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EIS QL Userguide

Quick links:

How do I start the QL?
How do I select and read a data file?
Xcontrol - the main QL control window for rasters.
XDETECTOR: Display data as CCD images.
XSPEC: Display data as spectroheliograms.
XWHISKER: Whisker images.
XMAP: Intensity maps
  • How do I run the software?

    In IDL (SSW IDL) type

    SSWIDL> xfiles

    to start the QL front widget called xfiles. This is the user interface to select data files (FITS) or CCSDS files to view. xfiles searches for locally stored EIS data. The default directory to start the search is specifies by the $EIS_DATA environment variable (see Setup for details).

  • The XFILES widget - How do I select and read a data file?

    The files selection dialog is the xfiles window. A screenshot of the xfiles interface is displayed below.

    The xfiles window, which is the EIS QL local file selection interface.

    The xfiles window has in it' upper left corner an exit-button, which will kill the window and terminate the EIS QL session. Below is a field that is not yet (as of june 2006) active. This is a search field based on time, where in principle one could search for rasters based on raster start and end time. Right now we don't have a conversion routine from spacecraft time to UTC, but this will hopefully be implemented well before launch.

    Next is a "Select data source" button box, where the user can select if the xiles program should search for telemetry files (CCSDS) or FITS files. The default is FITS. The default directories where the program will go to search for files are defined in the $EIS_CCSDS_DATA and $EIS_FITS_DATA environment variables, defined as a part of the setup procedure (see Setup for details).

    The next box displays the directory where the file search is performed. This field may be edited by the user. Type in a different directory and hit RETURN to list data files in that directory.

    The files found from the search in the directory dtermined by the "Search directory" box are listed in the bottom box of the xfiles window. It also displays files found in subdirectories of the search directory. By clicking one of the data files, a new window, xcontrol, will be opened.

  • XCONTROL - The mainQL Control Window

    The Xcontrol window may be decsribed as the QL main control window for the selected raster. From this window the user is presented with some basic information about the raster, and the basic displays are selections available fro here.

    The Xcontrol window, which is the EIS QL main control window for raster display.

    It has two menu items in the top menu bar. Under the file menu, "Close" terminates the Xcontrol session for this raster. Under the options menu, there are two items:

  • Display header: Launches a text window displaying the contents of the header.
  • Compare EIS/Chianti spectra: This is used to compare an average EIS spectrum calculated from the raster with a Chianti spectrum of the same wavelength region. An intermediate window pops up where the user must select the proper emission measure for the Chianti spectrum. The Chianti spectra have been pre-calculated for the EIS wavelength regions and the most relevant emssion measure regimes. The Chianti psectra are stored in proper files and distributed as a part of the EIS QL package.

    The first box in the left column lists the line windows contained in the raster, as well as line window information when available (from the planning tool). The line window selection is relevant for all display modes except the detector display, where full CCD images are displayed.

    The second box in the left column is used to select display mode.

  • The detector display shows full CCD images (see the XDETECTOR section below), i.e. count rates as a function of wavelength (abscissa) and slit position (ordinate). The ordinate translates into Solar-Y position.
  • The spectroheliogram display shows count rates for the selected line(s) as a function of wavelength (abscissa) and slit position (ordinate), one imager for each selected line and exposure.
  • The xwhisker mode shows launches one separate display window for each selected line. Here, the line countrates are displayed as a funtion of wavelength (abscissa) and exposure number (ordinate), which translates into time or raster position. If the raster is a sit-and-stare, the ordinate axis translates into time, if it is a scanning raster, the it is Solar-X coordinates.
  • The last display mode available from Xcontrol is intensity map. It displays data from one line window as a function of exposure number (abscissa) and slit position (ordinate). In order to do this, an average over the line profile (wavelength) has been calculated. Again, the abscissa dimesnion will be Solar-X for a scanning raster and time for a sit-and-stare.

    In the right column, there is a text window (not editable) that presents key parameters describing the raster, such as if it is a sit-and-stare or scanning raster, number of exposures, number os slit positions etc.

  • XDETECTOR - View the data on the detector

    The XDETECTOR GUI is used for viewing EIS data as detector images. If the raster contains lines on both detectors, two xdetector windows, one for each CCD will pop up. The xdetector interface will look something like the image below, where two line windows each of 256 pixels width are displayed on CCD A. This raster contains is a test pattern from negineering tests at MSSL. The abscissa in the image is wavelength (here shown as pixel numbers) and the ordinate axis is position along the slit (again in pixels). Slit position could for real data translate to Solar-Y position.
    The XDETECTOR interface, which is used to view data as detector images. Click the image to view a larger version of it.

