Astro-H/HSC/SZE. Nicole Czakon (ASIAA) Hiroshima, 08/27/2014

Transcription

1 Astro-H/HSC/SZE Nicole Czakon (ASIAA) Hiroshima, 08/27/2014

2 observatory_freq.html The Sunyaev-Zel dovich Effect A lot like X-Ray! Different dependence on electron density: More sensitive to outer regions Surface brightness independent of redshift. X-Ray nn 22 ee TT ee / 11 + zz 44 vs. SZE nn ee TT ee 1-particle 2-particle YY cyl = yy dωdll dω = 2 R 2500 YY sph = yy dv 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

3 Surface brightness independent of redshift allows surveys with flat mass limit out to large redshifts. X-Ray nn ee 2 TT ee / 1 + zz 4 vs. SZE nn ee TT ee erosita > 1000 z > 1.

4 Pointed vs. Survey SZE Instrumentation Bolocam, BICEP, BLAST -> Planck (Coma/Virgo) APEX-SZ -> SPT Access to Northern Hemisphere Clusters. Relatively Easy to Get Observing Time. Ability to get deep, resolved observations. Radio AMI, CARMA(?), AMiBA New Instrumentation: NIKA, MUSIC (Yet to be fully vetted..) Future Instrumentation: MUSTANG 1.5 &2, CCAT,.collaborative opportunities with SPT and ACT. Polar -> Bicep 3 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

5 BOXSZ: Bolocam XSZ ee CSO BOLOCAM CMB: 30 GHz 10 meter telescope Ø maps 1 PSF 140 GHz (& 268 GHz) 45 clusters, zz = 0.4 kk BB TT > 5 kkkkkk Decade in mass (Sayers, et al, 2008) Bolocam Blooper: Pursuing the angular power spectrum CMB: 150 GHz 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

6 BOXSZ: Bolocam XSZ ee CSO BOLOCAM 10 meter telescope Ø maps 1 PSF 140 GHz (& 268 GHz) 45 clusters, zz = 0.4 kk BB TT > 5 kkkkkk Decade in mass (Czakon, 2014, arxiv: in Review) 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

7 BOLOCAM SZE SCALING RELATIONS (Czakon, 2014, arxiv: in review) 1.06 ± SZE self-similar slope X-RAY Conclusion: This is made more complicated by our uncertainty in the X-ray Determined Masses. 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

8 BOLOCAM SZE SCALING RELATIONS Consistent with OVRO/BIMA 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

9 SZE/Astro-H: X-Ray Standards XMM vs. Chandra M gas agree! (Donahue, 2014, arxiv: , accepted) 8/27/2014 N. Czakon: Cross Strait Astrophysics 9

10 SZE/Astro-H: X-Ray Standards XMM vs. Chandra: T x don t From IM Stewart s website: (Donahue, 2014, arxiv: , accepted) Likely culprit? XMM PSF. 8/27/2014 N. Czakon: Cross Strait Astrophysics 10

11 If the non-self-similar scaling holds. Then the parameter space explodes.. I m looking forward to the following capabilities of Astro-H: 1. Non-thermal pressure characterization out to large radii. (well, probably done with existing X-ray observatories) a. Needed for low-resolution SZE data b. Needed to characterize CMB anisotropy at smaller angular scales 2. Characterization of hydrostatic mass bias. 3. Mergers, Filaments, peculiar velocity, bulk motion, and turbulence characterization. 4. In combination with SZE/lensing, 3D halo characterization. 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

12 SZE/X-Ray: Standards Stacked Pressure Profiles Useful for low resolution SZE surveys that are highly model-dependent. Can be done with X-rays, SZE, and simulations. Empirical need to estimate the SZE out to the virial radius.. X-Ray Observations Hydrodynamic N-Body Simulations Arnaud, et al, /27/2014 N. Czakon: Cross Strait Astrophysics 12

