Observing the SZ Effect with the IRAM 30-meter

and the Plateau de Bure Interferometer

(on behalf of Francois-Xavier Desert)

SZ effect- High resolution measurements

- Complement to X-ray data (XMM-Newton,

- Chandra, Rosat) and the future PlanckDiabolo cryostatat the nasmyth focus

IRAM 30m Pico Veleta

Diffraction is18" at 2 mm

2x3 bolometers @0.1K

coaligned with 22" beam

1.2 & 2.1 mm

Benoît et al 2000 A&AS

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

HUMBAHUMBA Hundred Millikelvin Bolometer Array(Kreysa, Reichertz, Raccanelli)

98

1 m

m

ø 420 mm

N2

He

Dilution fridge insert

1K pot

Still

Mixing chamber

Bolometer cavity

Horn array

Filters

0.7 K

4.2 K

77 K

FET box

● 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)

First HUMBA SZE ObservationsFirst HUMBA SZE Observations

150 arcsecRXC J1023.6+0411beam map

18" FWHM

ROSAT:

A. RaccanelliL. ReichertzNov. 2001

2.0 ± 0.5 mJy

Ho mass (profile)

Temperature (profile)clumpiness(hydrostatic equilibrium?)

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)

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 CamerasWork in progress in France

“Dream Bolometer Camera”@ IRAM 30m

mm 1.2 2.1

FOV Arcmin² 5x5 5x5Npix 64x64 32x32

Pixel size arcsecond 5 10Diffraction arcsecond 11 18Detectivity mJy/s1/2 per psf 50 30

YSZ 1 hour per psf 5E-5

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

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

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

Angular scale coverageComplementary between sensitivity and resolution

l(l+1)Cl /2pi

sensitivity

180 deg l=1

5 arcminl=2E3

20 arcsecl=3E4

0.1arcsecl=6E6

Planck/HFI30m, ApexCameras

l²PdB++

l4

Alma

l4

l²

Angular scales

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