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SZ effect

Observing the SZ Effect with the IRAM 30-meter and the Plateau de Bure Interferometer (on behalf of Francois-Xavier Desert). SZ effect. Diffraction is 18" at 2 mm. - High resolution measurements - Complement to X-ray data (XMM-Newton, Chandra, Rosat) and the future Planck. Diabolo cryostat

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SZ effect

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  1. Observing the SZ Effect with the IRAM 30-meterand the Plateau de Bure Interferometer(on behalf of Francois-Xavier Desert)

  2. SZ effect Diffraction is 18" at 2 mm - High resolution measurements - Complement to X-ray data (XMM-Newton, • Chandra, Rosat) and the future Planck Diabolo cryostat at the nasmyth focus IRAM 30m Pico Veleta 2x3 bolometers @0.1K coaligned with 22" beam 1.2 & 2.1 mm Benoît et al 2000 A&AS

  3. Colours = Diabolo 2.1mm (map obtained by scanning the 3 pixels across the field, @30m in15hours) Contours= X-ray (Rosat) (southern extension has since been confirmed by Chandra) Model Obs RXJ1347-1145 Most massive object (Pointecouteau et al. 2001)

  4. HUMBA Hundred Millikelvin Bolometer Array (Kreysa, Reichertz, Raccanelli) • Array of 19 bolometers • 3He/ 4He dilution refrigerator with a base temperature of 30 mK • Bandpass definition by 4 stages of filters (300K, 77K, 4.2K, 0.7K)

  5. First HUMBA SZE Observations beam map RXC J1023.6+0411 18" FWHM 150 arcsec ROSAT: A. Raccanelli L. Reichertz Nov. 2001 2.0 ± 0.5 mJy Ho mass (profile) Temperature (profile) clumpiness (hydrostatic equilibrium?)

  6. Challenges for new mm bolometer cameras • Filled vs. Horny arrays • Sky noise & Sky modulation techniques • Mapping speed and confusion noise • Multiplexing & optical quality • Connection between large scale surveys (WMap Spitzer Planck Herschel) and interferometers (Ami, Amiba, Alma): • filling sky vs. angular scale plane ( q, j ) vs (l, m)

  7. Bolometer CamerasWork in progress in France DCMB developments : A consortium of French Laboratories (CRTBT, LPSC, CSNSM, IAS, APC...) lead by A. Benoit Based on CEA/LETI cameras @ submm (32x32 used PACS Goal: High impedance and/or TES Working at 2 and 1 mm 1000 pixel camera, with time multiplexing (Hemt) and antenna coupling bolometer pixels. To be tested and operational in 2006-2007; ready for Planck

  8. “Dream Bolometer Camera”@ IRAM 30m Expect to detect one high redshift galaxy per hour of a deep survey (1 mJy 5 sigma @ 1.2 mm) Map SZ effect in one Planck cluster every few hours

  9. The Next Generation of Receivers at the PdBI(2005-2006) • New generation receivers (more compact, lower receiver • noise, closed cycle system) • Frequency coverage: 80-117, 125-180, 200-260 & 260-349 GHz • SSB tuning at all frequencies • Two polarizations • 4 GHz instantaneous bandwidth • One frequency setting at the time • Improved Sensitivity: ~2 for Spectroscopy and ~5 in Continuum as compared to the current system • Improved Frequency Coverage & Imaging • IF processing and transport (optical fibers) • Improvement on the Antenna Surface • Extension of the baselines: NS (368 m) & EW (800 m) •  HPBW of 0.3 arcsec at 230 GHz

  10. IRAM Long-Term Options >2008 PICO VELETA Large bolometer arrays (>1000/2000 pixels) / photometric sensit. Large heterodyne arrays Increase the instantaneous bandwidth (16 GHz per polar) Key role to play in combination with PdBI PLATEAU DE BURE INTERFEROMETER Dual-polarization Focal Plane Arrays (9 or 16 pixels) at 3 or 2 mm Increase the instantaneous bandwidth (to 8 or 16 GHz) More sensitive single-pixel receivers (factor of 1.4) Further extension of the EW baseline to 1.5 km. Additional antenna. Other frequency bands: 67-84 GHz, 180-210 GHz  Possible Cooperation with CARMA: ‘Software Merging’ would result in a sensitivity gain of ~1.4 (as compared to 1.8 for ‘Hard Merging’) for 2 Pol Rx.

  11. Angular scale coverageComplementary between sensitivity and resolution l(l+1)Cl /2pi sensitivity l4 l² PdB++ l² 30m, Apex Cameras Planck/HFI l4 Alma 180 deg l=1 5 arcmin l=2E3 0.1arcsec l=6E6 20 arcsec l=3E4 Angular scales

  12. Summary We gained a lot of instrumental and observational experiences with few SZ detections on a highly requested telescope (IRAM 30m) The way forward: investigate the ecological niche of intermediate angular scale High-angular resolution and large field coverage around the 1-2mm atmospheric windows SZ and secondary anisotropies High redshift galaxy surveys

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