; IDL common for hardwired instrument parameters used in calibration ; of maps ;!!!these values should be made as seldom-changed parameters ; nxtnd is number of points to which to extend spectral range. MUST BE POWER OF 2! nxtnd = 128 ; search range of pixels for cross-correlation, used in corshft_sbsp.pro ; and slitshft_sbsp.pro nsearch = 15 ; spectral pixel range for averaging reference ; variation of continuum along slit, used in slitshft_sbsp.pro cc1 = 6 & cc2 = 12 ; number of pixels at ends of array to be apodized with cosine bell, used ; in slitshft_sbsp.pro ; !! Not used for Solar-B ; napod = 50 ; range of spectral pixels to cross-correlate, isolate strong lines, used in ; specshft_sbsp.pro wc1 = 10 & wc2 = 108 ; hardwired CCD pixel range along the slit for fitting curvature, used in ; specross_sbsp.pro sr1 = 20 & sr2 = 1000 ; hardwired spectral range around spectrum lines for cross-correlation, ; used in specross_sbsp.pro wl1 = 10 & wl2 = 108 ; Define the range of CCD pixels along the slit to include in the final ; display of calibrated Stokes spectra to avoid vignetted areas, etc. dsx1 = 1 dsx2 = 1023 ; Active spectral pixel range of area after merging for removing spectral ; curvature. This range avoids vignetted areas on either extreme ; of the spectrum. msh1 = 1 msh2 = 111 ; fixed image ranges for two polarization image areas to process spectrally. ; ranges outside this are are flat-fielded without regard to division by ; spectral lines. Both CCDSIDEs should have the same number of pixels ; in each dimension. ; sp1 refers to bottom of spectrum for each side (bottom, top spectral images) ; spectral ranges sp1,sp2 are selected so as the lines occur at roughly ; the same pixels in each image sp1 = [1,1] ; bottom (start) of spectrum for each CCDSIDE sp2 = [111,111] ; top (end) of spectrum for each CCDSIDE sl1 = [1,1] ; left (start) along slit for each CCDSIDE ; lo res has some vignetting at top, so cut it at 640 sl2 = [1023,1023] ; right (end) along slit for each CCDSIDE ; Range of spectral pixels of CCDSIDE1 to shift spectrally in order to ; merge the two CCDSIDES. Range is restricted as such to avoid vignetted ; areas, which are left unshifted. ssh1 = 1 ssh2 = 111 ; For fringe correction after merging and removing spectral curvature, ; set weights for fitting fringes +/-12 pixels on either side of ; each solar line to zero so that the line polarization does not bias ; the fringe fitting. lc1 = 78 ; center of 6301 line lc2 = 125 ; center of 6302 line wss = 12 ; range of pixels about line to omit from fringe fit polsmr = 7 ; boxcar averaging width of spectra before fringe fit polimt = .006 ; wavelength integration of polarization limit below ; which full spectrum is fitted for fringes frfrq = 0.115 ; fringe spectral frequency, radians/pixel boxsmth = 51 ; boxcar smoothing range for fringe coefficients, pixels vlimit = 0.002 ; limit on amplitude of Stokes V polarization fringes tpi = 2.*!pi mfltrng = 17 ; range of pixels for median filtering of spikes guesq = [0.0006,1.5, 0.0016] ; initial guess for fringes in Q,U,V guesu = [0.001,-1.5,-0.0008] ; parameters = [amplitude, phase guesv = [0.0007,-0.7, 0.0008] ; (radians), offset]