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

2. SZ effect - 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 Diffraction is 18" at 2 mm 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 RXJ1347-1145 Most massive object (Pointecouteau et al. 2001) Obs

4. HUMBA Hundred Millikelvin Bolometer Array (Kreysa, Reichertz, Raccanelli) ● Array of 19 bolometers ● 3 He/ 4 He 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 150 arcsec RXC J1023.6+0411 beam map 18" FWHM ROSAT : A. Raccanelli L. Reichertz Nov. 2001  2.0 ± 0.5 mJy H o 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 (  vs (l, m)

7. 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 Bolometer Cameras Work in progress in France

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.  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. IRAM Long-Term Options >2008

11. Angular scale coverage Complementary between sensitivity and resolution l(l+1)C l /2pi sensitivity 180 deg l=1 5 arcmin l=2E3 20 arcsec l=3E4 0.1arcsec l=6E6 Planck/HFI 30m, Apex Cameras l² PdB++ l4l4 Alma l4l4 l² 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