1. A. Takada (Kyoto University)  Our motivation   -PIC and MeV gamma-ray telescope   -PIC applications  New type  -PIC

2. ~30 objects/10 years V. Schönfelder+ (A&AS, 2000) MeV sky map CGRO/COMPTEL ~3000 objects/4 years F. Acero+ (ApJS, 2015) Fermi/LAT > 1 GeV GeV sky map Sensitivity Astro-H 1mCrab EGRET Air Cherenkov Fermi Good Bad erg / (cm 2 sec) Obs. Time : 10 6 sec 1-30 MeV goal Requirements for the next-generation detectors are … Wide-band detection Large Field of View Sharp Point Spread Function Nucleosynthesis SNR : Radio-isotopes Galactic plane : 26 Al ・ Annihilation Particle acceleration Jet (AGN) : Synchrotron + Inverse Compton Strong gravitational potential Black hole : accretion disk,  0 Etc. Gamma-ray Pulsar, solar flare

3.  1 photon  direction + energy  Well-define PSF  Large FOV (~3str)  Simple structure  Compton Kinematical test with angle   Particle identify with dE/dx  No VETO & shield around ETCC  Gaseous TPC : Tracker track and energy of recoil electron  Scintillator : Absorber position and energy of scattered gamma ray Reconstruct Compton scattering event by event stopped scattered ~4 cm 30 cm without electron tracks Using electron tracks T. Tanimori+, ApJ (2015) α 137 Cs (662 keV) x 3

4. Micro Pixel Chamber (  -PIC) 2D gaseous imaging detector by Print Circuit Board technology Each pixel works as like a proportional counter Large detection area ： 10×10 cm 2 and 30×30 cm 2 High gas gain ： max ~15000 Fine position resolution ： RMS ~120 μm Good gain uniformity Stable operation over several months with the gain of ~6000 400  m

5. Garfield++ Experiments: □ ： SN040426-1 ▲ ： SN050921-1 Ar 90% + Ethane 10%  Strong electric field near anodes -> Avalanche occurs only near anodes  Single electron spectrum -> well fit by Polya-distribution  Gas gain -> Experiment data are well consistent with simulation. anode cathode by Garfield++ A. Takada+, JINST (2013) 10 4 10 3

6. 55 Fe spectrum @ 10cm  10cm Test chart image 0.5mm slits Xe:C 2 H 6 = 7:3 Gain uniformity(  ) 4.5% FWHM 30% MnK  Ar-esc Length along the edge [mm] Counts Knife edge test position resolution σ=120  m 10cm 5.9keV T. Nagayoshi+, NIM A (2004), A. Takeda+, IEEE TNS (2004) Gas gain

7. Sub-MeV gamma-ray imaging Loaded-on-balloon Experiment ETCC Launched on Sep. 1, 2006 @ Sanriku (ISAS/JAXA) Test flight using (10 cm) 3 ETCC Measure diffuse cosmic and atmospheric gamma ray 0.1 – 1 MeV, @ 35 km, 3 hours Measured : 420 events Simulation : ~400 events (cosmic + atmospheric) A. Takada+, ApJ, 733(2011), 13 Diffuse Cosmic  SMILE-I Compton kinematic test and Particle identify provided low-background observation.

8. 30 cm cube tracker×√10 Updating of data acquisition system×√10 Improvement of imaging ability×10 Target: Crab nebula 5  detection (40 km, several hours) Effective area : > 0.5 cm 2 (300 keV) Angular resolution : < 10˚ (600 keV) Sensitivity : ×100 SMILE-I Requirements time threshold Time-Over-Threshold (TOT) stopped scattered TOT Obtained recoil electron ~1 m Improvements for SMILE-II Sensitivity will reach to (×100 SMILE-I) ! ~4 cm SMILE-II Compton e Escape e MIPs time strip

9. 0.025 0.020 0.015 0.010 0.005 ~10 min/frame 835 keV±10% 30˚ 60˚ 120˚ Zenith ~0˚ 120˚ 60˚ Zenith ~90˚ Zenith ~60˚ 120˚ 60˚ Zenith ~30˚ 60˚ 120˚ 60° 30° RIs @ ~2m No energy-cut 662 keV 511 keV 356 keV 22 Na 133 Ba 0.85 MBq 137 Cs 22 Na 0.16 MBq 133 Ba 0.63 MBq

10. ～ 5.5 m SMILE-II ETCC 22 Na shielded by thin Pb 27 kBq equivalent No cut very week excess @ 511 keV on source (4 o radius) dE/dx & Fiducial cut off source 15 o 30 o 45 o 60 o 511 keV±10% ～ 15 ph/s 22 Na T. Tanimori+, ApJ 2015 Dose by RI ： ~0.0003 uSv/h Space dose ： 0.05-0.1 uSv/h ⇒ Source = 1/200-300 BG By imaging spectroscopy, ETCC can detect a very weak source without any shield ! ―

11. Neutron imaging Resolution with PID: 105~130 µm(σ) J. D. Parker+, NIM A (2013) Dark matter search  3 He + n -> p + 3 H  Using template of ToT, we obtain neutron incident position  Dark-matter scatters the nuclear of detector.  Because a TPC can detect the angle θ between directions od DM-wind and recoil nuclear, we can detect the DM-wind by measurement of asymmetry of cos θ. K. Miuchi+, PhL B (2007), K. Nakamura+, PTEP (2015)  NID NEWAGE

12. Requirements from applications: 1.Higher gas gain 2.Suppression of discharge 3.Higher position resolution  Thick substrate  Precise manufacturing  Fine pitch PCB technology : Thicker substrate causes thicker anode Precision of manufacturing is ~10  m Minimum of anode diameter is 50  m -> Pixel pitch is limited by anode Micro Electro Mechanical Systems MEMS technology can make deep through-hole keeping anode diameter Precision of manufacturing is a few  m

13. Experiment: ● MEMS  -PIC ▲ PCB  -PIC Garfield++ (PCB) Garfield++ (MEMS) 21.2 % (FWHM)  MEMS  -PIC successfully detected X-ray.  Large gain with stable operation : 22000 (no discharge during 20 hours) 15000 (no discharge over 300 hours)  Good energy resolution : 21.2% @ 5.89 keV (FWHM)  Discharge rate of MEMS  -PIC is less than that of PCB  -PIC. Performance of test production improved those of current detectors. MEMS  -PIC may become a next standard.

14.  Performance of PCB  -PIC : - Large Detection area10x10, 30x30 cm 2 - High gas gain~6000 (stable operation), 15000 (max) - Energy resolution~30% @ 5.89 keV (FWHM) - Fine position resolution~120  m (RMS) - Good gain uniformity< 5-7% (RMS, 100 cm 2 )  Applications of  -PIC : - Electron-Tracking Compton Camera MeV gamma-ray astronomy, Medical imaging, Environmental monitoring - Neutron Imaging - Dark matter search  Development of MEMS  -PIC : - High gas gain~22000 during 20 hours - Stable operation~15000 over 300 hours Discharge rate is less than that of PCB type - Good energy resolution21.2% @ 5.89 keV (FWHM)