High Energy Polarimetry Missons in Japan; PoGOLite, SPHiNX, PolariS

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1 High Energy Polarimetry Missons in Japan; PoGOLite, SPHiNX, PolariS Hiromitsu Takahashi (Hiroshima University) PoGOLite balloon 10m (2013~) SPHiNX satellite 0.5m (Plan: 2016~) PolariS satellite 6m (Plan: 2020~)

2 Crab Polarized Sources Synchrotron emission: - Rotation-powered neutron stars (e.g. Crab pulsar) - Pulsar wind nebulae (e.g. Crab nebula) - Jets in active galactic nuclei (e.g. Mkn 501, 1E ) - Gamma-ray bursts Compton scattering: - Accretion disk around black holes (e.g. Cygnus X-1) Propagation in strong magnetic field: - Highly magnetized neutron stars (e.g. Hercules X-1, Magnetars) Cygnus X-1 Scattering Synchrotron emission

3 Polarization Measurement (X/gamma-ray) - Polarization measurements in X/gamma-rays have been expected to provide a powerful probe into high-energy emission mechanism around pulsars, black hole binaries, active galactic nuclei etc. - However, X/gamma-ray polarization has been measured only GRBs and at 2.6/5.2 kev and above 200 kev from the Crab nebula and Cyg X-1. - Additional measurements (middle10s kev band / other sources) are needed (New missions: TSUBAME, ASTRO-H, SPHiNX, GEMS, Polaris ). (c) astro.psu.edu Gamma-ray (25-80 kev) ~40 km

4 Polarimeter Design Figure of Merit: Minimum Detectable Polarisation (3σ) Bragg-reflected photons, Photo-electrons Compton-scattered photons Pair-created e+/etend to be detected one direction. Background rate Good mirror, Shielding Modulation for 100% polarized source Good position resolution Signal rate Good mirror, Large effective area Observation time

5 Polarimeter Design Modulation curve Figure of Merit: Minimum Detectable Polarisation (3σ) Bragg-reflected photons, Photo-electrons Compton-scattered photons Pair-created e+/etend to be detected one direction. Background rate Good mirror, Shielding Modulation factor Modulation for 100% polarized source Good position resolution Signal rate Good mirror, Large effective area Observation time Polarization degree

6 Future Satellite Missions (by Tamagawa) PoGOLite balloon (2010~) Source : faint Mirror/background rejection : needed => US: SMEX, JP: Small satellite AOs GAP (2010~) GRB : bright Very small satellite: OK Green: will be launched Red: Plan 日 :Japan, ス :Sweden 米 :US

7 Polarized Gamma-ray Observer (PoGOLite) Hiromitsu Takahashi (Hiroshima University) Sweden (KTH, Stockholm Univ., Esrange, DST Control) Japan (Hiroshima Univ., Nagoya Univ., Waseda Univ., Tokyo Tech., ISAS/JAXA) US (SLAC, Univ. of Hawaii) PI: Mark Pearce (KTH, Royal Institute of Technology)

8 Polarized Gamma-ray Observer (PoGOLite) - The Polarized Gamma-ray Observer, PoGOLite, is a balloon experiment with the capability of detecting 10% polarization from a 200 mcrab celestial object in the energy-range kev. (1 Crab ~ 0.2 kev, power-law index ~ 2.1) - The project is international collaboration including Japan, Sweden and US. - Its pathfinder flight took place in the summer of 2013 from Kiruna, Sweden (c) astro.psu.edu Gamma-ray (25-80 kev) ~40 km Weight (wo ballast) : ~1750 kg Power : ~300 W (Instrument) ~200 W (Gondola, etc.)

9 Pathfinder Flight from Sweden Flight Plan (1-day long) Crab nebula (Pulsar) Cyg X-1 (Black hole binary) (c) ESA Solar flare (c) JAXA (c) astro.psu.edu PoGOLite: - large effective area, low background => Suitable for bright sources. - long exposure => high statistics, variability, flaring activities.

