Description of the SPECTROSCOPY AND PHOTOMETRY OF JUPITER  
        TROJANS bundle V1.0
=========================================================

Bundle Generation Date: 2020-02-28
Peer Review: 2008 Asteroid Review, 2008-06-12                                 
Discipline node: Small Bodies Node


Content description based on the data set catalog file description for the PDS3 version, EAR-A-EMMI-3-FORNASIER-V1.0
====================================================================================================================

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 results of the visible spectroscopic           
    and photometric survey of Jupiter Trojans reported in Fornasier et        
    al. 2004 and Fornasier et al. 2007.  The survey was carried out at        
    the 3.5 m New Technology Telescope of the European Southern               
    Observatory at La Silla, Chile.  The observing runs took place in         
    November 2002, April 2003, May 2004, and January 2005.  Included          
    are visible spectroscopy and BVRI photometry of 73 Jupiter                
    Trojans, focussing on members of dynamical families.  The results         
    include spectra of both the L4 swarm (24 objects) and the L5 swarm        
    (49 objects).                                                             
                                                                              
    All the data were acquired using the ESO Multi-Mode Instrument            
    (EMMI) in Low Dispersion Spectroscopy (RILD) mode, with a 2 x 1           
    mosaic of 2048 x 4096 CCDs with square 15 micron pixels.  The             
    instrumental setup was as follows:                                        
                                                                              
    Spectroscopy, Nov. 2002, May 2004 and Jan. 2005 runs:  Grism #1           
    (150 g/mm), wavelength range 4100-9400 A, dispersion of 3.1 A/pix         
    (200 A/mm) in first order, slit width of 1.0 arcsecond in Nov.            
    2002 and Jan. 2005, and 1.5 arcsecond in May 2004.                        
                                                                              
    Spectroscopy, April 2003 run:  Grism #7 (150 g/mm), wavelength            
    range 5200-9500 A, dispersion of 3.6 A/mm in first order, slit            
    width 1.0 arcsecond.                                                      
                                                                              
    Photometry for all runs:  Wide field imaging with Bessel-type             
    broadband B, V, R, and I filters (centered respectively at 4139,          
    5426, 6410, and 7985 Angstroms), in 2 x 2 binned mode, pixel scale        
    0.33 arcsec/pix.  Since the sky conditions were not photometric           
    for the May 2004 run, BVRI photometry was not obtained for the            
    targets of that run, specifically the Eurybates family members.           
                                                                              
    Spectra were reduced to reflectivity by dividing each spectrum by         
    that of the solar analog star observed closest in time and airmass        
    to the object observation.  The solar analog star used for each           
    spectrum is specified in the data label.  Full details of data            
    reduction are given in Fornasier et al. 2004 and Fornasier et al.         
    2007.                                                                     
                                                                              
    The spectra are included in this data set in the directory                
    data/spectra.  The observational circumstances for the                    
    spectroscopic observations are in the file data/spectrumtable.tab.        
    The photometric results, from Table 3 of each of the two papers,          
    are in the file data/photometry.tab,  The entries in this table           
    have been combined and sorted by asteroid number, but the column          
    entries are identical to those presented in the two papers.               
                                                                              
    References                                                                
    =======                                                                   
                                                                              
    Fornasier, S., E. Dotto, F. Marzari, M.A. Barucci, H. Boehnhardt,         
    O. Hainaut, and C. de Bergh, Visible spectroscopic and photometric        
    survey of L5 Trojans: Investigation of dynamical families, Icarus         
    172, 221-232, 2004.                                                       
                                                                              
    Fornasier, S., E. Dotto, O. Hainaut, F. Marzari, H. Boehnhardt, F.        
    De Luise, and M.A. Barucci, Visible spectroscopic and photometric         
    survey of Jupiter Trojans: Final results on dynamical familes,            
    Icarus 190, 622-642, 2007.


Known issues or problems with the data
======================================

    The user is referred to Fornasier et al. 2004 and Fornasier et al.        
    2007 for a discussion of the confidence level of the data.

PDS3 Source
===========

Version 1.0 of this bundle was migrated from version 1.0 of the PDS3 data set EAR-A-EMMI-3-FORNASIER-V1.0.