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Introduction to SOT data analysis

Introduction to SOT data analysis. K.Ichimoto with help of T.Berger, Y.Katsukawa, T.Yokoyama, T.Shimizu, M.Shimojo. Hinode workshop , 2007.12.8-10, Beijing. How to find data?. DARTS JAXA data archive/ search system (  Kano) http://darts.isas.jaxa.jp/hinode/top.do

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Introduction to SOT data analysis

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  1. Introduction to SOT data analysis K.Ichimoto with help of T.Berger, Y.Katsukawa, T.Yokoyama, T.Shimizu, M.Shimojo Hinode workshop, 2007.12.8-10, Beijing

  2. How to find data? • DARTS JAXA data archive/ search system ( Kano) • http://darts.isas.jaxa.jp/hinode/top.do • Quick Look movies (NAOJ) • http://solar-b.nao.ac.jp/QLmovies/index_e.shtml • Operation info. (LMSAL) • (timeline for pointing, target, obs. purpose etc.) • https://sot.lmsal.com/operations/timeline/

  3. NAOJ Quick Look movies http://solar-b.nao.ac.jp/QLmovies/index_e.shtml

  4. LMSAL operation info. https://sot.lmsal.com/operations/timeline/

  5. How to get images on your WS? On SSW IDL… IDL> hinode_server_select, /darts ; set a remote server IDL> time0 = '09-Dec-2006T11:30:00' IDL> time1 = '09-Dec-2006T15:00:00' IDL> sot_cat, time0, time1, /level0, cat, files, /URLS IDL> help, files FILES STRING = Array[2994] IDL> ss = sot_umodes(cat,/int) ; interactive selection of data IDL> sock_copy, files[ss], out_dir='./demo‘ ; copy to local disk IDL> lfiles = file_list(‘./demo’, ’*.fits*') IDL> read_sot, lfiles[0], index, dat ; read SOT fits file IDL> help, index, dat INDEX STRUCT = -> MS_250671422001 Array[1] DAT INT = Array[2048, 1024] IDL> tvscl,dat : : Sample programs for tutorial are found in $SSW/hinode/sot/doc/paris/*.pro Courtesy by Dr. Tom Berger

  6. SOT analysis software 3 Dec 2007 Y. Katsukawa (NAOJ) T.Berger (LMSAL)

  7. FG Photometric corrections: Level-0 ⇒ Level-1 • Camera readout errors: fg_shift_pix.pro • Central 2 vertical lines of camera dropped in partial-camera readout. • Top line wrapped around to bottom. • 1x1 and 2x2 are supported. 4x4 still in development. • Dark current and pedestal subtraction: fg_dark_sub.pro • FG camera 4096 x 2048 split-frame read-out: 2048x2048 frames. Each has different pedestal. • Pedestal is temperature dependent. Linear combination of camera and electronics box temperatures. • 1x1 and 2x2 are supported. 4x4 still in development. • Flat field correction: fg_flatfield.pro • Flat fields are created by Kuhn-Lin algorithm. • Currently there are flat images only for • CN 388.3 (also used for Ca II H-line images) • G-band 430.5 • Blue continuum 450.5 • Green continuum 555.0 • Red continuum 668.4 • Fe I 630.2 (affected by a big bubble) • Na ID 589.6 (affected by a big bubble) • Mg Ib 517.3 (affected by a big bubble) • H-alpha 656.3 (affected by a big bubble) • Bad camera pixel correction via map: fg_bad_pix.pro • Cosmic ray removal: sot_nospike.pro • Correction for BFI/NFI plate-scale difference and image shifts: fg_reg_wave.pro

  8. Dark and flat field Avg. Pedestal = 192 Avg. Pedestal = 187 Dark frame example Flat field example (G-band)

  9. FG Photometric corrections • Accomplished via fg_prep.pro (Tom Berger: berger@lmsal.com, Yukio Katsukawa: yukio.katsukawa@nao.ac.jp) • BFI simple filtergrams corrected completely • NFI data product corrected: • FG (simple filtergram) • FGIV (shuttered IV) • FGIQUV (shuttered IQUV) • Shutterless modes still in development. • Polarization calibration still in development • Call formats IDL> fg_prep, index, data, index_out, data_out, /despike IDL> fg_prep, filename_list, -1, index_out, data_out, /despike IDL> fg_prep, index, data, index_out, data_out, /despike, $ x0=256,y0=256, subimgx=768, submigy=512

