Lbw cal values measured 22apr07
25apr07
Links to PLOTS:
hcorcal:
Fits
to the Average CalDeflection/Tsys (.ps) (.pdf):
Hcorcal
in kelvins (.ps) (.pdf).
diagnostics:
CalDeflection/Tsys
for the individual passes (.ps) (.pdf).
Fits
to the CalDeflection/Tsys for the individual passes (.ps) (.pdf).
othercals
The
average calValues in kelvins and the fits (.ps) (.pdf):
Over
plotting all of the cals (in deg K) (.ps) (.pdf).
diagnostics:
CalDeflectionCalX/calDeflectionHcorcal
for the 7 passes (.ps) (.pdf)
Fits
to the CalDeflX/calHcorcalDefl for the 7 passes (.ps) (.pdf).
Over
plotting the new and old cal values (.ps) (.pdf).
Links to SECTIONS:
Why the cals were remeasured.
Measuring the high correlated cal using
blank sky and absorber
Measuring the other cals on blank sky
relative to the high correlated cal.
Why the cals were
remeasured.
A resonance
had appeared in polA at 1400 Mhz after the jun05 dewar warmup. The
dewar was brought down to the lab in mar07 and the bolts on the omt
were tightened.
Measuring the high
correlated
cal using sky and absorber: (top)
The high correlated cal value (diode 1 going
to
polA and polB) for lband wide was measured 22apr07 and 23apr07 on the
telescope using
the sky/absorber
technique.
The sky observations tracked blank sky on 22apr07 starting at 17:45.
There was light
rain while these observations were made. The absorber measurements were
done on 23apr07 at 11:30.
The observations used 3 second calon followed by 3 second cal off. For
the sky observations, blank sky was tracked. In both cases (sky and
absorber) the lbw filter bank was used. The radar blanker was not used
since the painting project
caused the antenna to be removed.
The temperatures used in the computation were:
Tabsorber |
298 K |
Tsky |
5 K |
Treceiver |
from test shack feb03 |
Tscattered |
15 K |
The band 1120 to 1720 Mhz was covered 9 times on
absorber and 9 times on sky. The ratio (CalOn-CalOff)/CallOff was then
computed for the data. Each spectra of 600 Mhz (6144 points) was then
fit
to an 8th order harmonic and 1st order polynomial (the order was chosen
to include the ripples in the caldefl/Tsys spectra). The fit was
iterated
throwing out points whose residuals were greater than 3 sigma .
Whenever
a point was excluded, 5 points adjacent to the fit were also excluded .
A robust average of the 9 passes was
computed (iterating and throwing out outliers). The average spectra was
then fit with the same function. See reducing
the cal data for more info on the reduction.
The results of the reduction are:
-
Fits
to the Average CalDeflection/Tsys (.ps) (.pdf):
This shows the average Tcal/Tsys data with the fits over plotted in
red.
The top two plots are on the absorber (polA,polB) while the
bottom
two plots are on the sky. The averages were made from the 9
passes
through the frequency band. The units are Tsys (about 30K for sky
and 300 K for absorber). The fitRms is computed for the fraction of the
spectra used in fitting. The rms and fraction of spectrum used are
printed
on each plot. The radiometer equation should give:
rms=sqrt(2ratio)./sqrt(25e6bw/256chan*3secs*9loops*2hanning)=.0006
The absorber fits match this. The sky fits are about 6 time larger.
This
is because the fits are not fitting the 1 Mhz standing wave from the
dish.
This is ok since that ripple should not be in the cal value anyway.
- The Hcorcal
in kelvins (.ps) (.pdf).
-
The first two plots show the cal fits in kelvins measured from the Sky,
absorber, and the sky, absorber ratio (Y factor). The top plot is polA,
the middle plot is polB. The dashed line is the receiver temperature
used
for calSky.
- The calAbs and calY agree while the calSky is
different. The calsky Dc level can be shifted up or down by changing
the amount of Tscattered.
- Around 1300 Mhz Tcal absorber has a negative going bump. Tcal
sky polB and both Tcal sky and absorber polA have a positive going bump
here.
- The Trcvr curve will have the largest affect on Calsky.
-
The bottom plot is the cal In kelvins from the Y factor. The * are
spaced
every 10 Mhz. PolA is black and polB is red. These are the values that
will be used for the cal.
Diagnostics:
The first set of plots show the calOn-caloff/caloff
for each pass through the data. The second set over plots the fits to
each
pass to see how stable the system is.
-
CalDeflection/Tsys
for the 9 passes thru the frequency band (.ps) (.pdf).
-
The first page shows on absorber for the 9 passes through the
receiver
band. The top plot is polA while the bottom plot is polB. The spectra
have
been offset for plotting purposes. The units are Tsys (on absorber it
is
about 300K). The dashed vertical line shows the start of each 100 Mhz
integration
(4sbc*25Mhz each). The 1270/1290 birdies that are coming through are
from the
remy radar.
