Skip to content
Permalink
main
Switch branches/tags

web-hack-mirror/mirror/1999/11/23/international.gsfc.nasa.gov/International/Missions/Hete_2/Hete_2.html

Go to file
 
 
Cannot retrieve contributors at this time
121 lines (107 sloc) 6.29 KB
Raw Blame
Open in GitHub Desktop
<HTML>
<HEAD>
<META NAME="GENERATOR" CONTENT="Adobe PageMill 3.0 Win">
<TITLE>International Program Office - HETE 2 Project</TITLE>
</HEAD>
<BODY TEXT="#000099" BGCOLOR="#ffffff" VLINK="#990099">
<P><CENTER><TABLE WIDTH="570" BORDER="0" CELLSPACING="2" CELLPADDING="0">
<TR>
<TD WIDTH="25%">
&nbsp;<IMG SRC="../../../images/hete-2.gif" WIDTH="300" HEIGHT="200"
ALIGN="BOTTOM" BORDER="0" NATURALSIZEFLAG="3"></TD>
<TD WIDTH="75%">
<P><CENTER><B><FONT COLOR="#ff0000" SIZE="+2" FACE="Arial"><IMG
SRC="../../../images/INTL_HETE2_Title_LG.jpg" WIDTH="144" HEIGHT="72"
ALIGN="BOTTOM" BORDER="0" NATURALSIZEFLAG="3"></FONT></B></CENTER></TD>
</TR>
<TR>
<TD COLSPAN="2">
<P>&nbsp;</P>
<P><FONT COLOR="#000099" SIZE="-1" FACE="Arial">The HETE-II is
a cooperative mission between NASA and a consortium of institutions:
</FONT><FONT SIZE="-1" FACE="Arial"><A HREF="http://space.mit.edu/HETE/">MIT</A></FONT><FONT
COLOR="#000099" SIZE="-1" FACE="Arial"> CSR (</FONT><FONT SIZE="-1"
FACE="Arial">PI Institution</FONT><FONT COLOR="#000099" SIZE="-1"
FACE="Arial">), </FONT><FONT SIZE="-1" FACE="Arial"><A HREF="http://www.riken.go.jp/ehome.html">RIKEN
(Japan)</A></FONT><FONT COLOR="#000099" SIZE="-1" FACE="Arial">,
</FONT><FONT SIZE="-1" FACE="Arial"><A HREF="http://nis-www.lanl.gov/nis-projects/hete/index.html">Los
Alamos National Laboratory</A></FONT><FONT COLOR="#000099" SIZE="-1"
FACE="Arial">, </FONT><FONT SIZE="-1" FACE="Arial"><A HREF="http://www.cesr.fr/">CESR
(France)</A></FONT><FONT COLOR="#000099" SIZE="-1" FACE="Arial">,
CNR-TESRE (Italy), UC-Berkeley, University of Chicago, UC-Santa
Cruz, and </FONT><FONT SIZE="-1" FACE="Arial"><A HREF="http://www.supaero.fr/">Supaero</A></FONT><FONT
COLOR="#000099" SIZE="-1" FACE="Arial">.</FONT></P>
<P><FONT COLOR="#000099" SIZE="-1" FACE="Arial">HETE's prime objective
is to carry out a multiwavelength study of Gamma Ray Bursts (GRBs) with
UV, X-Ray, and gamma ray instruments. A unique feature of the mission
will be its capability to localize bursts with several arcsecond accuracy,
in near real-time aboard the spacecraft. These positions are transmitted
to the ground, and picked up by a global network of primary and secondary
ground stations, enabling sensitive follow-up studies.</FONT></P>
<P><B><FONT COLOR="#000099" SIZE="-1" FACE="Arial">Salient Features:</FONT></B></P>
<P><B><FONT COLOR="#000099" SIZE="-1" FACE="Arial">Project Start:</FONT></B><FONT
COLOR="#000099" SIZE="-1" FACE="Arial"> 2nd quarter 1997<BR>
<B>Spacecraft Weight:</B> 150 kg<BR>
<B>Planned Lifetime:</B> 6 months, nothing to preclude 2+ years<BR>
<B>Orbit: </B>600-km x 650-km, &lt; 5 degrees inclination<BR>
<B>Launch:</B> 1/23/00, from Kwajalein Missile Range</FONT></P>
<P><B><FONT COLOR="#000099" SIZE="-1" FACE="Arial">Program Overview:</FONT></B></P>
