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. ; EXAMPLE: ; Create an object: ; IDL> eisfile = 'eis_l1_20070202_104212.fits' ; IDL> eisfile = 'eis_er_20070202_104212.fits' ; IDL> obj = obj_new('eis_data',eisfile) ; IDL> obj_er = obj_new('eis_data',errfile) ; And extract data from window 0. ; IDL> data = obj -> getwindata(0, data_er=obj_er)
eis_data__getwinheader.pro: ; Returns the FITS header for a spectral window ; Example: ; IDL> data = obj_new('eis_data') ; IDL> eisfile = '$HINODE/eis/mission/2007/02/02/eis_l0_20070202_104212.fits.gz' ; IDL> header=data->getwinheader(eisfile,0)
eis_debias.pro: ; Removes the CCD bias from an EIS data window.
eis_despike.pro: ; EIS_DESPIKE is part of the SOLAR-B EIS analysis software . It 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/atest/pyoung/headcat_tags.txt.
eis_get_iwin.pro: ; PURPOSE : To find the data window given the line id or the ; wavelength. ; EXAMPLE : IDL> iwin = eis_get_iwin('eis_l0_20061214_192012',195) ; IDL> print,iwin ; 4
eis_get_wininfo.pro : ; PURPOSE : To return information on the windows contained in ; an eis fits file. ; EXAMPLE : IDL> file = 'eis_l0_20061214_192012' ; IDL> wininfo = eis_get_winfo(file,/list,nwin=nwin) ; iwin line_id wvl_min wvl_max ; 0 FE X 184.540 184.29 184.80 ; 1 FE VIII 185.210 184.96 185.47 ; 2 FE XI 188.230 187.97 188.48 ; 3 CA XVII 192.820 192.56 193.07 ; 4 FE XII 195.120 194.85 195.37 ; 5 FE XIII 202.040 201.78 202.30 ; 6 HE II 256.320 256.06 256.58 ; 7 FE XIV 274.200 273.96 274.47 ; 8 FE XV 284.160 283.92 284.43 ; IDL> print,nwin ; 9
eis_getdata.pro: ; EIS_GETDATA is a script to extract data (one, sevceral or all ; line windows) from a (FITS or CCSDS) data file. ; example 1: Get line window 0 and hdr from CCSDS file1= 'file1.dat': ; IDL> eis_getdata, file1, wd, hdr=hdr, /ccsds ; If e.g 32 pixel wide line window *wavelength, ; 512 slit pos. and 100 raster pos, the dimension of ; wd will now be: wd = uint[32, 512, 100] ; example 2: Get line windows 2 and 3 from fitsfile file2='file2.fits': ; IDL> eis_getdata, file2, wd, iwin=[2,3] ; If same dimensions as above, wd will now be: ; wd = uintarr[32, 512, 100, 2], i.e. ; wd[nlam, nslit, nraster, nwin] ; example 3: Get all 25 line windows and hdr from FITS file 'file2.fits' ; IDL>eis_getdata, file2, hdr=hdr, /all ; wd is now uintarr[32, 512, 100, 25]
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. ; CALLING SEQUENCE: ; d = eis_getwindata(file, [iwin ,keywords])
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 standard EIS calibration
eis_raster_browser.pro: ; This routine is used to browse 3D EIS data-cubes. It is based on ; software available in the SOHO/CDS software.
eis_spike_viewer.pro: ; This tool is for browsing EIS data arrays that have been cleaned of ; cosmic ray hits. ; EXAMPLE ; IDL> data=obj_new('eis_data',filename) ; IDL> wd=data->getvar(iwin) ; IDL> eis_debias,wd ; IDL> eis_despike,wd,wd_clean,swtch=spikes ; IDL> EIS_SPIKE_VIEWER,wd,wd_clean,spikes
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, ; ref. Note that the accuracy of the derived wavelength is improved by ; having the input wavelength vector (str.wavel) on a fine scale. ; USE ; ; IDL> line_centroid, wvl, flx, [1030,1035]
eis_getfilename.pro: ; A simple routine for turning a file name into an absolute file ; name. The routine looks in three places for the file: the present ; directory, the mission archive and the quick look directory. If ; nothing is passed a widget comes up, but this isn't very useful. ; EXAMPLE: ; IDL> file=eis_getfilename('eis_l0_20061202_140632') ; IDL> print,file ; .../eis/mission/2006/12/02/eis_l0_20061202_140632.fits.gz
eis_help.pro: ; Instatiates the hw_help object and calls the display_all method to give a ; first introduction to the object help documentation for the eis/hw software.
