Hunting GRB Early Optical Emission with TAOS Telescopes Kuiyun Huang Academia Sinica, Institute of...
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Hunting GRB Early Optical Emission with TAOS Telescopes
Kuiyun Huang Academia Sinica, Institute of Astronomy and Astrophysics
(ASIAA),Taiwan
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TAOS ProjectTAOS Project(Taiwan-America Occultation Survey)
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No significant events were found in the first two years (2005-2006) Present upper bound to the size of KBO ( 0.5km < D < 10km) Construct TAOS 2 project
Zhang et al. 2008
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Special Features of TAOS project
Four robotic telescopes (50cm, F/1.9 Cassegrain) 2k x 2 k CCD Camera (EEV CCD 42-40) Field of View ~ 1.7 degree x 1.7 degree Pixel size ~ 3 “ Filter : 5000-7000 A (near R band ) Observational Mode – Zipper mode (0.2 sec exposure) - Stare mode Nearly real-time processing /correlation among
telescopes Response to GCN (GRB Coordinate Network) alert in 1 min
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TAOS GRB Alert System TAOS GRB Alert System
• Exposure time : 0.2s, 1s, 5s, 25s• Follow-up time : 30 minutes
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TAOS GRB observations in 2006-2007TAOS GRB observations in 2006-2007
(1) GRB 071010B Duration : 35s Afterglows : XT, OT Redshift : 0.947 Response telescopes :
TAOSA(1s),TAOSB(5s),TAOSD(25s)
Response time : 52s after trigger 38s after alert Fastest response in this event Time coverage : 63-230 s
(2) GRB 071112C Duration : 15s
Afterglows : XT, OT
Redshift : 0.823
Response telescopes : TAOSA(1s),TAOSB(5s)
Response time :
94s after trigger
41s after alert
Time coverage : 94-4000 s
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GRB 071010B GRB 071010B (Wang, Schwamb & Huang et al. 2008)(Wang, Schwamb & Huang et al. 2008)
No significant correction with the prompt -ray emission
Optical afterglow light curve up to 2 days after the burst
Use Equations of Molinari et al. (2007)Tpeak ~ 158 sInitial Lorentz factor Γ0 ~ 164 (ISM), Γ0 ~ 31 (Wind)
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GRB 071112CGRB 071112C
α = -0.81+/- 0.02
α = -1.36+/- 0.01
α = -1.6+/- 0.1
(Stratta et al. 2007)
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Advantages for GRB Observations Advantages for GRB Observations
(1) Fully automated observing system -- Telescopes can have quick response to GRBs -- Alert software has established to manage GRB alerts and send observing commands to telescopes.(2) Four 50cm-telescopes at same site -- Follow-up with different exposure time -- Obtain high time resolution light curve in early afterglow phase.
Bootes
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Two components of optical emission during the first
few minutes (Vestrand et al. 2006)
(a) The prompt optical emission
Correlated with prompt gamma-ray emission.
Could probe isolated jet from the surrounding medium
(b) The early optical afterglow emission
Uncorrelated with prompt gamma-ray emission
Strongly depends on the nature of medium
Probe early optical emission of Probe early optical emission of GRBsGRBs
T90 =520s T90 =110s
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TAOS
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照片由中央大學提供 ( 拍攝時間 :2007年八月 )
TAOSA, TAOSB
TAOSC
TAOSD
Lulin 1-m
40cm
Thank You!
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TAOSA and TASOB
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TAOS Observing Hours (2005TAOS Observing Hours (2005––2006)2006)
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TAOS TelescopesTAOS Telescopes
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TAOS Shutter-less Zipper ModeTAOS Shutter-less Zipper Mode
row-block(transient state)
CCD snapshotw. time tag(1 to 4)
row-block(steady state)
a more realistic case…
charge transfer(downward)
block readout
TAOSzipper image(a stack of row-blocks)
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data taken on 21 February 2004 (UTC)
TAOS ZIPPER MODE IMAGE
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GRB 050820A : The first case shows the GRB 050820A : The first case shows the two two opticaloptical components components
T90 = 85s
initial burst
major burst
Afterglow emission
Prompt optical emission +Afterglow emission
Vestrand et al. Nature 2006 422, 172
RAPTOR
KONUS
(1) Prompt emission broad-band spectra could constraint evolution of jet itself.
(2) Afterglow emission Afterglow of secondary energy release could merger the fading primary afterglow probe evolution of the interaction how the GRB environment is modified
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THE TAOS TEAM
Institute of Astronomy & Astrophysics and Institute of Earth Sciences, Academia Sinica, TaiwanTyphoon Lee(IES PI), Chi-Yuan(IAA PI), Sun-Kun King,
Andrew Wang, Shang-Yu Wang, Chih-Yi WenInstitute of Astronomy, National Central University, Taiwan
Wen-Ping Chen, Yung-Shin Chang, Soumen Mondal, Kiwi ZhangHarvard-Smithsonian Center for Astrophysics, USA
Charles Alcock, Matthew Lehner, Federica B. Bianco, Rahul DaveThe Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, USA
Kem CookYonsei University, Department of Astronomy, South Korea
Yong-Ik Byun
Department of Physics and Astronomy, University of Pennsylvania, USA Joseph GiammarcoUniversity of California, Berkeley, USA Imke de Pater, John RiceStanford Linear Accelerator Center, USA Stuart MarshallSteward Observatory, The University of Arizona, USA Tim AxelrodAmes Research Center, National Aeronautics & Space Administration, USA Jack Lissauer