10 Flight Record of PoGOLite - In the summer 2010, there was a plan of 1 or 2-day Kiruna However, it was cancelled due to NASA launch failure in Australia in April At 23:57, July 6th, 2011 (UTC), there was a successful Kiruna The flight was planned toward Canada (duration ~5 days). However, there was He-leak from the balloon, and the gondola was returned to ground after ~5 hours. - July, 2012, the gondola became flight Kiruna for 2-week circumpolar flight. However, weather was bad, flight was cancelled. - July 14~26, 2013, there was a successful flight from Kiruna, Sweden to Norilsk, Russia.

11 Detector Concept (1) : Detection - PoGOLite captures a pair of Compton scattering and photoabsorption for one X/gamma-ray event with 217 well-type phoswich detector cells (PDCs), and measure the azimuthal angle anisotropy of Compton-scattering. - In the pathfindr flight, there are 61 PDCs. - Instrument is rotated (5~15 mins/rotation) to cancel instrumental systematics. Gamma-ray Top view PDCs SAS 1 m Slow plastic scintillator Fast plastic scintillator Bottom BGO PMTs PDCs in one direction detect more events than ones in other directions.

12 Detector Concept (2) : Low background Count rate of background from charged particles, neutrons and X/gammaray from other sources is ~1000 times higher than that of the signal. Shields of BGO scintillator (SAS) and polyethylene locate around PDCs. Each PDC is a well-type phoswich detector has narrow FOV (~ 1 deg). Charged particles and X/gamma-rays are rejected ~100% The remaining background is neutron-scatter events. Gamma-ray 1 deg PDC unit PDCs SAS 1 m Slow plastic scintillator Fast plastic scintillator Bottom BGO PMTs

13 Principle Modulation curve Slow plastic scintillator collimator Valid event Off-axis event (vetoed by hit in slow scintillator) BGO anticoincidence Side-entering event (vetoed by hit side anticoincidence BGO shield) Fast plastic scintillator scatterer Modulation factor Polyethylene neutron shield Back-entering event (vetoed by hit in BGO) Neutron event (background) Polarization degree

14 Polarimeter Design Figure of Merit: Minimum Detectable Polarisation (3σ) Background rate Small field-of-view: low aperture background. BGO anticoincidence: low γ + particle backgrounds Polyethylene shielding: suppresses dominant neutron background μ Modulation for 100% polarized source Signal rate Area, geometry, efficiency. Hexagonal crosssection plastic scintillators: ~40 cm 2 (full-size: ~200 cm 2 50 kev for a reasonable MF 50 kev). Observation time Long duration balloon flight

15 Detector Installation All the 91 units are installed successfully.

16 Polarimeter and Star Trackers STM star tracker (2.57 x 1.92 deg) STR star tracker (5.0 x 3.7 deg) Aurora monitor unit

17 PoGOLite Overall View (2013)

18 PoGOLite Overall View (2011)

19 Launch 19

20 Launch 20

21 Operation 21

22 Trajectory (14 days) Kiruna Latitude 68 Altitude 39~40 km (day), ~36 km (night) 22

23 Trajectory (14 days) Launch :18 UT Cut :24 UT Landing :15 UT! 23

24 Attitude Control (for 7 hours) (Deg) RA DEC - Attitude Control System worked for 14 days Requirement (~0.1 deg accuracy) is archived (GOOD) - Polarimeter worked for first 3 days After that, there was a power trouble. (Time) 24

25 Landing Gondola has been delivered from Russia to Sweden in Jan. (Export is difficult ) 25

26 SPHiNX satellite 0.5m (Plan: 2016~) PolariS satellite 6m (Plan: 2020~) Launched by Swedish satellite - GRB dedicated ( kev) 25 detections / year - Large effective area: 120 cm 2 - Effective area is ~10 times larger than GAP/TSUBAME. - Modulation factor is similar to GAP (TSUBAME has twice better modulation factor). Launched by Japanese Epsilon rocket kev hard X-ray band >10 mcrab sources. - Hard X-ray mirror (like ASTRO-H) gain effective area reduce backgrounds

27 PolariS targets (by Hayashida)

28 Summary (by Tamagawa) PoGOLite balloon (2010~) Source : faint Mirror/background rejection : needed => US: SMEX, JP: Small satellite AOs GAP (2010~) GRB : bright Very small satellite: OK It is Green: high-time will be for launched dedicated instruments for polarized X-ray astrophysics. Several Red: Plan groups are pursuing balloon- and satellite-borne instruments.

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