Planck Mission and Technology

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1 Planck Mission and Technology Petri Jukkala, Nicholas Hughes, Mikko Laaninen, Ville-Hermanni Kilpiä YLINEN Electronics Ltd Jussi Tuovinen, Jussi Varis, Anna Karvonen MilliLab, VTT Information Technology

2 Contents Planck Mission - Cosmic Microwave Background (CMB) radiation - History of CMB measurements Planck Payload - High Frequency Instrument (HFI) - Low frequency Instrument (LFI) 70 GHz receiver - specifications - receiver technology - measurement system - performance Conclusions

The Big Bang Expansion or Collapse - depends on gravity Ω is the ratio of actual to critical density Ω=1 equilibrium; Ω>1 collapse free space shows ~0.2 atoms/m 3; planets, stars, etc ~0.

3 The Big Bang Expansion or Collapse - depends on gravity Ω is the ratio of actual to critical density Ω=1 equilibrium; Ω>1 collapse free space shows ~0.2 atoms/m 3; planets, stars, etc ~0.1 atoms/ 3 Ω=1 requires 5 atoms/m 3 Remaining density named dark matter can possibly be detected by gravitational lensing but is not known if enough for Ω=1 Current Inflation model shows a fireball after 3min to 300,000years gravity battling against thermal pressure (like a star) star converts hydrogen to helium during last stages helium to heavier elements not time in fireball - evidenced by min. He of 23% and fireball expanding and cooling At 300,000years gravity WINS and atoms form energy (photons) can propagate - end of dark age the cosmic background we can detect

4 Cosmic Structures IF transition to Gravity dominance smooth a smooth and even atomic structure created constant density, no grouping of atoms no dust clouds, no primordial stars, no galaxies However, if density (sonic) oscillations in Fireball at decoupling these would lead to density variations during expansion, gravity would, increase higher densities decrease lower densities thus dust clouds form & coalesce forming the first stars this implies a variable transition to atom forming the radiation should also show this variation radiation would be over a large frequency range thus anisotropies in CMB show fireball structure

Cosmic Microwave Background CMB CMB Anisotropies - ripples were noted by COBE have different sizes (wavelengths & amplitudes) Acoustic Horizon determines longest ripple (fundamental?

5 Cosmic Microwave Background CMB CMB Anisotropies - ripples were noted by COBE have different sizes (wavelengths & amplitudes) Acoustic Horizon determines longest ripple (fundamental?) above this smaller ripples (harmonics?) So mapping of these ripples, will provide a better model for the fireball a more reliable value of Ω possibly the expansion/collapse answer or something else So we need more sensitive measurements

Earlier Missions COBE (COsmic Background Explorer) provided the first

Millimetric Extragalactic Radiation And Geomagnetics) made more sensitive

showed strong evidence for CMB anisotropy 1997 WMAP, (Wilkinson Microwave

6 Earlier Missions COBE (COsmic Background Explorer) provided the first evidence of CMB anistropy launched 1989 BOOMERANG, (Balloon Observations Of Millimetric Extragalactic Radiation And Geomagnetics) made more sensitive measurements from a balloon over 3% sky area. showed strong evidence for CMB anisotropy 1997 WMAP, (Wilkinson Microwave Anisotropy Probe), launched 2001 provides an overall survey but with lower sensitivity and resolution than Planck

7 Mission comparision Planck vs. WMAP Sensitivity 10x Frequency coverage 10x Angular resolution 2x

The Planck Mission Planck and Herschel launched together on Ariane 5 separate before reaching L2 Planck will achieve orbit as shown LeGrange predicted neutral gravity po at L2 sun+earth

8 The Planck Mission Planck and Herschel launched together on Ariane 5 separate before reaching L2 Planck will achieve orbit as shown LeGrange predicted neutral gravity po at L2 sun+earth gravity balanced by solar centripedal force Check-out and calibration map complete sky rotating at 1rpm 1+ year mission data transmission direct to ground potential 100+ manyears data analysis

Planck Payload is comprised of support service module Hydrogen sorption cooler system passively cooled 1,5 m aperture off-set reflector antenna the HIGH Frequency Instrument (HFI) the LOW

9 Planck Payload is comprised of support service module Hydrogen sorption cooler system passively cooled 1,5 m aperture off-set reflector antenna the HIGH Frequency Instrument (HFI) the LOW Frequency Instrument (LFI) the HFI has bolometer receivers at 100, 143, 217, 353, 545, 857GHz cooled to 0.1 K the LFI has radiometric receivers at 30, 44, 70 GHz cooled to 20K with a 4K reference

10 Planck Payload module

11 LFI Payload Focal Plane Unit light blue blue red 2 x 30 GHz 3 x 44 GHz 6 x 70 GHz Waveguides Back End Unit

12 LFI Payload

13 70 GHz receiver continuous comparison provides continuous measurement, maximises available viewing opportunity and maximises sensitivity To other polarisation radiometer CMB Target OMT ½FEM ½BEM 1st.Hybird Phase LNA.1 LNA.2 (WG Magic-T) Shifter 2nd.Hybird (WG Magic-T) LNA.3 φ φ BPF Diode Voltage Detector Amplifier 4K Ref. single antenna horn + OMT, provides two orthogonally polarised outputs each output applied to separate radiometer each radiometer amplifies and detects Target and 4K reference noise detected signal appears as a noise voltage proportional to input noise power

