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Sunyaev-Zel'dovich Surveys: A Primer on Upcoming Observations

Learn about upcoming Sunyaev-Zel'dovich (SZ) effect surveys, observables, mass limits, and challenges. Explore how different telescopes will revolutionize cosmological measurements. Get insights into galaxy cluster detection and cosmological parameters. Find out about new science opportunities with SZ imaging and peculiar velocities. Stay informed on the latest developments in SZ surveys.

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Sunyaev-Zel'dovich Surveys: A Primer on Upcoming Observations

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  1. A Primer on SZ Surveys Gil Holder Institute for Advanced Study

  2. Outline • Sunyaev-Zel’dovich effect • Upcoming surveys • What’s next?

  3. Optical Image of Cl 0016+16(Clowe et al. 2000) ~ 7’ ~ 2 h-1 Mpc

  4. Hot Gas in Cl 0016+16 (Reese) kT ~ 7.5 keV

  5. Sunyaev-Zel’dovich Effect I Hot electrons CMB+ CMB  Optical depth: τ ~ 0.01 Fractional energy gain per scatter: ~ 0.01

  6. SZ Observables I Along a line of sight: DEPENDS ONLY ON CLUSTER PROPERTIES !!!! Independent of redshift Temperature weighted electron column density Unique spectral signature

  7. Non-Thermal Spectrum Abell 2163 Data from 3 experiments

  8. SZ Observables II Integrated effect from cluster: • proportional to total thermal energy of electrons • Temperature weighted electron inventory • angular diameter distance, not luminosity distance

  9. SZ Observables III In reasonable units ( i.e., 1/h): Assume a virial relation: uncertainties come in mass limit as ^(0.6)

  10. SZE Regularity Metzler ; astro-ph/9812295 dTo <dT> Average SZ flux vs Mass – 10% scatter Central decrement vs Mass – 40% scatter

  11. Searching for Galaxy Clusters Small area; very deep - AMI, AMIBA, BOLOCAM, SZA Large area; relatively shallow - ACBAR, PLANCK Large area; very deep - ACT, SPT

  12. Mass Limits Fluxes at 30 GHz PLANCK SZA

  13. Foregrounds • CMB – need good angular resolution and/or good spectral resolution; problem at all SZ frequencies • Radio point sources – need good angular resolution for frequencies <90 GHz • Dusty point sources – need good angular resolution and/or spectral resolution at frequencies >200 GHz • Radio halos and ghosts – could be a problem at frequencies < 15 GHz

  14. SZA • Survey 10 square degrees to a few uK at resolution of 2-3 arcminutes at 30 GHz • Expected mass limit ~ • Follow up catalog at 90 GHz for high resolution (<20”) • 100 – 500 clusters expected

  15. Example: RXJ1347-1145 Reese X-ray (colours) SZ only SZ (contours)

  16. 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

  17. Cosmology With the SZA Holder, Haiman & Mohr 2001

  18. Dark Energy With the SZA • 12 square degrees • assume NO systematic errors • assume redshifts measured to z=2

  19. PLANCK • Survey the full sky to a few uK at resolution of 5-10 arcminutes at many frequencies • Expected mass limit ~ • Cluster detections will be unresolved – point sources with SZE-like spectra • 1000 – 50000 clusters expected

  20. Cosmology With Planck Black: all z Red: z<0.5 only Holder, Haiman & Mohr 2001

  21. SPT/ACT/??? • Survey ~1000 square degrees to a few uK at resolution of 1-2 arcminutes at several frequencies • Expected mass limit ~ • Most powerful for cosmology • 5000 – 200000 clusters expected

  22. Cosmology with the SPT Holder, Haiman & Mohr 2001

  23. dN/dz for SPT

  24. Dark Energy With the SPT Also sensitive to time dependent equation of state (Weller, Battye & Kneissl 2001)

  25. Possible Plan of Action • Use AMI/AMIBA/BOLOCAM/SZA to define a significant SZE-selected sample • Follow up at many wavelengths: optical, X-ray, radio, cm, mm (including SZA!) • Do a very large, deep survey for precise measurements of cosmological parameters

  26. On the Horizon uK imaging between 30-400 GHz with arcminute resolution -- SPT, ACT, dedicated interferometers, ALMA, etc. New science opportunities & challenges -- peculiar velocities, -- spectral SZ -- CMB lensing

  27. Peculiar Velocities (Kinetic SZ) • Pure redshift, blueshift => thermal spectrum Arcminutes scales => CMB ~ 1 uK -- CMB noise contribution = 10 km/s (0.01/τ) Other contamination: 50 km/s ? (Fischer & Lange 1993)

  28. Relativistic Corrections

  29. Lensing of the CMB Typical CMB gradient -- 15 uK/arcmin Typical deflection angle -- ~ 0.1-1 arcmin (Seljak and Zaldarriaga )

  30. Summary • New cluster surveys coming soon • Detailed follow-up will be required of some sample of SZE-selected clusters • Ambitious survey machines in proposal stages could be extremely powerful

  31. Gallery of SZ Images Z=0.83 Z=0.14

  32. Green: shift in matter density by 10% Holder & Carlstrom 2001

  33. Counting Galaxy Clusters Mass limit Mass function Volume element (Jenkins, Press-Schechter)

  34. Self-Similar Evolution Holder & Carlstrom 2001

  35. Effects of Gas Evolution Holder & Carlstrom 2001

  36. Angular Power Spectrum of SZ Sources Holder & Carlstrom 2001

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