<P><FONT COLOR="#000099" SIZE="-1" FACE="Arial">The original HETE was
lost due to a Pegasus launch failure on November 4, 1996, but the scientific
importance and continuing relevance of the mission provided the impetus
for NASA, CESR, CNES, and RIKEN to fund a replacement satellite (HETE-2)
scheduled for launch in early 2000. The Study of GRBs has taken on an
even greater scientific significance since the demise of HETE-1 because
of the recent discovery of their cosmological origin that demonstrates
GRBs to be the most powerful explosions in the universe since it's creation
in the Big Bang. HETE-2 will retain nearly all of the original HETE
design elements. A new feature of the spacecraft is the Soft x-ray Cameras,
which takes the place of the UV cameras.</FONT></P>
<P><FONT COLOR="#000099" SIZE="-1" FACE="Arial">The three instruments
on HETE-2 are:</FONT></P>
<P><FONT COLOR="#000099" SIZE="-1" FACE="Arial">1) The French Gamma Telescope
(FREGATE) supplied by the CESR is derived from the design of the successful
Gamma Ray Burst experiment Lilas aboard the Russian Phobos mission.
Its prime objectives are the detection and spectroscopy of gamma-ray
bursts and the monitoring of variable X-Ray source.</FONT></P>
<P><FONT COLOR="#000099" SIZE="-1" FACE="Arial">2) The Wide-Field
X-Ray Monitor (WXM) supplied by the Japanese and Los Alamos consists
of two, crossed one dimensional position sensitive detectors
with a coded aperture. Since it is unlikely that two transients
will occur at the same time, two 1-D coded aperture imaging systems
(in the x and y directions) can be used, simplifying the construction
and software.</FONT></P>
<P><FONT COLOR="#000099" SIZE="-1" FACE="Arial">3) The MIT Soft
X-Ray Cameras (SXC) are two 1-D coded mask systems using CCID-20's
as the detecting elements. The CCD-20's used were fabricated
by MIT Lincoln Lab, each consisting of 2048x4096 pixels measuring
15 um square.</FONT></P>
<P><FONT COLOR="#000099" SIZE="-2" FACE="Arial">Last Updated: 4/21/99</FONT>
</TD>
</TR>
<TR>
<TD COLSPAN="2">
<P><CENTER><TABLE WIDTH="360" BORDER="0" CELLSPACING="2" CELLPADDING="0"
HEIGHT="62">
<TR>
<TD WIDTH="25%" HEIGHT="50">
<P><CENTER><A HREF="http://www.nasa.gov/"><IMG SRC="../../../images/3dmeatball1.gif"
WIDTH="42" HEIGHT="37" ALIGN="BOTTOM" BORDER="0" NATURALSIZEFLAG="0"></A></CENTER></TD>
<TD WIDTH="25%">
<P><CENTER>&nbsp;<A HREF="http://www.gsfc.nasa.gov/"><IMG SRC="../../../images/gsfc_hp_button.gif"
WIDTH="48" HEIGHT="48" ALIGN="BOTTOM" BORDER="0" NATURALSIZEFLAG="0"></A></CENTER></TD>
<TD WIDTH="25%">
<P><CENTER><A HREF="../../../international.html"><IMG SRC="../../../images/INTL_HP_Button.gif"
WIDTH="50" HEIGHT="50" ALIGN="BOTTOM" BORDER="0" NATURALSIZEFLAG="3"></A></CENTER></TD>
<TD WIDTH="25%">
<P><CENTER>
&nbsp;<A HREF="mailto:niacona@ifmp.nasa.gov"><IMG
SRC="../../../images/INTL_Feedback.gif" WIDTH="53" HEIGHT="90"
ALIGN="BOTTOM" BORDER="0" NATURALSIZEFLAG="3"></A>
</CENTER></TD>
</TR>
</TABLE></CENTER></TD>
</TR>
</TABLE></CENTER>
</BODY>
</HTML>