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ALMA Band-1 Receiver. Chau-Ching CHIONG 章朝盛. Institute of Astronomy and Astrophysics, Academia Sinica (ASIAA). Contributions from …. ASIAA Microwave Group: Dr. Y.-J. Hwang, Dr. Y.-F. Kuo, Dr. C.-C. Lin, C.-C. Chuang, C.-T. Ho . Receiver Group: Dr. M.-T. Chen, T.-S. Wei. - PowerPoint PPT Presentation
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ALMA Band-1 Receiver
Chau-Ching CHIONG 章朝盛Institute of Astronomy and Astrophysics, Academia Sinica (ASIA
A)
Contributions from …• ASIAA
– Microwave Group: Dr. Y.-J. Hwang, Dr. Y.-F. Kuo, Dr. C.-C. Lin, C.-C. Chuang, C.-T. Ho.
– Receiver Group: Dr. M.-T. Chen, T.-S. Wei.
• National Taiwan University EE– Prof. H. Wang: Dr. Z.-M. Tsai, Dr. B.-J. Huang, W.-J. Tzeng, Y.-
C. Wu, B.-H. Tsai, C.-C. Hung.
• National Central University EE– Prof. H.-Y. Chang: S.-H. Weng.– Prof. Y.-S. Lin: Y.-S. Hsieh.
Science of ALMA Band 1 (30-45 GHz)• High resolution Sunyae
v-Zel’dovich effect imaging
• Anisotropy of cosmic microwave background radiation
• High-redshifted CO lines
• Probing magnetic field strength via Zeeman measurement
Transistion Redshift rangeCO J=1-0 1.55 – 2.67
CO J=2-1 4.11 – 6.35
Transistion Frequency(GHz)
Zeeman splitting (Hz/uG)
CCS JN = 32-21 33.75 0.70
CCS JN = 43-32 45.38 0.63
SO JN = 10-01 30.00 1.74
SiO v=1, J =1-0 43.12 Very small
• International cooperation of Taiwan (ASIAA), Canada (HIA) and Chile (Uni. of Chile).
• ASIAA deliver key components, mostly in MMIC technologies (LNA, mixer, filter, IF amp.), while HIA focuses on optics, LNA (hybrid) and system integration.
• Proto-type receiver will be assembling in Chile.
Band-1 Development Plan
Main challenges:• Longest wavelength, thus largest component size.• LNA Noise < 7 K.• More than 60 copies required.
HIA Band-1 cartridge layout
Band 1 System Requirements
• Observation frequency: 31.3-45 GHz (36%)• Operation mode: single side band (USB), dual linear polarization feed• Image suppression: > 20 dB• Aperture efficiency: > 78 %• IF bandwidth: 4-12 GHz• IF output power: -31 to -18 dBm. IF power variation: 6dB peak-t
o-peak in any 2GHz BW. 10 dB peak to peak across the complete IF band.
• Receiver noise temperature: 17 K (80 % bandwidth) and 28 K (full bandwidth) when operating at 15 K.
• LO tuning range: 27.3-33 GHz (18.9%). No mechanical tuning• RMS LO phase noise in jitter: 53 fs (short-term), 17.7 fs (long-term)• LO output power: 10 mW• Front-end cartridge size: diameter 170mm, length ~ 500mm
ALMA Band 1 Front-end System15K
• Optics design + Feedhorn• OrthoMode Transducor (OMT)• Cryogenic Low Noise Amplifier (LNA)• Bandpass Filter + Mixer• Intermediate Frequency (IF) Amplifier• Local Oscillator (LO) + PLL
Reasons for MMIC Approach• Easy integration• High reliability• Mass production
(> 200 pcs.)• Low cost (?)• But still high noise.
Hybrid IC MMIC
Design Time Fast Slow
Noise Low High
Assembling & Mass Production Hard Easy
Circuit Density Large Small
Integration Hard Easy
Experts No Yes
Hybrid X-band LNA from JPL, Weinreb (2007)
MMICs for Front End
Q-band Cascode PHEMT Mixer
Z.-M. Tsai et. al, EuMIC, 2009
The cascode mixer using WIN 0.15 um pHEMT shows• Good conversion gain flatness over 4-12GHz IF frequency.• Low LO power drive.
December 01-03, 2010
28 30 32 34 36 38 40 42 44 46 48 50Frequency (GHz)
-30
-20
-10
0
10
20
30
40DB(|S(2,1)|)2f50_LNA_28K
DB(|S(2,1)|)2f50_LNA_RT
DB(|S(1,1)|)2f50_LNA_28K
DB(|S(1,1)|)2f50_LNA_RT
DB(|S(2,2)|)2f50_LNA_28K
DB(|S(2,2)|)2f50_LNA_RT
Vd1=Vd2=Vd3=1V, Id1=Id2=Id3=10mA
Both with 2 mm x 1 mm
|S| (
dB)
2f50m 3-stage mHEMT LNA
28 30 32 34 36 38 40 42 44 46 48 50Frequency (GHz)
-30
-20
-10
0
10
20
30
40DB(|S(2,1)|)2f100_LNA_29K
DB(|S(2,1)|)2f100_LNA_RT
DB(|S(1,1)|)2f100_LNA_29K
DB(|S(1,1)|)2f100_LNA_RT
DB(|S(2,2)|)2f100_LNA_29K
DB(|S(2,2)|)2f100_LNA_RT
|S| (
dB)
2f100m 2-stage mHEMT LNA
Vd=2V, Id_dev=37mA, Id_mea=30, 33mA
31-45 GHz 0.15 um MHEMT LNA
Cryogenic Measurements
Weng et al., EuMIC, 2011
Packaging
Test Dewar
December 01-03, 2010
30 35 40 45 50Frequency (GHz)
-30
-20
-10
0
10
20
30
DB(|S(1,1)|)Balance_Amp_RT
DB(|S(1,1)|)Single_End_RT
DB(|S(2,1)|)Balance_Amp_RT
DB(|S(2,1)|)Single_End_RT
DB(|S(2,2)|)Balance_Amp_RT
DB(|S(2,2)|)Single_End_RT
Balanced LNA as Second Stage• The same design of the 3-
stage version. • Better input/output
matching.
