JS/2006/oct/09
R&D Division
1(C) ASTRON 2006
Jan Simons simons@astron.nl
10-oct-2006
Basic Detection Techniques Radio components
and system characterisation
Contents
Antenna - electromagnetics Transmission lines
S-parameters
Noise in RF components
Systems of RF components
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R&D Division
3(C) ASTRON 2006
Radio frequency radiation
Characteristics
f = 30 MHz - 300 GHz λ = 10 m - 1 mm
300 GHz photon energy
h ν = k T = q
eV
=> 12 K , 1.25 mV
Sources cold matter .
Power detection limit
Minimum detectable noise power
T
sys.
∆ T
rms= sqrt (∆ ν T
int) Minimum flux density
∆ P .
∆ S = η B A
antSensitivity of a radio telescope
T
sys/ A
effJS/2006/oct/09
R&D Division
5(C) ASTRON 2006
What is an antenna
Conversion of guided waves in a transmission line to waves in free space
Concentrator of waves from specific directions
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R&D Division
7(C) ASTRON 2006
Wire antennas
Dipole
Loop antenna Helix antenna
X Y
Z
Horn antennas
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R&D Division
9(C) ASTRON 2006
Reciprocity in antennas
Identical behaviour for transmit and receive situations
I
+
V
-
energy
antenna 1 antenna 2 transmit
V
+ -
energy
Iantenna 1 antenna 2 receive
Antenna circuit substitution
+ -
V1I1
Receive and transmit antenna together form a two-port
+ -
V2 I2For a two-port we have:
V
1= Z
11I
1+ Z
12I
2V
2= Z
21I
1+ Z
22I
2Z
21= Z
12(reciprocity)
Z
22= Z
11for identical antennas
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R&D Division
11(C) ASTRON 2006
Antenna circuit substitution
Receive and transmit antenna together form a two-port
For a two-port we have:
V
1= Z
11I
1+ Z
12I
2V
2= Z
21I
1+ Z
22I
2Z
21= Z
12(reciprocity)
Z
22= Z
11for identical antennas
In this case: I
2<< I
1thus
V
1= Z
11I
1+ -
V1I1
+ -
V2 I2Antenna circuit substitution 2
I
1+
- V
1Z
22Z
21I
1I
2+
V
2+
- Z
11V
1= Z
11I
1V
2= Z
21I
1+ Z
22I
2transmit receive
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R&D Division
13(C) ASTRON 2006
Antenna circuit substitution 3
Z
antZ
load=Z
ant*V
openMaximum power is received in Z
loadwhen Z
loadcomplex conjugated to Z
ant(network theory)
Why does an antenna radiate ?
Maxwell equations
• Every alternating current creates Electric and Magnetic fields
But why no radiation from “ordinary” electronics ?• All currents run in closed loops
• The total current distribution can be split in many small line current segment
• For every current line segment there is an opposite
one of equal amplitude (red arrows)
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15(C) ASTRON 2006
Why does an antenna radiate ? 2
Compare the contribution of the two opposite line current segments far away from the antenna
• At low frequencies there is no phase difference
• The two opposite contributions cancel out
⇒
no radiation
At high frequencies there are two effects:
• Phase difference between the line current segments is significant
• Amplitude of the line current segments may differ
⇒
radiation
Current distribution on a dipole
Current distribution from a two wire (open)
transmission line
⇒ varying magnetic fields
⇒ EM fields
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R&D Division
17(C) ASTRON 2006
Dipole radiation principle
t=0
t=T/8 t=T/4=2/8 T
t=3/8 T t=T/2=4/8 T
t=T/4=2/8 T
Antenna field zones
• Reactive (near) zone
• E and H 90o out of phase
•
Average power radiated during one period close to zero• Energy storage in electric and magnetic fields
• Contributes to imaginary part of antenna impedance
• Radiating near zone (Fresnel zone)
• E and H field in phase
• Energy is radiated
• Radiating pattern strongly depends on distance
• Radiating far field (Fraunhofer zone)
φ
2φ
1∆φ=φ
2-φ
1Contributions from many line current segments. Phase differences between any two contributions depend strongly on distance.