-
The second page shows on the sky for the 9 passes through
the receiver band. The top plot is polA while the bottom plot is polB.
The spectra have been offset for plotting purposes. The units are Tsys
(about 30K on the sky). The dashed lines show the 100 Mhz boundaries
(that
were taken separately). The birdie around 1240/1260 are the aerostat
radar and the punta salinas radar.
-
Fits
to the CalDeflection/Tsys for the 9 passes thru the frequency band (.ps)
(.pdf).
This over plots the fits to each pass (6144 points covering the
600
Mhz.). The absorber fits vary by more than the Sky fits since deltaTsys
is a larger fraction of the cal when you are on absorber.
processing:
x101/lb/cals/apr07/hcorcal/lbwinp.pro,lbwfit.pro,lbwcmp.pro,lbwplot.pro
Measuring the other
cals using sky and the high correlated cal (top)
The high correlated cal was measured (see above)
using
sky and absorber as the hot and cold load. The other cals were then
measured
relative to the high correlated cal on 22apr07 starting around 16:15.
Blank
sky was tracked, the filter bank was used, the radar blanker was not
used,
and the following cal sequence was run:
-
hcorcal(on,off)
-
hcal(on,off),hxcal(on,off),h90cal(on,off)
-
hcorcal(on,off)
-
lcorcal(on,off),lcal(on,off),lxcal(on,off),l90cal(on,off)
-
hcorcal(on,off)
100 Mhz at a time was measured (4 by 25Mhz) going
from
1120 to 1720 Mhz. The cal was cycled on/off for 3 secs at each
step.
The entire frequency range was repeated 6 times.
The ratio (calOnX-calOffX)/caloffX was computed
(X is the other cals) and then it was divided by
(calOnHcor-calOffHcor)/calOffHcor).
A spectrum for the entire pass was then constructed of the other cals
relative
to the hcorcal. The spectral fits for the 6 passes were averaged. The
average
spectra was multiplied by the hcorCal value in kelvins (this
removed
the hcorCal shape). The resulting spectra was fit with an 8th order
harmonic
and 1st order polynomial. For more info see
computing the cal value.
The results of the reduction are:
-
The
average calValues in kelvins and the fits (.ps) (.pdf):
The fits to the 6 passes have been averaged together and then
multiplied
by the hcorcal fit (in kelvins). There are 14 plots. 7 cals each with
polA
and polB. The red lines are the fits to the data. The fit rms's are
better
than 1% over the full band.
- Over
plotting all of the cals (in deg K) (.ps) (.pdf).
The top plot is the high cals and the bottom plot is the low cals. The
solid lines are polA while the dashed lines are polB. There are two
sets
of lines that follow each other. That is because the same diode always
feeds two types of cals (e.g. diode1 goes to polA for hcorcal and for
huncorcal). Diode 2 --> polB has a large frequency dependance across
the band. After taking the data we found a bad relay in the cal
switching box that could cause this (we need to fix it and then after
the painting project remeasure the cals).
Diagnostics:
-
CalDeflectionCalX/calDeflectionHcorcal
for the 6 passes (.ps) (.pdf).
There is 1 page for each calType (7 pages). The top plot is polA and
the
bottom plot is polB. The 6 passes through the freq range are over
plotted
with an offset. The units for the y axis are TcalHcorcal since each of
the cal deflections have been divided by the hcorcal deflection.
-
Fits
to the CalDeflX/calHcorcalDefl for the 6 passes (.ps) (.pdf).
This over plots the fits to each pass (6144 points covering the
600
Mhz.).
-
Over
plotting the new and old cal values (.ps) (.pdf).
The solid lines are the new cals. The dash lines are the old cal
values.
The plots are:
-
Top HiCalsPolA: black Diode1 -> polA, Red diode2->polA.
-
2nd HiCalsPolB: black Diode1->polB, Red diode2->polB
-
3rd LoCalsPolA: black Diode1 -> polA, Red diode2->polA.
-
4th LoCalsPolB: black Diode1->polB, Red diode2->polB
The 2nd and 4th plots show diodes going to polB. The new cal
values (solid lines) are about 25% larger than the old cal values
(dashed
lines). When the cable in the dewar was tightened, more cal would get
to
the receiver.
The 1 and 3rd plots show diodes going to polA. These agree until you
get to 1500 Mhz where they start to diverge. The new cal values have
less
power than the old cal values. This same trend was seen back in
23feb06.
The cal values of 23feb06 polA had more power at high freq (gt 1500
Mhz)
than the cal values from 24Nov05 (when these diodes were installed).
processing:
x101/lb/cals/apr07/othercals/lbwinp.pro,lbwcmp.pro,lbwfit.pro,lbwplot.pro
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