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HETE history

HETE-2 (High Energy Transient Explorer) a small satellite for studying the cosmic gamma-ray bursts and beyond …. Atsumasa Yoshida (RIKEN). HETE history. 1983— recommended in Santa Cruz meeting Feb 1991— official start of HETE US - Japan - France collaboration

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HETE history

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  1. HETE-2 (High Energy Transient Explorer)a small satellite for studying the cosmic gamma-ray burstsand beyond ….Atsumasa Yoshida (RIKEN)

  2. HETE history • 1983— recommended in Santa Cruz meeting • Feb 1991— official start of HETE • US - Japan - France collaboration • multiwavelength study of GRB in UV, X-ray and gamma-ray • real-time localization and rapid notification • Nov 1996— HETE-1 launch: • lost in failure of 3rd stage separation • Feb 1997— Discovery of GRB afterglow • HETE concept proven, (but by different mission) • Jul 1997— HETE-2 started • UV camera replaced by Soft X-ray Camera in HETE-2

  3. HETE-1 HETE-1 mounted on the Pegasus rocket. The small red object immediately to the left of the solar panel is a set of pyrotechnic bolt cutters, which releases the satellite from the third stage. The second and third stages of the rocket can be seen.

  4. HETE-1 3rd stage + HETE + SAC-B attached. The third stage is the short, black unit behind the DPAF can (along with the instrumentation ring and RCS systems ring), attached to the white second stage. This assembly is still circling the earth as one unit, after failure of the 3rd stage pyrotechnics to release both satellites. HETE-1 inside the DPAF (Dual Payload Attachment Fitting) can. This structure protects HETE-1 while SAC-B is deployed.

  5. HETE-1 Launch in November 1996 ... and Lost

  6. HETE-2 Instruments

  7. The HETE Mission • Prime objective: multiwavelength study of gamma ray bursts (GRBs) with soft/medium X-ray, and gamma ray instruments • Unique feature: capability to localize bursts with several arcsecond accuracy, in near real-time aboard the spacecraft • GRB positions transmitted to the global network of primary and secondary ground stations, enabling sensitive follow-up studies

  8. Primary Science Goals: GRBs • provide accurate postions (±10 arcsec to ±10 arcmin) for ~30 bursts in real time each year. • factor of ~4 more sensitive than the BATSE SDs for low energy spectral features and will provide ~25 GRBs per year on which high-quality spectral studies can be performed. • The 2-25 keV and 3-400 keV sensitivities of the X-ray and gamma ray instruments: effective for studying cyclotron lines and spectra of GRBs at low energies. • ~7.5 times more sensitive than BATSE to bursts from Soft Gamma Ray repeaters: event rate ~ 55 times higher than BATSE.

  9. Secondary Science Goals • detect as many as 500-1000 X-ray bursts per year. • monitor the evolution of X-ray bursts and X-ray transients in the FOV of the X-ray detector. • discover and study X-ray pulsars for ~2 month intervals. • discover and study black hole transients .

  10. Spacecraft Specification • Mass: 126 kg. • Envelope: Fits within cylinder 89cm x 66 cm dia. • Desired orbit: 600 km circular, 0 degree inclination • Operating life: 6 months, nothing to preclude 2+ years • Attitude: Sun pointing. Momentum bias. Attitude controlled to +/- 2 degrees • Data processing: Multi-processor, 80 VAX MIPS • Data Buffering: 96 MBytes of EDAC mass memory • Downlink: 250 kbits/sec data rate with overall bit error rate <2e-8 from data storage to ground archive. • Uplink: 31.25 kbits/sec data rate, overall bit error rate < 1e-8 • Radio Frequencies: S-band uplink (2.092 GHz) and downlink (2.272 GHz) for primary groundstation(s), • VHF downlink only (137.9622 MHz) for secondary stations.

