ATCA synthesis workshop - May 20031 ATCA – Calibration at mm wavelengths Rick Forster University...
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![Page 1: ATCA synthesis workshop - May 20031 ATCA – Calibration at mm wavelengths Rick Forster University of California, Berkeley Hat Creek Radio Observatory Berkeley-Illinois-Maryland.](https://reader036.fdocuments.net/reader036/viewer/2022081514/56649ead5503460f94bb464f/html5/thumbnails/1.jpg)
ATCA synthesis workshop - May 2003
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ATCA – Calibration at mm wavelengths
Rick Forster University of California, Berkeley
Hat Creek Radio Observatory
Berkeley-Illinois-Maryland Association
Topics: Basics of interferometry
The atmosphere
Amplitude & phase calibration
Atmospheric & instrumental effects
Antenna effects
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L 20 1.5 0.19 33
S 13 2.3 0.24 22
C 6 5.6 0.22 10
X 3 8.6 0.21 5
K 1.2 20.5 0.53 2
W 0.35 87.5 2.70 0.6
Band cm GHz mJy/b beam
ATCA Bands
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V2 or the total output power is TSYS = TR + TSKY + TA K
(100+200+.04 K)
Brightness B = 2k TB/2 W/Hz m2
Flux density S = B d W/Hz m-2 Effective area Aeff = D2 m2
A few definitions
Janskys/K S/TA = 3510/D2 Jy/K
V(volts)
Received power VA2 = Aeff S Watts
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Tsys – ‘Paddle’ or Chopper Wheel method
s
~RF
LOG PB Sampler Delay
IF
Digitized IF (V)
Amb
Sky
Tsys sets the flux scale and the noise level!
Tsys = Tamb - Tsky
V2amb – V2sky( ) V2sky -Tsky
n
)
= sin-1(n/s)
s
n=0.2 Jy = sin-1(0.2) ~ 12o
n = 2 k Tsys
Jy
tbw
Tsys=300 KA=380 m2
bw=128 MHz=0.3
t=10 sec
k=1380 Jy m2/K
TambTskyTsys
V2
T
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Basic Interferometry
_g = B sx
B_s
g = geometrical delay
correlation coefficient =Ny–Nn
N
Tsys = system temperature
Tant = antenna temperature
Ant 1
Ant 2
Correlator
1x2
Digitized IF from two antennas
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Tsys ~ 200 KJy/K ~ 150
~ 5 10-4
S = Tsys Jy/K ~ 15 Jy
Cor
rela
tion
Coe
ffie
ient
Am
pl (
Jy)
& P
hase
64 lag channels (+/- 32)
32 freq channels (amp & pha)
FourierTransform
V = Aei
Visibility
Correlation Function
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Atmosphere
Tsky = Tatm (1-e-)
TA = Tsou ( e-)
Tsys = TR+Tsky+TA
Tsys = TR+Tatm(1-e-)+Tsou(e-)
T’sys = TRe+Tatm(e-1)+Tsou
delay absorption
T’sys = Tsyse
Lay, 1997
for = 1, e= 2.7
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Opacity of the Atmosphere – O2 & H2O
H2O
O2
50-70 GHz
O2
118 GHz
H2O180-190
GHz
H2O
22 GHz
Frequency (GHz)50 100 150
O2
84.9-87.3H42
SOSiO 88.5-91.3
HCNHCO+
CH3OH
HC3N
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Log time
Pow
er d
ensi
ty
30 sec3 hrs
10 min
D
Log
Log Distance (D)
D saturation
= 1.0 (Gaussian)
= 5/6 (Kolmogorov)
= 1/2 (Lorentzian)
Structure Function ( vs D)
“Frozen Turbulence” Model ( power vs t)
= 5/6, 1km layer, 5km/s wind, 500m D
Longer baselines shifts peak rightStronger winds shifts peak left
Lay, 1997
Butler & Desai, 1999
~ 0
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M87 data calibrated with 3C273Amplitude Phase
80m
45m
15m
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Baseline Solution – C-array, March 2003Phases BEFORE Correction Phases AFTER Correction
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Absolute flux calibration Test source
MWC 349 (HII)
0909+013 (QSO)1310+323 (QSO)
cal
source
test
Use a test source to help quantify the effects of
atmospheric decorrelation in the image plane.
Use a primary flux calibrator (planet or HII region) to check the value of Jy/K.
Use your phase calibrator to monitor temporal gain changes.
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Passband – 32 visibility channels over 100 MHz
Channel BW = 3.125 MHz (~11 km/s)
n = 2 k Tsys
Jy
tbw
k = 1380 Jy m2/KTsys = 560 KA = 28 m2
= ac = .70x.88 = .61bw = 100/32 = 3.125 MHzt = 6m = 360 s
n = 2.6 Jy (each 11 km/s channel)
s/n = 12/2.6 ~ 4.6phase noise ~ 11 deg
4 MHz = 14 km/s 64ch = 0.2 km/s
At 0.2 km/s channeln = 8x2.6 ~ 21 Jy
(ave 100 MHz ~ 6 times better)
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30 min
Az
El
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A few final suggestions
Calibrate Tsys often Check Jy/K on a flux cal Mosaic sources larger than ½ fwhm Use offset pointing for extended sources In a pinch total power correction might help Choose nearby calibrator if baseline is uncertain Choose integration time so S/N > 5 on calibrator Use a guest calibrator to gauge atmospheric effects Don’t push your observations beyond the seeing limit Avoid unnecessary PB calibration, & check sensitivity Monitor the atmosphere – abort 3mm in severe conditions Fast-switching might be worth a try in reasonable conditions
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