Observing proposals for the
array are due typically in January, July, and September of each year. Usually
you can request all available array configurations in a single proposal
(if your science requires it). The Executive
Board decides what frequencies ranges and arrays will be offered in
each proposal period.
Proposals are reviewed and
graded by five referees. Three referees are from institutions in the BIMA
consortium, two are outside. The average grade is used to determine if
your proposal will get scheduled. After your proposal has been reviewed,
you are sent a referee's report by e-mail.
Proposals should be submitted
electronically; we will grudgingly accept paper copy only in extreme circumstances.
In either case, you MUST prepare your proposal with the LaTeX
cover sheet and style
file. FAX proposals will not be accepted.
For more details, see the
recent call for proposals and the full
proposal submission procedure.
To aid you in preparation
of your proposal, we suggest the following:
You should start with the
detailing the array capabilities. It will tell you about array configurations,
receiver and system temperatures, the correlator spectrometer, how to calculate
map sensitivity, and phase & amplitude calibration.
If you are proposing for the cm-wave
the document detailing BIMA's 1 cm capabilities.
Once you understand the array
capabilities, you need to find calibrators.
is a Java applet to help you locate phase
and amplitude calibrators near your source. You should try to find a calibrator
of sufficient strength within 20 degrees of your source (closer is better). "Sufficient
strength" depends on what wavelength you are operating at.
At 3mm, S > 1.0 Jy is reasonable for a 3-4 minute observation; at 1mm you would need a calibrator with
S > 2.0 Jy. The long baseline
configuration, A-array, is a special case that requires a technique of
fast-switching between multiple calibrators, and you should consult the
calibration section of the array technical description. There are also
many Atacama Large Millimeter Array (ALMA) Memos
Another applet, GetHA,
will help you determine the optimum hour angle range over which to observe
your source (and also how much time per track your project is likely to be allocated).
you gain very little signal-to-noise by
observing horizon to horizon.
RMS noise calculation applet lets you use the latest BIMA receiver
and system temperatures to estimate the point source sensitivity of your
Please direct comments, criticisms, corrections
and contributions to:
Page last modified:
Monday, 16-Jun-2003 11:23:12 EDT.