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19(C) ASTRON 2006
Antenna field zones 2
• Reactive (near) zone
• Radiating near zone (Fresnel zone)
• Radiating far field (Fraunhofer zone)
• E and H field in phase
• Energy is radiated
• Radiating pattern does not strongly depend on distance
• E and H components perpendicular to direction of propagation
∆φ
→
E
→H
→
S
E and H-vectors perpendicularPoynting (E x H) vector indicates energy flow Ratio of |E| / |H| vectors is always 377 Ω (this is the free space wave impedance)
Antenna field zones 3
Near field
Far field
D
R=2D2/λ
R=0.62 sqrt(D3/λ)
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21(C) ASTRON 2006
Radiated power density
Unit: W / m 2
Isotropic radiator:
r
Spherical surface:
A=4πr
2Directivity
[W/sterad]
rad
0
P
) , ( 4 P
) , ( P
) , ( ) P
, (
D π θ φ
φ θ
φ φ θ
θ = =
P
0: reference antenna isotropic radiator:
.
1 ) ,
( θ φ = D
)
2, ( )
,
( W r
P θ φ = θ φ ⋅
π 4 P 0 = P rad
D
0= 1.5
= 1.8 dB
θ
Electric dipole radiation diagram
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23(C) ASTRON 2006
Efficiency, Gain
Losses in an antenna (Ohmic, dielectric) Definition of antenna gain:
[dBi]
Efficiency
0 dBd = 2.15 dBi
) , ( D )
, (
G θ ϕ = η θ ϕ
Radiation diagram
angle (deg)
θ
ϕ
Main lobe
Side lobes
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25(C) ASTRON 2006
Transmission line examples
Telegraph lines
Two-wire line
Coaxial cable
Microstrip
Transmission line examples
ground-layer below
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R&D Division
27(C) ASTRON 2006
Stripline
Transmission line examples
ground-plane on top and bottom
Wave guides
Transmission line examples
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29(C) ASTRON 2006
Electromagnetic fields in transmission lines
Transverse E and H fields
(perpendicular to direction of transport)
Poynting vector
→S = E
→× H
→Network approach to transmission lines
Substituting a short section
Equivalent schematic
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R&D Division
31(C) ASTRON 2006
x y x y f
x t f
z u c t z u g t
z i
t z i l t z i r t
z u
x t
t
∂
= ∂
∂ ∂
⋅
−
⋅
−
=
∂
∂
⋅
−
⋅
−
=
∂ ( , )
) , ( where )
, ( )
, ( )
, (
) , ( )
, ( )
, (
z z
Telegraphers’ equations:
Combining ...
2 2 2
2 2
2
2
( , )
) , ( where 0
) , ( )
, (
0 ) , ( )
, (
x y x y f
x t f
z i lc t z i
t z u lc t z u
x t
z
t z
∂
= ∂
= ∂
∂
−
∂
=
∂
−
∂
Solutions: travelling wave equations
• Functions f(z,t) = g(x-vt) and g(x+vt)
• Travelling waves in +z and -z direction
• Propagating with speed v
c v l
= 1 ⋅
Network approach to transmission lines
RF signals
Voltage and current equations
} )
( Re{
) , ( and } )
( Re{
) ,
( z t U z e
j ti z t I z e
j tu = ⋅
ω= ⋅
ωBack substitution ...
) ( ) ) (
(
) ( ) ) (
(
z U c j dz g
z dI
z I l j dz r
z dU
ω ω +
−
=
+
−
=
⇒(Lossy) wave equations:
) ( } }{
) { (
) ( } }{
) { (
2 2 2
z I c j g l j z r
I d
z U c j g l j dz r
z U d
ω ω
ω ω
+ +
=
+ +
=
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33(C) ASTRON 2006
RF signals 2 - lossy lines
