;****************************************************************** ; ; UVCS Calibration File - DRAF Version D1.29.A.97.01.30.001 ; Equivalent to Quick-Look Version Q1.29.A.96.04.30.001 ; ; Applicable to A-side electronics only. ; ; Note: number of polynomial coefficients in WAVE, RAD, etc. must be ; the same in LYA, OVI and RED channels. If necessary add zeros. ; ; All values to be checked (TBC). ; ; Updated 2/14/96 by L. Gardner ; Updated 3/22/96 by A. van Ballegooijen - modify WAVE params. ; Updated 3/21-26/96 by L. Gardner ; Updated 4/17/96 by L. Gardner to set reference pixels along the slits ; Updated 4/22/96 by L. Gardner to install G. Naletto's distortion and ; wavelength calibration; wavelength range of Radiometric ; Calibration applicability extended. ; ; Updated 4/25/96 by A. Ciaravella to correct for the dispersion coefficients ; of OVI (primary and redundant) channels ; ; Updated 4/30/96 by A. Ciaravella to correct for the dispersion coefficients ; of primary OVI and Lya channels ; ; Updated 1/30/97 by L. Gardner to modify VLD calibration parameters ; based on info received from M. Romoli. ; ; Updated 2/15/97 by A. Ciaravella to change the lower wavelength reference for ; OVI channel (945 to 935) to allow the calibration of ; esposures with high grating position ; ; Updated 7/25/97 by A. Ciaravella to correct the effective area values as ; obtained with the new efficency formula (1/24/97 correction). ;CHECK THIS The effective area values used on 1/24/97 were wrong. The ; efficency in fact was ; defined as 0.002*(1+0.005(lambda -1240)) ; instead of 0.002/(1+0.005(lambda -1240)) ; ; Updated 9/15/98 by L. Gardner to modify wavelength dependence of LYA ; radiometric calibration at long wavelengths ; ; Updated 4/07/99 by R. Suleiman RED LYA efficiency was corrected from 0.001 to ; 0.0014 ; Updated 10/18/00 by D. Phillips to add OVI slit non-linear correction below ; 50 um, for compatibility with DAS 33. ; Updated 1/11/01 by D. Phillips with new mirror height calibrations ; Updated 3/15/01 by D. Phillips to extend range for wavelength efficiencies ; Updated 6/13/01 by D. Phillips: ; OVI redundant efficiency -> *1.12, LyA efficiency -> *.88 ; Updated 10/01 D. Phillips: New mirror height calibration ; Updated 12/02 D. Phillips: Modified mirror height again ; Updated 5/04 D. Phillips: cross-talk calibration ; Updated 10/04 S. Giordano: VLD Radiometric calibration factor update ; from M. Romoli input - cross-talk commented ;****************************************************************** ; TELECOPE ASSEMBLY: ;****************************************************************** ; ; Calibration of Roll Mechanism position: ; ; At the zero point of the roll angle the UVCS aperture is "on top", ; i.e., furthest away from the +Y panel. The roll angle increases for ; clockwise (CW) motion when looking toward the Sun. The CW limit of the ; roll mechanism is at a roll angle of +192.4 degrees (TBC), and the CCW ; limit is at -166.8 degrees (TBC). The roll limit given below the is ; middle of the dead zone between these CW and CCW limits. ; The launch locked position is -25.7 degrees. ; The resolver readout decreases with increasing roll angle, ; so the CW Limit in