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The Large Programmes section of the ALMA Proposers Guide
[http://almascience.org/documents-and-tools] states:
"A maximum of 15% of the time available for science observations will
be dedicated to the execution of Large Programmes, corresponding to
645 h...
Yes, you may request monitoring observations with the standalone ACA.
When setting up time constraints in a standalone ACA Scheduling Block,
make sure that the LAS is set so that only the ACA is used. If the TP
array is also selected, you will receive a...
You can specify a range of dates when your observations should be
executed in the ALMA Observing Tool. Proposals may involve
time-critical, multiple-epoch observations, and continuous monitoring
of a target over a fixed time interval, but their execution ...
Yes. A Director Discretionary Time (DDT) proposal for the current
cycle can be submitted anytime during that cycle. One important thing
for the DDT proposal submission is that OT FOR THE CURRENT CYCLE
should be used (even when OT for the next cycle is rel...
Registration in the Science Portal of the Principal Investigator (PI)
and of all co-Investigators (co-Is) is required for submission of ALMA
proposals. Furthermore, this service is available at any time.
To avoid last-minute problems with registration, ...
By default, the ALMA Observatory will identify and conduct all
calibrations that are necessary. Detailed information on calibration
and the default ALMA approach can be found in Chapter "Calibration and
Calibration Strategies" of the ALMA Technical Handbo...
We assume that the input model is a single Stokes I plane, and that
the object to be simulated in CASA is an unpolarized continuum source.
The bandwidth of the observations can be set using the "inwidth"
parameter of the task simobserve
[https://casa.nr...
Yes, the ALMA Sensitivity Calculator takes into account the shadowing
by reducing the effective antenna surface area by a factor related to
the target declination. As the Sensitivity Calculator always assumes
that the target is observed at transit, the sh...
In solar observations, when the lifetime of your target structure is
long (> a few days, like a sunspot), your observation will only be
carried out if your target structure is present on the Sun. If your
proposal is ranked as Grade A and your target struc...
APIs for querying Splatalogue from IDL and Python are available on the
Splatalogue Applications page:
http://www.cv.nrao.edu/php/splat/SLAPNotes.html
[http://www.cv.nrao.edu/php/splat/SLAPNotes.html].
The CASA simulation task simobserve simulate an observation based on
a given antenna configuration, which is specified in the antenna
position file. A user may wish to see the effect of combining data
from two or more separate observations, taken with dif...
You need not give coordinates for a proposal to validate successfully.
For a target-of-opportunity (ToO) observations of an unknown target
(e.g. a gamma ray burst), or observations of a moving target, you only
need to specify the name (e.g. GRB1) and leav...
For observation planning, the ALMA 12m antennas have a measured
primary beam Half Power Beam Width (HPBW) of ~1.13 * λ / D; see the
ALMA Technical Handbook
[http://almascience.org/documents-and-tools/latest/alma-technical-handbook]
(Chapter "Principles an...
In the Control & Performance editor of the OT you can choose between
two types of time-constrained observations:
* Single visit: the observation needs to be executed only once
within either one or several possible time windows. You can enter
these pos...
For interferometric observations, we have to observe a quasar as a
phase calibrator every ~10 minutes for single-pointing, ~5 minuets for
MOSAIC observations at Bands 3 and 6. Therefore, the duration of a
continuous solar observation is approximately 10 o...
In each Science Goal, sources are selected in one of two ways: by
specifying a rectangular field or by specifying individual pointing
positions. Each involves some restrictions.
MAXIMUM NUMBER OF POINTINGS:
The maximum number of pointings allowed in a _...
The Observing Tool (OT) version of the sensitivity calculator uses two
distinct formulas depending on whether a double sideband (DSB)
receiver is being used, or not. The equation used for the Java applet
and the GUI that is accessible from within the OT i...
It is not required to accompany your proposal with results from
simulated ALMA observations (see Section "Science Case"of the
Proposer's Guide
[http://almascience.org/documents-and-tools/latest/alma-proposers-guide]).
However, there are several situations...
Proposals from the same team pursuing similar science but with
different targets and PIs are acceptable. As there is a single
international review process, such proposals will very likely be
assigned to the same review panel, which will be given instructi...
Section 4.4.2 of the ALMA Proposer's Guide
[http://almascience.org/documents-and-tools] states:
Proposal teams that submit a new proposal to observe some or all SGs
of a currently active but unfinished project will have the relevant
SGs identified as a ...
Individual targets that are larger than 1/3 of the Field of View (FOV)
of the 12-m Array will require a Nyquist sampled mosaic to obtain
uniform sensitivity across the field due to the sensitivity fall-off
towards the edges of the primary beam. This can b...
In the ALMA system, no portion of the baseband or spectral window can
lie outside of either the IF or RF range. This fact alone does not
present any unforeseen limitations on what can be observed within the
specified ranges. However, an issue arises becau...
Images made from interferometric data are usually subject to
calibration errors that limit the quality of the image. Errors
remaining after phase referencing are most common and move flux around
the map, lowering the peak flux density and increasing the i...
Spectral dynamic range is the ratio of the brightnesses of the
strongest and weakest detectable features in one channel of a spectrum
in a spectral line image with obvious generalizations to smoothed or
integrated data. Since the weakest detectable featur...
The QA0 criteria that have been adopted by ALMA requires an amplitude
wiggles across the spectral window of < 3 dB on the autocorrelations
(not due to atmospheric features). QA0 is given SEMIPASS if the
bandpass calibrator signal is too weak, with ampl...
CASA task simobserve
[https://casa.nrao.edu/docs/TaskRef/simobserve-task.html#x121-1200000.1.118]
is capable of adding thermal and/or phase noise to simulated
observations of a known intensity distribution, provided that one has
an estimate of the average...
All of the High Priority ALMA projects from previous and current
cycles are listed at the "High Priority Projects" page
[http://almascience.org/observing/highest-priority-projects] of the
Science Portal. Priority C, or "Filler", projects are not listed he...
Representative array configuration files for Cycles 1 and after are
linked to from the "CASA Simulator and Configuration Files
[http://almascience.org/tools/casa-simulator]" section of the Tools
page [http://almascience.org/tools] in the ALMA Science Port...
Please go to:
http://almaost.jb.man.ac.uk [http://almaost.jb.man.ac.uk]
The LO1 frequency for solar observations is fixed to 100 GHz for Band
3, 239 GHz for Band 6 and 346.6 GHz for Band 7. Only proposals for
continuum observations will be accepted. For the interferometric
observations, these will be obtained using the low ...
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