Low noise millimeter wave receivers for Cosmic Microwave Background radiometers
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1 Low noise millimeter wave receivers for Cosmic Microwave Background radiometers Eduardo Artal, Beatriz Aja, Luisa de la Fuente, Juan Luis Cano, Enrique Villa, Jaime Cagigas (1) Enrique Martínez-González, Francisco Casas, David Ortiz (2) (1) Departamento de Ingeniería de Comunicaciones, Universidad de Cantabria. Santander. (2) Instituto de Física de Cantabria. Santander. Jornadas de Instrumentación Espacial Astro Madrid June
2 Summary Introduction Cosmic Microwave Background. Spatial missions NASA missions European Space Agency and Planck mission Planck satellite receivers Microwave polarimeters in El Teide Polar modulators, orthomode transducers Low noise receivers 2
3 Big Bang and Cosmic Microwave Background Time line of the Universe First stars 200 millions years CMB last interaction 380,000 years Inflation At present 13,700 millions years (42)..001 seconds 3
4 Cosmic Microwave Background The earliest image of the Universe (thousands of millions of years) Cosmic Microwave Image obtained by COBE satellite (NASA) (Celestial sphere deployed) Today: Cosmic Microwave Background (CMB) radiation temperature ºC CMB: the relic radiation from the Big Bang, the earliest print of the origin of the Universe (a lot of information about the early state) 4
5 Discovery of Cosmic Microwave Background 1964 Isotropic radio noise from the sky The Horn Antenna, at Bell Telephone Laboratories in Holmdel, New Jersey (constructed in 1959) 5
6 NASA missions: COBE satellite Satellite launched by NASA in 1989 to test CMB radiation and CMB Far-InfraRed spectrum. First evidence of CMB anisotropies (1 part in 100,000) 6
7 COBE satellite Artist s view of COBE satellite in orbit Instruments DMR= Differential Microwave Radiometer FIRAS = Far-InfraRed Absolute Spectrophotometer DIRBE = Diffuse InfraRed Background Experiment 7
8 NASA missions: WMAP (2001) WMAP (Wilkinson Microwave Anisotropy Probe) WMAP (Wilkinson Microwave Anisotropy Probe) better sensitivity and resolution than COBE a complete map of the sky now it is still providing science data 8
9 NASA missions: WMAP (2001) Temperature fluctuations map (CMB) after 5 years tests with WMAP satellite (variations of degrees) 9
10 ESA Planck mission Telescope of ESA Planck mission: dedicated to study the microwave background radiation Planck satellite will give answers about the origin and evolution of the universe by mapping the sky temperature: Cosmic background anisotropies 10
11 Missions comparison Cosmic Microwave Background anisotropies CMB anisotropies simulation at the Planck mission expected level PLANCK versus WMAP: Sensitivity 10x Frequency coverage 10x Angular resolution 2x 11
12 Planck and Herschel missions Launched together on Ariane V on 14-May-2009 Separated before reaching their orbit (Lagrangian 2 point, Lissajous orbit) Herschel Planck 12
13 Planck payload Planck mission instruments: HFI - High Frequency Instrument bolometer receivers GHz (6 bands) cooled to 0.1 K LFI - Low Frequency Instrument radiometric receivers at 30, 44 and 70 GHz cooled to 20 K with a reference load cooled to 4K 13
14 Planck receivers (LFI+HFI) 14
15 Planck-LFI radiometers 4 K load reference Feed-horn Radiometer Feed-horn 20K WG 300K Channel 4 Channel 3 OMT FEM BEM to DAE 20K WG 300K Channel 2 Channel 1 Radiometer 4 K load reference Feed-horn LNA Back End Module: BEM LNA BPF DET DC Amp LNA LNA BPF DET DC Amp 15
16 One branch of the 30 GHz BEM EBB L 50 mm LNA (MMIC) Detector output Filter Detector DC amplifier 16
17 One branch of the 44 GHz BEM EBB LNA (MMIC) Attenuator Filter Detector Detector output DC amplifier 17
