Planck – Mission and Technology - VTTursi2004.vtt.fi/ursi2004_jukkala.pdf · Planck – Mission...

© YLINEN Electronics Ltd 2004

Planck –Mission and Technology

Petri Jukkala, Nicholas Hughes, Mikko Laaninen, Ville-Hermanni KilpiäYLINEN Electronics Ltd

Jussi Tuovinen, Jussi Varis, Anna KarvonenMilliLab, VTT Information Technology


ContentsPlanck 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/m3;

• planets, stars, etc ~0.1 atoms/3• Ω=1 requires 5 atoms/m3

• 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


Cosmic StructuresIF 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?)• 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 evidence of CMB anistropy• launched 1989

• BOOMERANG, (Balloon Observations Of MillimetricExtragalactic 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


Mission comparision

Planck vs. WMAPSensitivity 10xFrequency coverage 10xAngular 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 points• at L2 sun+earth gravity balanced bysolar 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 Payloadis 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


Planck Payload module


LFI Payload

Focal Plane Unitlight blue 2 x 30 GHzblue 3 x 44 GHzred 6 x 70 GHz

Waveguides

Back End Unit


LFI Payload


70 GHz receiver

φ

φ

4K Ref.

CMBTarget

1st.Hybird(WG Magic-T) LNA.1 LNA.2

PhaseShifter 2nd.Hybird

(WG Magic-T)OMT

To other polarisation radiometer

½FEM ½BEM

LNA.3 BPFDiode

DetectorVoltageAmplifier

• “continuous comparison” provides continuous measurement, • maximises available viewing opportunity• and maximises sensitivity

• 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


Receiver structure

4K Ref.Antenna

Waveguide Input fromAntenna via OMT

4K Ref.Source

π0

FEM_Body

FEM_ACA

FEM_ACA

Amplifier/Detector

AnalogueData output

DAE Interface

DC Amplifier

π0

InterconnectionWaveguide

Filter


70 GHz receiver main requirements

• Frequency 63 – 77 GHz• Noise temperature 29 K, when cooled to 20 K• Isolation (phase switching) 13 dB (goal 20 dB)• 1/f noise knee frequency 50 mHz• RF Gain ~50 dB• FEM power consumption 24 mW (2 polarisations incl. 4 ACAs)• BEM power consumption 604 mW (4 back end receivers)


Receiver technologyFEM and ACA body: nickel/gold plated aluminiumBEM body: cromatized and black painted aluminiumAmplifiers (PHEMT) and switches (PIN) based on InP MMICsMMICs processed in NGST (TRW)Antenna horns, OMTs and interconnecting waveguides supplied by Italy


Test system• 1,6 x 1,0 x 0.4 meter thermal vacuum chamber used for testing

• Weight 1000 kg

• 4 K (reference) and 20 K (receivers) coolers

• WR12 waveguide Vector Network Analyzer

• Noise temperature measurement with noise diode and thermal vane attenuator

• Power meter

• Data acquisition system

• Low noise power supplies

• Temperature sensors

• Testing in class 100 000 clean room


General configuration within the cryogenic shroud


Test system


General cryo chamber setup

φ

φOMTAntenna

4KLoad

4KLoad

AntennaLoad

Radiation Shield

Cryo. Chamber boundaryFEM OutputBEM Input

WaveguideTest Points

3dB"Magic-T"couplers

Data outputs

BEM

FEM

Input stimulusWaveguide


On-chip measurement resultsMeasurements made by MilliLab, both Room Temperature and Cryogenic, cryo measurements shown.

NGST MLAB2, wafer 4246-015, design 02004A_6, MMIC ID R2 C2 M0, T=20 K; August 11, 2004

-5

-4,5

-4

-3,5

-3

-2,5

-2

-1,5

-1

-0,5

0

50 52,5 55 57,5 60 62,5 65 67,5 70 72,5 75 77,5 80

Frequency (GHz)

mag

S21

(dB

)

-200

-150

-100

-50

0

50

100

150

200

phas

e S2

1 (d

eg)

magS21 (dB) - 1magS21 (dB) - 2phS21 (deg) - 1phS21 (deg) - 2

NGST CRYOx & MLAB1, designs 70LN5B & 5C, Vds=0.4 V, Ids=7.5 mA, T=20 K; June 24, 2004

0

5

10

15

20

25

30

35

40

45

50 52,5 55 57,5 60 62,5 65 67,5 70 72,5 75 77,5 80

Frequency (GHz)

Inse

rtio

n ga

in (d

B)

0

20

40

60

80

100

120

140

160

180

Noi

se te

mpe

ratu

re (K

)Gt_425_old_cryo4Gt_121_new_cryo4Gt_410_new_cryo4Gt_235_mlab1Gt_330_cryo9Gt_410_cryo9Gt_710_cryo7Gt_820_cryo7Te_425_old_cryo4Te_121_new_cryo4Te_410_new_cryo4Te_235_mlab1Te_330_cryo9Te_410_cryo9Te_710_cryo7Te_820_cryo7


FM ACA measuremet results, cryo

MEP02: FEM_ACA Noise Temperature Measurement - Forward biased phase shifter

0,0

20,0

40,0

60,0

80,0

100,0

60 65 70 75 80Frequency - GHz

FEM_ACA Noise Temp. K

MEP01: FEM_ACA Gain Measurement

0,0

5,0

10,0

15,0

20,0

25,0

30,0

35,0

40,0

45,0

50,055 60 65 70 75 80 85

Frequency - GHz

Gain - dB

FEM_ACA Gain, Phase shifter state 0

FEM_ACA Gain, Phase shifter state 1


EM FEM and BEM measurement resultsFEM noiseFEM gain and switching isolationBEM response (DC/RF)

FEM Input.1 to Output.2 (for all phase states)

-10

0

10

20

30

40

50

55 60 65 70 75 80 85Frequency GHz

Gain dB

00011011

60

62

64

66

68

70

72

55 60 65 70 75 80 85

Frequency GHz

SensitivitydB(mV/mW)

Att_20Att=30Att=40Att=50Att=70Att=90Att=110Att=130

FEM Noise Temp. - TVA measurement

0102030405060708090

100

62 64 66 68 70 72 74 76 78

Frequency (GHz)

NT (K)

Phase shifter state 00 - Input.4 - Output.8Phase shifter state 01 - Input.4 - Output.7

Phase shifter state 10 - Input.4 - Output.7Phase shifter state 10 - Input.4 - Output.8


EM Receiver measurement resultsResponse (DC/RF)1/f noise

Sensitivity vs Frequency

90100110120130140150160

55 60 65 70 75 80 85

Frequency (GHz)

Sensitivity (dBmV/mW)

Attenuator setting = 20Attenuator setting = 30Attenuator setting = 40Attenuator setting = 50Attenuator setting = 70Attenuator setting = 90Attenuator setting = 110


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

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