( ) }
Re{
) ,
( z t U
0e
ze
j t zu
+=
+⋅
−α⋅
ω −β( ) }
Re{
) ,
( z t U
0e
ze
j t zu
−=
−⋅
α⋅
ω +βComplex coefficient
β α
ω ω
γ = ( r + j l )( g + j c ) = + j
Solutions
Wave in +z and -z direction
) , ( )
, ( )
,
( z t u z t u z t
u =
++
−RF signals 2 - lossy lines
( ) }
Re{
) ,
( z t U
0e
ze
j t zu
+=
+⋅
−α⋅
ω −β( ) }
Re{
) ,
( z t U
0e
ze
j t zu
−=
−⋅
α⋅
ω +β)
(compare c = λ ⋅ f Complex coefficient
β α
ω ω
γ = ( r + j l )( g + j c ) = + j
Solutions
Wave in +z and -z direction
2 ) and
2 (
ω π β π λ
ω β = ⋅ =
= f
v
z
z
e
e
−αand
+αPropagation speed Extinction
) , ( )
, ( )
,
( z t u z t u z t
u =
++
−JS/2006/oct/09
R&D Division
35(C) ASTRON 2006
Voltage / current relationship
Solution for i(z,t) similar to u(z,t)
Characteristic impedance
large
0
ω
ω ω
c l c
j g
l j
Z r ≈
+
= +
and
0 0 0
0 0
0
and
Z I U
Z I U
− −
+
=
+= −
( )
( ) } Re{
) , (
} Re{
) , (
0 0
z t j z
z t j z
e e
I t
z i
e e
I t
z i
β ω α
β ω α
+
−
−
−
−
− + +
⋅
⋅
=
⋅
⋅
=
Voltage / current / power relationship
) (
) (
0 0
n n n
n n n
b a Z i
b a Z u
−
=
+
=
0 0
0 0
Z Z i
b u
Z Z i
a u
n n
n
n n
n
⋅
−
=
=
⋅
=
=
− − + +
} 2 {
1
} 2 Re{
1
2 2
*
n n
n
n n n
b a
P
i u P
−
=
⋅
= Power waves
(n=1, 2)
port_1 port_2
a1 a2
b1 b2
<=>
⎟⎟ ⎞
⎜⎜ ⎛
⎥ ⎤
⎢ ⎡
⎟⎟ =
⎜⎜ ⎞
⎛ b
1S
11S
12a
1JS/2006/oct/09
R&D Division
37(C) ASTRON 2006
Reflections
Terminating with an impedance Z
LAt z = 0
On the transmission line
)
00 (
) 0
( Z
I
U
++=
At z=0
Z
LI U =
No reflection if ZL = Z0
Reflections 2
If Z
L≠ Z
0An U-(0) arises, fulfilling Ohm’s law at z=0
0
)
00 ( )
0
( Z Z
Z U Z
U
L L
+
⋅ −
=
+−
Reflection coefficient
0
)
00
( Z Z
Z Z
L L
+
= − Γ
Along the transmission line we have
e
zz ) ( 0 )
2γ( = Γ ⋅
Γ
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R&D Division
39(C) ASTRON 2006
Reflections 3
Lossless line
Complex Γ-plane 4 )
)
(0 ( )
( z e
j λ z⋅
πΓ
= Γ
Standing waves
• The voltage U(z) follows (with no loss)
| )
0 ( 1
|
| ) 0 (
|
| ) ( )
(
|
| ) (
| U z = U
+z + U
−z = U
+⋅ + Γ ⋅ e
2γz• The Voltage Standing Wave Ratio (VSWR) is
| ) 0 (
|
max
= 1 + Γ
= U VSWR
-L 0
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R&D Division
41(C) ASTRON 2006
Line impedance
Input impedance at location z
) ( 1
) ( 1
) (
) ) (
(
0z Z z
z I
z z V
Z − Γ
Γ
⋅ +
=
=
If z= λ/4 we have special behaviour
R Z
iZ
2
=
0Circuit characterisation
Two-port
+ Vs -
+ V1
-
+ V2 - ZS
ZL
I1 I2
Characterisation
• Signal amplification
• Frequency behaviour
• Noise behaviour
• Input impedance
• Output impedance
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R&D Division
43(C) ASTRON 2006
Gain
Signal power
Periodic (sinusoidal) RF signals
) cos(
|
| } Re{
) (
) cos(
|
| } Re{
) (
2 0
1 0
0 0
ϕ ω
ϕ ω
ω ω
+
=
⋅
=
+
=
⋅
=
t I
e I t
i
t V
e V t
v
t j
t j
Power
∫ ⋅ = ⋅ ⋅
∗=
Tv t i t dt V I P T
0
} 2 Re{
) 1 ( ) 1 (
Impedance matching
2 2
,
2 | |
Re
|
|
L S
L S
L
S
Z Z
Z P V
+
⋅
= ⋅
=
S∗L
Z
Z
ZS
ZL +
Vs - Source output power into ZL
Maximum when (available source power)
S S av
S
Z
P V
Re
|
| 8
1
2,
= ⋅
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R&D Division
