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U. Chicago Caltech MSFC/U. Alabama Columbia

U. Chicago Caltech MSFC/U. Alabama Columbia. Interferometric Cluster Imaging with the Sunyaev-Zel’dovich Array Marshall Joy NASA/MSFC. In this talk:. Overview of the Sunyaev-Zeldovich Array - Design and construction - Observing - Array evolution

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U. Chicago Caltech MSFC/U. Alabama Columbia

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  1. U. Chicago Caltech MSFC/U. Alabama Columbia Interferometric Cluster Imaging with the Sunyaev-Zel’dovichArray Marshall Joy NASA/MSFC

  2. In this talk: Overview of the Sunyaev-Zeldovich Array - Design and construction - Observing - Array evolution Scientific focus of the SZA: detailed studies of galaxy clusters (individual objects & cluster samples) • High redshift clusters • Cluster mass proxies: Ysz and Yx • SZ scaling relations, part 1: strong lensing mass vs. integrated Y • In Graham Smith’s talk tomorrow: SZ scaling relations, part 2: weak lensing mass vs. integrated Y

  3. Sunyaev-Zel'dovich Array 8 elements, 3.5m diameter Designed for sensitivity to cluster virial radius Large bandwidth for high sensitivity: 8 GHz (25% at 30 GHz) 6 central antennas for SZ sensitivity, 2 outriggers for foreground source removal Two frequencies 30 GHz: primary observations 90 GHz: higher resolution follow up, contamination checks Science operations began Nov 2005 1.5yrs: 6sq deg survey, CMB anisotropy Pointed cluster observations since Sep 2007

  4. The SZA Collaboration University of Chicago John Carlstrom Tom Culverhouse Erik Leitch Dan Marrone Kelsey Morgan Clem Pryke Megan Roscioli Matthew Sharp – 2008 PhD, CMB Anisotropy Alan Zablocki NASA MSFC Marshall Joy University of Alabama, Huntsville Max Bonamente Nicole Hasler Esra Bulbul Nazirah Jetha Owens Valley Radio Observatory David Hawkins James Lamb David Woody Columbia University Amber Miller Tony Mroczkowski – 2008 PhD, Cluster Modeling Stephen Muchovej – 2008 PhD, Blank Field Survey Funding: NSF, KICP, McDonnell Foundation, UChicago

  5. Pointed cluster observations with SZA 68 Clusters observed (so far) • ~50 with X-ray, ~40 with weak lensing, ~50 with strong lensing

  6. Array evolution

  7. BIMA

  8. OVRO

  9. CARMA: Combined Array for Research in Millimeter Astronomy CARMA = OVRO + BIMA + SZA (six 10.4m + nine 6.1m + eight 3.5m telescopes) Merger timeline: Proposals to SZA through CARMA TAC – starting August 2009 September 2009: 10+3.5m (14-element) SZ interferometry (10-45” scales) Fully integrated heterogeneous array – 2010-2011

  10. Simulated Cluster z=0.25, M=1.71014 MSun SZA 30 GHz SZA 30 + 90 GHz CARMA+SZA 30 GHz 3’ Nagai et al. (2007) SZA+CARMA What can we do with the combined array? Sensitivity, angular resolution, dynamic range all significantly improved Detailed cluster imaging becomes possible Simulated observation: Erik Leitch

  11. Cluster Science with the SZA detailed studies of galaxy clusters (individual objects & cluster samples) • High redshift clusters • Cluster mass proxies: Ysz vs. Yx • SZ scaling relations: gravitational lensing mass vs. integrated Y

  12. SZ Imaging of high redshift clusters: XMMXCS J2235-2557 at z=1.39

  13. XMMXCS J2235-2557 (z=1.39) SZ: Y DA2 = 1.92 +/- 0.4 x 10-5 Mpc2 X-ray: Mtotal = 1.9 +/- 0.5 x 1014 Msun

  14. Local Cluster Substructure Survey (LoCuSS) PI: Graham Smith (Birmingham) Morphologically unbiased, X-ray selected cluster sample, z=0.15-0.3 • Strong lensing – HST/ACS+WFPC2, Keck • Weak lensing – Subaru • X-ray – XMM/Chandra • SZ – SZA/CARMA • UV – star formation – GALEX • Near-infrared – stellar mass maps – Palomar+NOAO • Spitzer/MIPS – AGN/SF 24um • Far-infrared – Star formation – Herschel Key Project Scaling relations, calibration of SZ systematic effects: • Examine scatter in Mass – Y relationship from cluster core to virial radius • Determine hydrostatic mass bias • Effects of morphology/merging on the SZ signal

  15. Local Cluster Substructure Survey (LoCuSS) 68 Clusters observed with SZA (so far) • ~50 with X-ray, ~40 with weak lensing, ~50 with strong lensing

  16. Cluster mass proxy: Compton Y parameter Kravtsov et al. (2006) introduced an X-ray analogue for SZ signal Constructed from X-ray observables (M, T) Pressure-like, should behave like SZ Simulations show tight M-YX correlation Simulated M vs. YX – Kravtsov et al. (2006)

  17. Mass – Y Scaling Relation (pre-SZA) Key ingredient for SZ cluster survey cosmology • Little observational constraint to date • M-Y scatter unconstrained Bonamente et al. (2008): • 38 clusters • Y from SZ(+X-ray) versus X-ray hydrostatic Mass at r2500 • Measurement errors too large to constrain scatter

  18. SZA measurements of Ysz vs. Yx - X-ray analysis of 35 LoCuSS XMM clusters published (Zhang et al. 2008) - All of these clusters (north of δ=-14°) observed with SZA - Compare YSZ and YX

  19. Intrinsic Scatter 14% 9% 9%

  20. Cool-Core vs. Non-Cool Core

  21. Relaxed vs. Unrelaxed

  22. Integrated Y vs. strong lensing mass in cluster cores Marrone et al. 2009, ApJ, in press MSL = 0.98 +/- 0.13 MHSE

  23. More on SZ scaling relations in Graham Smith’s talk tomorrow: Cluster mass measurements at large radii -- weak lensing mass vs. integrated Ysz measurements.

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