TY - GEN
T1 - A next generation Ultra-Fast Flash Observatory (UFFO-100) for IR/optical observations of the rise phase of gamma-ray bursts
AU - Grossan, B.
AU - Park, I. H.
AU - Ahmade, S.
AU - Ahnf, K. B.
AU - Barrillone, P.
AU - Brandtg, S.
AU - Budtz-Jørgenseng, C.
AU - Castro-Tiradoh, A. J.
AU - Cheni, P.
AU - Choig, H. S.
AU - Choij, Y. J.
AU - Connellk, P.
AU - Dagoret-Campagnee, S.
AU - De La Taille, C.
AU - Eyles, C.
AU - Hermann, I.
AU - Huang, M. H.A.
AU - Jung, A.
AU - Jeong, S.
AU - Kim, J. E.
AU - Kim, M.
AU - Kim, S. W.
AU - Kim, Y. W.
AU - Lee, J.
AU - Lim, H.
AU - Linder, E. V.
AU - Liu, T. C.
AU - Lund, N.
AU - Min, K. W.
AU - Na, G. W.
AU - Nam, J. W.
AU - Panasyuk, M. I.
AU - Ripa, J.
AU - Reglero, V.
AU - Rodrigo, J. M.
AU - Smoot, G. F.
AU - Suh, J. E.
AU - Svertilov, S.
AU - Vedenkin, N.
AU - Wang, M. Z.
AU - Yashin, I.
AU - Zhao, M. H.
PY - 2012/12/1
Y1 - 2012/12/1
N2 - The Swift Gamma-ray Burst (GRB) observatory responds to GRB triggers with optical observations in ̃ 100 s, but cannot respond faster than ̃ 60 s. While some rapid-response ground-based telescopes have responded quickly, the number of sub-60 s detections remains small. In 2013, the Ultra-Fast Flash Observatory-Pathfinder is expected to be launched on the Lomonosov spacecraft to investigate early optical GRB emission. Though possessing unique capability for optical rapid-response, this pathfinder mission is necessarily limited in sensitivity and event rate; here we discuss the next generation of rapid-response space observatory instruments. We list science topics motivating our instruments, those that require rapid optical-IR GRB response, including: A survey of GRB rise shapes/times, measurements of optical bulk Lorentz factors, investigation of magnetic dominated (vs. non-magnetic) jet models, internal vs. external shock origin of prompt optical emission, the use of GRBs for cosmology, and dust evaporation in the GRB environment. We also address the impacts of the characteristics of GRB observing on our instrument and observatory design. We describe our instrument designs and choices for a next generation space observatory as a second instrument on a lowearth orbit spacecraft, with a 120 kg instrument mass budget. Restricted to relatively modest mass, power, and launch resources, we find that a coded mask X-ray camera with 1024 cm2 of detector area could rapidly locate about 64 GRB triggers/year. Responding to the locations from the X-ray camera, a 30 cm aperture telescope with a beam-steering system for rapid (̃ 1 s) response and a near-IR camera should detect ̃ 29 GRB, given Swift GRB properties. The additional optical camera would permit the measurement of a broadband optical-IR slope, allowing better characterization of the emission, and dynamic measurement of dust extinction at the source, for the first time.
AB - The Swift Gamma-ray Burst (GRB) observatory responds to GRB triggers with optical observations in ̃ 100 s, but cannot respond faster than ̃ 60 s. While some rapid-response ground-based telescopes have responded quickly, the number of sub-60 s detections remains small. In 2013, the Ultra-Fast Flash Observatory-Pathfinder is expected to be launched on the Lomonosov spacecraft to investigate early optical GRB emission. Though possessing unique capability for optical rapid-response, this pathfinder mission is necessarily limited in sensitivity and event rate; here we discuss the next generation of rapid-response space observatory instruments. We list science topics motivating our instruments, those that require rapid optical-IR GRB response, including: A survey of GRB rise shapes/times, measurements of optical bulk Lorentz factors, investigation of magnetic dominated (vs. non-magnetic) jet models, internal vs. external shock origin of prompt optical emission, the use of GRBs for cosmology, and dust evaporation in the GRB environment. We also address the impacts of the characteristics of GRB observing on our instrument and observatory design. We describe our instrument designs and choices for a next generation space observatory as a second instrument on a lowearth orbit spacecraft, with a 120 kg instrument mass budget. Restricted to relatively modest mass, power, and launch resources, we find that a coded mask X-ray camera with 1024 cm2 of detector area could rapidly locate about 64 GRB triggers/year. Responding to the locations from the X-ray camera, a 30 cm aperture telescope with a beam-steering system for rapid (̃ 1 s) response and a near-IR camera should detect ̃ 29 GRB, given Swift GRB properties. The additional optical camera would permit the measurement of a broadband optical-IR slope, allowing better characterization of the emission, and dynamic measurement of dust extinction at the source, for the first time.
KW - Gamma-ray bursts
KW - Space astrophysics instrumentation
KW - Space astrophysics missions
KW - Ultra-Fast Flash Observatory (UFFO)
KW - X-ray instrumentation
UR - https://www.scopus.com/pages/publications/84871799162
U2 - 10.1117/12.926391
DO - 10.1117/12.926391
M3 - Conference contribution
AN - SCOPUS:84871799162
SN - 9780819491442
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Space Telescopes and Instrumentation 2012
T2 - Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray
Y2 - 1 July 2012 through 6 July 2012
ER -