the onboard ROLLT table is a number near 0 and ; the CCW Limit is near 65535. The Roll Offset is a correction added ; to the positions read off the resolver: the parameter ROLLRW contained ; in diagnostic telemetry packets is the uncorrected resolver position, ; and the ROLL contained in housekeeping and science packets is ; the corrected position (ROLL = ROLLRW + Roll_Offset, modulo 65536). ; The roll position sent as part of the ROLL command is a "corrected" ; resolver position. The CW and CCW Limits included in the ROLLT table ; also correspond to "corrected" resolver positions. ; CAL.INS.ROLL.REF= 35156. ; ROLL reference value (corrected position) CAL.INS.ROLL.NUM= 1 ; Number of coefficients for ROLANGL CAL.INS.ROLL.VAL= -0.00549316 ; Coefficient r_0 (degrees/LSB) CAL.INS.ROLL.LIM= 192.8 ; Roll limit (degrees) ; ; Calibration of X1 and X2 Pointing Mechanism positions: ; ; The X1 mechanism is on the +Yu side of the instrument (left-hand side ; when looking at the instrument from the front, see EID-B Figure 2.1.1D), ; and the X2 mechanism is on the -Yu side (TBC). Range of motion of each ; mechanism is 110 mm (TBC). Calibrated positions POSX1 and POSX2 are in mm. ; POSX1 = POSX2 = 0 when the instrument axis is nominally pointed at solar ; disk center. Positions increase with distance away from the instrument ; midplane. ; CAL.INS.PTG.X1REF= 2940. ; PTGX1 reference value CAL.INS.PTG.X2REF= 2893. ; PTGX2 reference value CAL.INS.PTG.NUM= 1 ; Number of coefficients for POSX1 and POSX2 CAL.INS.PTG.X1VAL= 0.092199 ; Coefficient p_{1,0} (mm/LSB) CAL.INS.PTG.X2VAL= 0.092199 ; Coefficient p_{2,0} (mm/LSB) ; ; Calibration of angular offset of UVCS roll axis: ; ; The resulting coordinates (INS_Y0,INS_Z0) are relative to the spacecraft ; reference frame. The transformation takes into account that UVCS is ; mounted on the +Y panel of the spacecraft. ; CAL.INS.AXIS.NUM = 3 ; Number of coefficients for INS_Y0 and ; INS_Z0 as functions of POSX1 (first index) ; and POSX2 (second index) CAL.INS.AXIS.YVAL= 0.0, & ; Coefficient Y_00 (arcsec) -38.058, & ; Coefficient Y_10 (arcsec/mm) -38.058, & ; Coefficient Y_01 (arcsec/mm) -0.1312, & ; Coefficient Y_11 (arcsec/mm^2) -0.065605, & ; Coefficient Y_20 (arcsec/mm^2) -0.065605, & ; Coefficient Y_02 (arcsec/mm^2) 0.0, & ; Coefficient Y_22 (arcsec/mm^4) 0.0, & ; Coefficient Y_21 (arcsec/mm^3) 0.0 ; Coefficient Y_12 (arcsec/mm^3) CAL.INS.AXIS.ZVAL= 0.0, & ; Coefficient Z_00 (arcsec) 52.647, & ; Coefficient Z_10 (arcsec/mm) -52.647, & ; Coefficient Z_01 (arcsec/mm) 0.0, & ; Coefficient Z_11 (arcsec/mm^2) 0.0, & ; Coefficient Z_20 (arcsec/mm^2) 0.0, & ; Coefficient Z_02 (arcsec/mm^2) 0.0, & ; Coefficient Z_22 (arcsec/mm^4) 0.0, & ; Coefficient Z_21 (arcsec/mm^3) 0.0 ; Coefficient Z_12 (arcsec/mm^3) ; CAL.INS.AXIS.ROLL= 90.0 ; Roll angle (degrees) of instrument Y-axis ; relative to spacecraft Z axis when ROLANGL ; = 0.0 degrees, measured counter-clockwise ; when looking toward the Sun. ; ; Calibration of Mirror Mechanism *commanded* position: ; Valid for grating positions LYA = 128000, OVI = 176000; 11/15/2000, LDG ; This variable is now a reference, so the parameters below won't need updating DP ; CAL.INS.MIRCMD.REF= 18224.6 ; MIRROR