Description of the HIGH-INCLINATION ASTEROID FAMILIES bundle V1.0
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Bundle Generation Date: 2020-06-12
Peer Review: 2007 Asteroid Review, 2007-05-24                                 
Discipline node: Small Bodies Node


Content description based on the data set catalog file description for the PDS3 version, EAR-A-COMPIL-5-HIFAM-V1.0
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Note: for PDS3 data sets migrated to PDS4, the following text is taken
verbatim from the data set description and confidence level note of the
PDS3 data set catalog file. In these cases, some details may not be correct
as a description of the PDS4 bundle.
                                                           
    This data set contains the high-inclination asteroid families of          
    Gil-Hutton (2006).  A data set of 3652 high-inclination numbered          
    asteroids was analyzed to search for dynamical families.  The             
    basic data set was the list of 3697 asteroid synthetic proper             
    elements taken from the Asteroid Dynamic Site, March 2005 version;        
    Knezevic and Milani (2000).  For this analysis, only asteroids            
    with sine of proper inclination greater than 0.3 were used.               
                                                                              
    Three data files are included.  Families.tab contains a list of           
    the members of each of the thirteen families, along with their            
    proper elements.  Clumps.tab contains a list of the members of            
    each of the 22 clumps, along with their proper elements.                  
    Summary.tab lists the families and clumps, with the number of the         
    least-numbered member, the proper elements of the least-numbered          
    member, and the range of proper elements for each family and              
    clump.  A cluster of objects in proper element space is considered        
    a nominal family (clusters related to the breakup of an asteroid)         
    or a clump (clusters not necessarily related to breakup events) if        
    they have a number of members larger or smaller than a limiting           
    number, which is defined as 2.5 times the minimum number of               
    objects for a cluster to be considered significant (Zappala et al.        
    1995).                                                                    
                                                                              
    Further information about the analysis can be found in Gil-Hutton         
    (2006).                                                                   
                                                                              
    Gil-Hutton, R. 2006.  Identification of families among highly             
    inclined asteroids.  Icarus 183, 93-100.                                  
                                                                              
    Knesevic, Z., and A. Milani 2000.  Synthetic proper elements for          
    outer main belt asteroids.  Celest. Mech. 78, 17-46.                      
                                                                              
    Zappala, V., Ph. Bendjoya, A. Cellino, P. Farinella, and C.               
    Froeschle 1995.  Asteroid Families: Search of a 12,487-Asteroid           
    Sample using Two Different Clustering Techniques. Icarus 116,             
    291-314.


Known issues or problems with the data
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    Membership in the families is strongle dependent upon the choice          
    of d(0), the cutoff distance.  See the original paper, Gil-Hutton         
    (2006) for details of the analysis.

PDS3 Source
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Version 1.0 of this bundle was migrated from version 1.0 of the PDS3 data set EAR-A-COMPIL-5-HIFAM-V1.0.