30 35 40 45 50Frequency (GHz)
-30
-20
-10
0
10
20
30
DB(|S(1,1)|)Balance Amp_28K
DB(|S(1,1)|)Balance_Amp_RT
DB(|S(2,1)|)Balance Amp_28K
DB(|S(2,1)|)Balance_Amp_RT
DB(|S(2,2)|)Balance Amp_28K
DB(|S(2,2)|)Balance_Amp_RT
IF Amplifier
0
5
10
15
20
25
30
35
40
45
50
0 2 4 6 8 10 12 14 16
Freq. (GHz)
Noi
se T
emp.
(K)
0
50
100
150
200
250
300
350
400
20 K300 K
-30
-20
-10
0
10
20
30
0 2 4 6 8 10 12 14 16Freq. (GHz)
S-p
aram
eter
s (d
B)
S11 (300K) S21 (300K)
S22 (300K) S11 (20K)
S22 (20K) S21 (20K)
Chiong et al., EuMIC, 2009
Total DC power < 150mW 2nd-stage LNA
LO Input
IF amplifier
cascode HEMT mixer
Bandpass filter(Lin et al. ‘09)
Integrated LNA-Mixer-Filter-IFA Chip
• Highly integrated design of the module.• Saving space inside the cryogenic section of the front-
end cartridge.• Reducing the possibility of failure in assembling.
LNA
LO System: YTO or VCO
YIG-Tuned Oscillator (YTO) in Current ALMA System
• Coarse/fine tune• 30 MHz ref.• Excellent phase
noise
MixerYIG OSC
Amplifier28dB
Vfine
fYTO,in
Isolator
fSYN
fIF
fDIV
fREF =30MHz
LoopFilter
PhaseDetector
fYTO
ON PLL Board
30MHz
X 2Coupler
10dB
12bitsCoarse tune
ActiveMultiplier
fLO
fYTO
fSYN
fREF=fIF
30MHzTuning range ofYIG-OSC
f
30MHz UnwantedSignal
Frequency Plan
Ka BandKu Band K BandHF
26.5 4018120.003 0.03 GHz13 17 26 34
30MHz
fLO
YTO + Doubler: Phase Noise• Jitter (1 kHz to 1MHz) ~ 45 fs• ALMA spec: 53 fs
VCO Approach
• VCO has almost all advantages over YTO except phase noise.
• PLL board for YTO has to be modified for VCO operation, because single-tuned VCO has large gain and large gain variation.
• Frequency divider is added so that VCO-based PLL can be used in ALMA environment (using 30 MHz reference).
Differential VCO layout
D e
O ut +
V eeV tu
V bb
D bIee
O ut -
Q 1
Q 2
D e
D b
L c
L c
C
C
L e2 L e1
L e2 L e1
R 1 R 2L bb
L bb
R
R
RF out
RF out
Tuning Voltage
-2.5 V-0.6 V
WIN 0.15 um HBT
Total dc power consumption: 85 mW
Chiong et al., EuMIC, 2008
PN ~ -100 dBc/Hz @ 1MHz offset
Adaptive Loop Bandwidth TechniqueAdaptive Loop Bandwidth Technique
• The VCO gain variation is large. For osc. Freq. > 33GHz, Kvco ~ 200MHz/V, with Filter 1, PLL BW~ 200 kHz.
• By switching to Filter 2, the PLL BW can be increased from 200kHz to 1MHz.
• The phase noise can be improved more than 22dB at the offset frequency of 250kHz under such adaptive loop bandwidth.
2020
-3 -2 -1 0 1 2 3 4 5 6 727.5
28.0
28.5
29.0
29.5
30.0
30.5
31.0
31.5
32.0
32.5
33.0
33.5
34.0
34.5
0
300
600
900
1200
1500
1800
2100
2400
2700
3000
3300
3600
3900
4200
Kvc
o (M
Hz/
V)
Ope
ratin
g F
requ
ency
(GH
z)
Controlled Voltage (V)
Tuning Range
Gain
Phase Locked Spectra of VCO
Phase Noise Comparison between Phase-locked YTO and VCO
RMS Jitter/Degree of YTO (@1kHz to 1MHz) is 44.6fs/0.59o RMS Jitter/Degree of VCO (@1kHz to 1MHz) is 63.8fs/0.77o
102 103 104 105 106 107-160
-150
-140
-130
-120
-110
-100
-90
-80
-70
-60
-50
fLO-YTO:34GHz
free-running YTOfree-running YTOx2
Pha
se N
oise
(dB
c/H
z)
Frequency Offset (Hz)
free-running VCO
fREF:30MHz Reference
fLO-VCO:33.4GHz
YIG vs. VCO• Using adaptive loop bandwidth technique, the whol
e tuning range of VCO can be locked by single PLL board.
• Phase noise within the loop bandwidth (~ 100 kHz) is compatible.
• Worse VCO phase noise at larger offset frequency contribute a lot of noise.
• Need more advanced InP HBT to meet ALMA spec.
Possible Timeline for Band-1
• 2012: Proposal to ALMA• 2013: Preliminary Design Review. First
prototype front-end• 2014: Critical Design Review. Production starts• 2018: Project finishes
Thank you.
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