LABOCA observing time calculator
You can either calculate the RMS for a given integration time, or calculate the integration time needed to reach a certain RMS.
The mean point-source sensitivity of the array, determined from on-sky integrations, is 75 mJy sqrt(s). This value is achieved only by filtering the low frequencies (hence large scale emission) to reject residual sky-noise. Without low frequency filtering the observations become sensitive to extended emission at the cost of the mean array sensitivity increasing to 120 mJy sqrt(s). The proper value is selected based on if "Point source(s)" or "Extended source(s)" is checked.
Scanning area should correspond to the area covered by the scanning pattern. For a single point source, this value should be set to 0. Note that the unit is square arc minutes (arcmin2).
The calculated integration time does not include any overhead times. This overhead includes setup, target acquisition, software setup, data transfer time (writing the FITS file), telescope slewing time, and calibrations (skydips, focus, pointings and flux calibration). In order to facilitate the calculation of the total observing time needed to achive a certain goal in rms noise, a time calculation including an avarage combined overhead of 90% is also presented by the observing time calculator.
Line-of-sight opacity of 0.3 has been assumed. A line-of-sight opacity of 0.3 at an elevation of 45 degrees corresponds to a PWV of 1.0 mm
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