Call for Observing Proposals on the 30m Telescope

Summary

Proposals for three types of receivers will be considered for the coming winter semester:

1. the observatory's set of four dual polarization heterodyne receivers centered at wavelengths of 3, 2, 1.3, and 1.1 mm.
2. the 9 pixel dual-polarization heterodyne receiver array, HERA, operating at 1.3 mm wavelength
3. The MAMBO-2 bolometer array with 117 pixels operating at 1.2 mm; the smaller MAMBO-1 array with 37 pixels is kept as a backup.

Emphasis will be put on observations at the shorter wavelengths, but 3mm proposals are also encouraged inasmuch as they are suited for medium or low quality weather backup observations. About 2000 hours of observing time are expected to be available.

The main news relevant for the coming winter semester are described here. Details of proposal formalities, instrumentation, observing modes, and estimation of observing time are described on the IRAM web site.

What is new?

In addition to the normal observing proposals, IRAM invites applications for special Large Observing Programmes (see the announcement by P. Cox elsewhere in this Newsletter). On the 30m telescope, these Large Observing Proposals are restricted for the coming winter semester to the bolometer and HERA instruments. The proposal cover page provides a checkbox for identifying a Large Programme.

The next generation single pixel heterodyne receiver for Pico Veleta, EMIR (Eight MIxer Receiver), consisting of dual-polarization 4 GHz bandwidth mixers operating at 3, 2, 1.3, and 0.9mm, will provide a boost in sensitivity and observing capabilities, fully justifying its installation as soon as possible during the coming winter semester. Installation and commissioning will take about 4 weeks. During installation, observation with HERA or MAMBO can still proceed during night time, since the Nasmyth cabin optics are not affected at this stage. In view of the uncertain time scale and our lack of experience with EMIR, we request 30m proposers to use the performance of the current receivers for their estimate of observing time. Proposals scheduled after the installation of EMIR may see their time allocation adjusted accordingly.

An effort was made with EMIR to keep as much as possible of the frequency range below 83 GHz. As the final outcome will not be known before the proposal deadline, we recommend to interested astronomers to consider applying for these low frequencies now.

Remote observing is available from the IRAM offices in Granada and Grenoble, and from the remote stations in Madrid and Bonn. A remote station in Paris may also become available soon.

Clemens THUM & Carsten KRAMER