13 Sayers, Czakon, et al 2012 SZE/X-Ray: Standards Bolocam Pressure Profiles 5 free parameters -> use 4 parameters Normalization Radial Scale Inner Slope Transition Slope Full Data Set Disturbed Data Set Cool-Core Data Set 8/27/2014 N. Czakon: Cross Strait Astrophysics 13

14 SZE/Astro-H: Merging Clusters Astro-H should have the energy resolution to parametrically constrain the velocities of sub-clusters. Nagai, 2013 arxiv: v2 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

15 MACSJ Resolved KSZ Has the largest known Einstein radius at 55. Triple merger system, 4 distinct sub-clusters. (Ma 2008/2009) spectroscopically measure subcluster B is moving at a velocity of more than 3000 km/s along the line of sight. Ma, 2009, Galaxies Sayers,,Czakon, et al ApJ, /27/2014 N. Czakon: Bolocam/Optical/IR Symbiosis 15

16 Bolocam MACSJ Resolved KSZ Multiwavelength data justify the inclusion of an additional parameter, allowing the sub-clusters to move relative to each other along the line-of-sight Use the X-ray data as a pressure prior. Mroczkowski,,Czakon, et al ApJ, /27/2014 N. Czakon: Bolocam/Optical/IR Symbiosis 16

17 Bolocam MACSJ Resolved KSZ Multiwavelength data justify the inclusion of an additional parameter, allowing the sub-clusters to move relative to each other along the line-of-sight B C Sayers,,Czakon, et al ApJ, /27/2014 N. Czakon: Bolocam/Optical/IR Symbiosis 17

18 Sub-cluster B, enhancement at 140 GHz. Sub-cluster B, reduction at 268 GHz. Sub-cluster C has opposite response. C B Red curves: estimated thermal SZ contribution. Blue curves: best fit including kinetic SZ component. vv ZZ = km/s 4.2σσ away from 0 vv ZZ = km/s 2.9σσ away from 0 Sayers, ApJ, /27/2014 N. Czakon: Bolocam/Optical/IR Symbiosis 18 Sayers,,Czakon, et al ApJ, 2013

19 Herschel-SPIRE Point Sources Account for DSFG contamination using Herschel-SPIRE 250, 350, and 500 μμm. Negligible for 140 GHz 10-20% reduction the 268 GHz surface brightness uncertainties % reduction in the derived uncertainties on vv ZZ. Best-fit 268 GHz surface brightness values change by 10%. Comparable effect with 140 GHz. Blue Contours 268 GHz S/N 1 (+4) - 1 diameter aperture + - Bolocam PCA detection + - Likely SPIRE counterparts + - SPIRE detections S/N > 2 Sayers,,Czakon, et al ApJ, /27/2014 N. Czakon: Bolocam/Optical/IR Symbiosis 19

20 SZE/Astro-H:Low-Z/ High-Z Cosmological Tension MacCrann, et al, 2014, arxiv: v 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

21 SPT Power Spectrum The level of the tsz signal strongly depends on the model used to characterize the amount of nonthermal pressure support. Shaw, 2010, Apj 725: /27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

22 SPT Power Spectrum The level of the tsz signal strongly depends on the model used to characterize the amount of nonthermal pressure support. George, et al, 2014, arxiv: v1 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima

23 SZE/Astro-H: 3D Surface brightness does not dim with redshift Ysz n e : Sensitive to more mass and less-sensitive to clump biases in the outskirts. Provides another independent measure to break degeneracy. χχ = / Solid Line: HSE Prediction Data: Flattened entropy profile -> Non-thermal pressure support 18 +/- 5 deg 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima LOS Astro-H identification of filamentary structure also important 0.6: Minor/Major axis ratio

24 Conclusions I m looking forward to the scientific opportunities that Astro-H will provide! Individual pointed cluster studies are key to understanding the level of non-thermal pressure support, turbulence, impact of mergers, filamentary structure and 3-D morphology. Astro-H will allow us to resolve many of the systematics that are currently limiting the impact SZE cluster cosmology. 8/27/2014 Czakon, Atsro-H/HSC/SZE Hiroshima