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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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slide1

U. Chicago Caltech MSFC/U. Alabama Columbia

Interferometric Cluster Imaging with the Sunyaev-Zel’dovichArray

Marshall Joy NASA/MSFC

in this talk
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

sunyaev zel dovich array
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

slide4

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

slide5
Pointed cluster observations with SZA

68 Clusters observed (so far)

  • ~50 with X-ray, ~40 with weak lensing, ~50 with strong lensing
carma combined array for research in millimeter astronomy
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

sza carma

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

cluster science with the sza
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
slide12

SZ Imaging of high redshift clusters:

XMMXCS J2235-2557 at z=1.39

slide13

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

local cluster substructure survey locuss
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
local cluster substructure survey locuss1
Local Cluster Substructure Survey (LoCuSS)

68 Clusters observed with SZA (so far)

  • ~50 with X-ray, ~40 with weak lensing, ~50 with strong lensing
cluster mass proxy compton y parameter
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)

mass y scaling relation pre sza
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
sza measurements of y sz vs y x
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

integrated y vs strong lensing mass in cluster cores
Integrated Y vs. strong lensing mass in cluster cores

Marrone et al. 2009, ApJ, in press

MSL = 0.98 +/- 0.13 MHSE

slide23
More on SZ scaling relations in Graham Smith’s talk tomorrow:

Cluster mass measurements at large radii --

weak lensing mass vs. integrated Ysz measurements.