18 MMIC amplifiers (LNA) at 44 GHz Two LNA (Low Noise Amplifier): same topology PHEMT OMMIC ED02AH Gate Width : 90 m (6x15 m) Gate Length : 0.18 m LNA (HEMT-Depletion) LNA (HEMT-Enhancement) Size: 3x1 mm 2 18
19 30 GHz BEM. Qualification Model (QM) RF channels 19
20 30 GHz BEM. Flight Model (FM) Size: 60 x 65 x 39 mm 3 DC amplifiers 20
21 44 GHz BEM. Flight Model (FM) RF channels 21
22 Low frequency instrument (LFI) integration 3 Back End Modules at 44 GHz 2 Back End Modules at 30 GHz 22
23 Planck satellite: first results 17 September 2009, (News from ESA): Preliminary results from ESA s Planck mission to study the early Universe indicate that the data quality is excellent 23
24 QUIJOTE CMB experiment overview Q-U-I JOint TEnerife (Stokes parameters Q, U and I) Cosmic Microwave Background (CMB) polarization receivers To obtain five polarization maps in the frequency range GHz Angular resolution: ~1 degree
25 QUIJOTE experiment consortium Instituto de Astrofísica de Canarias (IAC), Tenerife (Spain): Coordinator Instituto de Física de Cantabria (IFCA), Santander (Spain) Universidad de Cantabria (UC), Santander (Spain) University of Cambridge, (UK) University of Manchester, Jodrell Bank Centre for Astrophysics (UK) IDOM, Bilbao (Spain)
26 Observatorio del Teide (Tenerife, Canary Islands) Izaña site, m QUIJOTE Instruments 1 and 2 and enclosure
27 QUIJOTE experiment. Basic features Instrument 1 Instrument 2 Frequency (GHz) Bandwidth (GHz) Number of channels Beam FWHM (deg) (*) T sys (K) Sensitivity (mk s 1/2 ) Sensitivity per beam (Jy s 1/2 ) (*) Pixel = a square with each side is FWHM (Full Width at Half Maximum) of the beam.
28 Radiometer scheme for QUIJOTE 1 Simultaneous Q and U detection
29 QUIJOTE 1: Corrugated feed-horns (Sept. 2010) GHz GHz GHz
30 QUIJOTE 1: Receivers integration LNA GHz OMT GHz
31 Polar Modulator Key component of the polarimeter Rotating polar modulator (40 Hz): switch out 1/f noise Incoming signal modulated at 4 x (modulator frequency) Cryogenically cooled: low losses, low impact on noise Waveguide component: turnstile 4-way junction Units: GHz GHz GHz
32 Orthomode Transducer (OMT) Units: GHz GHz GHz
33 Cryo-LNA. Gain and Noise Temperature 30 GHz Channel (26-36 GHz) Te (K) LNA#40A39, Vd = 0.8V, Vg1 = 0.3V, Vg2 = 0.3V, Id = 23mA, Tp = 11.5K Frequency (GHz) Gi (db) Te (K) Gain (db) Gain and noise temperature of Caltech LNA at 12 K
34 30 GHz BEM (QUIJOTE 1) RF circuits DC circuits BEM branch (top cover removed)
35 30 GHz BEM (QUIJOTE 1) Waveguide input RF sample output (K connector)
36 Test results (30 GHz BEM) BEM_QUIJOTE_ *log(Vo(mV)) Frequency, GHz UNIT#1 UNIT#2 Gain vs. frequency for two units (detector included)
37 Facilities at Universidad de Cantabria Test equipment from DC to 50 GHz: Gain, Noise temperature, Signal analysis, Spectrum analysis, 1/f noise, at Room temperature (300 K) and at cryogenic temperature (20 K) Cryostats general view Two LNA units installed inside
38 QUIJOTE 2 30 GHz Instrument FOCAL PLANE Connectors for 26-36GHz Receivers Displacer GHz Feedhorn Motor mount Telescope Mounting Interface Flange Connector for Temperature sensors and heaters Pressure Sensor Vacuum Valve FRONT VIEW Hermetic Feedthroughs for encoders signals
39 Telescope QUIJOTE 1 IAC (La Laguna, Tenerife) May 2009
40 Acknowledgments Spanish participation in Planck mission and QUIJOTE experiment is funded by the Ministry of Science and Innovation. Grants: AYA C03 AYA C03 40
41 End
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Product Description Sirenza Microdevices SGC-689Z is a high performance SiGe HBT MMIC amplifier utilizing a Darlington configuration with a patented active-bias network. The active bias network provides