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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 - PowerPoint PPT Presentation
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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
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