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\title{ABSOLUTE FLUX DISTRIBUTIONS OF SOLAR ANALOGS FROM THE UV TO THE 
	NEAR-IR}
\author{Luis Colina\thanks{Affiliated with the Astrophysics Division,
Space Sciences Department of ESA.} and Ralph Bohlin\\
\\
Space Telescope Science Institute\\
\\
3700 San Martin Drive\\
\\
Baltimore, MD 21218\\
\\
Email: colina@stsci.edu, bohlin@stsci.edu}

\maketitle

\abstract{
The 0.225$-$2.695$\mu$m absolute flux distributions of the solar analogs 
P041C, P177D, and P330E are presented. The ultraviolet and
optical wavelength range from 0.225$\mu$m to 0.825$\mu$m is based on
high signal-to-noise spectra obtained with the HST Faint Object Spectrograph 
(FOS). The spectra in the near-infrared longward of
0.825$\mu$m are scaled versions of the absolute flux calibrated
reference spectrum of the Sun from Colina, Bohlin, \& Castelli (1996).

In the 0.400$\mu$m to 0.825$\mu$m range,
the spectral energy distribution of P041C is 
slightly hotter than the Sun, 5900K vs.\ 5777K, and agrees with
the shape of the solar spectrum to 5\% in the optical. P177D shows
evidence for interstellar absorption from the dust that corresponds 
to A$_V$=0.03 magnitudes in the visual. The spectral energy distribution of
P330E is the same as the reference spectrum within 2\%--3\%. 

At wavelengths shortward of 0.4$\mu$m, the differences in the spectral energy
distribution between the Sun and the solar analogs are larger, and not well 
understood. When normalized to the same V~flux, P041C and P330E are brighter 
than the Sun by up to 50\% below 0.25$\mu$m,
whereas P177D is as much as 10\% fainter.

The synthesized visual magnitudes and B$-$V colors of the FOS absolute 
fluxes of P041C, P177D, and P330E
agree with ground-based broad-band photometry to 0.02 magnitudes.

The flux distributions of our new solar analogs will help
establish the absolute calibration of NICMOS, the HST near-infrared camera
and multi-object spectrograph. The spectra are available via the WWW.}