Computing the cal values
june 2005
The cal values are normally measured using the
sky/absorber
technique. The data taking setup is normally 25Mhz*4 bands
of 256 lags each. Do 3 seconds calOn followed by 3 seconds calOff. Then
step the band by 100 Mhz until the entire receiver band is done. Cycle
through the receiver band N times. For the high correlated cal (hcorcal)
do this on the absorber and while tracking blank sky. For the other
cals (huncor, h90, hxcal, lcor, luncor, l90, lxcal) track blank sky
and perform the sequence:
hcor, huncor, hxcal, h90cal, hcor,
lcor, luncor, lxcal, l90cal, hcor
At each step do a 3 second calOn, and 3 second caloff. After the 10
steps, increment the frequency by 100 Mhz and continue. Make N complete
passes through the receiver. At each step you can measure (calOncalOff)/caloff
(call it calRatio). You then take the ratio of calRatioOther/calRatioHcorcal.
In case the gain is drifting, interpolate hcor to each of the other
cals. We can then multiply by hcorcal in kelvins to the the other cals
in kelvins.
When processing the data we need to use the values:

Trcvr This gets measured on the antenna test range.

Tsky We ask a smart astronomer (and hope it's not raining..)

Tabs We measure the absorber temperature with a thermometer.

Tscattered The stuff scattered into the receiver (not from the main
beam). We will measure a cal value from the Sky, the absorber, and the
ratio of sky,absorber (Y factor). We can adjust Tscattered so that the
cal value from the sky agrees with the cal Value from the absorber and
the Y factor.
The data reduction has been done in two ways.

Computing a single value for each 25 Mhz band (up to jun05)

Computing the spectrum of calOncaloff/caloff for the entire receiver band
and then fitting it all at once.
The two methods are described below.
Averaging over each 25 Mhz band
(old method):
This has been used up to jun05 on all receivers. The
steps are:

Compute (calOncalOff)/calOff (calRatio) for each spectra (normally
25 Mhz). This removes the IF bandpass.

Compute the median value of calRatio over each 25 Mhz bandpass.

Normally the receiver band is covered N times. This gives N values for
calRatio
at
each 25 Mhz band. Compute a robust mean of these N duplicate values of
calRatio.

We've done the computation on the sky (calRsky) and on the absorber
(calRAbs). Using calRsky and calRabs we can then eliminate
Trcvr
from the equation to get:
calK = (Tsky + Tscattered  Tabs)*(calRAbs*calRSky)/(calRabscalRSky)
(see sky/absorber
technique for more info). This cal value uses the Y factor
so call it calK_Y.

It is also possible to measure the cals using just the absorber or just
the sky if you know the receiver temperature (and you assume the reflection
coef in the receiver is small). This gives you calK_abs and calK_sky. These
values can be plotted with calK_Y for comparison. You can adjust Tscattered
so that the Tcal_sky agrees with the TcalK_Y and _abs.

calK_Y can then be fit by a low order polynomial (say 3rd or 4th).
The online Tsys monitor and idl use a lookup table of cal values for processing.
In this case the polynomial is then sampled every 25 Mhz and stored in
the table.
The sky/absorber is done only for the high correlated
cal (you'd never see the low cals on the 300K absorber). The other cals
are measured relative to the hcorcal while tracking blank sky. The steps
1,2,3 are the same (except that we use calRatioOther/calRatioHcorcal. Multiplying
the ratio of calRatioOther/CalRatioHcorcal * hcorCalK gives the other cals
in kelvins. The values are then fit to a low order polynomial and sampled
at 25 Mhz for storage in the lookup table.
Fitting to the entire receiver
band at once (new method):
The above method has some troubles:

Compute (calOncalOff)/calOff (calRatio) for each spectra (normally
25 Mhz). This removes the IF bandpass.

For each of the N passes through the receiver band , make 1 large
spectra of calRatio. Take these N spectra and do a robust average
(averaging the N values at each channel).

Using the average spectra of the entire receiver band, fit a low order
polynomial (typically 1st) and an M order harmonic function. M is
determined by the ripples in the cal and the bandwidth of the data.
The routine corblauto()
is
used for the fitting. It will iterate the fit throwing out outliers and
then refitting.

The fits can now be used to compute the CalK with:
calK = (Tsky + Tscattered  Tabs)*(calRAbs*calRSky)/(calRabscalRSky)
CalRabs and CalRSky now come from the fits rather than the data.
This gives a function for the Hcorcal in degrees
K. The other cals are relative to the hcorcal.

For each setting compute calRatioX/calRatioHcorcal. Interpolate calRatioHcorcal
to the position of each of each calRatioX measurement. This gives a spectra
of each cal relative to the hcorcal.

For each pass through the data make a single spectra of calRatioX/calRatioHcorcal.

Multiply the spectra in 2 by the hcorcal function in kelvins. This gives
the calX in kelvins.

Do a robust average of the N passes through the receiver.

Now fit the average with a low order polynomial (1st order) and an M order
harmonic function. This will be the calX value in kelvins.

Sample the other cals at whatever looks reasonable and store them in the
lookup table.
The full band fitting procedure
does a better job of interpolating across rfi. The problemw will be:

whether the fitting functions do a good job of modeling the data. For lbw
they did.

Tsys changes while we track across the dish: in za and somewhat in azimuth.
The caldeflection/Tsys is an average of these values. To keep this to a
minimum we keep the za below 15 degrees when doing the measurements (this
problem also occurs in the old method where we average across each
25mhz band).
We are dividing (caloncalOff)/caloff. The 1
Mhz standing waves are not in caloncaloff and the are in caloff so the
functions that are being fit include the 1 Mhz standing wave. The order
of the fits used do not fit this 1 Mhz ripple. This is correct since
we are trying to measure the cal value which should not include the ripple.
When computing the fit residuals, the rms's do not decrease as 1/sqrt(b*Tau)
because of the 1 Mhz ripple (at least not while on the sky).
home_~phil