Command reference value for ; which MIRANGL = 2.0 solar radii CAL.INS.MIRCMD.NUM= 4 ; Number of coefficients for MIRANGL CAL.INS.MIRCMD.VAL= 3.41579E-04, & ; Coefficient m_0 (solar_radii/LSB) -4.86398E-09, & ; Coefficient m_1 (solar_radii/LSB^2) 1.18572E-13, & ; Coefficient m_2 (solar_radii/LSB^3) -3.76083e-19 ; Coefficient m_3 (solar_radii/LSB^4) ; ; Calibration of Mirror Mechanism DIT position (16-bit A/D): ; Last update: 3/20/96; 11/15/00 Valid for grtpos mentioned above. ; This is the actual mirror calibration. DP ; CAL.INS.MIRPOS.REF= 18597.4 ; MIRPOS reference value for which ; MIRANGL = 2.0 solar radii CAL.INS.MIRPOS.NUM= 4 ; Number of coefficients CAL.INS.MIRPOS.VAL= 3.48372E-4, & ; Coefficient m_0 (solar_radii/LSB) -5.79016e-09, & ; Coefficient m_1 (solar_radii/LSB^2) 1.91496e-13, & ; Coefficient m_2 (solar_radii/LSB^3) -2.24673e-18 ; Coefficient m_3 (solar_radii/LSB^4) ; ;; Cross-talk calibration DP 04 ;; This comes in the form of reference grating positions for OVI and LYA ;; and a correction for the mirror engineering units based on the 2 grating positions ;CAL.INS.XTALK.OVIREF= 176000 ; reference OVI grtpos for mirror ht calibration ;CAL.INS.XTALK.OVINUM= 1 ;CAL.INS.XTALK.OVIVAL= 0.002005 ; crosstalk slope (mir. units/grt. unit) ;CAL.INS.XTALK.LYAREF= 128000 ; reference OVI grtpos for mirror ht calibration ;CAL.INS.XTALK.LYANUM= 1 ;CAL.INS.XTALK.LYAVAL= 0.002005 ; Calibration of Occulter Mechanism position: ; ; Calibrated position is the width of the exposed area of the telescope ; mirror (in mm). There is no direct readout; the OCCPOS telemetry is ; the commanded mechanism position. ; CAL.INS.OCC.REF= 41109. ; OCCPOS reference value for which ; OCCWDTH = 5.0 mm CAL.INS.OCC.NUM= 2 ; Number of coefficients CAL.INS.OCC.VAL=-0.003521082, & ; Coefficient w_{occ,0} (mm/LSB) -1.576831E-09 ; Coefficient w_{occ,0} (mm/LSB) ; ; Calibration of Sun Sensor voltages: ; CAL.INS.SUN.REF= 2625. ; SUNVT,B,R,L reference value for which ; flux on diode is 0.5 solar flux units CAL.INS.SUN.NUM= 1 ; Number of coefficients CAL.INS.SUN.TOP= 0.000840 ; Coefficient V_{top,0} (solar_flux/LSB) CAL.INS.SUN.BOT= 0.000840 ; Coefficient V_{bot,0} (solar_flux/LSB) CAL.INS.SUN.RHT= 0.000840 ; Coefficient V_{rht,0} (solar_flux/LSB) CAL.INS.SUN.LFT= 0.000840 ; Coefficient V_{lft,0} (solar_flux/LSB) ; ; Calibration of Sun Sensor pointing: ; CAL.INS.SUN.YREF= -6.5 ; Offset of sun sensor optical axis relative CAL.INS.SUN.ZREF= +65.8 ; to the instrument reference frame (arcsec) CAL.INS.SUN.Q1 = 0.7854 ; Linear coefficient of response function CAL.INS.SUN.Q3 = 0.0807 ; Cubic coefficient of response function ; ;****************************************************************** ; VISIBLE LIGHT CHANNEL: ;****************************************************************** ; ; Pointing coordinates relatives to instrument reference frame for ; center of VLD entrance aperture. ; CAL.VLD.REF.ROW = 0.0 ; Not used for VLD CAL.VLD.REF.SCL = 0.0 ; Not used for VLD CAL.VLD.REF.YR = +10.0 ; Angular offset (arcsec) of VLD entrance slit CAL.VLD.REF.ZR = -231.0 ; in instrument reference frame (for MIRANGL=0) ; ; Transmission of VLD filter: ; CAL.VLD.FILTER = 0.001 ; transmission coefficient (not in use, 