A Primer on SZ Surveys

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A Primer on SZ Surveys. Gil Holder. Institute for Advanced Study. Outline. Sunyaev-Zeldovich effect Upcoming surveys Whats next?. Optical Image of Cl 0016+16 (Clowe et al. 2000). ~ 7. ~ 2 h -1 Mpc. Hot Gas in Cl 0016+16. (Reese). kT ~ 7.5 keV. Sunyaev-Zeldovich Effect. I. - PowerPoint PPT Presentation


<ul><li><p>A Primer on SZ SurveysGil HolderInstitute for Advanced Study</p></li><li><p>OutlineSunyaev-Zeldovich effectUpcoming surveysWhats next?</p></li><li><p>Optical Image of Cl 0016+16(Clowe et al. 2000)~ 7~ 2 h-1 Mpc</p></li><li><p>kT ~ 7.5 keVHot Gas in Cl 0016+16(Reese)</p></li><li><p>Sunyaev-Zeldovich EffectCMBHot electronsCMB+IOptical depth: ~ 0.01Fractional energy gain per scatter: ~ 0.01</p></li><li><p>SZ Observables IAlong a line of sight:DEPENDS ONLY ON CLUSTER PROPERTIES !!!!Independent of redshiftTemperature weighted electron column densityUnique spectral signature</p></li><li><p>Non-Thermal SpectrumAbell 2163</p><p>Data from 3 experiments</p></li><li><p>SZ Observables IIIntegrated effect from cluster: proportional to total thermal energy of electrons Temperature weighted electron inventory angular diameter distance, not luminosity distance</p></li><li><p>SZ Observables IIIIn reasonable units ( i.e., 1/h):Assume a virial relation:uncertainties come in mass limit as ^(0.6)</p></li><li><p>SZE RegularityCentral decrement vs Mass 40% scatterAverage SZ flux vs Mass 10% scatterMetzler ; astro-ph/9812295dTo</p></li><li><p>Searching for Galaxy Clusters Small area; very deep - AMI, AMIBA, BOLOCAM, SZA Large area; relatively shallow - ACBAR, PLANCK Large area; very deep - ACT, SPT</p></li><li><p>Mass LimitsFluxes at 30 GHzPLANCKSZA</p></li><li><p>ForegroundsCMB need good angular resolution and/or good spectral resolution; problem at all SZ frequenciesRadio point sources need good angular resolution for frequencies 200 GHzRadio halos and ghosts could be a problem at frequencies &lt; 15 GHz</p></li><li>SZASurvey 10 square degrees to a few uK at resolution of 2-3 arcminutes at 30 GHzExpected mass limit ~Follow up catalog at 90 GHz for high resolution (</li><li><p>Example: RXJ1347-1145X-ray (colours)SZ (contours)SZ onlyReese</p></li><li><p>CMB contamination?? clusters are clearly at a different spatial scale close amplitudes means beam dilution catches up fast !!!Roughly 1 deg x 1deg labels are uK</p></li><li><p>Cosmology With the SZAHolder, Haiman &amp; Mohr 2001</p></li><li><p>Dark Energy With the SZA 12 square degrees assume NO systematic errors assume redshifts measured to z=2</p></li><li><p>PLANCKSurvey the full sky to a few uK at resolution of 5-10 arcminutes at many frequenciesExpected mass limit ~Cluster detections will be unresolved point sources with SZE-like spectra1000 50000 clusters expected</p></li><li><p>Cosmology With PlanckBlack: all z</p><p>Red: z</p></li><li><p>SPT/ACT/???Survey ~1000 square degrees to a few uK at resolution of 1-2 arcminutes at several frequenciesExpected mass limit ~Most powerful for cosmology5000 200000 clusters expected</p></li><li><p>Cosmology with the SPTHolder, Haiman &amp; Mohr 2001</p></li><li><p>dN/dz for SPT</p></li><li><p>Dark Energy With the SPT Also sensitive to time dependent equation of state(Weller, Battye &amp; Kneissl 2001)</p></li><li><p>Possible Plan of ActionUse AMI/AMIBA/BOLOCAM/SZA to define a significant SZE-selected sampleFollow up at many wavelengths: optical, X-ray, radio, cm, mm (including SZA!)Do a very large, deep survey for precise measurements of cosmological parameters</p></li><li><p>On the HorizonuK imaging between 30-400 GHz with arcminute resolution -- SPT, ACT, dedicated interferometers, ALMA, etc.New science opportunities &amp; challenges -- peculiar velocities, -- spectral SZ -- CMB lensing</p></li><li><p>Peculiar Velocities (Kinetic SZ)Pure redshift, blueshift =&gt; thermal spectrumArcminutes scales =&gt; CMB ~ 1 uK -- CMB noise contribution = 10 km/s (0.01/)Other contamination: 50 km/s ? (Fischer &amp; Lange 1993)</p></li><li><p>Relativistic Corrections</p></li><li><p>Lensing of the CMBTypical CMB gradient -- 15 uK/arcminTypical deflection angle -- ~ 0.1-1 arcmin(Seljak and Zaldarriaga )</p></li><li><p>SummaryNew cluster surveys coming soonDetailed follow-up will be required of some sample of SZE-selected clustersAmbitious survey machines in proposal stages could be extremely powerful</p></li><li><p>Gallery of SZ ImagesZ=0.83Z=0.14</p></li><li><p>Holder &amp; Carlstrom 2001Green: shift in matter density by 10%</p></li><li><p>Counting Galaxy ClustersMass functionVolume element(Jenkins, Press-Schechter)Mass limit</p></li><li><p>Self-Similar EvolutionHolder &amp; Carlstrom 2001</p></li><li><p>Effects of Gas EvolutionHolder &amp; Carlstrom 2001</p></li><li><p>Angular Power Spectrum of SZ SourcesHolder &amp; Carlstrom 2001</p></li></ul>