + SZ constrain thermal pressure. The difference yields a measurement of the non-thermal pressure support. Cluster masses inferred from X-ray biased low due to non-thermal pressure Cosmological constraints derived from SZ power spectrum measurements by SPT and ACT are limited by theoretical modeling uncertainties of the thermal state of the ICM 6

7 Joint Analysis of Cluster Observations (JACO) Using JACO software to perform analysis (Mahdavi et al. 2007) Provides self-consistent framework for forward model fitting of multiwavelength datasets XMM Chandra Bolocam SZ Written in C Weak lensing Strong lensing Velocity Dispersion Models dark, gaseous, and stellar mass profiles separately Uses MCMC to explore parameter space Well understood: used to examine X-ray - WL scaling relations in the Canadian Cluster Comparison Project (Mahdavi et al. 2013) Both spherical and triaxial versions now exist 7

8 Spherical Sample Defined subsample of 6 clusters to perform initial spherical analysis. Criteria: SZ image does not favor elliptical model (Czakon et al. 2014) X-ray centroid shift parameter w < r500c (Maughan et al. 2007) Seth Siegel SnowCluster - The Physics of Galaxy Clusters 8

9 Spherical Sample Defined subsample of 6 clusters to perform initial spherical analysis. Criteria: SZ image does not favor elliptical model (Czakon et al. 2013) X-ray centroid shift parameter w < r500c (Maughan et al. 2007) abell0383 abell0611 macsj macsj macsj macsj Postman et al Taken from the Archive of Chandra Cluster Entropy Profiles (ACCEPT) database 9

10 Cluster Model Total density modeled with NFW profile ρ tot (r) = ρ tot,0 (r/r s )(1+r/r s ) 2 ( ) ( Gas density modeled with modified beta model (Vikhlinin et al. 2006) ( ) α ( ) ) 2 (α 3β)/2 ( ( ) ) 4 ϵ/4 r r r ρ gas (r) =ρ gas,0 ( ρ gas,c (1+ r x 3β 2 r x r o ( r r c ) 2 ) 3βc /2 Nelson et al. (2014) model for non-thermal pressure support { (r) =1 A 1+exp P = P th + P nt P nt P [ ( ) γ ]} r/r200m B + f inner (r) Float A B = 0.84 γ = 1.63 Integrate generalized equation of hydrostatic equilibrium to obtain radial temperature profile P = ρ gas Φ = ( ) 1 d ρgas k B T + P nt = GM tot ρ gas dr µm p r 2 = k B T (r) = µm [ rc ] p GM tot ρ gas dr + P ρ gas r 2 c P nt r 10

11 JACO Fit Likelihood function L / exp Seth Siegel 2 /2 where χ2 = χ2x-ray + χ2sz + χ2sawlens SnowCluster - The Physics of Galaxy Clusters 11

12 JACO Fit Likelihood function L / exp 2 /2 where χ 2 = χ 2 + χ 2 + χ 2 X-ray SZ SaWLens Counts/s/keV Triaxial version: Add 2D XMM + Chandra Surface Brightness Photon Energy [kev] 12

13 JACO Fit Likelihood function L / exp 2 /2 where χ 2 = χ 2 + χ 2 + χ 2 X-ray SZ SaWLens Radius [Mpc] Subaru WL Convergence κ Triaxial version: 2D SaWLens Convergence Map HST SL Surface Mass Density HST WL Radius [arcmin] 13

14 Mass Estimates 14

15 Mass Estimates 15

16 Non-thermal Pressure 16

17 Non-thermal Pressure at r200m Preliminary Simulation Nelson et al

18 Entropy 18

19 Summary In principle, multiwavelength observations can be used to constrain: Triaxial shape Level of non-thermal pressure support Yield more accurate/precise mass estimates. We are using JACO to jointly fit: Chandra X-ray spectra Bolocam SZ image HST + Subaru convergence profile (strong & weak lensing) Spherical analysis of subset of 6 (best behaved) CLASH clusters find: Good agreement between datasets Low levels of non-thermal pressure support Triaxial analysis necessary for full CLASH sample. Add XMM + Chandra surface brightness to characterize gas density out to larger radii 19

20 Additional Slides

21 X-ray and SZ Pressure Comparison 21

22 Mass Estimates (with Non-thermal Pressure) 22

23 BOXSZ Cluster Sample 45 galaxy clusters observed with Bolocam at 140 GHz z = 0.15 Abell 2204 Abell 383 Abell 209 Abell 963 Abell 1423 Abell 2261 Abell 2219 Bolocam Abell 267 RX J Abell 1835 Abell 697 Abell 611 MS 2137 Abell S element bolometric array 58 FWHM MACS J MACS J MACS J Abell 370 MACS J ZWCL 0024 MACS J Data collected at the CSO in 14 observing runs between Fall 2006 and Spring 2012 MACS J MACS J MACS J MACS J MACS J MACS J MACS J Existing Chandra X-ray data MACS J MACS J MACS J MACS J MACS J MACS J MACS J Median redshift = 0.42 MACS J MACS J MS 2053 MACS J MACS J MACS J MACS J Median X-ray derived mass M500 = 9 x M MS 1054 CL J CL J Czakon et al arxiv: z = 0.89 Median S/N = 12 Radial size r = 6-7 arcmin S/N 23 Fig. D.5. Thumbnails showing the S/N per beam in the processed SZE images for all 45 BOXSZ clusters. The images are

24 Non-thermal Pressure Support Using high resolution hydrodynamical simulations, Nelson et al. (2014) found universal non-thermal pressure profile when radii are defined with respect to the mean matter density of the universe. Independent of redshift, mass Normalization dependent on mass accretion rate Empirical fitting formula 1 + exp P rand P total (r)=1- A apple - r/r200m A = 0.45 B = 0.84 γ = 1.63 B ± Nelson et al

25 Abell 0383 Nonthermal Thermal 25

26 Abell