MMICs for multi pixel receivers

Transcription

INSTITUTE of RADIOASTRONOMY
INAF
MMICs for multi pixel receivers
A. Cremonini
INAF
Workshop on Receivers & Arrays 2010 -19,20 September 2010, MPIfR/Bonn
INAF
Outline
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Introduction
MMICs
Semiconductor technology
Scenario
Examples of MMICs used in array receivers for radioastronomy
Projects in progress
Remarks on MMIC based devices
Conclusions
Introduction
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The evolution of instruments for radioastronomical observation is nowadays strongly
oriented on developing and exploiting the array concept.
Array of antennas
VLA
ATCA
ALMA
SKA
Ka-Band
K-band
Array of receivers
C-band
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Introduction
Several aspects of this concept are attractive:
Focal plane array receivers
Improve antenna observing efficiency allowing faster surveys
Increase Sensitivity especially for radiometric purposes
Phase Array receivers
Increase System Flexibility allowing beamforming and steering
Allow the generation of more than one beam
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MMICs
In the technologies applied to radioastronomy interest in MMICs
grows as the needs of low cost, small scale production,
high integrated solution.
Hybrid devices, created with discrete components provide paramount
performances, but the realisation on large scale has high
cost, assembling time, reliability strictly related on
manufacturing.
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MIC vs MMIC
Active devices are manufactured using the same process
Active device
MMICs selection is
selection is possible
Passive Catalog is the
entire market
MMIC is a MUST for mass
production
possible
And
Passive Catalog is
MIC “fine Art” Skills are a MUST in
order to maximize MMICs
performances exploitation
limited by foundry
MMICs performances are less human skills dependant
MMICs developing cost is higher
MMICs is less expensive for small mass production
process
MMIC technology allows to include in a single chip several active
and passive components in order to realise a function or a
set of functions.
Assets:
Lower cost
Fast production
Higher repeatability and reliability
Fundamental requirements are:
Low power consumption
Low noise
An asset for radioastronomical application : CryoREL
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Semiconductor technology
InP HEMT
o Best consolidated process for noise and cryo applications
o State of the art at 35nm with applications up to 350 GHz
InP mHEMT 
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InP on GaAs : one more degree of freedom in the process
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EU foundries, no ITAR , no geopolitical availability dependency
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Preliminary cryo results in Q and W band
InSb HEMT  Extremely Low power consumption .
Could be the future for Large arrays cryogenic applications
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Scenario
InP HEMT
InP mHEMT
InP , InSb HEMT
IAF (D)
Chalmers Univ. (S)
OMMIC (F)
OPTEL (I)
NCG
HRL
UMAN (UK)
ETH (CH)
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Some examples of MMICs
used on Array receivers for
radioastronomy
FARADAY
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Designed By INAF-IRA
Tested on 32 mt Medicina radiotelescope
Final Destination 64mt SRT
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Multifeed Focal Plane Array
7 Horns - 14 Channels
Working from 18-26 GHz
For Secondary Focus
Heterodyne architecture
Cryogenically cooled
Medicina
VLBI 32m
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MMICs application :LNAs
NGC 0.1 InP HEMT
14 Cryo LNAs
14 “warm” LNAs
Cryo LNA
Spar 22LNA07A 020201
20
Noise Performances 4245-020 22LNA_07A
30
340
DB(|S[2,2]|) (R)
020101 1V35-18mA
300
15
020201
020201 High Accuracy
Simulated
260
DB(|S[2,1]|) (L)
020101 1V35-18mA
-20
0
-40
-15
-60
-30
Te [K]
DB(|S[1,1]|) (R)
020101 1V35-18mA
0
220
180
140
100
31
33
35
Frequency [GHz]
26
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25
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24
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25
23
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17 19 21 23
Frequency (GHz)
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15
21
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13
20
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11
19
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9
18
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7
17
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5
16
,5
“Warm” LNA
15
,5
60
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MMICs Extra results
NGC 0.1 InP HEMT
7 Cryo LNAs Designs between
4 to 120 GHz
4-8 Ghz
8 - 12 Ghz
33-50 Ghz
26 - 40 Ghz
60-85 Ghz
70 - 100 Ghz
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OCRA-F
Designed By JBO (UK)
Final Destination Torun (PL)
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Multifeed Focal Plane Array receiver
8 (later 16) Beams
Working from 26-36 GHz
Pseudo correlation Direct Detection Architecture
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MMICs application :LNAs, Phase switches
