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Particle Physics School Munich Colloquium December 13th, 2013

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Presentation on theme: "Particle Physics School Munich Colloquium December 13th, 2013"— Presentation transcript:

1 GRB observation of The MAGIC telescopes and PMT for Next Generation Telescope
Particle Physics School Munich Colloquium December 13th, 2013 Max-Planck-Institut für Physik Föhringer Ring, Munich, Main Auditorium Thank you Chairman and thank you for attending this meeting I would like to talk Takeshi Toyama

2 Contents 3 Messages! How MAGIC telescopes observe Gamma ray
Photo sensor for Next generation Gamma Ray Burst observation by MAGIC - Motivation, Way, Difficulty, Result 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

3 MAGIC telescope 17m 85m Location Canary Island La Palma Energy range
Angular resolution Sensitivity Canary Island La Palma 50GeV - 50TeV ~0.06%Crab with 50h observation ) 2013/Jan/11 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope Takeshi Toyama GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama 3

4 blah-blah-blah MAGIC telescope 17m 85m Location Canary Island La Palma
Energy range Angular resolution Sensitivity Canary Island La Palma 50GeV - 50TeV ~0.06%Crab with 50h observation ) GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama 4

5 Before talk 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

6 A big glass cube 10km * 10km * 10Km 2013/Dec/13
GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

7 100GeV 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

8 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

9 We measure gamma ray by using this phenomenon
These reactions continue until particles become enough low energy. We measure gamma ray by using this phenomenon 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

10 Cherenkov Light is directional radiation, not isotropic
Charged particle has velocity more than one of light in medium. The particle emits Cherenkov Light Cherenkov Light is directional radiation, not isotropic 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

11 Replace a glass with just atmosphere
Angle of light emitting is narrow θ= 1° Atmosphere n: β≒1 θ= 1°　 n: index of refraction β= vp/c vp: velocity of particle　 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

12 ~100m 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

13 You can count particles Investigate which particle
If we put fast (time resolution <~10nsec) sensitive ( < ~10photon) sensor You can count particles Investigate which particle 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

14 Then put many sensors 2013/Dec/13
GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama 14

15 You can distinguish between gamma and the others
Air shower by gamma ray Air shower by hadron You can distinguish between gamma and the others to some extent 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama 15

16 You can distinguish between gamma and the others
I want to track a object in sky You can distinguish between gamma and the others to some extent 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama 16

17 Tracking Device 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

18 Well, no significant signal…
Let`s collect more photon to get signal! Tracking Device 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

19 Get significant signal from CrabNebula! (the Whipple Observatory 1989)
Mirror Tracking Device 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

20 Get significant signal from CrabNebula! (the Whipple Observatory 1989)
Mirror More sensitive! Tracking Device 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

21 Better sensitivity & resolution
2013/Dec/13

22 MAGIC telescope 17m 85m Location Canary Island La Palma Energy range
Angular resolution Field of View Canary Island La Palma 50GeV - 50TeV 3.5° 2013/Dec/13 22

23 Photo sensor for Next generation
2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

24 Next Generation Project Cherenkov Telescope Array (CTA)
G. Perez, SMM, IAC from CTA web site Before several groups built Telescopes In next generation, They all are going to build Telescopes in one project. -> To achieve 10 time better sensitivity than current Telescopes We need better photo sensor! 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

25 Photomultiplier Requirement
New PMTs are almost satisfied with requirement Today I want to focus two parameter “Quantum Efficiency & Afterpulse” 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

26 PhotoMultiplier Tube (PMT)
Vacuum ~0.1Pa (10-7 atm) Cathode Anode Dynodes 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

27 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

28 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

29 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

30 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

31 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

32 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

33 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

34 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

35 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

36 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

37 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

38 Quantum Efficiency(QE)
Ratio to convert from Photon to electron If we got better QE -> we can measure weak signal -> It leads to lower threshold energy Hamamastu and Electron Tube produce Good PMT having QE. c.f. MAGIC current PMT is 〜32% 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

39 AfterPulse(AP) 2us Signal Afterpulse is dummy signal after signal.
Current 2us Signal Time Afterpulse is dummy signal after signal. -> We want to reduce this AP as much as possible

40 Cause of After Pulse 1 2013/Dec/13
GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

41 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

42 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

43 On 1st dynode, plus ION can be produced
2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

44 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

45 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

46 These electrons will go 1 st dynode
-> it will be cause of After Pulse. 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

47 Cause of After Pulse 2 2013/Dec/13
GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

48 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

49 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

50 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

51 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

52 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

53 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

54 Results of After Pulse measurement
2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

55 GRB observation of MAGIC telescope
2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

56 Gamma Ray Burst No anisotropy 1. It occurs at cosmological distances.
Number of burst No anisotropy duration time (sec) 1. It occurs at cosmological distances. 2. two different population of bursts 3. Some of the Long GRBs are related to hypernova. 4. Afterglow is observed in X ray band. However, GRB is not a well-understood phenomena yet. なぞ エネルギー、等方的、天文学的な距離にあることが判明、2種類、Hノバと関連 未だに分かっていないこととして放射機構、（モデル）、10GeV以上のスペクトラム No anisotropy Total energy of GRB is around … Short GRB Long GRB 2013/Jan/11 GRB observation of MAGIC telescopes and PMT for Next Generation telescope Takeshi Toyama

57 Motivation No detection of GRB by this type of Telescope (Imaging Atmospheric Cherenkov Telescope) in history. Nobody knows - Energy spectrum more than 300GeV -What is central engine? ADVANTAGE of MAGIC for GRB obseration 1.MAGIC can measure more than 50GeV, effective area is over 1000times than Fermi LAT 2. MAGIC can track available source within 25sec at least 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

58 GRB observation in MAGIC
MAGIC FoV is 6 times bigger than moon in angular diameter. So it is very low probability that GRB happen in MAGIC FoV. () We need to repointing after GRB 2013/Jan/11 GRB observation of MAGIC telescopes and PMT for Next Generation telescope Takeshi Toyama

59 Preliminary GRB13YYYY Onset 2013/Dec/13
GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

60 Preliminary GRB13XXXX 2013/Dec/13
GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

61 Summary PMT for Next generation telescope has good performance
GRB observation by MAGIC, unfortunately still no detection, But we have the biggest chance as long as CTA will start. 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

62 Thank you !!! 2013/Dec/13 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

63 2013/Jan/11 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

64 2013/Jan/11 GRB observation of MAGIC telescopes and PMT for Next Generation telescope 　　　　Takeshi Toyama

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