2/18/97) ; ; Calibration of VLD Polarizer Mechanism position: ; CAL.VLD.POL.REF = 3847. ; Reference value for 0.0 degrees CAL.VLD.POL.NUM = 1 ; Number of coefficients CAL.VLD.POL.VAL = 0.0235 ; Coefficient alpha_0 (deg/LSB) ; ; Calibration of VLD HVPS: ; CAL.VLD.HVPS.REF= 127. ; Reference value for 2000 V CAL.VLD.HVPS.NUM= 1 ; Number of coefficients CAL.VLD.HVPS.VAL= 10.0 ; Coefficient k_0 (Volt/LSB) ; ; Radiometric calibration factor for VLD: ; CAL.VLD.FACTOR = 7.67486e+10/3.31 ;(counts/sec/cm) ; ;****************************************************************** ; LYMAN-ALPHA SPECTROMETER: ;****************************************************************** ; ; Note: The LYA channel is on the right-hand-side of the instrument ; (+Y panel of the S/C facing upward; ROLANGL = 0.0 deg; looking ; toward to Sun). ; ; Transformation from (ROW,COL) on detector to WAVELENGTH ; (in Angstrom) and POSITION along entrance slit (in arcsec). ; ; Wavelength calibration updated Mar. '96, see memo by G. Naletto ; and A. Ciaravella dated Feb '96. In effect the values have been ; changed to include also the distortion effect (G. Naletto, 3/28/96). ; ; COL = W/DW + sum_i=0,7 { A_i G^i } ; ; where: W = lambda - CAL.(det).WAVE.REF ; G = GRTPOS/100000 ; COL = corrected column position ; ; Note: 1) for the LYA channel, the wavelength decreases with ; increasing column number; ; 2) wavelength at fixed column decreases with increasing ; grating position; ; 3) pixel (0,0) on the detector is the pixel closest to the ; entrance slit and closest to the VL channel. ; 4) if ROLANGL = 0.0 [deg], then the field-of-view is over ; the East limb of the Sun, the slit is oriented NS, ; and the row number increases from South to North. ; ; ************ PRELIMINARY VALUES - TO BE CHECKED ************ ; CAL.LYA.WAVE.REF= 1215.67 ; Reference wavelength (Angstrom) CAL.LYA.WAVE.DW = -0.1437 ; Wavelength per pixel (Angstrom) CAL.LYA.WAVE.NUM= 8 ; Number of coefficients CAL.LYA.WAVE.VAL= & ; Coefficients of polynomial in G 1922.25, -4680.68, 9531.44, -11857.5, 8818.56, & -3873.34, 926.696, -93.3883 ; ; Radiometric calibration: effective area of LYA Mirror as function ; of wavelength and occulter position (vignetting fuction): ; (Efficiency = 0.002 at 1216A) ; ; DP 11/00 changed RAD1.* items for new radiometric calibration scheme CAL.LYA.RAD1.WAVNUM= 12 ; Number of wavelengths ; DP 3/01 added 1090 A to cover extreme grating positions CAL.LYA.RAD1.WAVLEN= 1090., 1100., 1125., 1150., & ; Wavelengths (Angstrom) 1175., 1200., 1216., 1250., 1288., & 1325., 1362., 1400 CAL.LYA.RAD1.EFF_WAVE = & ; Efficiency coeffs by wavelength 0.0, 0.0, 0.0518, 0.653, & 0.806, 0.903, 1., 1., 0.799, & 0.681, 0.563, 0.454 CAL.LYA.RAD1.OCCNUM= 6 ; Number of coeffs in occulter polynomial CAL.LYA.RAD1.EFF_OCC = & ; polynomial for effective area based on occulter width 0.00108486, & 0.0326169, & 0.00344229, & -0.000106400, & 1.43375e-06, & -7.54616e-09 CAL.LYA.RAD1.FOCLEN= 750.0 ; Mirror focal length (mm) ; ; Coefficients of polynomials for correction of pixel positions ; on LYA detector (version 03/28/96 G. Naletto): ; CAL.LYA.POLY.NUM= 6 ; Number of coefficients (degree=5) CAL.LYA.POLY.KX = & ; Values of KX coefficients -20.9533 