planck – mission and technology - vttursi2004.vtt.fi/ursi2004_jukkala.pdf · planck – mission...
TRANSCRIPT
© 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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
Mission comparision
Planck vs. WMAPSensitivity 10xFrequency coverage 10xAngular resolution 2x
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
Planck Payload module
© YLINEN Electronics Ltd 2004
LFI Payload
Focal Plane Unitlight blue 2 x 30 GHzblue 3 x 44 GHzred 6 x 70 GHz
Waveguides
Back End Unit
© YLINEN Electronics Ltd 2004
LFI Payload
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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)
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
General configuration within the cryogenic shroud
© YLINEN Electronics Ltd 2004
Test system
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
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