I. Operating Systems Test
       HESSI and associated SSW software has been installed and the
       base model successfully run on the following machines:
       SB - Sunburst, Ultra 2, 2X200MHz, 1GB RAM, IDL 5.1, UNIX Sys. V v4.0
       PC - Gandalf, PII 233MHz, 96MB RAM, IDL 5.2, Win98
       PC2 - Cardon, PII 233MHz, 160MB RAM, IDL 5.2, RedHat Linux 5.2
       PC3 - AMD K6 233MHz, 32MB RAM, IDL 5.0, Win95 ***Note: this is an
             unsupported version of IDL so users should not expect
             everything to work, but tests below are useful for timing
             comparisons***
       (see time tests for comparisons)
       Note: No documented support for Windows installation.

  II. Rate Test
       A. Normal Rates (dead time is unimportant)
       B. High Rates (dead time corrections become important)
       C. Very High Rates (actually in Rate Mode)
           Note: choose photon energy range to correspond to rate
                 energy ranges

 III. Position Tests
       A. Assymetric Source Properly Recovered (size, morphology, and
          orientation) with proper photometry
       B. What Happens for Pure Background Source  -  artifacts ??
          1. Using a Bright Source Which Fully Illuminates Image -
             release I of hessi_image not ready to handle individually
             specified gaussians
          2. Using only the simulated background

  IV. Time Tests
       A. How Computing Time Scales with Map Size
          1. model=fltarr(64,64) with (50,14)=1.0
             hessi_image,model=model,photons=5000
             SB - 1:19
          2. model=fltarr(128,128) & model(100,28)=1.0
             hessi_image,model=model,photons=5000
             SB - 4:16
          3. model=fltarr(256,256) & model(200,56)=1.0
             hessi_image,model=model,photons=5000
             SB - crashed
             see error message 5
       B. How Computing Time Scales with Number of Photons
          1. hessi_image,/model,photons=5000
             SB - 1:17
             PC - 1:45
             PC2 - 1:42
             PC3 - 3:06
          2. hessi_image,/model,photons=10000
             SB - 2:25
             PC - 3:28
             PC2 - 3:20
             PC3 - 6:07
          4. hessi_image,/model,photons=20000
             SB - 4:44
             PC - 6:45
             PC2 - 6:30
             PC3 - 12:04
          5. hessi_image,/model,photons=40000
             SB - 9:24
             PC - 13:24
             PC3 - 12:50
       C. How Computing Time scales with integration time.

   V. Pixel Size
       A. Photometry Recovered Properly on Different Pixel Sizes
          Note: default pixel size not listed in header info of hessi_image
          1. hessi_image,image,/model,photons=5000
             produces image with 14981.0 photons
          2. hessi_image,image,/model,photons=5000,pixel_size=4.0
             produces image with 14716.1 photons
          3. hessi_image,image,model=model,photons=5000,pixel_size=4.0 with
             model=fltarr(128,128) & model(40,80)=1.
             produces image with 15086.4 pixels
       B. Degradation of an Asymmetric Source as Pixel Size Increases

  VI. Statistics Test
       A. Poor Statistics (marginal detection)
       B. Good Statistics (well-detected, but noise dominated by statistics)
       C. Very Good (limited by systematics)

 VII. Energy-dependence test
       A. Explore Effect of Energy Range on Recovered Images
           1. Image at very low energies where windows attenuate
           2. Image at energies observed in front of detector (<60 keV)
           3. Image at energies observed in rear of detector (>100 keV)
           4. Image at energies above and below where specific grids
             become transparent

VIII. Dynamic Range Tests
      A. How well can a weak source be imaged in presence of a strong
         source.  Basically, try to establish the maximum flux ratio between
         2 well-separated sources.
      B. Does presence of strong source bias the photometry of weaker source ?
      C. Photometric performance with a combination of a compact and extended
         source (core / halo)

  IX. Sub-Region Imaging
       A. Create full sun models and see how well images are recovered
          when only imaging a small region

   X. Image Quality versus Position
       A. Run test III at different positions on the Sun
          1. define model=fltarr(64,64) & model(35:45,21)=1.
             and run hessi_image with xoffsets of 0, 600, and 900.
             **Looks like there may be some forshortening of image at solar
               limb
       B. Run test VIII at different positions on the Sun

  XI. Adding Harmonics
       A. How does adding 2nd Harmonics help
       B. How does adding 3rd Harmonics help

 XII. Smoothing
       A. What is the best way to smooth to reduce side-lobes
 
 

This site last updated November 10, 2008.