0.0588863 -5.39639e-05 -4.09356e-07 -6.91488e-10 2.64620e-12 & 1.13609 -0.000540781 2.85484e-06 -1.80237e-08 8.51916e-11 -1.23653e-13 & -0.000349114 1.23239e-06 -7.46319e-09 7.36256e-11 -3.96597e-13 6.00397e-16 & 4.78641e-07 -8.86403e-10 3.05777e-12 -7.97271e-14 5.83896e-16 -9.66678e-19 & -3.94627e-10 -3.10089e-14 4.92033e-15 7.19149e-18 -2.79501e-19 5.58098e-22 & 1.62872e-13 1.48150e-16 -3.66944e-18 2.05735e-20 -2.03447e-24 -5.95631e-26 CAL.LYA.POLY.KY = & ; Values of KY coefficients -4.43203 0.922718 0.000589815 -4.76252e-07 -1.99360e-09 3.76627e-12 & -0.0278391 -0.000575268 1.92734e-05 -1.39952e-07 3.93846e-10 -4.02552e-13 & 0.000439788 3.49534e-06 -1.40401e-07 1.01160e-09 -2.84561e-12 2.87147e-15 & -1.08218e-06 -8.90283e-09 3.35193e-10 -2.36788e-12 6.54739e-15 -6.45471e-18 & 1.01115e-09 9.46002e-12 -3.32191e-13 2.33266e-15 -6.41507e-18 6.24891e-21 & -3.38928e-13 -3.52993e-15 1.18844e-16 -8.40047e-19 2.32420e-21 -2.26093e-24 ; ; Pointing coordinates relatives to instrument reference frame for ; reference point on LYA entrance slit. ; CAL.LYA.REF.ROW = 240.5 ; Reference row on the detector CAL.LYA.REF.SCL = 7.0 ; Spatial scale in arcsec per corrected pixel CAL.LYA.REF.YR = +10.0 ; Angular offset (arcsec) of LYA entrance slit CAL.LYA.REF.ZR = 0.0 ; in instrument reference frame (for MIRANGL=0) ; ; Calibration of LYA Slit Mechanism position: ; CAL.LYA.SLT.REF= 1354. ; Reference value for 0.05 mm slit width CAL.LYA.SLT.NUM= 1 ; Number of coefficients CAL.LYA.SLT.VAL= 0.00009563 ; Coefficient w_{slit,0} (mm/LSB) ; ; Calibration of LYA Filter transmission as function of wavelength: ; CAL.LYA.FLT.WAVNUM= 3 ; Number of wavelengths CAL.LYA.FLT.WAVLEN= 1100., & ; Wavelengths (Angstrom) 1190., & 1400. CAL.LYA.FLT.TRANS = 0.000, & ; Filter transmission coefficients 0.001, & 0.001 ; ; Calibration of LYA HVPS: ; CAL.LYA.HVPS.REF = 127. ; Reference value for 4600 V CAL.LYA.HVPS.NUM = 1 ; Number of coefficients CAL.LYA.HVPS.VAL = 10.0 ; Coefficient k_0 (Volt/LSB) ; ; Detector nonlinear response rate: ; CAL.LYA.DETLIN = 100.0 ; count/sec/pixel ; ;****************************************************************** ; O VI SPECTROMETER: ;****************************************************************** ; ; Transformation from (ROW,COL) on detector to WAVELENGTH ; (in Angstrom) and POSITION along entrance slit (in arcsec). ; ; Wavelength calibration updated Mar. '96, see memo by G. Naletto ; and A. Ciaravella dated Feb '96. In effect the values have been ; changed to include also the distortion effect (G. Naletto, 3/28/96). ; ; COL = W/DW + sum_i=0,7 { A_i G^i } ; ; where: W = lambda - CAL.(det).WAVE.REF ; G = GRTPOS/100000 ; COL = corrected column position ; ; Note: 1) for the OVI channel, the wavelength decreases with ; increasing column number; ; 2) wavelength at fixed column decreases with increasing ; grating position; ; 3) pixel (0,0) on the detector is the pixel closest to the ; entrance slit and closest to the VL channel. ; 4) if ROLANGL = 0.0 [deg], then the field-of-view is over ; the East limb of the Sun, the slit is oriented NS, ; and the row number increases from South to North. ; ; ************ PRELIMINARY VALUES - TO BE CHECKED ************ ; CAL.OVI.WAVE.REF= 1031.91 ; Reference wavelength (Angstrom) CAL.OVI.WAVE.DW = -0.0993 ; Wavelength per pixel (Angstrom) CAL.OVI.WAVE.NUM= 8 ; Number of coefficients CAL.OVI.WAVE.VAL= & ; Coefficients of polynomial in G 1870.88, -5042.91, 11528.0, -15805.0, 12790.1, & -6035.55, 1533.02, -162.037 ; ; Radiometric calibration: effective area of OVI Mirror as function ; of wavelength and occulter position (vignetting fuction): ; (Efficiency = 0.0035 at 1032A) ; ; DP 11/00 changed RAD1.