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List of Figures
1.1 Screen shot of the default CASA inputs for task clean.
1.2 The clean inputs after setting values away from their defaults (blue text). Note that some of the boldface ones have opened up new dependent sub-parameters (indented and green).
1.3 The clean inputs where one parameter has been set to an invalid value. This is drawn in red to draw attention to the problem. This hapless user probably confused the ’hogbom’ clean algorithm with Harry Potter.
1.4 The CASA Logger GUI window under Linux. Note that under MacOSX a stripped down logger will instead appear as a Console.
1.5 Using the Search facility in the casalogger. Here we have specified the string ’plotted’ and it has highlighted all instances in green.
1.6 Using the casalogger Filter facility. The log output can be sorted by Priority, Time, Origin, and Message. In this example we are filtering by Origin using ’clean’, and it now shows all the log output from the clean task.
1.7 CASA Logger - Insert facility: The log output can be augmented by adding notes or comments during the reduction. The file should then be saved to disk to retain these changes.
1.8 Flow chart of the data processing operations that a general user will carry out in an end-to-end CASA reduction session.
2.1 The contents of a Measurement Set. These tables compose a Measurement Set named ngc5921.demo.ms on disk. This display is obtained by using the File:Open menu in browsetable and left double-clicking on the ngc5921.demo.ms directory.
3.1 A freshly-started plotms GUI window. Note that the Plots > Data tab is selected, which is discussed in § 3.3.1.1, 3.3.1.6, and 3.3.1.8.
3.2 The Plots > Axes tab in the plotms GUI window, used to make a plot of Amp versus Channel.
3.3 Plot of amplitude versus time, before (left) and after (right) flagging two marked regions. To unflag these regions, mark the two same regions and click the Unflag button.
3.4 The plotxy plotter, showing the Jupiter data versus uv-distance. You can see bad data in this plot. The bottom set of buttons on the lower left are: 1,2,3) Home, Back, and Forward. Click to navigate between previously defined views (akin to web navigation). 4) Pan. Click and drag to pan to a new position. 5) Zoom. Click to define a rectangular region for zooming. 6) Subplot Configuration. Click to configure the parameters of the subplot and spaces for the figures. 7) Save. Click to launch a file save dialog box. The upper set of buttons in the lower left are: 1) Mark Region. Press this to begin marking regions (rather than zooming or panning). 2,3,4) Flag, Unflag, Locate. Click on these to flag, unflag, or list the data within the marked regions. 5) Next. Click to move to the next in a series of iterated plots. Finally, the cursor readout is on the bottom right.
3.5 The plotxy iteration plot. The first set of plots from the example in § 3.3.2.3 with iteration=’antenna’. Each time you press the Next button, you get the next series of plots.
3.6 Multi-panel display of visibility versus channel (top), antenna array configuration (bottom left) and the resulting uv coverage (bottom right). The commands to make these three panels respectively are: 1) plotxy(’ngc5921.ms’, xaxis=’channel’, datacolumn=’data’, field=’0’, subplot=211, plotcolor=’’, plotsymbol=’go’) 2) plotxy(’ngc5921.ms’, xaxis=’x’, field=’0’, subplot=223, plotsymbol=’r.’), 3) plotxy(’ngc5921.ms’, xaxis=’u’, yaxis=’v’, field=’0’, subplot=224, plotsymbol=’b,’,figfile=’ngc5921_multiplot.png’).
3.7 Plot of amplitude versus uv distance, before (left) and after (right) flagging two marked regions. The call was: plotxy(vis=’ngc5921.ms’,xaxis=’uvdist’, field=’1445*’).
3.8 tflagdata: Example showing before and after displays using a selection of one antenna and a range of channels. Note that each invocation of the flagdata2 task represents a cumulative selection, i.e., running antenna=’0’ will flag all data with antenna 0, while antenna=’0’, spw=’0:10 15’ will flag only those channels on antenna 0.
3.9 tflagdata: Flagging example using the clip mode.
