Ultra-fast flash observatory for detecting the early photons from gamma-ray bursts

H. Lim, S. Ahmad, K. B. Ahn, P. Barrillon, S. Blin-Bondil, S. Brandt, C. Budtz-Jørgensen, A. J. Castro-Tirado, P. Chen, H. S. Choi, Y. J. Choi, P. Connell, S. Dagoret-Campagne, C. De La Taille, C. Eyles, B. Grossan, I. Hermann, M. H.A. Huang, S. Jeong, A. JungJ. E. Kim, S. W. Kim, Y. W. Kim, J. Lee, E. V. Linder, T. C. Liu, N. Lund, K. W. Min, G. W. Na, J. W. Nam, K. H. Nam, M. I. Panasyuk, I. H. Park, V. Reglero, J. M. Rodrigo, G. F. Smoot, Y. D. Suh, S. Svetilov, N. Vedenkin, M. Z. Wang, I. Yashin, M. H. Zhao

Research output: Chapter in Book/Report/Conference proceedingConference contribution

1 Citation (Scopus)

Abstract

Gamma-ray bursts (GRBs) are the most luminous transient events with short intense flashes that have been detected in random directions in the sky once or twice per day. Their durations have been measured in seconds, especially short GRBs with duration of < 2 sec. The Ultra-Fast Flash Observatory (UFFO) space mission aims to detect the earliest moments of an explosion which presents the nature of GRBs, resulting into the enhancement of GRB mechanism understanding. The UFFO consists of a couple of wide Field-of-View (FOV) trigger telescopes, a narrow-FOV Slewing Mirror Telescope (SMT) for the fast measurement of the UV-optical photons from GRBs, and a gamma-ray monitor for energy measurement. The triggering is done by the UFFO burst Alert & Trigger telescope (UBAT) using the hard X-ray from GRBs and the UV/optical Trigger Assistant Telescope (UTAT) using the UV/optical photons from GRBs. The UBAT monitors the sky for GRB, and determines their position with sufficient accuracy (10′ at 7.0σ) for follow-up UV/optical observations with the SMT. The primary trigger telescope is based on a fast recognition of position using hard X-ray from GRBs. Whereas the fastest previous experiment, the SWIFT observatory, rarely observed GRB in less than 60 seconds after trigger, the UFFO is designed to begin the UV/optical observations in less than a few seconds after trigger. The SMT uses the novel approach of steering our telescope beam using the rotatable mirror, instead of re-orienting the instrument platform like SWIFT and other previous instruments. The UFFO pathfinder is scheduled to launch into orbit on 2011 November by the Lomonosov spacecraft. This pathfinder is the scaled-down version of UFFO in order to make the first systematic study of early UV/optical light curves, including the rise phase of GRBs. It contains two instruments of UBAT and SMT. It only allows the payload mass of 20 kg and the power consumption of 20 W. The SMT has a fast rotatable mirror, a modified Ritchey-Chrètien telescope with the aperture size of 10 cm diameter, and an image intensifier readout by CCD. The UBAT is using a coded-mask aperture for position detection and their X-ray photons are readout by LYSO crystals and Multi-Anode photomultiplier tubes (MAPMTs) with the effective active area size of 191.1 cm2. With this design, we expect UBAT to trigger ∼44 GRBs/yr and expect SMT to detect ∼10 GRBs/yr.

Original languageEnglish
Title of host publication2nd International Conference on Space Technology, ICST 2011
DOIs
Publication statusPublished - 2011 Nov 29
Event2nd International Conference on Space Technology, ICST 2011 - Athens, Greece
Duration: 2011 Sep 152011 Sep 17

Publication series

Name2nd International Conference on Space Technology, ICST 2011

Other

Other2nd International Conference on Space Technology, ICST 2011
CountryGreece
CityAthens
Period11/9/1511/9/17

Fingerprint

Observatories
Gamma rays
Telescopes
Photons
Mirrors
X rays
Electric power measurement
Electron tubes
Photomultipliers
Charge coupled devices
Explosions
Spacecraft
Masks
Anodes
Orbits
Electric power utilization