45(C) ASTRON 2006
Power gain
in out
p
P
g = P
+ Vs -
+ V1
-
+ VO
- ZS
ZL
I1 I2
2 2
|
| 2
Re
|
|
in S
in S
in
Z Z
Z P V
+
⋅
= ⋅
Two-port with input and output impedances Z
inand Z
out2 2
|
| 2
Re
|
|
L out
L O
out
Z Z
Z P V
+
⋅
= ⋅
Input power
Output power
Gain
Power gain 2
Available power gain
Matching at in- and outputs
out S S
O av
in av out
av
Z
Z V
V P
g P
Re Re
|
|
|
|
2 2
,
,
= ⋅
=
+ Vs -
+ V1
-
+ VO
- ZS
ZL
I1 I2
out in
S
S in
O
Z Z
Z
Z Z
V V
Re
|
|
Re
|
|
|
|
|
|
2 2 2
1 2
⋅ +
⋅ ⋅
=
Z
s= Z
inZ
L= Z
outJS/2006/oct/09
R&D Division
47(C) ASTRON 2006
Logarithmic units
dB 110 dB
60 dB 50 10
10
5⋅
6⇒ + =
(dB) decibel log
10 10
in out
dB P
g = ⋅ P
• Decibel
(ref. Alexander Graham Bell) Large ranges of gainMultiplication becomes addition
( ) dBm mW
log 1
10
10⎟
⎠
⎜ ⎞
⎝
⋅ ⎛
= P
P
dBm• Absolute powers in decibel dBm: relative to 1 milli Watt
1 mW => 0 dBm 2 mW => 3 dBm 100 mW => 20 dBm
1 W => 30 dBm
dBi en dBc/Hz
• dBi
Antenna gain relative to isotropic transmitter
• dBc/Hz
Noise power per Hz of bandwidth
relative to the carrier
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49(C) ASTRON 2006
Noise
Many different origins
• Thermal noise, resistors and lossy materials
• Shot noise, from electron particle behaviour
• 1/f noise, in semi conductors
• Generation-recombination noise (semi conductors)
• Phase noise (oscillators)
Thermal noise
RN
ZL +
VN -
• Resistor noise, voltage V
N• With matching (ZL = RN) the noise dissipated in ZL
T
Rk f
G ( ) = ⋅
k Boltzman’s constant TR Resistor temperature
• Bandwidth limited noise power
Filter B = f
h-f
lG(f) N
Watt )
( f B k T B
G
N = ⋅ = ⋅
R⋅
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51(C) ASTRON 2006
Noise figure
x i
o
i o
N N g N
S g S
+
⋅
=
⋅
=
• Signal to Noise Ratio (SNR) deterioration in a two port
(S/N)
i(S/N)
oN
xg
i x i
x i i
o o
i
N g
N N
g
N N g N g
N N
S N F S
+ ⋅
⋅ = +
= ⋅
= ⋅
= 1
) / (
) / (
• Noise figure F
Ni at T = 290 K
Noise temperature
At a fixed bandwidth noise is represented as an equivalent temperature
k f G B
k
T
noiseN = ( )
= ⋅
Noise temperature with gain
N
iN
o=g.N
i+N
xT
xT
ig T
o=g.T
i+T
xN
xJS/2006/oct/09
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53(C) ASTRON 2006
Noise temperature of an amplifier
T
iT
o=g.T
i+T
xT
xg
Relate noise power back to the amplifier input
T
i+T
x/g T
o=g.(T
i+T
x/g)
thus
g T
NF= T
xNoise figure and noise temperature
0 0
1 1
1 T
T T
g T N
g
F N
x NFi
x
= +
+ ⋅
⋅ = +
=
)
01
( F T
T
NF= − ⋅
K 67 290 ) 1 23 , 1 ( 23
,
1 ⇒ = − ⋅ =
= T
NFF
Reference to the noise N
iat room temperature (T
0= 290 K)
For T
NFthis gives
• Example
• Example T
NF= 25 K
dB 36 , 0 086 , 290 1
1 + 25 = =
F =
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55(C) ASTRON 2006
Cascading
⋅
⋅
⋅
⋅
⋅ + +
+
=
2 1
3 1
2
1
g g
T g
T T T
CA series of amplifiers
T
1g
1T
2g
2T
3g
3Refer back to the input of the chain (Friis’ equation)
⋅
⋅
⋅
⋅
⋅ + + ⋅
+ ⋅ +
= +
=
0 2 1
3 0
1 2 0
1 0
1
1 g g T
T T
g T T
T T
F
CT
C+8
Smith chart
Line impedance Reflection coefficient
Combine the two ?
