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GSAOI OT Details
An introduction to the Gemini Observing Tool (OT) is presented elsewhere. This page provides detailed information on GSAOI component, GeMS component and GSAOI iterator.
- GSAOI Component
- GeMS AO Component
- Defining the CANOPUS AO WFS Stars and GSAOI ODGW Stars
- GSAOI Sequence Iterator
- GSAOI Offset Iterator
The GSAOI component editor is accessed by selecting the GSAOI component in the science program, and is shown in the figure below:
Choice of filter is made by clicking on the "Filter" pull down menu (i.e. the down-pointing arrows). The filter is chosen by selecting one from the list (by clicking on it). The central wavelength is given for each filter to assist with identification. You can move the vertical slider bar or click on the arrow buttons to browse the list.
The exposure time is set by clicking in the relevant window and typing the required number of seconds. Each occurrence of the observe element will cause N exposures to be taken and coadded in the instrument control system. The value of N is set by typing an integer in the "coadds" window. The total exposure in each output image will be the exposure times the number of coadds.
The facility Cassegrain Rotator can rotate the instrument to any desired position angle. The angle (in conventional astronomical notation of degrees east of north) is set by typing in the "position angle" box. The view of the science field in the position editor will reflect the selected angle. Alternatively the angle may be set or adjusted in the position editor itself by interactively rotating the science field.
The GSAOI arrays are read in three different modes for different kinds of observations. Select the button corresponding to the desired mode (Bright Objects, Faint Objects or Very Faint Objects). Note that the low noise reads, the read noise, the recommended exposure time and the minimum exposure time will get updated when a different readmode is selected. Details about the read out modes can be found in the GSAOI Detector page.
GeMS AO Component
GSAOI can be used "only" with GeMS. The GeMs AO component is automatically included in the GSAOI observation element. The GeMS component editor is accessed by selecting the GeMS component in the science program.
Observers should choose the default values for "Atmospheric Dispersion Corrector" (disable) and for the Astrometric Mode ("Regular). The beamsplitter can be modified by clicking over the desired Dichoric (0.85 µm or 1 µm).
Defining the CANOPUS AO WFS Stars and GSAOI ODGW Stars
GeMS uses 1 to 3 Optical Natural Guide Stars for tip-tilt wave front sensing ( CANOPUS WFS or CWFS) and 1 to 3 GSAOI near-infrared On-Detector Guide Windows (ODGW) stars. The CWFS stars and the ODGW stars are specified in the target component of the main observation.
Information about the base position (i.e. the science object) and guide star(s) may be editied by clicking the appropriate line in the target table and then editing the various fields through the text boxes below. Changing the type of target may be done using the pull down menu at the middle left.
Details on how to add guide stars (of any type) can be found in the OT Tutorial. Guide stars can be added by clicking the green "plus" symbol in the target table. Guide stars can be deleted manually by clicking the red "cross" symbol in the table target.
A better way to define guide stars is to use the position editor to query an image of the field and add stars interactively from the on-line catalogs. The UCAC3 catalog, the 2MASS catalog and the PPMX catalog give accurate positions for visible and near infrared sources.
An example, from the position editor, is given below. The GSAOI detector arrays are the large squares (cyan) and identified with a number (the orientation is N-up, E-left). The GSAOI base position, defined in the target component, is marked as a small cross within a circle (yellow). It is located at the bottom right corner of array 4, ∼7.6" from the center of the CANOPUS field. The CANOPUS field of view is represented by a large (red) circle with a radius of 1′. The probes of the CWFS1 and CWFS2 are shown as a red rectangle in the figure. Three CWFS guide stars have to be available for tip-tilt wave front sensing. One of the GSAOI ODGW stars has to be selected in order to compensate possible flexure drifts between CANOPUS and GSAOI.
The selection of the CWFS and ODGW guide stars can be done automatically using the "Auto GS" button or manually using the "Manual GS" button in the position editor (or using the buttons in the target component if the position editor is not already open). in both cases, the search of the guide stars is performed using MASCOT (Multi-Conjugate Adaptive Optics Tool) algorithm. The algorithm searches different catalogs for tip-tilt guide stars at given coordinates, compute the best tip-tilt guide star groups that will provide the best compensation (best Strehl) across the 2' CANOPUS field of view. The best asterism, based on the best average Strhel, is then selected by default. More details on the algorithm can be found in the How to find the best NGS Asterism web page.
In manual mode, the "GeMS Guide Star Search" window is displayed (upper panel in the figure below). The user can configure the catalog, the near-infrared band and the asterism (CANOPUS and GSAOI, CANOPUS alone or GSAOI alone) by clicking on the "Catalog", "NIR" and "Asterism" pull down menus respectively (i.e. the down-pointing arrows). If required, the position angle can be adjusted (every 90 degrees) by enabling or disabling the "Allow position angle adjustments" button. When a "Query" is requested, then a list of guide star candidates inside the CANOPUS field of view is given (lower panel in the figure below). The list can be reviewed and modified.
In automatic mode ("AUTO GS"), the "CANOPUS (CWFS)" is the default asterism search and the "UCAC3 Catalog" is the default catalog for MASCOT. The bright magnitude limit for CWFS is R=8.0 mag and the faint magnitude limit for CWFS is R=16.0 mag.