3.10 browsetable: The browser displays the main table within a frame. You can scroll through the data (x=columns of the MAIN table, and y=the rows) or select a specific page or row as desired. By default, 1000 rows of the table are loaded at a time, but you can step through the MS in batches.
3.11 browsetable: You can use the tab for Table Keywords to look at other tables within an MS. You can then double-click on a table to view its contents.
3.12 browsetable: Viewing the SOURCE table of the MS.
4.1 Flow chart of synthesis calibration operations. Not shown are use of table manipulation and plotting tasks accum, plotcal, and smoothcal (see Figure 4.2).
4.2 Chart of the table flow during calibration. The parameter names for input or output of the tasks are shown on the connectors. Note that from the output solver through the accumulator only a single calibration type (e.g. ’B’, ’G’) can be smoothed, interpolated or accumulated at a time. accum is optional and all calibration files. The final set of cumulative calibration tables of all types (accummulated or as a list of caltables) are then input to applycal as shown in Figure 4.1.
4.3 The weather information for a MS as plotted by the task plotweather.
4.4 The relative change of apparent brightness per day for some popular Solar System flux density calibrators. Note that when Mars is varies fastest near opposition, when it is closest to us and thus probably too resolved to use as a calibrator anyway.
4.5 Display of the amplitude (upper) and phase (lower) gain solutions for all antennas and polarizations in the ngc5921 post-fluxscale table.
4.6 Display of the amplitude (upper), phase (middle), and signal-to-noise ratio (lower) of the bandpass’B’ solutions for antenna=’0’ and both polarizations for ngc5921. Note the falloff of the SNR at the band edges in the lower panel.
4.7 Display of the amplitude of the bandpass ’B’ solutions. Iteration over antennas was turned on using iteration=’antenna’. The first page is shown. The user would use the Next button to advance to the next set of antennas.
4.8 The ’amp’ of gain solutions for NGC4826 before (top) and after (bottom) smoothing with a 7200 sec smoothtime and smoothtype=’mean’. Note that the first solution is in a different spw and on a different source, and is not smoothed together with the subsequent solutions.
4.9 The ’phase’ of gain solutions for NGC4826 before (top) and after (bottom) ’linear’ interpolation onto a 20 sec accumtime grid. The first scan was 3C273 in spw=’0’ while the calibrator scans on 1331+305 were in spw=’1’. The use of spwmap was necessary to transfer the interpolation correctly onto the NGC4826 scans.
4.10 The final ’amp’ (top) and ’phase’ (bottom) of the self-calibration gain solutions for Jupiter. An initial phase calibration on 10s solint was followed by an incremental gain solution on each scan. These were accumulated into the cumulative solution shown here.
4.11 The final ’amp’ versus ’uvdist’ plot of the self-calibrated Jupiter data, as shown in plotxy. The ’RR LL’ correlations are selected. No outliers that need flagging are seen.
4.12 Use of plotxy to display corrected data (red and blue points) and uv model fit data (green circles).
5.1 Close-up of the top of the interactive clean window. Note the boxes at the left (where the iterations, cycles, and threshold can be changed), the buttons that control add/erase, the application of mask to channels, and whether to stop, complete, or continue cleaning, and the row of Mouse-button tool assignment icons.
5.2 Screen-shots of the interactive clean window during deconvolution of the VLA 6m Jupiter dataset. We start from the calibrated data, but before any self-calibration. In the initial stage (left), the window pops up and you can see it dominated by a bright source in the center. Next (right), we zoom in and draw a box around this emission. We have also at this stage dismissed the tape deck and Position Tracking parts of the display (§ 7.2.1) as they are not used here. We have also changed the iterations to 30 for this boxed clean. We will now hit the Next Action Continue Cleaning button (the green clockwise arrow) to start cleaning.
5.3 We continue in our interactive cleaning of Jupiter from where Figure 5.2 left off. In the first (left) panel, we have cleaned 30 iterations in the region previously marked, and are zoomed in again ready to extend the mask to pick up the newly revealed emission. Next (right), we have used the Polygon tool to redraw the mask around the emission, and are ready to Continue Cleaning for another 100 iterations.
