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Knowledgebase : Project Planning
     
Single-dish observing modes are available for Cycle 4 using the Total Power (TP) Array as part of the ALMA Compact Array (ACA). The use of the TP Array is limited to spectral line observations in Bands 3-8. No TP Array Band 9 and Band 10 observations a...
You can observe continuum by using the 7-m Array but you cannot with the Total Power (TP) Array in Cycle 3. Also the TP array is not offered for Bands 9 or 10 in Cycle 3. Please also see Appendix A.4 of the Cycle 3 Proposer's Guide and Capabilities [1]...
You can observe continuum by using the 7-m Array but you cannot with the Total Power (TP) Array in Cycle 4. Also the TP array is not offered for Bands 9 or 10 in Cycle 4. Please also see Appendix A.3 of the Cycle 4 Proposer's Guide and Capabilities [1]. ...
Yes, you may request monitoring observations with the standalone ACA. However, this is not supported by the OT: if you enter an angular resolution corresponding to the synthesised beamsize of the ACA and at the same time click the Time Constraints radi...
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 executi...
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 executi...
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 10 and Appendix C of the ALMA Technical Handbook [1]. The defau...
Does Simdata account for both polarizations when simulating continuum observations? We assume that the input model is a single Stokes I plane, and that the object to be simulated in CASA/Simdata is an unpolarized continuum source. The bandwidth of...
Neither the sensitivity calculator accessed online through the science portal nor the sensitivity calculator in the observing tool account for shadowing of antennas observing at low elevation.
APIs for querying Splatalogue from IDL and Python are available on the Splatalogue Applications page: http://www.cv.nrao.edu/php/splat/SLAPNotes.html.
The "refdate" and "hourangle" keywords can be used in the CASA task [1] simobserve for time specification. Also, one can produce an ms for a full track (e.g. 8 or 12-hour) and then use flagdata to flag specific time ranges prior to imaging the data. A C...
The CASA simulation [1] tasks (simobserve and simanalyze) 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 observ...
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...
Information about polarization in Cycle 4 can be found in the ALMA Cycle 4 Proposer's Guide [1] section A.7 For Cycle 4, on top of the dual polarizations (XX, YY) and single polarization modes (XX), observations to measure the full intrinsic pola...
For observation planning, the ALMA 12m antennas have a measured primary beam Half Power Beam Width (HPBW) of ~1.13 * lambda / D; see the ALMA Technical Handbook [1], Chapter 3, for further details. Also ALMA Memo 456 [2] (available at the Science Porta...
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 ...
To increase the density of the data points on the u-v plane for obtaining high dynamic range, PIs might need to observe the Sun with the same observing parameters twice in the morning and afternoon. In this case, please follow the following procedure. ...
In each Science Goal, sources are selected in one of two ways: by specifying a rectangular field, or by specifying individual positions, with or without offsets. Each involves some restrictions. A Cycle 4 proposal may contain up to a total of 150 po...
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 O...
It is not required to accompany your Cycle 4 proposal with results from simulated ALMA observations (see Sec. 6.2.2 of the Proposer's Guide [1]). However, there are several situations that it may be wise to use CASA's simulation capabilities to underst...
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...
The Cycle 3 Call for Proposals [1] includes the following instructions for PI's of previously successfully proposals that were not completed by the Cycle 3 proposal deadline: _\"INFORMATION FOR PROPOSERS WITH UNDELIVERED DATA_ _Proposers of active ...
The Cycle 4 Proposer's Guide [1] mentions resubmissions in section 5.4.2: Proposal teams that submit a Cycle 4 proposal to observe some or all science goals of a currently active but unfinished project should identify their Cycle 4 proposal as a "Re...
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...
The scientific and technical justification guidelines are given in Sections 6.2 \">Proposer's Guide. [1] The scientific justification must be submitted as a single PDF document. The total length of the PDF document is limited to 4 pages for Regular,...
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 th...
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 fea...
In Cycle 3, standard observing modes are those that have been used in previous Cycles and for which the data can be reduced by the pipeline. Non-standard modes are observing modes that are less well characterized, or for which the data need to b...
In Cycle 4, standard observing modes are those that have been used in previous Cycles and for which the data can be reduced by the pipeline. Please see Section 5.2 of the Cycle 4 Proposer's Guide [1]. Non-standard modes are observing modes that a...
The QA0 criteria that have been adopted by ALMA during Cycle 4 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 t...
What pwv and delta-pwv should I use in my simdata simulations to prepare an ALMA proposal? Simdata 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 ...
All of the High Priority ALMA projects from Cycles 0, 1 and 2 are listed at the ALMA Science Portal [1]. Priority C, or "Filler", projects are not listed here. Target lists are not listed at the Science Portal but by querying the ALMA Science Archi...
Representative array configuration files are linked to from the "Array Configuration Files" section of the Documents and Tools page [1] in the ALMA Science Portal. Configuration files for Cycle 0 are available from the Cycle 0 Documentation page [2]. W...
It was recently discovered that the ACA 7m configuration files for Cycle 4 in the casa simulator use an incorrect primary beam, so 7m simulations may have incorrect fluxes. Simulations of the 12m array are fine. In order to fix the problem, the first l...
The LO1 frequency for solar observations is fixed to 100 GHz for Band 3 and 239 GHz for Band 6. Only proposals for continuum observations will be accepted. For the interferometric observations, these will be obtained using the low spectral resolution (TDM...
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