• Example 1: Basic plot with multi-instrument data (STIS, FOS, IUE).
• Example 2: The above plot was expanded around the Lyman-α region, colors were changed, and the panoramic window and grid where brougth on.
• Example 3:The same data set was augmented with UBV and IR data, units where changed to a νF(ν) versus frequency plot, the WCS mapping was changed to log-log mode, and a few annotations were put in place.
• Example 4:Going back to Example 1, a editor window associated with the IUE spectrogram was brought up. This window enables browsing of the FITS header, and allows the user to customize the color and line style of the plot associated with the specific piece of IUE data.
• Example 5:Data from Example 1 was re-displayed using a secondary display window to plot the error array associated with the flux array. Note that different physical units settings were selected in each display window. Nevertheless, the cross hair cursor (and its associated X and Y text display) in both windows keeps pointing to the same point in WCS space regardless of which units are selected. This capability comes in handy when one needs to compare spectral features in different data sets.
• Example 6:A screen shot of a data fitting session. This is a full screen shot so it may require that you hit the expand button, and/or maximize your browser window.
• Example 7:Data from Example 1 was re-displayed using an inverse color motif. Color preferences for all plot elements can be custom-defined via a graphic editor. This plot also shows the Data Quality selector window that enables the individual flagging and exclusion of bad pixels in a instrument-specific way.
• Example 8:An attempt to hand-fit a power law plus extinction to multi-instrument data. This is a full screen shot so it may require that you hit the expand button, and/or maximize your browser window.
• Example 9:An ISO LWS spectrogram being processed by the spectrogram processor. This is a full screen shot so it may require that you hit the expand button, and/or maximize your browser window.
• Example 10:The quick measurement tool being applied to a spectral feature.The picture may require that you hit the browser's expand button, and/or maximize the browser window.
• Example 11A wide-band SED of an extragalactic source, assembled from a variety of data. You might want to compare it with the NED plot for the same object: http://nedwww.ipac.caltech.edu/cgi-bin/nph-datasearch?objname=NGC+3516&meas_type=pub&ebars_spec=ebars&label_spec=no&x_spec=freq&y_spec=Fnu_jy&xr=-1
• Example 12:The SED from Example 11 is being modeled with a three component model: (i) power law to account for the overall broad band nature of the spectrum; (ii) black body that attempts to model the excess flux at the IR; (iii) interestellar extinction to account for the depression in the UV.
• Example 13:The line identification tool is being used to plot subsets of line identifications taken from a line list. The picture may require that you hit the browser's expand button, and/or maximize the browser window.