Data Set Overview
  =================
    An extended set of new thermal infrared observations of NEOs in
    the range between 5 and 25 microns was obtained during the years
    2000-2003 by Marco Delbo, Alan W. Harris, Rick Binzel, Bobby Bus,
    Michael Mueller, and Mario Di Martino. These observations, on
    which Marco Delbo's Ph.D. dissertation is based, were used to
    derive radiometric albedos and diameters using three different
    thermal models.  The results are reported in Delbo (2004), Delbo
    et al. (2003), and Harris et al. (2003).  The data set includes 32
    asteroids.
 
    The observations were carried out at three different telescopes as
    follows:
 
       - Keck-1 telescope on Mauna Kea, Hawaii, using the Long
         Wavelength Spectrograph (LWS)
 
       - ESO 3.6m telescope at La Silla, Chile, using the Thermal
         Infrared Multi-Mode Instrument (TIMMI2)
 
       - The NASA Infrared Telescope Facilty (IRTF) on Mauna Kea,
         using the MIRSI Mid-Infrared Spectrometer for observations
         of asteroid 35386 (1997 XF11), and using the MIRLIN
         Mid-Infrared Large-Well Imager for all other asteroids.
 
    The resulting infrared fluxes reported in Appendix A of Delbo
    (2004) are included here in the file 'fluxes.tab'.
 
    These infrared observations were used to derive diameters and
    albedos using three different thermal models, the Standard Thermal
    Model (STM, see Lebofsky and Spencer 1989), the Fast Rotating
    Model (FRM, see Lebofsky and Spencer 1989), and the Near Earth
    Asteroid Thermal Model (NEATM, see Harris 1989).  The resulting
    diameters and albedos, reported in Tables 4.2.1, 4.2.2, and 4.2.3
    in Delbo (2004) are included here in the file 'diamalb.tab'.  This
    file also includes the applicable date of observation and phase
    angle extracted from Tables 3.11.1, 3.11.2, and 3.11.3 of Delbo
    (2004).
 
    The error bars shown in the file 'diamalb.tab' represent a
    reanalysis of the errors done by Delbo in 2006.
 
    References:
 
    Delbo, M., The nature of near-earth asteroids from the study of
    their thermal infrared emission, Ph.D. thesis, Freie Universitat
    Berlin, 2004. [DELBO2004]
 
    Delbo, M., A.W. Harris, R.P. Binzel, P. Pravec, and J.K. Davies,
    Keck observations of near-earth asteroids in the thermal infrared,
    Icarus 166, 116-130, 2003.  [DELBOETAL2003]
 
    Harris, A.W., M. Mueller, M. Delbo, and S.J. Bus, The surface
    properties of small asteroids: Peculiar Betulia - A case study,
    Icarus 179, 95-108, 2005.  [HARRISETAL2005]
 
    Harris, A.W. and J.S.V. Lagerros, Asteroids in the thermal
    infrared, in 'Asteroids III', Bottke, W., A. Cellino, P. Paolicci,
    and R.P. Binzel, Eds., University of Arizona Press, Tucson, pp.
    205-218, 2002. [HARRIS&LAGERROS2002]
 
    Harris, A.W., A thermal model for near-Earth asteroids, Icarus
    131, 291-301, 1998. [HARRIS1998]
 
    Lebofsky, L.A. and J.R. Spencer, Radiometry and thermal modeling
    of asteroids, In 'Asteroids II', Binzel, R.P., T. Gehrels, and
    M.S. Matthews, Eds., University of Arizona Press, Tucson, pp.
    128-147, 1989.  [LEBOFSKY&SPENCER1989]
 
    Mueller, M., A.W. Harris, M. Delbo, and S.J. Bus, The sizes and
    albedos of near-earth asteroids, including 6489 Golevka, from
    recent IRTF observations, American Astronomical Society, DPS
    meeting #35, #22.04, Bulletin of the American Astronomical
    Society, Vol. 35, p. 955, 2003.  [MUELLERETAL2003]

Confidence Level Overview
  =========================
    The quoted uncertainties in the diameters and albedos derived from
    the three thermal models refer to the statistical uncertainties in
    the flux measurements.
 
    For discussion of the model uncertainties and sources of error see
    the original publications, Delbo (2004), Harris (1989), and Harris
    and Lagerros (2002).
 
    Note:  The MIRLIN instrument was known to have readout problems
    during the period of time covered by the observations.  However
    the observed objects were all sufficiently bright that the results
    were unaffected.