  10. SP Photometric corrections: Level-0 ⇒ Level-1 • Camera readout errors • Dark current and pedestal subtraction • No shutter for SP: darks only taken before SOT door-open. • Eclipses may offer more. • Flat field correction • Polarimetric calibration • FPP temperature warping • Slit positions wanders vertically during scans. • Spectral lines also wander in the diespersion direction • Combine two spectra • Accomplished by sp_prep.pro (Bruce Lites: lites@hao.ucar.edu, Kiyoshi Ichimoto: ichimoto@solar.mtk.nao.ac.jp , Sam Freeland) • Call formats IDL> sp_prep, filename_list, outdir=directory_name

  11. BFI red continuum, level-0

  12. BFI red continuum, level-1

  13. SP4D20070228_183214.2.fits level-0 I -Q -U -V I Q U V

  14. SP4D20070228_183214.2.fits level-1 I Q U V

  15. S/C +Y S/C +X Definition of SOT polarization coordinate This definition is applied to the Stokes vectors obtained after application of the X-matrix. Raw Stokes products of FPP are not consistent with this definition. -Q N -U -V +U -Q -U +U +V FPP +Q W +Q E -V +V S View from the top of SOT View towards the sun This definition is the same as that used in the analysis of the suntest data of 2004.8 and consistent with the ASP definition, ie. positive V at blue side of spectral line gives positive magnetic flux. This is also consistent with the definition of Stokes V: (right circ. – left circ.), where right circular polarization is positive when electric vector rotates clockwise looking at the source.

  16. IDL program to obtain X X = nfi_pcalx(wav, obs_id=obs_id, expo=expo, $ id_table=id_table, calver=calver, progver=progver) INPUT: wav - wavelength [nm], 517.2, 525.0, 589.6, 630.2, 656.3 obs_id - Obs_ID expo - exposure time [ms], input for shutter mode, output for shutterless mode. id_table- Obs_id list file, default: 'C:\Hinode\ops\dbase\fpptbl\OBS_ID_060208.txt' OUTPUT: calver - version of calibration data ex. ‘delay_2006.1.30/Tmat_2006.1.30’ progver - program version RETURN: X = X[4,4] for shuttered IQUV mode = X[4,4,2] for shutterless IQUV mode giving X for left and right CCD = X[4,2] for shuttered IV mode = X[4,2,2] for shutterless IV mode = X[4] for shuttered FG

  17. Usage of X to calibrate the SOT products: • g Stokes IQUV X[4,4] orX[4,4,2] • shuttered S = X-1 Sobs • shutterless Sleft = X[*,*,0]-1 Sobs,left • Srigh = X[*,*,1]-1 Sobs,right g IV (mag.) X[4,2] or X[4,2,2] shuttered I = Iobs, X[1,0] gives degree of QI crosstalk V = Vobs/ X[3,1], shutterless I = Iobs, X[1,0,*] gives degree of QI crosstalk Vleft = Vobs,left/ X[3,1,0] Vright= Vobs,right/ X[3,1,1] g I simple X[4] (only shutter mode) I = Iobs, X[1-3] gives degree of Q,U,VI crosstalk g IUV X[4,3,2] (only shutterless mode) I = Iobs, X[1,0,*] gives degree of Q I crosstalk Uleft = Uobs,left/ X[3,1,0], Uright = Uobs,right/ X[3,1,1] Vleft = Vobs,left/ X[3,2,0], Vright = Vobs,right/ X[3,2,1] and so on..

  18. Diagnostics using SP data slit Obtain magnetic field vectors and motions in solar atmosphere. Zeeman effect produces polarization in spectral lines

  19. Kosugi Memorial workshop 2007.4.25. NAOJ, Mitaka Milne-Eddington fitting program of the Hinode SOT/SP data T. Yokoyama (U. Tokyo) Y. Katsukawa, M. Shimojo S. Tsuneta, Y. Suematsu, K. Ichimoto (NAOJ) T. Shimizu (JAXA), S. Nagata (Kyoto U.) M. Kubo, B. Lites, H. Socas-Navarro (HAO) Hinode SOT Japan/US team

  20. Introduction – Stokes ME fitting • Fitting (inversion) • In the fitting procedure, we iteratively solve a “forward problem” which is described by the radiative transfer equations including the Zeeman effect. • It is necessary to do a huge amount of computations. So we need an approximation for the efficient (semi-automatic pipeline) process of the data. • The Milne-Eddington (ME) atmosphere model • The Unno-Rachkovsky solution • The solution is simply described by a set of algebraic eqs. • Previous codes • ASP code (Skumanich & Lites 1987) • MELANIE (Socas-Navarro) • …