5.4 We continue in our interactive cleaning of Jupiter from where Figure 5.3 left off. In the first (left) panel, it has cleaned deeper, and we come back and zoom in to see that our current mask is good and we should clean further. We change npercycle to 500 (from 100) in the box at upper right of the window. In the final panel (right), we see the results after this clean. The residuals are such that we should terminate the clean using the red X button and use our model for self-calibration.
5.5 After clean and self-calibration using the intensity image, we arrive at the final polarization image of Jupiter. Shown in the viewer superimposed on the intensity raster is the linear polarization intensity (green contours) and linear polarization B-vectors (vectors). The color of the contours and the sampling and rotation by 90 degrees of the vectors was set in the Display Options panel. A LEL expression was used in the Load Data panel to mask the vectors on the polarized intensity.
5.6 Screen-shot of the interactive clean window during deconvolution of the NGC5921 spectral line dataset. Note where we have selected the mask to apply to the Displayed Plane rather than All Channels. We have just used the Polygon tool to draw a mask region around the emission in this channel, which will apply to this channel only.
6.1 NGC2403 VLA moment zero (left) and NGC4826 BIMA moment one (right) images as shown in the viewer.
7.1 The Viewer Display Panel (left) and Data Display Options (right) panels that appear when the viewer is called with the image cube from NGC5921 (viewer(’ngc5921.demo.cleanimg.image’)). The initial display is of the first channel of the cube.
7.2 The Viewer Display Panel (left) and Data Display Options (right) panels that appear when the viewer is called with the NGC5921 Measurement Set (viewer(’ngc5921.demo.ms’)).
7.3 The display panel’s Main Toolbar appears directly below the menus and contains ’shortcut’ buttons for most of the frequently-used menu items.
7.4 The ’Mouse Tool’ Bar allows you to assign separate mouse buttons to tools you control with the mouse within the image display area. Initially, zooming, color adjustment, and rectangular regions are assigned to the left, middle and right mouse buttons, respectively.
7.5 The Load Data - Viewer panel that appears if you open the viewer without any infile specified, or if you use the Data:Open menu or Open icon. You can see all available files (e.g. images and MS) in the current directory that could be loaded into the viewer.
7.6 The Save Data - Viewer panel that appears when pressing the ’save data’ icon in the Main Toolbar (Figure 7.3).
7.7 The Load Data - Viewer panel as it appears if you select an image. You can see all options are available to load the image as a raster image, contour map, vector map, or marker map. In this example, clicking on the raster image button would bring up the displays shown in Figure 7.1.
7.8 The basic settings category of the Data Display Options panel as it appears if you load the image as a raster image. This is a zoom-in for the data displayed in Figure 7.1.
7.9 Example curves for scaling power cycles.
7.10 The Viewer Display Panel (left) and Data Display Options panel (right) after choosing contour map from the Load Data panel. The image shown is for channel 11 of the NGC5921 cube, selected using the Animator tape deck, and zoomed in using the tool bar icon. Note the different options in the open basic settings category of the Data Display Options panel (as compared to raster image in Figure 7.1).
7.11 The Viewer Display Panel (left) and Data Display Options panel (right) after overlaying a Contour Map of velocity on a Raster Image of intensity. The image shown is for the moments of the NGC5921 cube, zoomed in using the tool bar icon. The tab for the contour plot is open in the Data Display Options panel.
7.12 The Spectral Profile panel (right) that appears when pressing the button Open the Spectrum Profiler in the Main Toolbar and then use the tools to select a region in the image, such as the rectangular region on the left panel. The profile changes to track movements of the region if moved by dragging with the mouse.
7.13 The toolbar of the Spectral Profile contains a couple of action icons to save data or manipulate the displayed xy-range.
7.14 With dragging the left mouse button over the main window the user can interactively zoom into the profile (yellow box in left panel). Pressing the shift-key while dragging the left mouse button marks a spectral range with a gray area (middle panel) and provides start and end values for the tabs collapse/moments and linefit. With the ctrl-key pressed, a gray line marks the cursor position. Clicking the left mouse button displays the corresponding spectral channel in the Viewer Display Panel.
