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NOISE DIODE CONFIGURATION

This chooses which noise diode configuration you wish to use when calling the ``cal" commands. One of the high cals is often a good choice, although if you are unsure of which diode to use you should consult with your Friend of the Telescope. Additionally, it should be noted that not all receivers have the choice of all configurations. If you choose a noise diode configuration which is not available for a given receiver, your request will be ignored and you will instead end up with the default setting for that receiver. The list of choices is given below, and the availability is listed in Table 4.

Description:
nocal: run no calibration scans. This saves time but is rarely a good idea
lcal: low uncorrelated cal. diodes A,B straight through (D1$\rightarrow$Pol A, D2$\rightarrow$Pol B)
hcal: high uncorrelated cal. diodes A,B straight through (D1$\rightarrow$Pol A, D2$\rightarrow$Pol B)
lxcal: low uncorrelated cal. diodes A,B with crossover (D2$\rightarrow$Pol A, D1$\rightarrow$Pol B)
hxcal: high uncorrelated cal. diodes A,B with crossover (D2$\rightarrow$Pol A, D1$\rightarrow$Pol B)
l90cal: low correlated cal with 90 deg phase shift (D2+90$^\circ$$\rightarrow$Pol A, D2$\rightarrow$Pol B)
h90cal: high correlated cal with 90 deg phase shift (D2+90$^\circ$$\rightarrow$Pol A, D2$\rightarrow$Pol B)
lcorcal: low correlated cal with 0 deg phase shift (D1$\rightarrow$Pol A, D1$\rightarrow$Pol B)
hcorcal: high correlated cal with 0 deg phase shift (D1$\rightarrow$Pol A, D1$\rightarrow$Pol B)
Here, D1 is noise diode 1 and D2 is noise diode 2. The diode values can be found both in the telescope control room (ask the operator on duty for the book) or on the web sites of the individual receivers.


Table 4: Noise Diode Options
RECEIVER
Lamp 327 430 610 LBN LBW SB SBW CB XB
nocal X X X X X X X X X
lcal   X   X X   X X X
hcal   X     X   X X X
lxcal   X     X   X X X
hxcal   X     X   X X X
l90cal   X     X   X X X
h90cal   X     X   X X X
lcorcal   X X   X X X X X
hcorcal X X     X   X X X


next up previous
Next: THE RADAR BLANKER Up: Spectral-Line Observing at AO Previous: INTEGRATION TIME (per Data
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