photons_to_energy.pro: ; Convert intensity from photons [ph m-2 s-1 sr-1] to energy in SI units ; [W m-2 sr-1]
eis_get_compression_factor: ; PURPOSE: Returns the reciprocal of the latest EIS compression factor
eis_colors.pro: ; set eis colortable for velocity & width maps display
_eis_raster_fov.pro: ; PURPOSE : to calculate information about the field of view ; for an EIS raster ; EXAMPLE : IDL> d = eis_getwindata('eis_l0_20071221_001727') ; IDL> eis_raster_fov,d,scale,origin,fovx,fovy ; IDL> print,scale ; 1.00000 1.00000 ; IDL> print,origin ; -32.9291 -79.1299 ; IDL> print,fovx,fovy ; 128.000 184.000
eis_element2mass.pro: ; Returns the mass (in grams or kilograms) of an element. ; EXAMPLE: ; ; IDL> Fe_mass = element2mass('Fe') ; IDL> print,Fe_mass ; 9.27339e-23
eis_slit_tilt.pro: ; PURPOSE : Calculates the slit tilt as a function position ; along the CCD. ; EXAMPLE : dw = eis_slit_tilt(256,512,/short,locations=y) ; wvl = wvl - dw ; plot,y,dw ; ALTERNATIVE USAGE: ; d = eis_getwindata(file,wave) ; dw = eis_slit_tilt(d,locations=y)
eis_wave_corr.pro: ; PURPOSE : PRELIMINARY EIS wavelength corrections for ; orbital variations and slit tilt using moments. ; EXAMPLE : IDL> eis_wave_corr,file,wvl_corr,dw_tilt,dw_t,/show ; IDL> d.wvl = d.wvl - wvl_corr[i,j]
eis_width2velocity.pro: ; Compute thermal and nonthermal velocities. ; EXAMPLE: ; ; Some example thermal widths: ; ; v_t = eis_width2velocity('C','II',1335,/thermal,ti_max=t,therm_fwhm=fwhm) ; ; ion wave A temp K fwhm A ; C II 1335.00 2.2e+04 0.041 ; C IV 1548.00 1.1e+05 0.105 ; N V 1238.00 1.8e+05 0.101 ; O I 1355.00 1.0e+04 0.024 ; O IV 1401.00 1.7e+05 0.102 ; Si II 1304.00 1.4e+04 0.021 ; Si III 1206.00 3.0e+04 0.028 ; Si IV 1393.00 6.3e+04 0.047 ; S I 1472.00 1.0e+04 0.019 ; ; Compare with Feldman, Doschek, and Patterson, ApJ, 209:270-281, 1976 ; ; An example nonthermal velocity: ; ; v_nt = eis_width2velocity('S','I',1900.29,0.04,ti_max=t) ; v_nt = 3.0 km/sec ; t = 10,000 K ; ; Compare with Mariska, Feldman, and Doschek, ApJ, 226:698-705, 1978
eis_add_wd_to_spec.pro: ; This routine takes an EIS spectrum structure and fills in the ; intensity, error and quality tags using the input EIS_GETWINDATA ; structure and a pixel mask.
eis_adjust_mask.pro: ; Because of the grating tilt and CCD offset in the EIS ; instrument, the same pixel position in an EIS image formed from ; one wavelength will not directly correspond to the same pixel ; position in an image from a different wavelength. For this ; reason a pixel mask generated with EIS_PIXEL_MASK needs to be ; adjusted when being used for another wavelength. ; ; This routine performs the adjustment using information from the ; routine EIS_CCD_OFFSET.