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57(C) ASTRON 2006
Deduction
Normalise
0
0
Z
j X Z
x R j r
z = + = +
Position in Γ-plane
z z
z
and z
z z
Γ
− Γ
= + +
= −
Γ 1
1 1
1
• Biliniar transformation
• one-to-one
• can be inverted
• circles become circles
• direction and left/ right maintained
Example: impedance transformation
Six steps
1. Normalise Z
Lby Z
02. Determine position in Smith chart 3. Line from origin to z
Lrepresents Γ
04. Rotate Γ
0over -2βl
5. Read back Γ(-L) and z(-L)
6. Denormalise by Z
0 (=> Z(-L))JS/2006/oct/09
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59(C) ASTRON 2006
Example 6.1: impedance transformation
• ZL = 100 + j 50 Ω
• Z0 = 50 Ω
• f = 2,5 GHz
• L = 2 cm
• εr = 3,5 (thus v < light speed, v= c/√εr = 1,6 108 m/s )
• Step 1
j j
z
L= + = 2 + 50
50 100
Example 6.1 (continued)
• Step 2: see figure
• Step 3
|Γ0| = 0,46 Arg(Γ0) = 26.6o
• Step 4
-2βL = -224.5o
• Step 5
z(-L) = 0,38 + 0,14 j
5 2
4
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61(C) ASTRON 2006
Example 6.1: impedance transformation
• ZL = 100 + j 50 Ω
• Z0 = 50 Ω
• f = 2,5 GHz
• L = 2 cm
• εr = 3,5 (thus v < light speed, v= c/√εr = 1,6 108 m/s )
• Step 6
Z(-L) = 18,9 + 6.8 j Ω
Useful tools
Smith.exe
http://www.hta-be.bfh.ch/~wwwel/projekte/cae/
Pasan (by Marien van Westen)
http://members.home.nl/mvanwesten/
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63(C) ASTRON 2006
Two-port characterisation
Relate V1, V2, I1 and I2
Admittance matrix
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⎥ ⎛
⎦
⎢ ⎤
⎣
= ⎡
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⇒ ⎛
⋅
=
2 1 22
21
12 11
2
1
V Y
I V
V Y
Y
Y Y
I I
Two-port
Two-port characterisation 2
Relate V1, V2, I1 and I2
Admittance matrix
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⎥ ⎛
⎦
⎢ ⎤
⎣
= ⎡
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⇒ ⎛
⋅
=
2 1 22
21
12 11
2
1
V Y
I V
V Y
Y
Y Y
I I
Two-port
Impedance matrix
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⎥ ⎛
⎦
⎢ ⎤
⎣
= ⎡
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⇒ ⎛
⋅
=
2 1 22
21
12 11
2
1
I Z
V I
I Z
Z
Z Z
V
V
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65(C) ASTRON 2006
Two-port characterisation 3
Transmission ABCD-matrix
for cascading
⎟⎟⎠
⎜⎜ ⎞
⎝
⎥⎛
⎦
⎢ ⎤
⎣
=⎡
⎟⎟⎠
⎜⎜ ⎞
⎝
⎟⎟ ⎛
⎠
⎜⎜ ⎞
⎝
⎥⎛
⎦
⎢ ⎤
⎣
=⎡
⎟⎟⎠
⎜⎜ ⎞
⎝
⎛
3 3 2 2
2 2 2
2 2
2 1 1
1 1 1
1 and
I V D C
B A I
V I
V D C
B A I
V
⎟ ⎠
⎜ ⎞
⎝
⎥⎦ ⎛
⎢⎣ ⎤
⎥⎦ ⎡
⎢⎣ ⎤
= ⎡
⎟ ⎠
⎜ ⎞
⎝
⎛
3 3 2
2
2 2
1 1
1 1
1 1
I V D
C
B A
D C
B A I
V
Two-port characterisation 4
Relating ABCD and impedance matrices
( ) ⎥
⎦
⎢ ⎤
⎣
= ⎡
⎥ ⎦
⎢ ⎤
⎣
⎡
21 22
21
21 21
11
1
det
Z Z
Z
Z Z
Z D
C
B
A Z
Where det(Z) is the determinant
( )
11 22 12 21det Z = Z Z − Z Z
JS/2006/oct/09
R&D Division
67(C) ASTRON 2006
Two-port characterisation 5
S-parameter matrix
• At high frequencies V and I can not be measured near two-port
• We can measure V
+(z) and V
-(z)
• Determine amplitude and phase at some reference plane
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⎥⎦ ⎛
⎢⎣ ⎤
= ⎡
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⎛
+ +
−
−
2 1 22
21
12 11
2 1
V V S
S
S S
V V
ref.
plane_1 ref.
