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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

Hunting GRB Early Optical Emission with TAOS Telescopes

Kuiyun Huang

Academia Sinica, Institute of Astronomy and Astrophysics (ASIAA),Taiwan


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
special features of taos project
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

taos grb alert system
TAOS GRB Alert System
  • Exposure time : 0.2s, 1s, 5s, 25s
  • Follow-up time : 30 minutes
taos grb observations in 2006 2007
TAOS GRB observations in 2006-2007

(1) GRB 071010B

 Duration : 35s

 Afterglows : XT, OT

 Redshift : 0.947

 Response telescopes :


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 :


Response time :

94s after trigger

41s after alert

Time coverage : 94-4000 s

grb 071010b wang schwamb huang et al 2008
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)


GRB 071112C

α = -0.81+/- 0.02

(Stratta et al. 2007)

α = -1.36+/- 0.01

α = -1.6+/- 0.1

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.



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


Thank You!




Lulin 1-m



taos shutter less zipper mode
TAOS Shutter-less Zipper Mode

CCD snapshot

w. time tag

(1 to 4)

charge transfer


block readout




a more realistic case…


zipper image

(a stack of



(steady state)

taos zipper mode image
TAOS Zipper Mode Image

data taken on 21 February 2004 (UTC)

grb 050820a the first case shows the two optical components
GRB 050820A : The first case shows the two opticalcomponents


Prompt optical emission


Afterglow emission

(1)Prompt emission

broad-band spectra could

constraint evolution of jet


(2) Afterglow emission

Afterglow of secondary

energy release could

merger the fading

primary afterglow

 probe evolution of the


 how the GRB

environment is modified

Afterglow emission


major burst

T90 = 85s

initial burst

Vestrand et al. Nature 2006 422, 172

the taos team
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