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\centerline {\Large \bf PROJECT SUMMARY }
\bigskip
\centerline {\large \bf A High Elevation Antarctic Terahertz Telescope (HEAT)}

\vspace{0.5cm}

Based on the results of an NSF-funded design study in 2006 and the
successful deployment of a 
full prototype to Antarctica in 2007, we propose to develop and deploy an
automated, 0.5-meter THz observatory for remote operation at the
summit of Dome~A, the highest point on the Antarctic plateau.  
The High Elevation Antarctic Terahertz Telescope ({\tt HEAT}) will
operate from 158 to 372~$\mu$m, and observe the brightest and most
diagnostic spectral lines from the Galaxy.   It will replace {\tt
Pre-HEAT}, the NSF-funded prototype 450~$\mu$m tipper \& spectrometer that was
successfully deployed to Dome~A in 2007-8 with the University of New
South Wales' PLATeau Observatory ({\tt PLATO}).   
The full {\tt HEAT} telescope will be transported to Dome~A in the
first year of 
this work (2009-10) for integration with {\tt PLATO}.  Together, they
will operate autonomously from Dome A for up to a year at a time, with
commands 
and data being transfered to and from the experiment via satellite daily. At 
Dome~A, {\tt HEAT} will see good atmospheric transmission at 200$^+\mu$m during
much of the winter, and usable transmission in the pivotal 160~$\mu$m
window for $\sim$20\% of the winter.  The {\tt HEAT} heterodyne instrument 
package will utilize established mixer, local oscillator, amplifier,
cryogenic, and digital signal processing technologies. 
HEAT/PLATO is the Dome~A component of the multinational 
``AstroPoles'' program which has been offically endorsed by the Joint
Committee for the upcoming International Polar Year (IPY). 

\section*{What is the intellectual merit of the proposed activity?}

{\tt HEAT} will forge entirely new capabilities for ground based infrared
and submillimeter astronomy which otherwise would be 
unachievable except via expensive airborne or space-based
platforms.  {\tt HEAT} and {\tt PLATO} 
represent a new generation of polar instrumentation that permits the excellent 
conditions available from remote sites like Dome A to be harnessed
without the costs and hazards associated with manned operations. 
The unparalleled stability, exceptional dryness, low wind
and extreme cold make Dome~A a ground-based site without equal for
astronomy at infrared and submillimeter wavelengths.  {\tt HEAT} will operate in the 
atmospheric windows between 158 and 370~$\mu$m, in which the most crucial
astrophysical spectral diagnostics of the formation of galaxies,
stars, planets, and life are found.  {\tt HEAT} will answer timely and 
fundamental questions about the evolution
of the interstellar medium and star formation.  In particular, 
through large-scale Galactic surveys, 
the measurement and {\bf impact of the Galactic
environment} on the {\bf life cycles of interstellar clouds} and their
{\bf relation to star formation} will finally be realized. 
The receiver system itself serves as a flexible 
testbed for heterodyne Terahertz components.  Future upgrades of 
mixer, local oscillator, low-noise amplifier, cryogenic, and digital 
signal processing technologies are planned and will play essential roles in
future Terahertz observatories. 
This pioneering mission will pave the way for future astronomical
investigations from Dome~A. 

\section*{What are the broader impacts of the proposed activity?}

{\tt HEAT}'s key project is to map with great sensitivity and precision, 
the Southern Galactic Plane in the
spectral light of the dominant coolants of the interstellar medium.
Definitive and comprehensive science 
products from the survey and its many synergistic 
collaborations will be made available to the astronomical 
community via the Web in a timely manner.  These survey products
will enhance the value of numerous contemporary surveys.
Beneficiaries include the GLIMPSE and ``C2D'' Legacy
programs from the Spitzer Space Telescope, the most recent HI and CO
surveys of the Galactic Plane, and the 2MASS infrared sky survey.
{\tt HEAT} will serve both as a scientific and technological pathfinder for 
future suborbital and space-based missions. 
Finally, the design and fabrication of {\tt HEAT} will be an interdisciplinary
team effort involving students from astronomy, optical
sciences, and electrical engineering.  Astronomical instrumentation is
becoming ever more complex, requiring the talents of many individuals
to bring them to fruition.  Providing students with both technical 
training and team-work experience increases their probability of 
of success not only within astronomy, but society as a whole. 

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