7.15 A Gaussian fit (blue line)to the spectral profile (red line). The status line at the bottom of the panel contains the main fit results, all details are printed to standard output.
7.16 Selecting an image region with the region tools. The region panel is shown to the right.
7.17 The three vertical tabs of the region panel: properties, stats, and file.
7.18 A multi-panel display set up through the Viewer Canvas Manager.
7.19 The Load Data - Viewer panel as it appears if you select an MS. The only option available is to load this as a Raster Image. In this example, clicking on the Raster Image button would bring up the displays shown in Figure 7.2.
7.20 The MS for NGC4826 BIMA observations has been loaded into the viewer. We see the first of the spw in the Display Panel, and have opened up MS and Visibility Selections in the Data Display Options panel. The display panel raster is not full of visibilities because spw 0 is continuum and was only observed for the first few scans. This is a case where the different spectral windows have different numbers of channels also.
7.21 The MS for NGC4826 from Figure 7.20, now with the Display Axes open in the Data Display Options panel. By default, channels are on the Animation Axis and thus in the tapedeck, while spectral window and polarization are on the Display Axes sliders.
7.22 The MS for NGC4826, continuing from Figure 7.21. We have now put spectral window on the Animation Axis and used the tapedeck to step to spw 2, where we see the data from the rest of the scans. Now channels is on a Display Axes slider, which has been dragged to show Channel 33.
7.23 Setting up to print to a file. The background color has been set to white, the line width to 2, and the print resolution to 600 dpi (for an postscript plot). To make the plot, use the Save button on the Viewer Print Manager panel (positioned in the figure in the upper right) and select a format with the drop-down, or use the Print button to send directly to a printer.
7.24 Data selection in msview.
8.1 Wiring diagram for the SDtask sdreduce. The stages of processing within the task are shown, along with the parameters that control them.
8.2 The Flag plotter. The bottom set of buttons are the standard matplotlib toolbar. See the caption of Figure 3.4 for detailed descriptions. The upper set of buttons in the lower left are: 1) region. Press this to begin marking regions (rather than zooming or panning). 2) panel. Press this to begin marking panels to select the whole spectrum. 3,4,5,6) clear, flag, unflag, statistics. Click on these to clear, flag, unflag, or calculate statistics of the data within the marked regions and spectra. 7) notation. Press this to begin editing notes on the plotter. 8,9) +, -. Click to move to the next or previous page in a series of iterated plots. The page counter on their left shows the current page number. Finally, the Quit is on the bottom right.
8.3 The toolbars on ASAP plotter. The bottom set of buttons are the standard matplotlib toolbar. See the caption of Figure 3.4 for detailed descriptions. The upper set of buttons are: 1) notation. Press this to begin editing notes on the plotter. 2) statistics.Press this to begin printing statistics to the logger. 3,4) +, -. Click to move to the next or previous page in a series of iterated plots. The page counter on their left shows the current page number. Finally, the Quit is on the bottom right.
8.4 The Notation widget.
8.5 Total power data display using sdtpimaging, with calmode=’baseline’. The top panel shows uncalibrated data versus row numbers.The middle panel shows baseline fitting of each scan (only shown here the last scan). The bottom panel shows the calibrated (baseline subtracted) data.
8.6 Multi-panel display of the scantable. Subpanels are displayed per scan. There are two spectra in each scan indicating two polarization (RR and LL).
8.7 Two panel plot of the calibrated spectra. The GBT data have a separate scan for the SOURCE and REFERENCE positions so scans 20,21,22 and 23 result in these two spectra.
8.8 Calibrated spectrum with a line at zero (using histograms).
8.9 FLS3a HI emission. The display illustrates the visualization of the data cube (left) and the profile display of the cube at the cursor location (right); the Tools menu of the Viewer Display Panel has a Spectral Profile button which brings up this display. By default, it grabs the left-mouse button. Pressing down the button and moving in the display will show the profile variations.
