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Hunting GRB Early Optical Emission with TAOS Telescopes

Hunting GRB Early Optical Emission with TAOS Telescopes. Kuiyun Huang Academia Sinica, Institute of Astronomy and Astrophysics (ASIAA),Taiwan. TAOS Project (Taiwan-America Occultation Survey). No significant events were found in the first two years (2005-2006)

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Hunting GRB Early Optical Emission with TAOS Telescopes

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  1. Hunting GRB Early Optical Emission with TAOS Telescopes Kuiyun Huang Academia Sinica, Institute of Astronomy and Astrophysics (ASIAA),Taiwan

  2. TAOS Project(Taiwan-America Occultation Survey)

  3. 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

  4. Special Featuresof 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

  5. TAOS GRB Alert System • Exposure time : 0.2s, 1s, 5s, 25s • Follow-up time : 30 minutes

  6. TAOS 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

  7. GRB 071010B (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 s Initial Lorentz factor Γ0 ~ 164 (ISM), Γ0 ~ 31 (Wind)

  8. GRB 071112C α = -0.81+/- 0.02 (Stratta et al. 2007) α = -1.36+/- 0.01 α = -1.6+/- 0.1

  9. 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

  10. Probe early optical emission of GRBs • 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 T90 =520s T90 =110s

  11. TAOS

  12. Thank You! TAOSA, TAOSB 40cm TAOSC Lulin 1-m TAOSD 照片由中央大學提供(拍攝時間:2007年八月)

  13. TAOSA and TASOB

  14. TAOS Observing Hours (2005–2006)

  15. TAOS Telescopes

  16. TAOS Shutter-less Zipper Mode CCD snapshot w. time tag (1 to 4) charge transfer (downward) block readout row-block (transient state) a more realistic case… TAOS zipper image (a stack of row-blocks) row-block (steady state)

  17. TAOS Zipper Mode Image data taken on 21 February 2004 (UTC)

  18. GRB 050820A : The first case shows the two opticalcomponents RAPTOR Prompt optical emission + Afterglow emission (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 Afterglow emission KONUS major burst T90 = 85s initial burst Vestrand et al. Nature 2006 422, 172

  19. The TAOS Team Institute of Astronomy & Astrophysics and Institute of Earth Sciences, Academia Sinica, Taiwan Typhoon Lee(IES PI), Chi-Yuan(IAA PI), Sun-Kun King, Andrew Wang, Shang-Yu Wang, Chih-Yi Wen Institute of Astronomy, National Central University, Taiwan Wen-Ping Chen, Yung-Shin Chang, Soumen Mondal, Kiwi Zhang Harvard-Smithsonian Center for Astrophysics, USA Charles Alcock, Matthew Lehner, Federica B. Bianco, Rahul Dave The Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, USA Kem Cook Yonsei University, Department of Astronomy, South Korea Yong-Ik Byun Department of Physics and Astronomy, University of Pennsylvania, USAJoseph Giammarco University of California, Berkeley, USAImke de Pater, John Rice Stanford Linear Accelerator Center, USA Stuart Marshall Steward Observatory, The University of Arizona, USATim Axelrod Ames Research Center, National Aeronautics & Space Administration, USAJack Lissauer

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