14 Receiver structure 4K Ref. Source Analogue Data output DAE Interface 4K Ref. Antenna 0 π Filter Amplifier/Detector FEM_ACA FEM_Body DC Amplifier FEM_ACA 0 π Waveguide Input from Antenna via OMT Interconnection Waveguide

15 70 GHz receiver main requirements Frequency Noise temperature Isolation (phase switching) 1/f noise knee frequency RF Gain FEM power consumption BEM power consumption GHz 29 K, when cooled to 20 K 13 db (goal 20 db) 50 mhz ~50 db 24 mw (2 polarisations incl. 4 ACAs) 604 mw (4 back end receivers)

processed in NGST (TRW) Antenna horns, OMTs

16 FEM and ACA body: nickel/gold plated aluminium BEM body: cromatized and black painted aluminium Amplifiers (PHEMT) and switches (PIN) based on InP MMICs MMICs processed in NGST (TRW) Antenna horns, OMTs and interconnecting waveguides supplied by Italy Receiver technology

17 x 1,0 x 0.4 meter thermal vacuum chamber for testing ght 1000 kg (reference) and 20 K (receivers) coolers 12 waveguide Vector Network Analyzer e temperature measurement with noise diode ermal vane attenuator er meter acquisition system noise power supplies perature sensors ting in class clean room Test system

18 General configuration within the cryogenic shroud

19 Test system

20 General cryo chamber setup Radiation Shield 4K Load φ 3dB "Magic-T" couplers BEM Data outputs Antenna OMT FEM φ Antenna Load 4K Load Input stimulus Waveguide Waveguide Test Points FEM Output BEM Input Cryo. Chamber boundary

21 On-chip measurement results asurements made by MilliLab, both Room Temperature and Cryogenic, cryo measurements shown. NGST CRYOx & MLAB1, designs 70LN5B & 5C, Vds=0.4 V, Ids=7.5 ma, T=20 K; June 24, NGST MLAB2, wafer , design 02004A_6, MMIC ID R2 C2 M0, T=20 K; August 11, Noise temperature (K) Gt_425_old_cryo4 Gt_121_new_cryo4 Gt_410_new_cryo4 Gt_235_mlab1 Gt_330_cryo9 Gt_410_cryo9 Gt_710_cryo7 Gt_820_cryo7 Te_425_old_cryo4 Te_121_new_cryo4 Te_410_new_cryo4 Te_235_mlab1 Te_330_cryo9 Te_410_cryo9 Te_710_cryo7 Te_820_cryo7 mag S21 (db) -0,5-1 -1,5-2 -2,5-3 -3, p hase S21 (d eg) mags21 (db) - 1 mags21 (db) - 2 phs21 (deg) - 1 phs21 (deg) , , , , , , ,5 80 Frequency (GHz) , , , , , ,5 80 Frequency (GHz) -200

22 FM ACA measuremet results, cryo P01: FEM_ACA Gain Measurement 50,0 45,0 40,0 Gain - db 35,0 30,0 25,0 20, Frequency - GHz MEP02: FEM_ACA Noise Temperature Measurement - Forward biased phase shifter 100,0 FEM_ACA Noise Temp. K 80,0 60,0 40,0 15,0 10,0 5,0 0,0 FEM_ACA Gain, Phase shifter state 0 FEM_ACA Gain, Phase shifter state 1 20,0 0, Frequency 70 - GHz 75

23 - TVA measurement EM FEM and BEM measurement results Phase shifter state 00 - Input.4 - Output.8 Phase shifter state 01 - Input.4 - Output.7 Phase shifter state 10 - Input.4 - Output.7 Phase shifter state 10 - Input.4 - Output.8 FEM noise FEM gain and switching isolation BEM response (DC/RF) Frequency (GHz) 72 Frequency GHz t.1 to Output.2 (for all phase states) ain 50 db Frequency GHz 62 Sensitivity db(mv/mw)

Response (DC/RF) 1/f noise EM Receiver measurement results Sensitivity vs Frequency Sensitivity (dbmv/mw) 160 150 140 130 120 110 100 90 Attenuator setting = 20

24 Response (DC/RF) 1/f noise EM Receiver measurement results Sensitivity vs Frequency Sensitivity (dbmv/mw) Attenuator setting = 20 Attenuator setting = 30 Attenuator setting = 40 Attenuator setting = 50 Attenuator setting = 70 Attenuator setting = 90 Attenuator setting = Frequency (GHz)

25 Conclusions Planck mission has been presented Planck satellite payload (HFI and LFI) was explained State of the art 70 GHz continuous comparision receiver technology and performance was presented Planck satellite will be launched in summer 2007

Power spectrum exercise

Power spectrum exercise In this exercise, we will consider different power spectra and how they relate to observations. The intention is to give you some intuition so that when you look at a microwave