1.2 The clean inputs after setting values away from their defaults (blue text). Note that some of the boldface ones have opened up new dependent sub-parameters (indented and green).
1.3 The clean inputs where one parameter has been set to an invalid value. This is drawn in red to draw attention to the problem. This hapless user probably confused the ’hogbom’ clean algorithm with Harry Potter.
1.4 The CASA Logger GUI window under Linux. Note that under MacOSX a stripped down logger will instead appear as a Console.
1.5 Using the Search facility in the casalogger. Here we have specified the string ’plotted’ and it has highlighted all instances in green.
1.6 Using the casalogger Filter facility. The log output can be sorted by Priority, Time, Origin, and Message. In this example we are filtering by Origin using ’clean’, and it now shows all the log output from the clean task.
1.7 CASA Logger - Insert facility: The log output can be augmented by adding notes or comments during the reduction. The file should then be saved to disk to retain these changes.
1.8 Flow chart of the data processing operations that a general user will carry out in an end-to-end CASA reduction session.
2.1 The contents of a Measurement Set. These tables compose a Measurement Set named ngc5921.demo.ms on disk. This display is obtained by using the File:Open menu in browsetable and left double-clicking on the ngc5921.demo.ms directory.
3.1 A freshly-started plotms GUI window. Note that the Plots > Data tab is selected, which is discussed in § 3.3.1.1, 3.3.1.6, and 3.3.1.8.
3.2 The Plots > Axes tab in the plotms GUI window, used to make a plot of Amp versus Channel.
3.3 Plot of amplitude versus time, before (left) and after (right) flagging two marked regions. To unflag these regions, mark the two same regions and click the Unflag button.
3.4 The plotxy plotter, showing the Jupiter data versus uv-distance. You can see bad data in this plot. The bottom set of buttons on the lower left are: 1,2,3) Home, Back, and Forward. Click to navigate between previously defined views (akin to web navigation). 4) Pan. Click and drag to pan to a new position. 5) Zoom. Click to define a rectangular region for zooming. 6) Subplot Configuration. Click to configure the parameters of the subplot and spaces for the figures. 7) Save. Click to launch a file save dialog box. The upper set of buttons in the lower left are: 1) Mark Region. Press this to begin marking regions (rather than zooming or panning). 2,3,4) Flag, Unflag, Locate. Click on these to flag, unflag, or list the data within the marked regions. 5) Next. Click to move to the next in a series of iterated plots. Finally, the cursor readout is on the bottom right.
3.5 The plotxy iteration plot. The first set of plots from the example in § 3.3.2.3 with iteration=’antenna’. Each time you press the Next button, you get the next series of plots.
3.6 Multi-panel display of visibility versus channel (top), antenna array configuration (bottom left) and the resulting uv coverage (bottom right). The commands to make these three panels respectively are: 1) plotxy(’ngc5921.ms’, xaxis=’channel’, datacolumn=’data’, field=’0’, subplot=211, plotcolor=’’, plotsymbol=’go’) 2) plotxy(’ngc5921.ms’, xaxis=’x’, field=’0’, subplot=223, plotsymbol=’r.’), 3) plotxy(’ngc5921.ms’, xaxis=’u’, yaxis=’v’, field=’0’, subplot=224, plotsymbol=’b,’,figfile=’ngc5921_multiplot.png’).
3.7 Plot of amplitude versus uv distance, before (left) and after (right) flagging two marked regions. The call was: plotxy(vis=’ngc5921.ms’,xaxis=’uvdist’, field=’1445*’).
3.8 tflagdata: Example showing before and after displays using a selection of one antenna and a range of channels. Note that each invocation of the flagdata2 task represents a cumulative selection, i.e., running antenna=’0’ will flag all data with antenna 0, while antenna=’0’, spw=’0:10 15’ will flag only those channels on antenna 0.
3.9 tflagdata: Flagging example using the clip mode.
3.10 browsetable: The browser displays the main table within a frame. You can scroll through the data (x=columns of the MAIN table, and y=the rows) or select a specific page or row as desired. By default, 1000 rows of the table are loaded at a time, but you can step through the MS in batches.