plane_2
port_1 port_2
Two-port characterisation 5
S-parameter matrix
• At high frequencies V and I can not be measured near two-port
• We can measure V
+(z) and V
-(z)
• Determine amplitude and phase at some reference plane
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⎥⎦ ⎛
⎢⎣ ⎤
= ⎡
⎟⎟ ⎠
⎜⎜ ⎞
⎝
⎛
+ +
−
−
12 1
1 11
V
S S
S V S
ref.
plane_1 ref.
plane_2
port_1 port_2
S11 Reflection at the input S21 Forward transmission S12 Backward transmission Ref. sheet 68-32, Voltage/
current/ Power relationship
JS/2006/oct/09
R&D Division
69(C) ASTRON 2006
Example S-parameter matrix
Through connection
1 2
⎥ ⎦
⎢ ⎤
⎣
= ⎡
1 0
0 S 1
Amplifier
1 A 2
⎥ ⎦
⎢ ⎤
⎣
= ⎡
0 0
0 S A
Isolator (open)
1 2
⎥ ⎦
⎢ ⎤
⎣
= ⎡
0 0
0 S 1
Passive filter (R, L and C)
1 H(ω) 2
⎥ ⎦
⎢ ⎤
⎣
⎡
=
) ( 0
0 )
(
ω ω
H H
S
S-parameter matrix measurement
ref.
plane_1
port_1 requested ref.plane_1
ref.
plane_1 port_2
requested ref.plane_2
j k
Vk
j i
ij
V
S V
+= ∀ ≠
−
=
+, 0
Network analyser
S
11• V1+ input on port 1
• measure V1- (reflected wave)
• Keep V2+ null (Z0 terminated)
From S we can determine
Z
andY
JS/2006/oct/09
R&D Division
71(C) ASTRON 2006
Reference plane and calibration
• Requested planes of reference
E.g. in- and output of the LNA (near the circuit)
• Practical reference planes
Connectors of Network Analyser
Interconnected with stable transmission lines
• Calibrate NWA at practical planes of reference
Using calibration kit references screwed directly on the cables Choose correct calibration procedure
• Check if calibration was successful Using calibration kit standards
Possibly measuring a (known) test impedance
• Repeat calibration often (to counter variability)
S-parameter matrix measurement
• Connect two port to practical planes of reference and measure
• Transform to requested planes of reference (de-embedding)
⎥ ⎦
⎢ ⎤
⎣
= ⎡
m mm m
S S
S S
22 21
12 11
S
m⎥ ⎦
⎢ ⎤
⎣
⎥ ⎡
⎦
⎢ ⎤
⎣
⎥ ⎡
⎦
⎢ ⎤
⎣
= ⎡
⎥⎦ ⎤
⎢⎣ ⎡
β β
β β
2 1
2 1
0
0 0
0
22 21
12 11
22 21
12 11
jl jl
m m
m m
jl jl
e e
S S
S S
e e
S S
S S
• Network Analyser does this automatically after calibration
JS/2006/oct/09
R&D Division
73(C) ASTRON 2006
Practical assignment
Measuring using a Spectrum Analyser and a noise source
Measure with a Network Analyser
Determining S
11of an unkown impedance
www.astron.nl
The end
Acknowledgement:
P. de Vrijer, M. Arts, W. v. Cappellen, R. Halfwerk, J.G. bij de Vaate, M. Bentum, D. Kant, J. Hamakers, J. Bregman, B. Woestenburg
JS/2006/oct/09
R&D Division
75(C) ASTRON 2006
Literature
David M. Pozar; (Wiley 2005) Microwave engineering
C.R. Kitchin; (Taylor and Francis Group 2003) Astrophysical Techniques A.R. Thompson, J.M. Moran, G.W. Swenson Jr.; (Wiley 2004) Interferometry and Synthesis in Radio Astronomy
Web-books:
S. J. Orfanidis; Electromagnetic Waves and Antennas(802 pgs.) ECE Department, Rutgers University
http://www.ece.rutgers.edu/~orfanidi/ewa
D. Fisher; Basics of Radio Astronomy, for the Goldstone-Apple Valley Radio Telescope(91 pgs.)
Jet Propulsion Laboratory, JPL D-13835 (apr 1998) California Institute of Technology http://www.jpl.nasa.gov/radioastronomy
S. Mauch; Introduction to Methods of Applied Mathematics, or, Advanced Mathematical Methods for Scientists and Engineers(2321 pgs.)
CalTech 2004)
http://www.its.caltech.edu/˜sean