  11. FREnch GAmma-ray TElescope (FREGATE) • Built by CESR (France) • Instrument type NaI(TI);cleaved • Energy Range 6 keV to > 1 MeV • Timing Resolution 4 ms • Spectral Resolution ~40% @ 6 keV ~7% @ 662 keV • Effective Area 120 cm2 • Sensitivity (10 s) 3x10–8 erg cm–2 s–1 over 8 keV—1 MeV • Field of View ~2p sr

  12. Wide-field X-ray Monitor (WXM) • Built by RIKEN and Los Alamos National Laboratory • Instrument type Coded Mask with Position Sensitive Proportional Counter • Energy Range 2 to 25 keV • Timing Resolution 1 ms • Spectral Resolution ~15% @ 6 keV • Detector Quantum Efficiency 90% @ 5 keV • Effective Area ~200 cm2 for each of two units • Sensitivity (10 s) ~8x10–9 erg cm–2 s–1 over the 2-10 keV range • Field of View ~2 sr (total for 4 units) • Angular resolution (1 s) ±6 arcmin

  13. WXM • Two-layered multi-wire proportional counter • Be window • 10m mcarbon wire • Gas mixture: Xe (97%) +CO2 (3%) • Gas pressure 1.4atm

  14. GRB localization with1-D position sensitive detectors

  15. Soft X-ray Camera (SXC) • Built by MIT CSR • Instrument type 4 CCD20 Detectors, 2 optical CCD22 • Camera dimensions 10cmx10cmx17.5cm • Energy Range 500 eV to 14 keV • Timing Resolution ~1 s • Spectral Resolution 46 eV @ 525 eV, 129 eV @ 5.9 keV • Detector Quantum Efficiency 93% @ 5 keV, >20% (0.5-14 keV) • Effective Area 6.1x6.1 cm2 (each of 2 units) • Burst Sensitivity (4 s) 0.47 cts cm–2s–1 • Steady source Sensitivity (4 s) ~700 mCrab x t –1/2 • Field of View 0.91 sr • Focal Plane scale 33" per CCD pixel • Loaclization Precision Faint Burst, 5 s - 15", Bright burst, 22 s, 3" (1 Crab; 10s)

  16. HETE2 Operation Network

  17. 9 1 7 11 5 2 4 6 8 10 3 Secondary Ground Station Network 1 Kwajalein * 167.7 E 8.7 N 2 Christmas Island 157.1 W 1.9 N 3 Hiva Oa (French Polynesia) 139.0 W 9.8 S 4 Galapagos Island (Ecuador) 91.1 W 0.7 S 5 Cayenne (French Guiana) * 51.9 W 4.9 N 6 Natal (Brazil) 35.1 W 5.5 S 7 Accra (Ghana) 0.2 W 5.6 N 8 Malindi (Kenya) 40.2 E 3.0 S 9 Male (Maldives) 73.7 E 3.6 N 10 Singapore * 103.8 E 1.3 N 11 Koror (Palau) 134.5 E 7.3 N

  18. Vibration Test Lincoln Lab - MIT August 1999

  19. Thermal Vacuum Test Lincoln Lab - MIT August-September 1999

  20. Primary Ground Station in Singapore National University of Singapore

  21. Launch in January 2000 • The HETE-2 is scheduled to be launched in January 2000 from Kwajalein, Republic of the Marshall Islands.

  22. ROTSERobotic Optical Transient Search Experiment University of Michigan. Los Alamos National Laboratory Lawrence Livermore National Laboratory OPTICS Canon 200 mm focal length, f/1.8, telephoto lenses in FD mounts IMAGER Apogee Instruments AP-10 CCD cameras with Thomson 2048 x 2048 14 micron imagers. Estimated readout noise: 25 e- at 1.0 Megapixels/sec.

  23. Optical Flash! Up to 9 mag UTC exposure m_v 9:47:18.3 5 secs. 11.82 9:47:43.5 5 secs. 8.95 9:47:08.8 5 secs. 10.08 9:51:37.5 75 secs. 13.22 9:54:22.8 75 secs. 14.00 9:57:08.1 75 secs. 14.53

  24. GRB 990123: Optical Transient ROTSE (Optical) BATSE (gamma-ray)

  25. ROTSE-II ROTSE-II is a set of twin 0.45 meter aperture, f/1.9 telescopes to be operated in stereo mode. Apogee Instruments AP-10 CCD cameras with Thomson 2048 x 2048 14 micron imagers. Estimated readout noise: 25 e- at 1.0 Megapixels/second.

