These are a list of routines that are usful for EIS analysis. If you find others useful let us know and they can be added to the SSW tree.
eis_auto_fit.pro : ; This routine takes the output from EIS_GETWINDATA and performs a fit ; over the intensity array, returning values for the intensity, line width ; and centroid. ; ; The quality of the spectrum is checked to ensure that a good fit can be ; obtained (for bad data, the routine can hang while it tries to find a ; solution).
eis_data__getwindata.pro : Returns EIS data from a detector window.
eis_data__getwinheader.pro: Returns the FITS header for a spectral window
eis_debias.pro: Removes the CCD bias from an EIS data window.
eis_despike.pro: EIS_DESPIKE is used for de-spiking, i.e. to remove cosmic ray spikes from the pixel data.
eis_exposure_times.pro : This routine extracts the start times of each exposure in an EIS data object. The times are given in seconds relative to the first exposure.
eis_find_window.pro: Given the a header structure for an EIS data-set, this routine checks if the specified wavelength, WVL, is found in the data-set's wavelength windows. If yes, then the index of the wavelength window is returned.
eis_get_hdr_struc.pro: This routine extracts selected information from an EIS data header into a structure. The particular fields taken from the header are defined in the file $SSW/hinode/eis/idl/analysis/headcat_tags.txt.
eis_get_iwin.pro: To find the data window given the line id or the wavelength.
eis_get_wininfo.pro : To return information on the windows contained in an eis fits file.
eis_getdata.pro: EIS_GETDATA is a script to extract data (one, sevceral or all line windows) from a (FITS or CCSDS) data file.
eis_getlambda.pro : get the wavelength range of the CCDs
eis_getmoments.pro: EIS_GETMOMENTS is a script to calculate moments from one, several or all spectral line windows from a (fits or CCSDS) data file.
eis_getwindata.pro: Returns EIS data from one spectral window.
eis_orbit_correction.pro: Calculates the wavelength vector for each exposure in the EIS data-set, corrected for the orbital variation.
eis_orbit_spline_quick.pro: Represents the orbital variation of EIS line centroids by a spline function with nodes spaced at 5 minute intervals. Returns the value of the centroid at the input times.
eis_prep.pro: carries out EIS calibration
eis_raster_browser.pro: This routine is used to browse 3D EIS data-cubes.
eis_spike_viewer.pro: This tool is for browsing EIS data arrays that have been cleaned of cosmic ray hits.
fig_tsmean.pro: plots temporal mean of spectrum
line_centroid.pro: Finds the centroid of an emission or absorption line by minmizing the function SUM( (wavel_i-ref) * flux_i ), for the centroid wavelength
xmoment.pro: XMOMENT plots mean line profile, and has interactive mouse functions to mark where the line is (start/stop pixels) and where the continuum is.
xfiles.pro: ; XFILES is used to select data files from data bases. It reads ; data from many data sources. The user can also specify own ; data sources, in which case data-read procedures must be ; provided. XFILES defines the data objects, header objects and ; auxiliary objects and sends them to XDISPLAY. The XDISPLAY ; window is opened when the user selects a data file in XFILES.
xmap.pro: calling by xfiles.pro ; XMAP is used to display 2-D (or higher) data. It is a ; widget based program with several options and functions that ; allows data to be displayed in a nukmber of modes.
xcontrol.pro: calling by xfiles.pro ; XCONTROL is the main QL control window. After selecting a file (CCSDS or ; FITS) this windows opens with information about the data, and control ; buttons etc. for the various display methods and data processing ; options available for a particular set of data.
xdetector.pro: calling by xfiles.pro ; XDETECTOR is used to display 2-D (or higher) data. It is a ; widget based program with several options and functions that ; allows data to be displayed in a nukmber of modes.
xraster.pro: calling by xfiles.pro ; XRASTER is used to display 3-D spectroscopic data in the form ; of a raster (i.e. intensity[lambda, slit pos, raster pos.]. ; One line is displayed as I[lambda, slit pos] with one display window ; for each raster (using !p.multi). If more than one line, these ; are added as extra rows of display windows.
xwhisker.pro: calling by xfiles.pro ; xwhisker is used to display 2-D spectroscopic data as whisker plots ; (images). I.e. Intensity[wavelength, y]. ; Typically y will be solar_x (for a raster) or ; for sit-and-stare observations it will be time.