3.11 browsetable: You can use the tab for Table Keywords to look at other tables within an MS. You can then double-click on a table to view its contents.
3.12 browsetable: Viewing the SOURCE table of the MS.
4.1 Flow chart of synthesis calibration operations. Not shown are use of table manipulation and plotting tasks accum, plotcal, and smoothcal (see Figure 4.2).
4.2 Chart of the table flow during calibration. The parameter names for input or output of the tasks are shown on the connectors. Note that from the output solver through the accumulator only a single calibration type (e.g. ’B’, ’G’) can be smoothed, interpolated or accumulated at a time. accum is optional and all calibration files. The final set of cumulative calibration tables of all types (accummulated or as a list of caltables) are then input to applycal as shown in Figure 4.1.
4.3 The weather information for a MS as plotted by the task plotweather.
4.4 The relative change of apparent brightness per day for some popular Solar System flux density calibrators. Note that when Mars is varies fastest near opposition, when it is closest to us and thus probably too resolved to use as a calibrator anyway.
4.5 Display of the amplitude (upper) and phase (lower) gain solutions for all antennas and polarizations in the ngc5921 post-fluxscale table.
4.6 Display of the amplitude (upper), phase (middle), and signal-to-noise ratio (lower) of the bandpass’B’ solutions for antenna=’0’ and both polarizations for ngc5921. Note the falloff of the SNR at the band edges in the lower panel.
4.7 Display of the amplitude of the bandpass ’B’ solutions. Iteration over antennas was turned on using iteration=’antenna’. The first page is shown. The user would use the Next button to advance to the next set of antennas.
4.8 The ’amp’ of gain solutions for NGC4826 before (top) and after (bottom) smoothing with a 7200 sec smoothtime and smoothtype=’mean’. Note that the first solution is in a different spw and on a different source, and is not smoothed together with the subsequent solutions.
4.9 The ’phase’ of gain solutions for NGC4826 before (top) and after (bottom) ’linear’ interpolation onto a 20 sec accumtime grid. The first scan was 3C273 in spw=’0’ while the calibrator scans on 1331+305 were in spw=’1’. The use of spwmap was necessary to transfer the interpolation correctly onto the NGC4826 scans.
4.10 The final ’amp’ (top) and ’phase’ (bottom) of the self-calibration gain solutions for Jupiter. An initial phase calibration on 10s solint was followed by an incremental gain solution on each scan. These were accumulated into the cumulative solution shown here.
4.11 The final ’amp’ versus ’uvdist’ plot of the self-calibrated Jupiter data, as shown in plotxy. The ’RR LL’ correlations are selected. No outliers that need flagging are seen.
4.12 Use of plotxy to display corrected data (red and blue points) and uv model fit data (green circles).
5.1 Close-up of the top of the interactive clean window. Note the boxes at the left (where the iterations, cycles, and threshold can be changed), the buttons that control add/erase, the application of mask to channels, and whether to stop, complete, or continue cleaning, and the row of Mouse-button tool assignment icons.
5.2 Screen-shots of the interactive clean window during deconvolution of the VLA 6m Jupiter dataset. We start from the calibrated data, but before any self-calibration. In the initial stage (left), the window pops up and you can see it dominated by a bright source in the center. Next (right), we zoom in and draw a box around this emission. We have also at this stage dismissed the tape deck and Position Tracking parts of the display (§ 7.2.1) as they are not used here. We have also changed the iterations to 30 for this boxed clean. We will now hit the Next Action Continue Cleaning button (the green clockwise arrow) to start cleaning.
5.3 We continue in our interactive cleaning of Jupiter from where Figure 5.2 left off. In the first (left) panel, we have cleaned 30 iterations in the region previously marked, and are zoomed in again ready to extend the mask to pick up the newly revealed emission. Next (right), we have used the Polygon tool to redraw the mask around the emission, and are ready to Continue Cleaning for another 100 iterations.