* items for new radiometric calibration scheme CAL.OVI.RAD1.WAVNUM= 3 ; Number of wavelengths CAL.OVI.RAD1.WAVLEN= 935., & ; Wavelengths (Angstrom) 1032., & 1200. CAL.OVI.RAD1.EFF_WAVE = & ; Efficiency coeffs by wavelength 1., & ; Constant efficiency per wavelength 1., & 1. CAL.OVI.RAD1.OCCNUM= 10 ; Number of coeffs in occulter polynomial CAL.OVI.RAD1.EFF_OCC = & ; polynomial for effective area based on occulter width 0.00000, & 0.00978302, & 0.0103451, & -0.000411131, & 2.58258e-05, & -1.61248e-06, & 5.93175e-08, & -1.16442e-09, & 1.13942e-11, & -4.37996e-14 CAL.OVI.RAD1.FOCLEN= 750.0 ; Mirror focal length (mm) ; ; Coefficients of polynomials for correction of pixel positions ; on OVI detector (version 03/28/96 G. Naletto): ; CAL.OVI.POLY.NUM= 6 ; Number of coefficients (degree=5) CAL.OVI.POLY.KX = & ; Values of KX coefficients -11.0537 0.0972041 -0.000507072 1.78609e-06 -4.30022e-09 3.06577e-12 & 1.10329 -0.00107011 8.68807e-06 -3.76181e-08 7.41188e-11 -3.72586e-14 & -0.000375975 4.83571e-06 -4.54183e-08 1.98598e-10 -3.30380e-13 7.90579e-17 & 6.86296e-07 -1.05062e-08 1.04244e-10 -4.53520e-13 6.81105e-16 -3.45525e-20 & -6.35126e-10 1.05459e-11 -1.06255e-13 4.56037e-16 -6.30244e-19 -7.80846e-23 & 2.47020e-13 -3.97401e-15 3.93658e-17 -1.64317e-19 2.06109e-22 7.27404e-26 CAL.OVI.POLY.KY = & ; Values of KY coefficients -5.18417 0.810404 0.00355577 -2.33787e-05 7.18865e-08 -8.31768e-11 & 0.0615134 0.000527847 -1.30725e-05 8.67732e-08 -2.67122e-10 3.03894e-13 & -9.23805e-05 -2.90576e-06 4.68118e-08 -2.92026e-10 8.70642e-13 -9.74884e-16 & -3.80164e-08 5.54853e-09 -6.71873e-11 3.98597e-13 -1.16604e-15 1.29765e-18 & 1.94393e-10 -4.14772e-12 3.15332e-14 -1.60086e-16 4.42040e-19 -4.88736e-22 & -1.23762e-13 9.62330e-16 1.99520e-18 -3.33232e-20 1.18323e-22 -1.32924e-25 ; ; Pointing coordinates relatives to instrument reference frame for ; reference point on OVI entrance slit: ; CAL.OVI.REF.ROW = 200.5 ; Reference row on the detector CAL.OVI.REF.SCL = 7.0 ; Spatial scale in arcsec per corrected pixel CAL.OVI.REF.YR = -27.0 ; Angular offset (arcsec) of OVI entrance slit CAL.OVI.REF.ZR = 0.0 ; in instrument reference frame (for MIRANGL=0) ; ; Calibration of OVI Slit Mechanism position: ; CAL.OVI.SLT.REF= 770. ; Reference value for 0.05 mm slit width CAL.OVI.SLT.NUM= 1 ; Number of coefficients CAL.OVI.SLT.VAL= 0.0001046 ; Coefficient w_{slit,0} (mm/LSB) ; added <50 um slit correction 10/00 DP CAL.OVI.SLT.NUM2= 3 CAL.OVI.SLT.VAL2= -.029461 0.000111974 -1.0959e-08 ; ; Calibration of OVI Filter transmission as function of wavelength: ; CAL.OVI.FLT.WAVNUM= 3 ; Number of wavelengths CAL.OVI.FLT.WAVLEN= 950., & ; Wavelengths (Angstrom) 1150., & 1400. CAL.OVI.FLT.TRANS = 0.00, & ; Filter transmission coefficients 0.001, & 