NGC 0.1 InP HEMT
8 Cryo LNAs
8 Cryo phase switches
FARADAY MMIC LNA #1. Noise temperature and gain
measurements Tlna = 15 K 27.08.04
100
Te K
80
60
40
20
0
26
28
30
32
Frequency GHz
180
45
160
35
140
25
120
15
100
5
80
-5
60
40
-15
-25
20
-35
0
-45
26
28
30
32
34
36
phase diff
magnitude diff
dB
degs
MMIC Phase switch #2 @ 18 K. phase shift between states.
08.10.04
average across
10Ghz BW =
170degs
Frequency GHz
34
36
Te K
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Pharos
Facilities : JBO
Design :Pharos Consortioum leaded by ASTRON
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Vivaldi Dense Phased Array
4 beams electronically formed and steered
Single polarisation
Working from 4 to 8 GHz
For Primary Focus
MMICs application :LNAs, Phase switches
Facilities
: JBO
OMMIC ED02H
GaAs
HEMT Process
24 Cryo LNAs (20K)
52 Buffers Amplifiers (77K)
52 Phase controller (77K)
52 Amplitude controller (77K)
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Pharos MMICs Extra results
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OMMIC D007IH 70 nm InP on GaAs mHEMT Process
Q-band LNA
W-band LNA
GaAs 70nm LNA, Flanged, 300K
40
IRL
ORL
Gins
30
[dB]
20
10
0
-10
-20
75
85
95
105
freq. [GHz]
40
10
35
5
|S11| (dB)
|S21| (dB)
30
25
20
15
0
-5
-10
10
-15
5
0
-20
25
30
35
40
45
50
25
30
freq, GHz
35
40
freq, GHz
45
50
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Projects in Progress
Apricot (All Purpose Radio Imaging Cameras on Telescopes)
INAF
FP7 Project funded within Radionet
Partners: UMAN, MPfIR,IRA,UTV, CAY, TCfA, FG-IGN
Aim :
Define architecture and validate technologies for multi
purposes large format focal plane “radio camera”
Frequency range : 33-50 GHz (Q-Band).
Design a MMIC Q band heterodyne receiver chipset using mHEMT
foundry process available at OMMIC and IAF
LNA
Mixing
Multiplier
INAF
ASImm
Project funded by ASI (Italian Space Agency)
Partners: Thales (as prime contractor), Officine Pasquali
INAF, UNI-MI, UNI-GE, UNIROMA1,CNR
Aim : Validate technologies for future space experiments
Frequency range : W-band
Design W-band devices radiometric purposes using OMMIC MMIC
mHEMT foundry process and IAF mHEMT foundry process
Improve Packaging and Assembling Techniques
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Remarks on MMIC based
devices
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MMIC Design
Noise Performances 4245-020 22LNA_05A
MMIC is a ensemble of active
and passive elements
220
050201
050201 High Accuracy
Simulated
180
140
100
Frequency [GHz]
This could be a MMIC designer
trap
26
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25
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24
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23
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22
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18
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17
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60
15
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Te [K]
MMIC is NOT a receiver
COMPONENT but a PART OF
IT
260
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Wiring
100 Dual Polarization channels at WR-22
200 four stages LNAs
1800 Wires
Separate stage biasing is
important in order to compensate
the temperature effect and find
the best trade off between noise,
gain , match and... Oscillations
100 Dual Polarisation channels at WR-10
200 + 200 five stages LNAs
4400 Wires
Embed a cryogenic bias supply
“remotely controlled”
Improve cryomodels and
Foundry process
Release flexibility specifications
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MMIC Packaging
Housing could waste most of efforts devoted in MMIC design in order to obtain
state of the art results
Housing has influence on
Self resonances
Matching (Gain and Noise)
Reliability
Crucial Aspects are:
Housing Alloys
Attaching method
The choice is not unique BUT is
APPLICATION DEPENDANT
For Cryogenic MMICs devices,
Differential CTE between all the
joined elements MUST be
carefully taken into account ,
because STRESS between
components can DAMAGE them
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Conclusion
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Array receiver architecture make the MMIC opportunity more than
attractive. Several examples of array receivers already prove it.
Semiconductor scenario give several opportunity to exploit MMIC
potentiality
Excellent MMIC design is a necessary starting point but it is not
SUFFICIENT
MIC designers experiences and manufacturer skillness are
NECESSARY in order to realise the devices
Radioastronomy can get many advantages by MMICs
Developing an MMIC foundry process oriented to cryogenic
radioastronomical applications is NOT a foundry mainstream
MMICs R&D on foundry process and on devices is EXPENSIVE
Radioastronomical community MUST SYNERGICALLY INVEST on it
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Research Groups involved in the described activities
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PHAR S
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Thanks
For your attention
A. Cremonini

MMICs for multi pixel receivers

Transcription

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