All Science Journal Classification (ASJC) codes

  • Aerospace Engineering

Cite this

Lim, H., Ahmad, S., Ahn, K. B., Barrillon, P., Blin-Bondil, S., Brandt, S., ... Zhao, M. H. (2011). Ultra-fast flash observatory for detecting the early photons from gamma-ray bursts. In 2nd International Conference on Space Technology, ICST 2011 [6064669] (2nd International Conference on Space Technology, ICST 2011). https://doi.org/10.1109/ICSpT.2011.6064669
Lim, H. ; Ahmad, S. ; Ahn, K. B. ; Barrillon, P. ; Blin-Bondil, S. ; Brandt, S. ; Budtz-Jørgensen, C. ; Castro-Tirado, A. J. ; Chen, P. ; Choi, H. S. ; Choi, Y. J. ; Connell, P. ; Dagoret-Campagne, S. ; De La Taille, C. ; Eyles, C. ; Grossan, B. ; Hermann, I. ; Huang, M. H.A. ; Jeong, S. ; Jung, A. ; Kim, J. E. ; Kim, S. W. ; Kim, Y. W. ; Lee, J. ; Linder, E. V. ; Liu, T. C. ; Lund, N. ; Min, K. W. ; Na, G. W. ; Nam, J. W. ; Nam, K. H. ; Panasyuk, M. I. ; Park, I. H. ; Reglero, V. ; Rodrigo, J. M. ; Smoot, G. F. ; Suh, Y. D. ; Svetilov, S. ; Vedenkin, N. ; Wang, M. Z. ; Yashin, I. ; Zhao, M. H. / Ultra-fast flash observatory for detecting the early photons from gamma-ray bursts. 2nd International Conference on Space Technology, ICST 2011. 2011. (2nd International Conference on Space Technology, ICST 2011).
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title = "Ultra-fast flash observatory for detecting the early photons from gamma-ray bursts",
abstract = "Gamma-ray bursts (GRBs) are the most luminous transient events with short intense flashes that have been detected in random directions in the sky once or twice per day. Their durations have been measured in seconds, especially short GRBs with duration of < 2 sec. The Ultra-Fast Flash Observatory (UFFO) space mission aims to detect the earliest moments of an explosion which presents the nature of GRBs, resulting into the enhancement of GRB mechanism understanding. The UFFO consists of a couple of wide Field-of-View (FOV) trigger telescopes, a narrow-FOV Slewing Mirror Telescope (SMT) for the fast measurement of the UV-optical photons from GRBs, and a gamma-ray monitor for energy measurement. The triggering is done by the UFFO burst Alert & Trigger telescope (UBAT) using the hard X-ray from GRBs and the UV/optical Trigger Assistant Telescope (UTAT) using the UV/optical photons from GRBs. The UBAT monitors the sky for GRB, and determines their position with sufficient accuracy (10′ at 7.0σ) for follow-up UV/optical observations with the SMT. The primary trigger telescope is based on a fast recognition of position using hard X-ray from GRBs. Whereas the fastest previous experiment, the SWIFT observatory, rarely observed GRB in less than 60 seconds after trigger, the UFFO is designed to begin the UV/optical observations in less than a few seconds after trigger. The SMT uses the novel approach of steering our telescope beam using the rotatable mirror, instead of re-orienting the instrument platform like SWIFT and other previous instruments. The UFFO pathfinder is scheduled to launch into orbit on 2011 November by the Lomonosov spacecraft. This pathfinder is the scaled-down version of UFFO in order to make the first systematic study of early UV/optical light curves, including the rise phase of GRBs. It contains two instruments of UBAT and SMT. It only allows the payload mass of 20 kg and the power consumption of 20 W. The SMT has a fast rotatable mirror, a modified Ritchey-Chr{\`e}tien telescope with the aperture size of 10 cm diameter, and an image intensifier readout by CCD. The UBAT is using a coded-mask aperture for position detection and their X-ray photons are readout by LYSO crystals and Multi-Anode photomultiplier tubes (MAPMTs) with the effective active area size of 191.1 cm2. With this design, we expect UBAT to trigger ∼44 GRBs/yr and expect SMT to detect ∼10 GRBs/yr.",
author = "H. Lim and S. Ahmad and Ahn, {K. B.} and P. Barrillon and S. Blin-Bondil and S. Brandt and C. Budtz-J{\o}rgensen and Castro-Tirado, {A. J.} and P. Chen and Choi, {H. S.} and Choi, {Y. J.} and P. Connell and S. Dagoret-Campagne and {De La Taille}, C. and C. Eyles and B. Grossan and I. Hermann and Huang, {M. H.A.} and S. Jeong and A. Jung and Kim, {J. E.} and Kim, {S. W.} and Kim, {Y. W.} and J. Lee and Linder, {E. V.} and Liu, {T. C.} and N. Lund and Min, {K. W.} and Na, {G. W.} and Nam, {J. W.} and Nam, {K. H.} and Panasyuk, {M. I.} and Park, {I. H.} and V. Reglero and Rodrigo, {J. M.} and Smoot, {G. F.} and Suh, {Y. D.} and S. Svetilov and N. Vedenkin and Wang, {M. Z.} and I. Yashin and Zhao, {M. H.}",
year = "2011",
month = "11",
day = "29",
doi = "10.1109/ICSpT.2011.6064669",
language = "English",
isbn = "9781457718748",
series = "2nd International Conference on Space Technology, ICST 2011",
booktitle = "2nd International Conference on Space Technology, ICST 2011",

