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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

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30

DB(|S(1,1)|)Balance_Amp_RT

DB(|S(1,1)|)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

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DB(|S(1,1)|)Balance Amp_28K






IF Amplifier

0

5

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15

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0 2 4 6 8 10 12 14 16

Freq. (GHz)

Noi

se T

emp.

(K)

0

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400

20 K300 K

-30

-20

-10

0

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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

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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

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-100

-90

-80

-70

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-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.