1. The catalog from which we chose the event or from which we used information including:
   
   • ICMES During 1996-2002 [Cane 2003]
   • Helicity of Magnetic Clouds [Leamon 2003]
   • Internal Structure of Magnetic Clouds [Lynch 2003]
   • Halo CMES and Associated Activity [Webb 2003]
   • Solar Sources of Major Geomagnetic Storms [Zhang 2003]
2. The date and time at which each cloud reached 1 AU
   
3. The average speed of the cloud at 1 AU
   
4. The speed of the sheath at 1 AU
   
   • The sheath is the region directly preceding the magnetic cloud and can literally be thought of as a bow shock. It is often characterized by a rise in the temperature, density and speed of the solar winds.
5. The average transit speed of the cloud from the Sun to 1 AU
   • Cane and Richardson determined this by dividing the distance from the earth to the Sun by the time elapsed between when the cloud was seen by the Large Angle and Spectrometric Coronagraph (LASCO) and when it arrived at 1 AU.
6. The date and time at which each cloud was seen by LASCO
   
7. The speed of the cloud when seen by LASCO
   
8. The structure of the magnetic cloud, as described by Webb
   
9. The composition of the cloud including average hydrogen density, average radial temperature and average alpha/proton ratio.
   
10. The peak DST value during the disturbance.
    
    • The DST is a geomagnetic index which measures the world-wide magnetic storm level. Negative DST values indicate a magnetic storm is in progress; the more negative the value the more intense the storm is.
11. The approximate time of occurrence on the Sun as determined by the sheath velocity.
    
12. The actual time and date the event occurred on the Sun, as determined by observations in UV and X-rays.
    
13. The location the event occurred at on the Sun.
    
14. A comments section to give extra information and denote discrepencies between catalogs.
    

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