}

Lim, H, Ahmad, S, Ahn, KB, Barrillon, P, Blin-Bondil, S, Brandt, S, Budtz-Jørgensen, C, Castro-Tirado, AJ, Chen, P, Choi, HS, Choi, YJ, Connell, P, Dagoret-Campagne, S, De La Taille, C, Eyles, C, Grossan, B, Hermann, I, Huang, MHA, Jeong, S, Jung, A, Kim, JE, Kim, SW, Kim, YW, Lee, J, Linder, EV, Liu, TC, Lund, N, Min, KW, Na, GW, Nam, JW, Nam, KH, Panasyuk, MI, Park, IH, Reglero, V, Rodrigo, JM, Smoot, GF, Suh, YD, Svetilov, S, Vedenkin, N, Wang, MZ, Yashin, I & Zhao, MH 2011, Ultra-fast flash observatory for detecting the early photons from gamma-ray bursts. in 2nd International Conference on Space Technology, ICST 2011., 6064669, 2nd International Conference on Space Technology, ICST 2011, 2nd International Conference on Space Technology, ICST 2011, Athens, Greece, 11/9/15. https://doi.org/10.1109/ICSpT.2011.6064669

Ultra-fast flash observatory for detecting the early photons from gamma-ray bursts. / Lim, H.; Ahmad, S.; Ahn, K. B.; Barrillon, P.; Blin-Bondil, S.; Brandt, S.; Budtz-Jørgensen, C.; Castro-Tirado, A. J.; Chen, P.; Choi, H. S.; Choi, Y. J.; Connell, P.; Dagoret-Campagne, S.; De La Taille, C.; Eyles, C.; Grossan, B.; Hermann, I.; Huang, M. H.A.; Jeong, S.; Jung, A.; Kim, J. E.; Kim, S. W.; Kim, Y. W.; Lee, J.; Linder, E. V.; Liu, T. C.; Lund, N.; Min, K. W.; Na, G. W.; Nam, J. W.; Nam, K. H.; Panasyuk, M. I.; Park, I. H.; Reglero, V.; Rodrigo, J. M.; Smoot, G. F.; Suh, Y. D.; Svetilov, S.; Vedenkin, N.; Wang, M. Z.; Yashin, I.; Zhao, M. H.

2nd International Conference on Space Technology, ICST 2011. 2011. 6064669 (2nd International Conference on Space Technology, ICST 2011).

Research output: Chapter in Book/Report/Conference proceedingConference contribution

TY - GEN

T1 - Ultra-fast flash observatory for detecting the early photons from gamma-ray bursts

AU - Lim, H.

AU - Ahmad, S.

AU - Ahn, K. B.

AU - Barrillon, P.

AU - Blin-Bondil, S.

AU - Brandt, S.

AU - Budtz-Jørgensen, C.

AU - Castro-Tirado, A. J.

AU - Chen, P.

AU - Choi, H. S.

AU - Choi, Y. J.

AU - Connell, P.

AU - Dagoret-Campagne, S.

AU - De La Taille, C.

AU - Eyles, C.

AU - Grossan, B.

AU - Hermann, I.

AU - Huang, M. H.A.

AU - Jeong, S.

AU - Jung, A.

AU - Kim, J. E.

AU - Kim, S. W.

AU - Kim, Y. W.

AU - Lee, J.

AU - Linder, E. V.

AU - Liu, T. C.

AU - Lund, N.

AU - Min, K. W.

AU - Na, G. W.

AU - Nam, J. W.

AU - Nam, K. H.

AU - Panasyuk, M. I.

AU - Park, I. H.

AU - Reglero, V.

AU - Rodrigo, J. M.

AU - Smoot, G. F.

AU - Suh, Y. D.

AU - Svetilov, S.

AU - Vedenkin, N.

AU - Wang, M. Z.

AU - Yashin, I.

AU - Zhao, M. H.

