Values in the table below based on the file $BOA_HOME_SABOCA/saboca-secondary-fluxes.py, dated 2010-05-05.
| Source | RA(2000) | Dec(2000) | Flux[Jy] |
|---|---|---|---|
| HLTAU | 04:31:38.45 | +18:13:59.0 | 8.0 |
| CRL618 | 04:42:53.6 | +36:06:53.7 | 19.2 |
| V883-ORI | 05:38:19.0 | -07:02:20.0 | 12.33 |
| N2071IR | 05:47:04.85 | +00:21:47.1 | 36.4 |
| VYCma | 07:22:58.33 | -25:46:03.2 | 10.14 |
| CW-LEO | 09:47:57.38 | +13:16:43.6 | 26.0 |
| B13134 | 13:16:43.15 | -62:58:31.6 | 180.0 |
| IRAS16293 | 16:32:22.9 | -24:28:35.6 | 135.0 |
| G5.89 | 18:00:30.38 | -24:04:00.5 | 230.0 |
| G10.62 | 18:10:28.66 | -19:55:49.7 | 340.0 |
| G34.3 | 18:53:18.50 | +01:14:58.6 | 430.0 |
| G45.1 | 19:13:22.07 | +10:50:53.4 | 105.0 |
| K3-50A | 20:01:45.69 | +33:32:43.5 | 112.0 |
| CRL2688 | 21:02:18.80 | +36:41:37.7 | 49.0 |
| NGC253 | hh:mm:ss.ss | ddd:mm:dd.s | 45.0 |
| IRAS16342 | 16:37:40.10 | -38:20:17.0 | 9.5 |
From beam maps on Mars the angular size of the telescope beam was measured for individual bolometers. After deconvolution by the planet and pixel size we found:
The shape of the main beam is an almost circular Gaussian. At intensities below 6% of the peak, the beam starts to deviate from a Gaussian.
For a multi-channel receiver, the array parameters include the relative offsets
of the individual channels as well as their relative gains. Both can be estimated
from fully sampled maps (for all channels) on strong compact objects.
We have summarized the array parameters for all observing periods from
SABOCA commissioning until now. The channel offsets normally are expected to
change only if physical work is done at the rerceiver itself (repair, upgrade,
or maintenance). However, the relative gains can also change with every warm-up
of the instrument.