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\begin{document}
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% Title block, Authors and addresses
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{\Huge\bf%
The Far Ultraviolet Spectroscopic Explorer \\
(FUSE) Mission: Three Years and Counting}
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\begin{center}{\LARGE\vspace*{-5 pt}%
Operated by The Johns Hopkins University
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\titlebox{Overview}
%\titlebox{\Large\bf% Overview}
{\Large\bf%
\newpar 
The Far Ultraviolet Spectroscopic Explorer ({\it FUSE}) satellite was launched 
from Cape Canaveral on a Delta-II rocket on 24 June 1999.  It resides in a 
765 km (480 miles) circular orbit inclined 25 degrees to the Earth's equator, 
and orbits once every 100 minutes. 
}
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% Figure 1
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{{\vspace*{0.25 in}
  \epsscale{0.92}
  \begin{center}
  \plotone{liftoff2.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Figure~1.~~{\it FUSE} was launched on a Delta-II rocket on 24 June 1999 from
Cape Canaveral, Florida.  Three solid strap-on boosters were needed to lift the
3000 pound, 5-meter (18-foot) tall satellite into orbit.
  }
}
{\Large\bf%
\newpar The {\it FUSE} scientific instrument consists of four telescopes that
focus far-ultraviolet (900 - 1187 \AA) light from distant astronomical sources
into devices called ``spectrographs'' that break the light into a spectrum 
and record it electronically.  These spectra are then relayed to radio antennas 
on Earth, and then sent by ground link to a Satellite Control Center at JHU.
}
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{{\vspace*{0.25 in}
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  \begin{center}
  \plotone{toaster.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Figure~2.~~The {\it FUSE} science instrument is shown in schematic form. Four
telescope mirrors feed far-ultraviolet light to four spectrographs that image their data onto two
microchannel plate detectors. The data are encoded electronically and
downlinked to the ground for processing and analysis.  
  }
}
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% Figure 
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{{\vspace*{0.25 in}
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  \begin{center}
  \plotone{tricollab2.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Many Institutions and nearly 600 people participated in the development of 
the {\it FUSE} satellite. The mission is funded by NASA with significant
contributions from international partners:  The Canadian Space Agency, which
provided the Fine Error Sensor guide cameras for {\it FUSE}, and the French
Space Agency, Centre National d'Etudes Spatiale (CNES), which provided the
high quality holographic diffraction gratings that allow {\it FUSE} 
spectrographs to do their job.  The University of California, Berkeley, and
the University of Colorado Boulder built and qualified the detectors and
spectrographs, respectively.
  }
}
{\newpar
}
{\newpar
}
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% Figure 3
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{{\vspace*{0.25 in}
  \epsscale{0.95}
  \begin{center}
  \plotone{observatory.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Figure~3.~~All critical functions for operating the {\it FUSE} satellite as
an Observatory for the Astronomical community are handled at JHU. This includes
such things as processing and technical review of proposals from astronomers
who wish to use the satellite, creation of event and observation timelines,
uplink and downlink of commands and data from the satellite, and processing
of the data into a format useful to the astronomers who requested the data.
About 25 people are currently involved in satellite operations at
JHU.
  }
}
{\newpar
}
{\newpar
}
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% Figure 4
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{{\vspace*{0.25 in}
  \epsscale{0.95}
  \begin{center}
  \plotone{SCC.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Figure~4.~~The {\it FUSE} Satellite Control Center (SCC) is located on the
first floor in the Bloomberg Center for Physics and Astronomy on the Homewood 
campus at JHU. All command loads, ground station scheduling, satellite health 
and safety monitoring, and telemetry and data processing are handled by the
Mission Operations Team for {\it FUSE}.
  }
}
{\newpar
}
{\newpar
}
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% Figure 5
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{{\vspace*{0.25 in}
  \epsscale{0.95}
  \begin{center}
  \plotone{uprm_radome.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Figure~5.~~The {\it FUSE} ground station antenna is located at the University
of Puerto Rico in Mayaguez.  The antenna is housed in a protective Radome, 
which also allows the electronics to be climate controlled, improving reliability
in this subtropical climate.  (The Radome passes radio signals, and does not have
to move ``out of the way" to permit operation.) This antenna is operated remotely 
from JHU or by staging automated control of ground station passes when the 
control center is unstaffed.  The {\it FUSE} satellite passes over Puerto Rico 
about 6-7 times per day and can link to the satellite for 10-15 minutes per
contact.  At other times, the satellite operates autonomously using commands
stored onboard.
