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.


__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.
}}}