Acknowledgements CEA-Saclay / SAp Boulade Olivier, Doumayrou Eric, Horeau Benoit, Lepennec Yannick, Martignac Jerome, Okumura Koryo, Révéret Vincent,
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1 Recent Achievements in the Development of HERSCHEL/PACS Bolometer Arrays Nicolas BILLOT CEA - Saclay/DAPNIA/SAp UMR - Astrophysique Interaction Multi-echelle
2 Acknowledgements CEA-Saclay / SAp Boulade Olivier, Doumayrou Eric, Horeau Benoit, Lepennec Yannick, Martignac Jerome, Okumura Koryo, Révéret Vincent, Rodriguez Louis, Sauvage Marc CEA-Grenoble / LETI / LIR Agnèse Patrick, Cigna Jean-Charles, Pornin Jean-Louis, Simœns Francois IAP Vigroux Laurent
3 Overview What is Far-IR and Sub-millimeter Astronomy? The HERSCHEL Mission Bolometers and submm imagers PACS bolometers Some results from the lab Future
4 The cold Universe: a history of star formation What do we see in the sub-millimeter wavelength range? Warm dust 10-50K Star formation tracers Galaxy evolution Better longer λ Manytransition lines in submm Only 3 or 4 atmospheric windows!
5 HERSCHEL Mission 4th cornerstone of ESA's science programme Photometry and Spectroscopy in the µm range 4 years mission 2 nd Lagrangian point orbit Launch date 2007 (Ariane 5 at Kourou, French Guyana) Dimensions 7.5 x 4 x 4 m ISO-type superfluid Helium Cryostat (3500 liters) Giant 3.5 m telescope passively 70K (Silicon carbide, WFE < 6 µm, emissivity ~ 5%) 3 scientific instruments : HIFI, SPIRE and PACS Which technology for PACS photometer? Requirements: Photometry in µm range ( 10-5 ev!! ) Large format detector High mapping efficiency High sensitivity, photon noise limited Heterodyne? Photoconductors? BOLOMETERS
6 Bolometer principles An absorber convert incident power into heat High sensitivity = low heat capacity (=> low temperature) A thermometric sensor measures the temperature increase High sensitivity = strong dependence on T Heat is evacuated to a cold heat sink to reset the detector High thermal conductivity T0
7 So far in Submm Astronomy Submm imagers = bolometers UKT14 (1986) : 1 pixel SHARC I (1996) : linear monolithic array of 24 pixels SCUBA (1998) : pixels SHARC II (2002) : 12x32=384 pixels MAMBO 2 Absorption issues: Winston cones 2.44Fλ 2Fλ Nyquist sampling for pixel size of 0.5Fλ 2Fλ 16 pointings required to fully sample the PSF!
8 PACS Features to remember: 0.5Fλ pixels (750x750 µm): instantaneous PSF sampling λ/4 reflecting cavity for optimum absorption All-Silicon design (very high impedance doped Si thermometers) 10x16x16 = 2560 pixels (collective manufacturing of 16x16 matrices ) Cold multiplexed electronics ( CMOS 300mK, 16 to 1 ) Qualified for space λ/4
9 PACS
10 In the lab Specifications: Background flux: 2 pw/pixel Expected source fluxes: ~1% of background Sensitivity: 0.3 fw/pixel (5σ, 1h) Photon noise limited Qualified for Space? Vibration tests OK Irradiation tests OK γ Rays : cumulated dose 30 krad (equivalent 15 years in space) Protons (expected impacts/s/pixel) α particules (expected impacts/s/pixel) intensity (volts) time (s)
11 In the lab 0.25 Responsivity : V/W intensity (volts) intensity (volts) 0.25 Noise : white 3 Hz: 4 µv.hz -1/2 1/f noise knee frequency: 3 Hz time (s) time (s) NEP = Noise/Responsivity = W.Hz -1/2 Time constant = 3-5 Hz
12 Ground Adaptation Possible adaptation of CEA bolometers for Ground telescopes in the 350 and 450 µm atmospheric windows: KOSMA (Swiss Alpes) APEX (Atacama desert) Concordia (Antarctica)
13 Extras Blue channel: µm Red channel: µm 2048 active pixels 256 blind pixels diffraction 70µm pixel size 750 µm 3.5 Photos 512 active pixels 64 blind pixels diffraction 170µm- 24 pixel FOV-3.2 pixel FOV-6.5
14 PACS
15 PACS PACS Instrument Photometer Focal Plane Blue Channel Blue Array 2048 pixels
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