Planck – Mission and Technology

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
© YLINEN Electronics Ltd 2004
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
© 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 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
© 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 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
© YLINEN Electronics Ltd 2004
Mission comparision
Planck vs. WMAP
Sensitivity 10x
Frequency coverage 10x
Angular 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 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
© YLINEN Electronics Ltd 2004
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
© YLINEN Electronics Ltd 2004
Planck Payload module
© YLINEN Electronics Ltd 2004
LFI Payload
Focal Plane Unit
light blue
2 x 30 GHz
blue
3 x 44 GHz
red
6 x 70 GHz
Waveguides
Back End Unit
© YLINEN Electronics Ltd 2004
LFI Payload
© YLINEN Electronics Ltd 2004
70 GHz receiver
•
“continuous comparison” provides continuous measurement,
• maximises available viewing opportunity
• and maximises sensitivity
To other polarisation radiometer
½FEM
1st.Hybird
(WG Magic-T)
CMB
Target
½BEM
LNA.1 LNA.2
Phase
Shifter
φ
OMT
2nd.Hybird
(WG Magic-T)
LNA.3
BPF
Diode Voltage
Detector Amplifier
φ
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
© YLINEN Electronics Ltd 2004
Receiver structure
Analogue
Data output
DAE Interface
4K Ref.
Source
Filter
0
4K Ref.
Antenna
Amplifier/Detector
π
FEM_ACA
FEM_Body
DC Amplifier
FEM_ACA
0
π
Waveguide Input from
Antenna via OMT
Interconnection
Waveguide
© 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 technology
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
© 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
Radiation Shield
3dB
"Magic-T"
couplers
4K
Load
φ
Data outputs
BEM
Antenna
OMT
FEM
φ
Antenna
Load
4K
Load
Cryo. Chamber boundary
Input stimulus
Waveguide
Waveguide
Test Points
FEM Output
BEM Input
© YLINEN Electronics Ltd 2004
On-chip measurement results
Measurements 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, 2004
180
40
160
35
140
NGST MLAB2, wafer 4246-015, design 02004A_6,
MMIC ID R2 C2 M0, T=20 K; August 11, 2004
0
Gt_425_old_cryo4
-0,5
Gt_121_new_cryo4
Gt_410_new_cryo4
120
100
20
80
15
60
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_710_cryo7
40
5
20
0
0
-1,5
Gt_410_cryo9
Te_410_cryo9
10
100
Gt_330_cryo9
Te_820_cryo7
m a g S 2 1 (d B )
25
150
-1
Gt_235_mlab1
N o is e te m p e ra tu re (K )
In s e rtio n g a in (d B )
30
200
50
-2
0
-2,5
-3
-50
-3,5
-100
-4
-150
-4,5
-5
50
52,5
55
57,5
60
62,5
65
67,5
70
72,5
75
77,5
-200
50 52,5 55 57,5 60 62,5 65 67,5 70 72,5 75 77,5 80
80
Frequency (GHz)
Frequency (GHz)
© YLINEN Electronics Ltd 2004
p h a s e S 2 1 (d e g )
45
magS21 (dB) - 1
magS21 (dB) - 2
phS21 (deg) - 1
phS21 (deg) - 2
FM ACA measuremet results, cryo
MEP01: FEM_ACA Gain Measurement
55
50,0
60
65
Frequency - GHz
MEP02: FEM_ACA Noise Temperature Measurement - Forward biased phase
shifter
70
75
80
85
100,0
FEM_ACA Noise Temp.
K
45,0
80,0
40,0
Gain - dB
35,0
60,0
30,0
25,0
40,0
20,0
15,0
20,0
10,0
5,0
0,0
FEM_ACA Gain, Phase shifter state 0
FEM_ACA Gain, Phase shifter state 1
© YLINEN Electronics Ltd 2004
0,0
60
65
Frequency
70 - GHz
75
80
EM FEM and BEM measurement results
FEM Noise Temp. - TVA measurement
FEM noise
Phase shifter state 00 - Input.4 - Output.8
100
90
NT
80 (K)
70
60
50
40
30
20
10
0
62
Phase shifter state 01- Input.4 - Output.7
FEM gain and switching isolation
Phase shifter state 10 - Input.4 - Output.7
Phase shifter state 10 - Input.4 - Output.8
64
66
68
BEM response (DC/RF)
70
72
74
76
78
Frequency GHz
72
Frequency (GHz)
70
FEM Input.1 to Output.2 (for all phase states)
00
01
68
10
11
50 dB
Gain
40
Att_20
66
Att=30
30
Att=40
Att=50
64
20
Att=70
Att=90
10
0
-10
55
60
65
70
75
Frequency GHz
80
85
Att=110
62
Sensitivity
dB(mV/mW)
Att=130
60
55
© YLINEN Electronics Ltd 2004
60
65
70
75
80
85
EM Receiver measurement results
Response (DC/RF)
1/f noise
Sensitivity vs Frequency
A ttenuato r setting = 20
A ttenuato r setting = 30
A ttenuato r setting = 40
A ttenuato r setting = 50
A ttenuato r setting = 70
A ttenuato r setting = 90
A ttenuato r setting = 110
160
150
140
130
Sensitivity
120
(dBmV/mW)
110
100
90
55
60
65
70
75
80
85
Frequency (GHz)
© 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
© YLINEN Electronics Ltd 2004