By pressing on the "Analyze'" button (located at lower right in the above figure) the algorithm searches for the best asterisms and returns a list of candidates sorted by the average Strehl and the average rms (see figure below). The algorithm can handle also sub-optimal cases. For example, it can return the best two-star asterism if a three-star asterism is not available.The user can also select more than one candidate asterism. When two or more asterisms are included in the target component, they are grouped separately. To add the candidate asterisms to the GSAOI Target Component, just press the "Add" button located at lower right in the figure below (remember to press press the "save" button in the GSAOI Target Component to save the selected asterisms).
The selected asterism can be visualized in the position editor. In the figure below, the three CWFS stars and the ODGW star are marked as a small green square. The average Strehl ratio and the rms, calculated using the MASCOT algorithm, are shown at the bottom of the position editor. The Strehl map is visualized in the position editor as narrow curved green/yellow lines. To visualize the Strehl map, click on the "Strehl" button located in the left panel of the position editor.
Note that the algorithm returns an average Strehl ratio for the filter defined in the GSAOI Component. To estimate the average Strehl ratio for other filters (e.g. J and H), the user has to change the filter in the GSAOI Component. The calculation of the average "Strehl" ratio (and the visualization of the Strehl map) is performed automatically after a new filter in the GSAOI componente is selected and the action saved.
Important Note: The average Strehl, rms Strehl and the minimum and maximum Strehl delivered by the Mascot algorithm, and visualized in the OT Position Editor, corresponds to the best Image Quality Conditions (IQ=20%-ile). The Observing Tools does not provide, yet, Strehl values and maps for worse IQ conditions (IQ=70%-ile and 85%-ile). More accurate Strehl ratios and FWHM values, measured for different seeing conditions, can be found in the GeMS Performance and Limiting magnitud web page.
The MASCOT algorithm can search for the best asterism using catalogs provided by the users. To use this capability, in the "GeMS Guide Star Search" window, the user has to select "User Catalog" from the Catalog menu and then select the skycat catalog to use from the menu to the right. After selecting the options you click 'Query' to display the catalog (see the figure below). An example user file for coordinates "21:29:51.000 12:08:36.00" can be found here.
- All observations must have CWFS guide stars for tip-tilt wave front sensing and one ODGW guide star for flexure compensation.
- Only one guiding configuration mode will be available at the beginning of GeMS/GSAOI operations: 3 CWFS stars + 1 ODGW star.
- The CWFS guide stars and the ODGW star must have the following limiting magnitudes: CWFS: 8 mag < R < 15.5 mag; ODGW: 8.0 < H < 14.0 mag respectively.
Detailed information about the selection of GeMS guide stars, the restriction in magnitudes for the CWFS and ODGW guide stars, and the use of the ODGW stars for tip-tilt wave front sensing can be found in the GSAOI Guiding Options page.
The GSAOI Sequence Iterator is a member of a class of instrument iterators. Each works exactly the same way, except that different options are presented depending upon the instrument. The GSAOI iterators are required when the observations is stepping through different GSAOI components. Use this component to change the instrument configuration during the observation, for example, to repeat the same basic observation at two or more filter.
In right panel of the figure below we see a few iterator features (the left panel shows the GSAOI Science Observation).
An iteration sequence ("GSAOI Sequence" in the above image) is set by choosing "GSAOI Sequence" from the "iterator" menu. The table columns in the "GSAOI Sequence Component" are items over which to iterate (four at total). In the example given below, we are iterating over filters. Table rows correspond to iterator steps. When an observing sequence is started, all the values in a row are set at once. Since there are three GSAOI configuration steps in this example, an offset iterator is required. It would be embedded inside the GSAOI sequence iterator (see below). Then, an "observe" element would produce an observe command for each of three filter setups times the number of offsets defined in the offset iterator, using the specified integration time defined in the main GSAOI component.
Rows or columns may be added and removed at will. Rows (iteration steps) may be rearranged using the arrow buttons. Rows will be added or removed by clicking "Add Step" or "Delete Step" buttons, and columns can be deleted by clicking "Delete Item". Adding column can be done by selecting one from the "Available Items" box.
In the above figure, the iteration the table shows the observations for one of the filters. The first twenty exposures are taken with the step 1 configuration (in this case the J filter) with the telescope dithering at each exposure (p, q offsets). Note that in the first 10 exposures the telescope is dithering on-source, with all guiding loops in "guide" mode. For the next 9 exposures, the telescope is dithering "on-sky" (for sky subtraction), with all guiding loops in "freeze" mode. After step 20, the instrument is re-configured with the H filter for the next 20 offset exposures (10 on-source and 10 on-sky).
GSAOI Offset Iterator
The GSAOI Offset Iterator is a member of a class of offset iterator. The offset iterator is common to all instruments and is used to define the sequence of dithers and sky offsets to be used. The offset sequence from the example given in the previous section is shown below. The offset sequence can be visualized using the position editor by clicking in the "offset" box at the Target menu. The different offset positions can be visualized in the position editor by selectio different steps in the figure below. This visualization is very useful to check if the selected guide stars are within the CANOPUS patrol field area and the GSAOI detectors during the observation. Detailed information on some of the considerations to be taken into account when setting up offset sequences with GSAOI can be found in the observing strategies page.