  26. LOTIS Livermore Optical Transient Imaging System • 2 x 2 array of Canon EF 200 mm f/1.8L telephoto lenses w/ Loral 442A 2k x 2k CCDs as the imaging sensors. • Each focal plane area of 3.1 cm x 3.1 cm --- a field-of-view for each camera of 8.8° x 8.8°. • The total field-of-view for the telescope array (allowing for overlap) is therefore 17.4° x 17.4°. • The CCD pixel size of 15 μm x 15 μm results in a pixel resolution of 15 arcsec.

  27. Super-LOTIS • Telescope: Boller & Chivens 0.6 meter f/3.5 reflector w/ computer controllable motor drive. • Imager: a Loral 442A 2048 x 2048 CCD (15 x 15 micron pixels) with LLNL built readout electronics. The CCD is cooled with thermoelectric cooler (to -30 degrees C). • Field-of-View: 0.84 x 0.84 degree field-of-view (1.5 arcsec/pixel). • Resolution - < 1.5 arcsec • Sensitivity - V ~ 19 (10 s), V ~ 21 (60 s) at -30 deg C • Slew Speed - 5 deg/s

  28. 望遠鏡 LX200-30 シュミットカセグレン 口 径 300mm 焦点距離 1000mm (0.33倍RD使用) 視 野 47.2 ‘X 31.4‘ 導入速度 秒速6° 冷却ＣＣＤ ST8E (KAF1600E) 画素数 1530x1020 (160万画素) ２×２ ： ７６５×５１０ 角度分解能 ３．７“ ３×３ ： ５１０×３４０ 角度分解能５．６“ 波長帯 350～925nm (QE > 20%) フィルターなし RIBOTSＲＩｋｅｎ-Ｂｉｓｅｉ Ｏｐｔｉｃａｌ Ｔｒａｎｓｉｅｎｔ Ｓｅｅｋｅｒ RIBOTS Specification

  29. Swift Catching Gamma Ray Bursts on the Fly • Multiwavelength gamma ray burst observatory • Science • Determine origin of GRBs • Use GRBs to probe the early Universe • Three instruments • Gamma-ray camera • X-ray Telescope • UV and Optical Telescope • Rapidly re-pointing “swift” spacecraft • 20-70 s response

  30. Swift Mission Features • Rapid response satellite • 20 - 70 sec to slew within FOV of BAT • autonomous operations • factor 100 improved response time • continue monitoring of fading afterglow

  31. Swift Instrumentation Burst Alert Telescope (BAT) • Real time gamma ray burst positions • half coded FOV 2 steradians • 5200 cm2 CdZnTe pixel array • 10-150 keV band • based on Integral Imager design • 5 times more sensitive than BATSE • ~ 1 burst per day detected • (depends of logN-logS extrapolation) • angular resolution of 22 arcmin giving positions of 1-4 arcmin • onboard processing to provide prompt arc-minute position to satellite ACS and to the ground BAT CdZnTe detector module

  32. Swift mission summary • PI: N. Gehrels (GSFC) • Narrow Field Instruments - Penn State lead • X-ray Telescope & Focal Plane (XRT) - Penn State/Leicester/Brera • UV/Optical Telescope (UVOT) - MSSL/Penn State/UCSB • Burst Alert Telescope (BAT) - GSFC lead • Camera and mask - GSFC • Onboard processing - Los Alamos • LEO orbit, 600 km circular 19 degree inclination • Launch date 2003 • Three-year mission operation life • Orbit stable for 5+ years without propulsion

  33. Space Missions Capable of Localizing Gamma-Ray Bursts Mission loc/yr accuracy delay operating period BeppoSAX 10 1—10 arcmin hours present — 2001? CGRO BATSE 300 >4° 5 sec present — 2002? 100 >1.6° 15 min Interplanetary 70 5’x 10° ~1 day present —2001? network (IPN）1’x 20’ RXTE ASM 4 10 arcmin hours present — 2002? HETE-2 WXM 30 10 arcmin ~10 sec 2000 —2001 SXC 16 10 arcsec INTEGRAL IBIS 20 arcminutes ~10 sec 2001—2003 Swift BAT 300 1—4 arcmin 12 seconds 2003(2004)—2010 XRT ~arcsec 50—70 sec UVOT 0.3 arcsec 200 sec GLAST (>100 MeV) 50 10 arcmin 2005— (GBM) (200) (arcmin-arcsec) (10—300 sec)

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