5.4 We continue in our interactive cleaning of Jupiter from where Figure 5.3 left off. In the first (left) panel, it has cleaned deeper, and we come back and zoom in to see that our current mask is good and we should clean further. We change npercycle to 500 (from 100) in the box at upper right of the window. In the final panel (right), we see the results after this clean. The residuals are such that we should terminate the clean using the red X button and use our model for self-calibration.
5.5 After clean and self-calibration using the intensity image, we arrive at the final polarization image of Jupiter. Shown in the viewer superimposed on the intensity raster is the linear polarization intensity (green contours) and linear polarization B-vectors (vectors). The color of the contours and the sampling and rotation by 90 degrees of the vectors was set in the Display Options panel. A LEL expression was used in the Load Data panel to mask the vectors on the polarized intensity.
5.6 Screen-shot of the interactive clean window during deconvolution of the NGC5921 spectral line dataset. Note where we have selected the mask to apply to the Displayed Plane rather than All Channels. We have just used the Polygon tool to draw a mask region around the emission in this channel, which will apply to this channel only.
6.1 NGC2403 VLA moment zero (left) and NGC4826 BIMA moment one (right) images as shown in the viewer.
7.1 The Viewer Display Panel (left) and Data Display Options (right) panels that appear when the viewer is called with the image cube from NGC5921 (viewer(’ngc5921.demo.cleanimg.image’)). The initial display is of the first channel of the cube.
7.2 The Viewer Display Panel (left) and Data Display Options (right) panels that appear when the viewer is called with the NGC5921 Measurement Set (viewer(’ngc5921.demo.ms’)).
7.3 The display panel’s Main Toolbar appears directly below the menus and contains ’shortcut’ buttons for most of the frequently-used menu items.
7.4 The ’Mouse Tool’ Bar allows you to assign separate mouse buttons to tools you control with the mouse within the image display area. Initially, zooming, color adjustment, and rectangular regions are assigned to the left, middle and right mouse buttons, respectively.
7.5 The Load Data - Viewer panel that appears if you open the viewer without any infile specified, or if you use the Data:Open menu or Open icon. You can see all available files (e.g. images and MS) in the current directory that could be loaded into the viewer.
7.6 The Save Data - Viewer panel that appears when pressing the ’save data’ icon in the Main Toolbar (Figure 7.3).
7.7 The Load Data - Viewer panel as it appears if you select an image. You can see all options are available to load the image as a raster image, contour map, vector map, or marker map. In this example, clicking on the raster image button would bring up the displays shown in Figure 7.1.
7.8 The basic settings category of the Data Display Options panel as it appears if you load the image as a raster image. This is a zoom-in for the data displayed in Figure 7.1.
7.9 Example curves for scaling power cycles.
7.10 The Viewer Display Panel (left) and Data Display Options panel (right) after choosing contour map from the Load Data panel. The image shown is for channel 11 of the NGC5921 cube, selected using the Animator tape deck, and zoomed in using the tool bar icon. Note the different options in the open basic settings category of the Data Display Options panel (as compared to raster image in Figure 7.1).
7.11 The Viewer Display Panel (left) and Data Display Options panel (right) after overlaying a Contour Map of velocity on a Raster Image of intensity. The image shown is for the moments of the NGC5921 cube, zoomed in using the tool bar icon. The tab for the contour plot is open in the Data Display Options panel.
7.12 The Spectral Profile panel (right) that appears when pressing the button Open the Spectrum Profiler in the Main Toolbar and then use the tools to select a region in the image, such as the rectangular region on the left panel. The profile changes to track movements of the region if moved by dragging with the mouse.
7.13 The toolbar of the Spectral Profile contains a couple of action icons to save data or manipulate the displayed xy-range.
7.14 With dragging the left mouse button over the main window the user can interactively zoom into the profile (yellow box in left panel). Pressing the shift-key while dragging the left mouse button marks a spectral range with a gray area (middle panel) and provides start and end values for the tabs collapse/moments and linefit. With the ctrl-key pressed, a gray line marks the cursor position. Clicking the left mouse button displays the corresponding spectral channel in the Viewer Display Panel.