    The upper menu bar has to items:

  • File which has to submenus:
    Save as: Use this to save CCD image as either jpg or ps file.
    Close: Use this to close the xdetector window.
  • Options which has three submenus:
    Colour table: Use this to manipulate the color table of the CCD images.
    Create animation: If the raster contains more than 1 exposure, the data can be played as a movie. This is done for one line at a time, so the function requires a line selcetion, which is done in a line selection window that pops up.
    Change wavelength scale: Use this to change wavelength scale on the image from pixels to Ångstrøm or vice versa.
  • The left column is used for the various display functionalities available for the CCD images.

    The Window action box is used to focus on a subimage of the total CCD image.

    If the zoom-button is selected, a new window with a zoomed in image of the selected region appears on the screen. The zoom-region appears on the original xdetector image as a box, which is selected using the left mouse button in the image. The magification is presented in a separate window, and again there is a menu in this window to save the magnified image as jpg or ps.

    The zoom region is selected using the left mouse button and appears as a box in the xdetector image. The xzoom window displaying the magnified image of the selected region.

    The other two buttons in the window action box also takes effect once a region of the CCD image is selected using the left mouse button. The Average along wavelength has the effect that, in steadof a magnified image of the slected region, a line plot, showing average count rates over the selected region in wavelength, is displayed for the range og slit postions selected.

    Similarly, the Average along slit display count rates as a function of wavelength averaged over the slit area selected.

    The slider labeled exposure # is used to select exposure number when the raster contains more than one exposure. I.e. when the slider value is 1, the CCD image displays exposure nr 2 of the raster (slider counter starts at 0).

    The plot pixel valuesdrop menu is used to display actual count rates as line plots. The row plot is count rates (intensity) as a function of wavelength at a given raster position. The column plot is count rates as a function of slit position at a sepfic wavelength pixel.

    The line plots are presented using a tool called xlineplot. The image below shows an example of this, where the row plot has been selected, i.e. count rates as a function of wavelength at a given slit position. The top slider then may be used to change the slit position for the line plot. The plot can be narrowed down in wavelength using the Start/Stop [x] sliders. If the "Automatic - scale" button is de-selected, the y-scale of the plot may also be changed manually using to more sliders that then become active. One may mark each data point with a * using the proper button, and play the line plot as a movie for all slit positions by clicking the movie-button.

    Similarly, the wavelength could be changed, slit range narrowed down etc. if the plot is a column plot in stead of a row plot.

    The xlineplot tool for lineplots. In this case a row plot displaying CCD count rates.

    The Real size CCD display button is used to present the CCD image in real size, e.g. 2148 x 1024 pixels.

    The Close-button terminates the XDETECTOR window. Each window, if there are two is closed separately.

    The middle panel of the xdetector window displays the CCD image, while the right panel displays the colorbar, to indicate the count rates and colour table used to display the image.

  • Spectroheliograms

    The spectroheliogram way of displayingtha data is displayed below. It is launched by clcking the corresponding button in the XCONTROL window, if one or more line windows have been selected from the list.

    The spectroheliogram display mode. In this case a 4 line window raster, with 3 exposures is displayed. Each image contains count rates as a function of wavelength (abscissa) and slit position (ordinate).

    The spectroheliogram image shows line count rates as a function of wavelength (abscissa) and slit position (ordinate). The top row shows N number of images for the N exposures in the raster for the first selected line. Seconf row shows images for line number 2 etc. In this case there are 4 lines selected and 3 exposures in the raster.

    The menus are the same as those described for the detector display.

  • Whisker images

    The whisker display is selected from the XCONTROL display mode menu. whisker images shows line countrates as a function of wavelength (abscissa) and exposure number - time or solar-x - (ordinate). In a sit-ant-stare campaign the ordinate axis will be time, and for a scanning raster the ordinate axis will be solar-x position.


    The image then is for one specific slit position. Such images have proven in the past to be particularly useful for sit-and-stare raster, where the time evolution of the line at one position on the sun becomes evident. The image below displays a whisker plot for a line consisting of 100 exposures. There are no velocities in these artificial data, in real data, velocities would show up as horisontal "whiskers" - therfore the naming of this display mode.

    The menus available to this mode of display are the similar as those described for the detector display.

  • Intensity maps

    The intensity map mode of displaying data averages the line over the line profile. An example of artificial EIS data made by John Mariska from a TRACE image of an active region is displayed below.


    If more than one line is selected in xcontrol, several such windows will show up. For a raster containing M slit positions and N exposures, the map will have N x M pixels. For a scanning raster, the N exposures (abscissa) translates into solar-X position, while for a sit-and-stare the corresponding axis dimesnion will be time. The ordinate axis translates to solar-Y.

    The menus available to this mode of display are the similar as those described for the detector display.

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    Updated 20-June-2006 by Øivind Wikstøl