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EIS Data Analysis Demonstration

eis_prep. eis routines. EIS raw data eg. eis_l0_20061202_025412.fits.gz. EIS higher level data eg. eis_l2_20061202_025412.fits. EIS calibrated data eg. eis_l1_20061202_025412.fits ( eis_err_20070207_002712.fits ). level0. level1. level2. EIS Data Analysis Demonstration.

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EIS Data Analysis Demonstration

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  1. eis_prep eis routines EIS raw data eg. eis_l0_20061202_025412.fits.gz EIS higher level data eg. eis_l2_20061202_025412.fits EIS calibrated data eg. eis_l1_20061202_025412.fits (eis_err_20070207_002712.fits) level0 level1 level2 EIS Data Analysis Demonstration Jian Sun (MSSL)

  2. EIS FITS file structure: Some useful EIS FITS keywords: Conventional fits-reading routines (such as readfits.pro, mreadfits.pro) not suitable for EIS FITS files! http://solarb.uio.no/software/eis_usergide/fits_kw_list.htm

  3. Understanding EIS data cube: Line fitting Intensity Wavelength ()  Line width Instrument FWHM of 2~2.5 pixels Example: IDL> v_nt=eis_width2velocity(‘Fe’,’XII’,195.12,0.070,instr=instr)

  4. EIS_PREP routine: What does eis_prep do? * calibrate eis level-0 data to level-1 data and create an additional error file which contains 1σ errors the intensities * Apply EIS effective area curves: (curves are available in $SSW/hinode/eis/response directory) * Remove CCD pedestal and dark current (around of 1% of pixels will end up with a negative DN value after this process) * Mark any saturated, defective pixels and cosmic rays as missing data (by giving them the value -100 in the error fits file

  5. Cosmic ray Hot pixel Warm pixels Raw data Image cleaned with eis_despike * Use EIS cosmic ray routine (eis_despike) flag most of warm and hot pixels Peter Young, RAL Absolute Calibration. Then Data unit become: level-0: data number (DN) level-1: erg cm-2 s-1 sr-1Å-1 * No flat-field correction yet!

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