  21. Milne-Eddignton atmosphere ○ Radiative transfer eq. and assumption Atmospheric parameters B magnetic field strength、 g “ incliation Φ “ azimuth Λ0 line shift ΔλD Doppler width a damping Η0 line/continuum abs. ratio B0 source function B1 source function gradient e.g., J.C. del Toro Iniesta, ‘Spectropolarimetry’ 2002

  22. SOT/SP fitting code • demands • high-performance • Tune-up + Parallelization • Contents of the code • Written in Fortran 90 with IDL front-ends • Derivation of a first guess • PIKAIA code (HAO, Charbonneau) • Genetic algorithm • Fitting • Based on MELANIE (HAO, Socas-Navarro) • Lebenburg-Mardquard method • Infer the 180-degree azimuth ambiguity • MAGPACK2 (Sakurai) • By comparison with the potential field • performance • ~50 msec/pixel • 14 hours for a 1k^2 image. But < 1 hour by a 16-cpu parallel run.

  23. Doppler vel. Doppler width B strength inclination azimuth Line strength damping Source funct. Source grad. Macro turb. Straylit fract. Straylight shift Complement number of the filling factor Fitting results: NOAA 10923

  24. inclination Field strength Comparison with the ASP code’s results Left: SOT/SP Right: ASP code azimuth Straylight fraction

  25. Comparison with the results obtained by the ASP code Field strength inclination Almost consistent. There is a crosstalk between the field strength and the staylight fraction when B is weak. But the average magnetic flux density is consistent. Flux density Straylight fraction Inclination

  26. Level-2 data will be available on the web (DARTS) in near future. Program for simple IQUVD maps files[*] contains SP4D file names ;----------------------------------------------------------------------- iint=[95,105] ; interval for contin image l01=30 ; line (6301.5) position vint1=[5,50] ; interval for Dopp. (CG) <-- 6301.5 l0=75 & w1=2 & w2=10 ; line (6302.5) position and integ interval, sp_prep.pro vint=[57,100] ; interval for Dopp. (CG) <-- 6302.5 ;----------------------------------------------------------------------- nf=n_elements(files) xp=findgen(vint[1]-vint[0]+1)-(vint[1]-vint[0])/2. smap=fltarr(nf,ny,5) for i=0,nf-1 do begin print,i,' ',files[i] s1=gt_sotfits(files[i],fh=fh1,sth=h1) smap[i,*,0]=rebin(s1[iint[0]:iint[1],*,0],1,ny) ; I smap[i,*,1]=rebin(s1[l0-w2:l0-w1,*,1],1,ny)+rebin(s1[l0+w1:l0+w2,*,1],1,ny) ; Q smap[i,*,2]=rebin(s1[l0-w2:l0-w1,*,2],1,ny)+rebin(s1[l0+w1:l0+w2,*,2],1,ny) ; U smap[i,*,3]=rebin(s1[l0-w2:l0-w1,*,3],1,ny)-rebin(s1[l0+w1:l0+w2,*,3],1,ny) ; V iprof=s1(vint(0):vint(1),j,0) iprofr=max(iprof)-iprof smap[i,j,4]=total(xp*iprofr)/total(iprofr) ; CG Dop. endfor

  27. Image co-alignment Hinode Calibration for Precise Image Co-alignment between SOT and XRT (November 2006 - April 2007) T.Shimizu (ISAS/JAXA) et al, 2007, PASJ, 59, 845-852

  28. SOT internal image alignment & scale BFI from read data NFI from ground test (Okamoto etal 2007) Note (1): The offset at the center pixel (2047.5, 1023.5) of the full frame (4K×2K) images to the center pixel of G-band (4305) data. The offset is given in the pixel unit of original image at each wavelength before scaling its magnification. Note (2): Scale deviation from the G-band data. The value larger than 1 means that the pixel scale of original image at each wavelength is larger than that of G-band image.

  29. SOT-XRT offset from the Mercury transit on 2006-11-08 Roll angle offset of SOT/BFI and XRT CCD frames from the solar north direction.

  30. Time variation of pointing wrt. the sun (or sun-sensor) Orbital variation Long-term variation

  31. Need to be done • many Hinode Solar Optical Telescope Data Analysis Guide will appear soon

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