Gamma-ray Burst Real-time Sky Map

Burst Details

GRB ID	GRB 041006A
Mission	HETE 2
Date	2004/10/06
Time	12:18:08 UTC
Coordinates
Right ascension	00:54:50
Declination	01:07:14
Galactic Lon.	124.72°
Galactic Lat.	-61.74°
Constellation of	Cetus

Detecting Mission : HETE 2

Light Curve

Optical Afterglow

An afterglow was seen at magnitude 18.5 in the Optical Red (R) filter.

For more information visit http://space.mit.edu/HETE/.

Burst Description

The HETE Fregate and WXM instruments detected GRB 041006 (=H3570) at 12:18:08 UT (44288 SOD) on 06 October 2004. The WXM flight software localized the burst in real time, resulting in a GCN Notice 42 seconds after the burst trigger. The flight error region was a circle of 14 arcminutes radius (90% confidence) centered at

RA = 00h 54m 54s, DEC = +01d 18' 37" (J2000).

Ground analyses of the burst data allow the error region to be refined to a circle of 5.0 arcminutes radius (90% confidence) centered at

RA = 00h 54m 53s, DEC = +01d 12' 04" (J2000).

Preliminary spectral analyses show the 2-30 keV fluence of GRB 041006 to be 5e-6 erg/cm2 and the 30-400 keV fluence to be 7e-6 erg/cm2: the classification for GRB 041006 is, therefore, \"X-ray rich GRB\".

GRB 041006 is very similar to GRB 030329 in its lightcurve shape and spectral characteristics, although it is 20x fainter than GRB 030329. GRB 041006 shows a soft precursor before the main gamma-ray pulse. The empirical redshift indicator for this burst is 0.4; for GRB 030329, it was 0.2.

From: Roland Vanderspek at MIT

M. Galassi, G. Ricker, J-L. Atteia, N. Kawai, D. Lamb, and S. Woosley,
on behalf of the HETE Science Team;

T. Donaghy, E. Fenimore, C. Graziani, M. Matsuoka, Y. Nakagawa,
T. Sakamoto, R. Sato, Y. Shirasaki, M. Suzuki, T. Tamagawa, Y. Urata,
T. Yamazaki, Y. Yamamoto, and A. Yoshida, on behalf of the HETE WXM
Team;

N. Butler, G. Crew, J. Doty, A. Dullighan, G. Prigozhin, R. Vanderspek,
J. Villasenor, J. G. Jernigan, A. Levine, G. Azzibrouck, J. Braga,
R. Manchanda, and G. Pizzichini, on behalf of the HETE Operations and
HETE Optical-SXC Teams;

C. Barraud, M. Boer, J-F Olive, J-P Dezalay, and K. Hurley, on behalf
of the HETE FREGATE Team;

Chart Mode
Constellation Figures
Zoom:

Right Ascension	00:54:50
Declination	01:07:14
Constellation of	Cetus

Zoom:

Right Ascension	00:54:50
Declination	01:07:14
FOV	15 arc-minutes x 15 arc-minutes

Mission Dossier

Mission Name:	HETE 2
Full Mission Name:	High Energy Transient Explorer 2
Participating Nations:	United States of America, France, Japan
Primary Agencies:	Massachusetts Institute of Technology (MIT), National Aeronautics and Space Administration USA (NASA), RIKEN Institute for Physical and Chemical Research Japan, Los Alamos National Laboratory USA, Centre d'Etude Spatiale des Rayonnements (CSER)
Mission Heads:	Mission PI: Dr. George R. Ricker / MIT, Project Scientist: Dr. Thomas L. Cline / NASA Goddard, Program Executive: Marcus A. Watkins / NASA Headquarters, Program Scientist: Dr. Donald A. Kniffen / NASA Headquarters , Program Manager: Dino Machi / NASA Goddard , Mission Manager: Gustave J. Comeyne, Jr. / NASA Goddard , SXC: Dr. George R. Ricker / MIT , WXM: Dr. Nobuyuki Kawai / RIKEN , FREGATE: Dr. Jean-Luc Atteia / CESR
Cost:	$55,000,000.00 US
Expected Lifetime:	4 years
Mission Objective:
The High Energy Transient Explorer is a small scientific satellite designed to detect and localize gamma-ray bursts. The coordinates of GRBs detected by HETE are distributed to interested ground-based observers within seconds of burst detection, thereby allowing detailed observations of the initial phases of GRBs.
Spacecraft Specification:
Design: The HETE-2 spacecraft is a small satellite, weighing 273 pounds. The spacecraft structure of HETE-2 is comprised of two parts: the spacecraft bus (the bottom half closest to the solar panels, which is mostly spacecraft hardware - power, communications, attitude control), and the upper half (furthest from the solar panels), where the science instruments sit. In orbit, the science instruments will always be pointing away from the Sun, and the deployed solar panels will be directed toward the Sun. Orbit: 370 miles x 400 miles (600km X 650km) Dimensions: 2.9 feet x 2.2 feet Mass: 273 lbs.
Instrumentation:
HETE-2 is equipped with instruments sensitive to gamma- and X-ray radiation. These instruments share a common field of view of ~1.5 steradians, span a detectable energy range of about 3 decades, and are capable of immediate inter-instrument communication. French Gamma Telescope FREGATE FREGATE is sensitive to photons in the 6-400 keV energy range. It will provide accurate burst triggers and moderate resolution spectra. FREGATE was built by the CESR in Toulouse, France. Wide-field X-ray Monitor (WXM) WXM is sensitive in the 2-25 keV energy range, with good energy resolution and localization accuracy to ~10 arc-minutes or better. The WXM detectors were built by RIKEN, in Tokyo, Japan, based on a design by the Los Alamos National Laboratory. Soft X-ray Camera (SXC) SXC is sensitive in the 0.5-10 keV energy range, with very good energy resolution and localization accuracy to 30 arc-seconds or better. The SXC was built by the Center for Space Research at MIT Each HETE-2 instrument operates independently of the others; however, if a burst is detected by one of the instruments, the others are notified and begin collecting data at higher temporal and energy resolution. All instruments utilize on board sensors to determine safe and appropriate operational conditions.
Mission History:
In January, 2000, the HETE-2 satellite was fully complete and being prepared for launch from Kwajalein Atoll in the Republic of the Marshall Islands. On January 14, 2000, NASA decided to postpone the launch of HETE-2, for reasons described in a press release reproduced here. HETE-2 was successfully launched on October 9, 2000.

French Gamma Telescope FREGATE

Wide-field X-ray Monitor (WXM)

Soft X-ray Camera (SXC)