PY - 2011/11/29

Y1 - 2011/11/29

N2 - Gamma-ray bursts (GRBs) are the most luminous transient events with short intense flashes that have been detected in random directions in the sky once or twice per day. Their durations have been measured in seconds, especially short GRBs with duration of < 2 sec. The Ultra-Fast Flash Observatory (UFFO) space mission aims to detect the earliest moments of an explosion which presents the nature of GRBs, resulting into the enhancement of GRB mechanism understanding. The UFFO consists of a couple of wide Field-of-View (FOV) trigger telescopes, a narrow-FOV Slewing Mirror Telescope (SMT) for the fast measurement of the UV-optical photons from GRBs, and a gamma-ray monitor for energy measurement. The triggering is done by the UFFO burst Alert & Trigger telescope (UBAT) using the hard X-ray from GRBs and the UV/optical Trigger Assistant Telescope (UTAT) using the UV/optical photons from GRBs. The UBAT monitors the sky for GRB, and determines their position with sufficient accuracy (10′ at 7.0σ) for follow-up UV/optical observations with the SMT. The primary trigger telescope is based on a fast recognition of position using hard X-ray from GRBs. Whereas the fastest previous experiment, the SWIFT observatory, rarely observed GRB in less than 60 seconds after trigger, the UFFO is designed to begin the UV/optical observations in less than a few seconds after trigger. The SMT uses the novel approach of steering our telescope beam using the rotatable mirror, instead of re-orienting the instrument platform like SWIFT and other previous instruments. The UFFO pathfinder is scheduled to launch into orbit on 2011 November by the Lomonosov spacecraft. This pathfinder is the scaled-down version of UFFO in order to make the first systematic study of early UV/optical light curves, including the rise phase of GRBs. It contains two instruments of UBAT and SMT. It only allows the payload mass of 20 kg and the power consumption of 20 W. The SMT has a fast rotatable mirror, a modified Ritchey-Chrètien telescope with the aperture size of 10 cm diameter, and an image intensifier readout by CCD. The UBAT is using a coded-mask aperture for position detection and their X-ray photons are readout by LYSO crystals and Multi-Anode photomultiplier tubes (MAPMTs) with the effective active area size of 191.1 cm2. With this design, we expect UBAT to trigger ∼44 GRBs/yr and expect SMT to detect ∼10 GRBs/yr.

AB - Gamma-ray bursts (GRBs) are the most luminous transient events with short intense flashes that have been detected in random directions in the sky once or twice per day. Their durations have been measured in seconds, especially short GRBs with duration of < 2 sec. The Ultra-Fast Flash Observatory (UFFO) space mission aims to detect the earliest moments of an explosion which presents the nature of GRBs, resulting into the enhancement of GRB mechanism understanding. The UFFO consists of a couple of wide Field-of-View (FOV) trigger telescopes, a narrow-FOV Slewing Mirror Telescope (SMT) for the fast measurement of the UV-optical photons from GRBs, and a gamma-ray monitor for energy measurement. The triggering is done by the UFFO burst Alert & Trigger telescope (UBAT) using the hard X-ray from GRBs and the UV/optical Trigger Assistant Telescope (UTAT) using the UV/optical photons from GRBs. The UBAT monitors the sky for GRB, and determines their position with sufficient accuracy (10′ at 7.0σ) for follow-up UV/optical observations with the SMT. The primary trigger telescope is based on a fast recognition of position using hard X-ray from GRBs. Whereas the fastest previous experiment, the SWIFT observatory, rarely observed GRB in less than 60 seconds after trigger, the UFFO is designed to begin the UV/optical observations in less than a few seconds after trigger. The SMT uses the novel approach of steering our telescope beam using the rotatable mirror, instead of re-orienting the instrument platform like SWIFT and other previous instruments. The UFFO pathfinder is scheduled to launch into orbit on 2011 November by the Lomonosov spacecraft. This pathfinder is the scaled-down version of UFFO in order to make the first systematic study of early UV/optical light curves, including the rise phase of GRBs. It contains two instruments of UBAT and SMT. It only allows the payload mass of 20 kg and the power consumption of 20 W. The SMT has a fast rotatable mirror, a modified Ritchey-Chrètien telescope with the aperture size of 10 cm diameter, and an image intensifier readout by CCD. The UBAT is using a coded-mask aperture for position detection and their X-ray photons are readout by LYSO crystals and Multi-Anode photomultiplier tubes (MAPMTs) with the effective active area size of 191.1 cm2. With this design, we expect UBAT to trigger ∼44 GRBs/yr and expect SMT to detect ∼10 GRBs/yr.

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T3 - 2nd International Conference on Space Technology, ICST 2011

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Lim H, Ahmad S, Ahn KB, Barrillon P, Blin-Bondil S, Brandt S et al. Ultra-fast flash observatory for detecting the early photons from gamma-ray bursts. In 2nd International Conference on Space Technology, ICST 2011. 2011. 6064669. (2nd International Conference on Space Technology, ICST 2011). https://doi.org/10.1109/ICSpT.2011.6064669