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The 3mm1 and 230G1 receivers will be replaced by a more sensitive dual frequency (86-116 GHz/200-250 GHz) receiver next spring. Since the new receiver performances are not precisely known, we ask you to use the current 3mm1 and 230G1 noise figures (see below) for the calculation of integration times. The 3mm and 1.3mm channels of the new receiver have the same polarizations as the current 3mm1 and 230G1, and, like the latter, will be usable simultaneously either with the 2mm receiver, or the 3mm2 and 230G2 receivers (see below).

For programmes which are carried out in ``service observing'' (see below) we offer the possibility to receive a copy of the data file online via Internet during observations. With the present software this mode requires an HP Unix workstation, but it could be prepared for other operating systems.

For simple and relatively short programs, we will try to offer the possibility of ``remote observing'' via a digital (ISDN) telephone line. The remote observer will receive several screens (analogous to the setup at the telescope) with information on the telescope status, calibration, frontent/backend setup, spectra, and a talk window. The hardware and software requirements for this mode at the remote location are given in the corresponding section below.

Remote observing is possible from the Granada office, and we offer now this possibility for experienced observers. This mode may be useful in special cases and needs to be announced to IRAM Granada in advance.