'CHIANTI-format' effective areas

These 'CHIANTI-format' effective areas are to be used in conjunction with ch_ss, and contain:

1. The latest effective areas as of August 2006, available within Solarsoft:
   $SSW/hinode/eis/response/EIS_EFFArea_A.003
   $SSW/hinode/eis/response/EIS_EFFArea_B.003
   
2. The solid angle factor for 1 EIS pixel and 1" slit (2.3 10^{-11})
3. The conversion from detected photons to data numbers, with a CCD gain = 6.9

• the above effective areas, and the inclusion of the conversion to data numbers will result in total count rates somewhat different from those published in Del Zanna and Mason (2005). This paper is available through ADS
  or here as a draft document.
• The above effective areas and the CHIANTI simulations should only be used for approximate estimates of the count rates.
• Large discrepancies between predicted and observed count rates are to be expected for a few lines/ions, most notably the He lines (but also see Del Zanna et al. (2002) )

'CHIANTI-format' DEMs

• Average quiet Sun
• Average active region (SERTS-89)
• Average coronal hole

How to use CHIANTI ch_ss

1. Calculate the line intensities using one of the DEMs, appropriate densities and ion fraction, in the 170-290 Angstroms range.
2. Create a spectrum by selecting an appropriate set of elemental abundances.
   Select 170-210 for the SW channel, and the EIS_SW_003.area file [250-290 and EIS_LW_003.area for the LW channel]. Once you click on the effective area button you will be taken to the standard CHIANTI directory, so if you will have to type in the exact location of these files.
   Set the FWHM to 0.04, which is the [approximate] full-width-half-maximum for EIS.
3. Once the spectrum is created, clicking on single lines will give you the total count rates. There are options to save them as tables in ascii or latex.
   Follow the CHIANTI user guides for more details.

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