Calibration You never know – it might be important.
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Transcript of Calibration You never know – it might be important.
![Page 1: Calibration You never know – it might be important.](https://reader036.fdocuments.us/reader036/viewer/2022070413/5697bff61a28abf838cbe1ef/html5/thumbnails/1.jpg)
Calibration You never know – it might be important.
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Flux density : 1 Jansky = 10-26 W/m2/Hz
Pr = ½ Aeff S d(Aeff:= collecting area, S:=flux density)
Pc = kTref d
kTA = ½ Aeff.S
Tsys = TA + Tspill + Tsky + Trx
Equivalent noise temperature
Pr
Pc
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What are we measuring?
• Typical receiver systems have large gain which varies with time.
Abandon detected power for calibration: use only equivalent noise temperatures.
~100dB
( )2Sampler
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The noise equation
Tsys = TA + Tspill + Tsky + Trx + T2.7K
Atmospheric“seeing”
Time, temp etc
kTA = ½ Aeff.S
Elevation
Position on sky
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NAR – noise-addingradiometerJargon:
“noise tube”
=“noise diode”
=“noise source”
=“cal”
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A real receiver …
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Antenna gain
kTA = ½ Aeff.S
TA /S =1/2k . Aeff
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Bandpass calibration
Calibrate bandpass by observing “off source”
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Interferometers…. at last
• Single dish : amplitude (vs frequency)
• Interferometer– Amplitude (but no large DC term)– Phase– Delay (phase vs frequency)
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ATCA calibration practice
• Fiducial calibrator (delays, amplitude)
once per ~12 hour observation
• Secondary calibrators (phase, amplitude)once per 10 minutes ~ 2 hours
linear interpolation of amp, phase
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Atmosphere Ionosphere dominant < ~3 GHz , ~ eutral atmosphere , ~ ”Outer-scale” ~ 30km
nstrumental effects
Phase errors
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• Measured visibility vs true visibility:
• Assume errors small:
Interferometer calibration
j*
i ijij G GV V
) (1 Gj jj i )( 1 G G *
j i jiji i
Real = amplitudePerfect response Imaginary=phase
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Image distortion
Amplitude errors(symmetric)
Phase errors (antisymmetric)
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Self-calibration
• Standard calibration : image quality ~100:1
• Self-calibration:Gi : N complex gains
N*(N-1)/2 visibilities (complex constraints)
Can solve for the Gi
Image quality >> 1000:1
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More to think about
• Self-calibration• Polarization calibration: online XY phases• Spectral-line (bandpass) calibration• Data flagging/editing• Absolute flux calibration• Pointing calibration• RFI• Astrometry (milli-arcsecond positions)