  }
}
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% Figure 6
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{{\vspace*{0.25 in}
  \epsscale{0.95}
  \begin{center}
  \plotone{osc_satellite.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Figure~6.~~This is an artist's concept of what {\it FUSE} looks like 
on-orbit.  The model of {\it FUSE} to your right is full scale, but is
incomplete in the sense that portions have been left open so you can see
inside.  The box at the bottom is the spacecraft and the large section on top
is the science instrument.  The blue rectangles in the picture above are
the solar panels (not included on the model).  The pipe sticking out of one
side of the spacecraft represents one of two radio antennas used by the 
satellite to talk to the ground.  The white rectangles in the picture show
positions of radiators on {\it FUSE} that remove excess heat from the
onboard electronics.  The black circle at the bottom of the model matches the
size of the Delta-II rocket shroud into which {\it FUSE} had to fit to be 
launched. It was a tight fit!
  }
}
\titlebox{Pointing the FUSE Satellite}
%\titlebox{\Large\bf% Pointing the FUSE Satellite}
{\Large\bf%
\newpar 
{\it FUSE} does not carry any rockets or other expendable gas jets.  Rather,
its pointing and stability are controlled by devices in the spacecraft
section of the satellite that are computer-controlled.  Spinning wheels
called Reaction Wheel Assemblies (RWAs) create torques (forces) that control 
the pointing, and gyroscopes inside two Inertial Reference Units (IRUs) sense
the changes in position and feed this information to the control computer.
In late 2001, problems developed with two of the RWAs, and the control system
was updated to use other devices (called Magnetic Torquer Bars, essentially
electromagnets) to assist in controlling the pointing.  By running electric
current through the MTBs, magnetic fields are generated locally that interact
with the Earth's magnetic field to help stabilize the satellite pointing.
{\it FUSE} can be pointed to better than 1 arcsecond (1/3600th of a degree)
using this control system. 
}
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% Figure 7
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{{\vspace*{0.25 in}
  \epsscale{0.95}
  \begin{center}
  \plotone{Spacecraft_fig.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Figure 7.~~The inside of the {\it FUSE} spacecraft is mostly empty space!  Computers,
electronics, and attitude control (pointing) devices such as reaction wheels
and gyros are all needed to point {\it FUSE} around the sky and hold it
steady during observations of astronomical sources. 
  }
}
\titlebox{Prime and Extended Missions}
%\titlebox{\Large\bf% Prime and Extended Missions}
%{\Large\bf% 
{\newpar 
The {\it FUSE} project was initially funded by NASA for a Prime Mission
period that included three years of science operations.  During this time, 
{\it FUSE} has performed a mixture of observations proposed by the {\it FUSE} 
Science Team (the scientists who proposed {\it FUSE} to NASA) and Guest 
Investigators (astronomers selected by NASA to participate in the mission).
The Prime Science Mission concluded March 30, 2003.
}
{\newpar 
However, the demand to use {\it FUSE} remains high, and a peer review 
committee established by NASA has recommended that {\it FUSE} continue 
to be operated for at least several more years.  This time period, called 
the Extended Mission, will be devoted entirely to observations proposed 
by astronomers from around the world.
}
%{\Large\bf% 
{\newpar 
The {\it FUSE} project is part of NASA's {\it Origins} initiative, and
is supported by NASA Contract NAS5-32985 to The Johns Hopkins University. 
}
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% Figure 8
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{{\vspace*{0.25 in}
  \epsscale{0.95}
  \begin{center}
  \plotone{jhu_team_5_98.eps}
  \end{center}
 }
 \parbox{\cwd in}{\cappar \ \ \\
  Figure 8.~~The {\it FUSE} Science and Mission Operations team, near its peak 
size (photo from May 1998).
  }
}
{\newpar
}
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%\titlebox{Magellanic Cloud SNRs}
%{\newpar Morse, J. A., et al. 1996, AJ 112, 509.}
%{\newpar Blair, W. P., et al. 2000, ApJ 537, 667.}
%{\newpar Magellanic Cloud SNRs show a wealth of detail at HST resolution, and
%having the objects at a known distance is a great advantage. We have performed two
%detailed studies of the objects N132D (LMC) and E0102-7219 (SMC), two of the
%premiere remnants of core collapse SNe we have available for study.}
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%\titlebox{More Distant Galaxies}
%{\newpar Blair, W. P., unpublished.} 
%{\newpar Blair, W. P., Fesen, R. A., \& Schlegel, E. M. 2001, AJ, 121, 1497.}  
%{\newpar Even at distance of $\sim$5 Mpc, HST has the power to resolve SNR
%Cloud SNRs.}
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%% Conclusion
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%\titlebox{Epilogue}
%{\newpar 
%}
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%% References
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%\begin{figure}\caption{\label{rawimage}}\end{figure}
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%\begin{figure}\caption{\label{oimage}  }\end{figure}
\end{document}