1 / 11

Gamma-Ray Burst Polarimeter – GAP – aboard the Solar Powered Sail Mission

Gamma-Ray Burst Polarimeter – GAP – aboard the Solar Powered Sail Mission. Launch in May 18. Daisuke YONETOKU (Kanazawa UNIV.), Toshio MURAKAMI (Kanazawa UNIV.) Shuichi GUNJI (Yamagata UNIV.) Tatehiro MIHARA (RIKEN) and GAP Team. Poster #062. Theoretical Model. Inter-Stellar

cecilia-lindsey
Download Presentation

Gamma-Ray Burst Polarimeter – GAP – aboard the Solar Powered Sail Mission

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Gamma-Ray Burst Polarimeter – GAP – aboard the Solar Powered Sail Mission Launch in May 18 Daisuke YONETOKU (Kanazawa UNIV.), Toshio MURAKAMI (Kanazawa UNIV.) Shuichi GUNJI (Yamagata UNIV.) Tatehiro MIHARA (RIKEN)and GAP Team Poster #062

  2. Theoretical Model Inter-Stellar Medium Γ > 100 Internal Shock(prompt) External Shock(afterglow) Central engine B cv ■ Internal / External shock ■ Electron acceleration ■ Strong magnetic field (B > 104G) ■ Synchrotron radiation JET Central Engine Afterglow Polarization We expect to detect the strong linear polarization !! Its direct measurement is key to solve the emission mechanism. † Lazzati et al. † Prompt

  3. IKAROS (Solar Powered Sail) Radiation pressure Launch on May 18, NEXT MONTH Mission Span is 1 year 20m Interplanetary Kite-craft Accelerated by Radiation Of the Sun

  4. GAmma-rayburstPolarimeter dσ 2 dΩ ■ Angular Anisotropy of Compton Scattering ■ Geometrical Symmetry E’γ E’γ Eγ α2 rc2 – 1 + cos2θ ＝ ＋ 2 E’γ Eγ Eγ 140mm 偏光方向 Polarization α : Fine Structure Constant rc : Compton Radius 140mm 60 mm We can observe Polarization : 60 – 300 keV Time resolution of Pol. : 1 sec Time resolution of lightcurve : 125 msec for the IPN Spectrum : 30 – 300 keV Plastic Scintillator CsI R6041-SB R7400p analog HV Unit HV Unit 100 mm FPGA CPU (angle)

  5. GAPFlight Model GAP-P (Power) 6cm, 160g 20 cm, 3700g GAP-S (Sensor)

  6. the deck of GAP and Some Electronics The surface of GAP (Anti-Direction of Solar Panel)

  7. IKAROS

  8. Modulation Curve (π = 80%) KEK Highly Polarized X/Gamma-ray Pencil Beam M=0.446±0.028 Number of Events Pencil Beam (1x1mm) : 80keV, π=80%, 0 100 200 300 GEANT-4 Mass Model Rotation Angle [deg] ■ The experimental results with pencil X-ray are consistent with GEANT-4 simulations within 2% level. ■ Comparing the experimental data and simulation, we make effort to constrain the systematic uncertainty. Uniform irradiation (100keV) Efficiency=0.17, M100% = 0.31 80keV, π=80%, pencil beam, M=0.456

  9. Theoretical Expectation Rate Lazzati et al. (2005) Synchrotron “Ordered B” Synchrotron “Random B” Compton Drag Number Fraction (%) Polarization Degree

  10. According to the BATSE database 14 8 4 2 Expectation Rate(GRB/yr)(3σ) GRB rate in the entire field of view GRB rate within the 30deg from optical axis MDP(GRB’s Polarization Degree)

  11. Summary ■ We will install the GRB Polarimeter – GAP – aboard the solar powered sail “IKAROS”, launched in May 18. ■ GAP has a capability to detect the polarization for GRBs, bright magnetar flares, and Crab nebula. ■ We need the position information of GRBs by Swift, Fermi, IPN, INTEGRAL, Super-AGILE, MAXI, etc… IN NEARFUTURE

More Related