0.001 ; ; Calibration of OVI HVPS: ; CAL.OVI.HVPS.REF = 127. ; Reference value for 4600 V CAL.OVI.HVPS.NUM = 1 ; Number of coefficients CAL.OVI.HVPS.VAL = 10.0 ; Coefficient k_0 (Volt/LSB) ; ; Detector nonlinear response rate: ; CAL.OVI.DETLIN = 100.0 ; counts/sec/pixel ; ;****************************************************************** ; Redundant Ly_alpha Channel (RED) (in OVI channel): ;****************************************************************** ; ; Transformation from (ROW,COLUMN) on detector to WAVELENGTH ; (in Angstrom) and POSITION along entrance slit (in arcsec). ; ; Wavelength calibration updated Mar. '96, see memo by G. Naletto ; and A. Ciaravella dated Feb '96. ; ; COL = W/DW + sum_i=0,7 { A_i G^i } ; ; where: W = lambda - CAL.(det).WAVE.REF ; G = GRTPOS/100000 ; COL = corrected column position ; ; Note: 1) for the RED channel, the wavelength increases with ; increasing column number; ; 2) wavelength at fixed column increases with increasing ; grating position; ; 3) pixel (0,0) on the detector is the pixel closest to the ; entrance slit and closest to the VL channel. ; 4) if ROLANGL = 0.0 [deg], then the field-of-view is over ; the East limb of the Sun, the slit is oriented NS, ; and the row number increases from South to North. ; ; ************ PRELIMINARY VALUES - TO BE CHECKED ************ ; CAL.RED.WAVE.REF= 1215.67 ; Reference wavelength (Angstrom) CAL.RED.WAVE.DW = 0.0915 ; Wavelength per pixel (Angstrom) Value by AC CAL.RED.WAVE.NUM= 8 ; Number of coefficients CAL.RED.WAVE.VAL= & ; Coefficient of polynomial in G -644., 5502.87, -12579.5, 17246.6, -13956.7, 6586.04, & -1672.84, 176.816 ; OLD VALUES ; 1273.12, -2634.85, 3371.76, -1662.84, 302.640, & ; 0.0, 0.0, 0.0 ; ; Radiometric calibration: effective area of OVI Mirror (includes ; mirror reflectance, grating efficiency, redundant Ly-alpha mirror ; reflectance and vignetting function) as function of wavelength, ; grating position, and occulter position: ; ; DP 11/00 changed RAD2.* items for new radiometric calibration scheme CAL.RED.RAD2.WAVNUM= 3 ; Number of wavelengths ; DP 3/01 changed to 1090 for extreme grating positions CAL.RED.RAD2.WAVLEN= 1090., & ; Wavelengths (Angstrom) 1200., & 1400. CAL.RED.RAD2.EFF_WAVE = & ; Efficiency coeffs by wavelength 1., & ; Constant efficiency per wavelength 1., & 1. CAL.RED.RAD2.OCCNUM= 10 ; Number of occulter positions CAL.RED.RAD2.EFF_OCC = & ; polynomial for effective area based on occulter width 0.00000, & 0.00747797, & 0.00266865, & -0.000245202, & 2.16369e-05, & -1.08414e-06, & 3.01310e-08, & -4.69067e-10, & 3.83522e-12, & -1.28257e-14 ; FIRST and LAST are functions to return the beginning and end values for the ; occulter width that contribute to the redundant path image at a given pixel. ; At present, they are each interpolated based on two straight lines. DP 11/00 CAL.RED.RAD2.FIRSTNUM= 3 ; Number of interpolation points CAL.RED.RAD2.FIRSTPIX= -33.9785, & 880.00, & 1256.34 CAL.RED.RAD2.FIRSTVAL= 71.0, & 0.0 , & 0.0 CAL.RED.RAD2.LASTNUM= 3 ; Number of interpolation points CAL.RED.RAD2.LASTPIX= -33.9785, & 127.312, & 1256.34 CAL.RED.RAD2.LASTVAL= 71.0, & 71.0 , & 18.0 CAL.RED.RAD2.FOCLEN= 750.0 ; Mirror focal length (mm) ; ; Done. ;