New Capabilities in High Energy Astrophysics using the Astro-E2
X-Ray Observatory
Richard Kelley
The Astro-E2 observatory is a rebuild of the original Astro-E
observatory that was lost during launch in February 2000. It is
scheduled for launch into low earth orbit on a Japanese M-V rocket in
a few months. The observatory has been developed jointly by the the
Institute of Space and Astronautical Science/Japan Aerospace
Exploration Agency and the NASA/Goddard Space Flight Center. The
three instruments on the observatory are the high-resolution x-ray
spectrometer (the XRS) featuring a 30-pixel x-ray microcalorimeter
array with 6 eV resolution (FWHM), a set of four CCD cameras (the
XIS) and a combination photo-diode/scintillator detector system (the
HXD) that will extend the band pass up to over 600 keV. A significant
feature of Astro-E2 is that all of the instruments are coaligned and
operated simultaneously. Prime areas for investigation are supernova
remnants, active galaxies and the measurement of black hole
properties via relativistically-broadened Fe-K emission lines, and
the dynamics and inflow properties of the x-ray emitting gas in
clusters of galaxies. A number of enhancements have been made for the
Astro-E2/XRS, including a higher resolution microcalorimeter array, a
mechanical cooler for longer cryogen life, and an improved in-flight
calibration system. The Astro-E2/XIS has also been improved to
include a back-side-illuminated CCD to enhance the low energy
response. Improvements have been made to the x-ray mirrors used for
both the XRS and XIS to sharpen the point spread function and reduce
stray light. In this talk we will present the essential features of
Astro-E2, paying particular attention to the enhancements, and
describe the major scientific strengths of the observatory and the
opportunities for guest investigators.