7.15 A Gaussian fit (blue line)to the spectral profile (red line). The status line at the bottom of the panel contains the main fit results, all details are printed to standard output.
7.16 Selecting an image region with the region tools. The region panel is shown to the right.
7.17 The three vertical tabs of the region panel: properties, stats, and file.
7.18 A multi-panel display set up through the Viewer Canvas Manager.
7.19 The Load Data - Viewer panel as it appears if you select an MS. The only option available is to load this as a Raster Image. In this example, clicking on the Raster Image button would bring up the displays shown in Figure 7.2.
7.20 The MS for NGC4826 BIMA observations has been loaded into the viewer. We see the first of the spw in the Display Panel, and have opened up MS and Visibility Selections in the Data Display Options panel. The display panel raster is not full of visibilities because spw 0 is continuum and was only observed for the first few scans. This is a case where the different spectral windows have different numbers of channels also.
7.21 The MS for NGC4826 from Figure 7.20, now with the Display Axes open in the Data Display Options panel. By default, channels are on the Animation Axis and thus in the tapedeck, while spectral window and polarization are on the Display Axes sliders.
7.22 The MS for NGC4826, continuing from Figure 7.21. We have now put spectral window on the Animation Axis and used the tapedeck to step to spw 2, where we see the data from the rest of the scans. Now channels is on a Display Axes slider, which has been dragged to show Channel 33.
7.23 Setting up to print to a file. The background color has been set to white, the line width to 2, and the print resolution to 600 dpi (for an postscript plot). To make the plot, use the Save button on the Viewer Print Manager panel (positioned in the figure in the upper right) and select a format with the drop-down, or use the Print button to send directly to a printer.
7.24 Data selection in msview.
8.1 Wiring diagram for the SDtask sdreduce. The stages of processing within the task are shown, along with the parameters that control them.
8.2 The Flag plotter. The bottom set of buttons are the standard matplotlib toolbar. See the caption of Figure 3.4 for detailed descriptions. The upper set of buttons in the lower left are: 1) region. Press this to begin marking regions (rather than zooming or panning). 2) panel. Press this to begin marking panels to select the whole spectrum. 3,4,5,6) clear, flag, unflag, statistics. Click on these to clear, flag, unflag, or calculate statistics of the data within the marked regions and spectra. 7) notation. Press this to begin editing notes on the plotter. 8,9) +, -. Click to move to the next or previous page in a series of iterated plots. The page counter on their left shows the current page number. Finally, the Quit is on the bottom right.
8.3 The toolbars on ASAP plotter. The bottom set of buttons are the standard matplotlib toolbar. See the caption of Figure 3.4 for detailed descriptions. The upper set of buttons are: 1) notation. Press this to begin editing notes on the plotter. 2) statistics.Press this to begin printing statistics to the logger. 3,4) +, -. Click to move to the next or previous page in a series of iterated plots. The page counter on their left shows the current page number. Finally, the Quit is on the bottom right.
8.4 The Notation widget.
8.5 Total power data display using sdtpimaging, with calmode=’baseline’. The top panel shows uncalibrated data versus row numbers.The middle panel shows baseline fitting of each scan (only shown here the last scan). The bottom panel shows the calibrated (baseline subtracted) data.
8.6 Multi-panel display of the scantable. Subpanels are displayed per scan. There are two spectra in each scan indicating two polarization (RR and LL).
8.7 Two panel plot of the calibrated spectra. The GBT data have a separate scan for the SOURCE and REFERENCE positions so scans 20,21,22 and 23 result in these two spectra.
8.8 Calibrated spectrum with a line at zero (using histograms).
8.9 FLS3a HI emission. The display illustrates the visualization of the data cube (left) and the profile display of the cube at the cursor location (right); the Tools menu of the Viewer Display Panel has a Spectral Profile button which brings up this display. By default, it grabs the left-mouse button. Pressing down the button and moving in the display will show the profile variations.
More information about CASA may be found at the
CASA web page
Copyright © 2010 Associated Universities Inc., Washington, D.C.
This code is available under the terms of the GNU General Public Lincense
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