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In this wiki we aim to create a guide of the info displayed by the different monitors running at the telescope. The monitors Mopsic Monitor, and MonCoo must be running always at the telescope. The only exception is in case of maintenance time, when the version of mopsic can be changed, or doing Absorber measurements with MAMBO2 in stow position (in which case the mopsic monitor must be replaced by the MonInst monitor).

It is recommended to have a look to the plots prior to reading the explanation, and try to understand them, in order to get a more fluent training in the monitors.


This monitor displays and reduces all the observations of the bolometer MAMBO2 and continuum data from heterodyne receivers. The vncviewer port of this monitor is the 27.

Information displayed

General Info


This figure shows the normal display of the monitor.

From this snapshot we can see that the last pointing was done on G34.3, using the bands E1 and E3, at freq. 173.507GHz and 267.557 GH, 2160 seconds ago, the scan was the 214 and it consisted on 4 subscans. There were some spikes. We can also see the previous pointing and focus corrections and the elevation and azimuth of the source. All this information and more is shown in the monitor. Where all these is would be explained in the following lines. However, before reading futher, I recommend you to have a first look to the snapshot and try to locate this info by yourselves.




In general, expect of the skydips, the bolometer plots are always divided in 5 panels, and a central section with the information of the observation. From top to bottom and left to right the panels are:

  1. For pointing and focus shows the fitting. For on-off and maps it shows the reduced map.
  2. For pointing and focus shows the map of the signal observed with MAMBO. For pointings shows the signal .vs time result of the reference pixel with the flux and rms. For maps the double beam map with the rms.
  3. Total power panels. The upper panel show the variation of the opacity in the line of sight along the observation. The stars correspond to skydip measurements. For each of these measurements a value of the opacity in the line is plotter (e.g. losTau1). The red, green and dark blue lines correspond to the three total power channels of MAMBO2. The light blue shows an average of the other three lines. The bottom panel shows the change of the signal received by these total power channels, in Jy/beam.
  4. It shows the a map of the rms for the different bolos. This is plotted twice, the first without filtering the correlated signal, which gives the mean rms shown in red in at the top of the panel, and then it overplots the rms map after filtering the correlated signal, which give a new mean rms show in blue at the top of this panel. /!\ In case it appears an increase of the rms in the righ-hand edge of the panel, the pool coordinator should be informed immediately (an example of this can be seen below).

  5. Signal vs. time panel, showing the signal evolution for different included the reference one. The red signal corresponds to the raw signal, and the blue one with the signal after filtering the correlated noise.

In the central section, it can be found from left to right ordered by line from top to bottom the following info :

MAMBO2 Pointing


The screen is snapshot of a pointing. As mentioned the screen is divided in 5 panels and one info section. Here we will only discuss those aspects not covered already, panel by panel.

  1. Here it is shown the result from the fitting of the pointing. Most of the info in this panel is the same as for the heterodyne pointings. For MAMBO2 all the pointings are done with wobbler switching, allowing us to fit the throw as the distance between the two gaussians in azimuth. This throw must be similar to that commanded (see info section). This, as well as the FWHM gives an idea of the quality of the pointing.

  2. This map shows the double beam map obtained for MAMBO. We can see the source in positive and negative, as expected for the double beam (see panel 1.). Since the wobbling is done is az. one would expect to have, in addition to the source in positive and negative emission, two semicircles for the sky emission. This spillover is not this way, but is the best we have been able to obtain lately. /!\ In case this spillover changes, the Pool manager should be informed immediately.

  3. Explained above.
  4. In case a strong source is observed it is normal to see a elongation of high noise in the center of this panel (if pixel 53 is used) or in the upper-left corner (if pixel 20).
  5. Explained above.

MAMBO2 Focus


The screen is snapshot of a focus. All the info of the panels is already explained.

MAMBO2 Onoff


The screen is snapshot of an On-Off. The inf

  1. On-off RA/DEC map of all pixels. The RA/DEC 0/0 denotes the reference pixel.
  2. As explained before, this maps shows the signal for the reference pixel. The positive-negative order is similar to what happens with the pointings. The source is observed in the four scans following the next sequence: on-off, off-on , off-on , on-off. The resulting flux and rms are shown in the upper part of the panel in blue. For the strong sources the skynoise reduction is not performed, and therefore no blue line is plotted. In case the source is a calibration source, it will be display in green the flux percentage of the observation. /!\ note that normal observations require a calibration above 80%. In case it is not this way a) MAMBO is losing sensitivity (warming up) or b) we are out of focus, pointing or bad calibrated (skydip).

  3. E.a.
  4. E.a.
  5. E.a.




MAMBO2 Skydip



Indication of Problems

Monitor stacked

New data not shown

Right Edge Problem


Signal Jumps



abba-20100111s105_point_mon.gif abba-20100111s106_o-o_mon.gif

Error Messages


Information displayed


Indication of Problems


Information displayed


The plots shown by the monInst can be divided in two set of two panels, one for DC and another for AC, and the info section, common for all MAMBO plots.

The upper panels are devoted to DC signal. The left panel shows the phases of the observation (two for wobbler observations and one for total power observations). This signal can show slopes, but not jumps or changes in the slope. The right plot shows the variation of the intensity with the subscans.

The lower panels are devoted to AC signal of the reference pixel, as labeled in the upper-left corned of the signal vs. time plots. The AC signal must be flat, with a mean value of 0, and with an rms at least of 40 mJy/beam. This should be the rms under good conditions. The wind can shake the telescope and make this rms bigger. /!\ This is why is so important to comment on wind conditions while doing absorber measurements.

Indication of Problems



Signal Jumps


Warming up

abswarming.png abswarming1.png

Warmed up


MonitorGuide (last edited 2010-12-16 14:24:17 by gra-lx17)