eis_ccd_offset.pro: ; Evaluates the spatial offset of the specified wavelength relative ; to He II 256. ; EXAMPLES ; IDL> offset=eis_ccd_offset(195.12) ; IDL> l=findgen(120)+170 ; IDL> plot,l,eis_ccd_offset(l)
eis_cubic_spline.pro: ; Creates an optimised cubic spline fit to the orbital variation of EIS ; emission line centroids. The spline is used by eis_orbit_spline to ; perform the orbital variation correction to the output of eis_auto_fit.
eis_fit_viewer.pro: ; Widget-based routine for studying the Gaussian fits produced by ; EIS_AUTO_FIT.PRO.
eis_flag_night.pro: ; Takes the fit structure from eis_auto_fit and estimates which ; data-columns fall into orbital night. Any columns identified are set ; to missing data in the fitdata data arrays, and the new structure 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/atest/pyoung/headcat_tags.txt.
eis_make_image.pro: ; Given a level-1 FITS file name and a wavelength, this routine ; creates an image at the specified wavelength by summing 7 pixels ; across the line profile.
eis_orbit_spline.pro: ; Takes the centroid tag from the output of the EIS_AUTO_FIT ; routine and computes a fit to the orbital variation. The velocity array ; is averaged in the Y-direction (see the keyword YRANGE=), and a cubic ; spline is fit to the averaged function (see the routine ; EIS_CUBIC_SPLINE). The spline fit is then subtracted from the centroid ; array to give the corrected centroid array. The velocity array is also ; corrected by converting the centroid to km/s.
eis_pixel_mask.pro: ; This is a mouse-based routine that requires for input an image ; array. The image is displayed and a `menu' will appear in the ; IDL window. The options are: ; ; LEFT: Go into `polygon' mode ; MIDDLE: Go into `painting' mode ; RIGHT: Exit ; EXAMPLES: ; EIS_PIXEL_MASK, IMAGE, MASK, WVL, SLIT ; EIS_PIXEL_MASK, IMAGE, MASK, WVL, SLIT, COL=255, MAXIMAGE=0.5
eis_mask_spectrum.pro: ; Using a pixel mask created with EIS_PIXEL_MASK, this routine ; averages the EIS spectra over the specified spatial pixels to ; create an averaged spectrum. The error bars on the intensities ; are correctly calculated. ; EXAMPLE: ; IDL> eis_mask_spectrum, l1name, mask, swspec=swspec, lwspec=lwspec'
eis_tilt_correction.pro: ; Corrects the eis_auto_fit fit structure for the tilt of the EIS slit. ; Both the 1" and 2" slits are accounted for.
eis_winwvl_hdr.pro: ; For the specifed wavelength window in an EIS data object, this routine ; returns the wavelength vector for the window.
errors.pro: ; Given two line intensities/fluxes and their 1-sigma errors, ; calculates the ratio and the 1-sigma error on the ratio.
fe12_density.pro: ; Takes the Fe XII 195 and 186 fit structures produced by eis_auto_fit, ; and creates a density structure containing a density map. The densities ; are derived used the CHIANTI atomic database.
spec_gauss_eis.pro: ; This routine is a 'wrapper' for calling the general purpose ; line fitting routine SPEC_GAUSS_WIDGET. For creating the input ; spectrum in the correct format, try using the routine ; EIS_MASK_SPECTRUM.
eis_find_lineraster.pro: ; Searches if a specific wavelength is within the wavelength ; range of observation of the rasters in the EIS database. ; Example: ; Look for 195.33: ; IDL> acronyms=eis_find_lineraster(195.33,summary=summary,rasters=rasters,lines=lines)
Quicklook tools#
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 only ; 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 only ; 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 only ; 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 only ; 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 only ; 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.
xmoment.pro: calling by xfiles.pro only ; XMOMENT plots mean line profile, and has interactive mouse ; functions to mark where the line is (start/stop pixels) and ; where the continuum is. This information is used by the ; eis_moment__moment program to calulate moments of the line ; profile.
ximovie.pro: calling by xfiles.pro only ; XIMOVIE provides a widget interface to run and control ; images displayed as a movie. The images must be written ; as an assoc file.
Other useful routines#
eis_cat.pro: ; Purpose : widget interface to EIS AS-RUN catalog ; Syntax : IDL> eis_cat
eis_search_rasters.pro: ; PURPOSE : To search the EIS raster database ; EXAMPLE : eis_search_rasters
