PPC AMS2 (Lecture 10)

Transcription

1 PPC AMS2 (Lectre 10) 掃部輝機 PHYS 823 1

2 PPC Projects at A Glance Phys. Lett. B 505 (2001) 161 (Tevatron) Phys. Lett. B 538 (2002) 121 (Tevatron) Phys. Lett. B 611 (2005) 223 (ILC) Phys. Lett. B 618 (2005) 182 (ILC) 1 Lectre 3 Er. Phys. J. C46 (2006) 43 (LHC+ILC) Spersymmetry Parameter Analysis: SPA Convention and Project Phys. Lett. B 639 (2006) 46 (LHC) Phys. Lett. B 649 (2007) 73 (LHC) Phys. Rev. Lett. 100 (2008) (LHC) 2 Phys. Rev. D 79 (2009) (LHC) Phys. Rev. D 82 (2010) (LHC) 3 Phys. Lett. B 703 (2011) 475 ( BEST at LHC) Lectre 6 Lectre 9 Something is missing... 2

3 AMS 2 Alpha Magnetic Spectrometer on ISS Find how one can search for the dark matter annihilation. 3

4 The Alpha Magnetic Spectrometer (AMS) Experiment AMS Yan-Hann Chang, NCU PPP9, Chng-Li, AMS is a Particle detector in Space Particle detector: The cosmic rays carry a lot of information. Detailed stdy of cosmic ray is key to nderstand certain aspect of the niverse. Space: These particles cannot be observed on grond, becase the earth is protected by a thick layer of atmosphere. Traditionally the stdy of cosmic rays are carried ot by balloon experiments. They typically operates for jst a few days. AMS is a large magnetic spectrometer in orbit, to be operating for 20 years on ISS. The key problem is a magnet that can be delivered to and operate in space. AMS: A TeV precision, mltiprpose particle physics spectrometer in space. TRD Identify e+, e- Silicon Tracker Z, P ECAL E of e+, e-, Particles and nclei are defined by their charge (Z) and energy (E ~ P) Tracker TOF Z, E Magnet Z RICH Z, E AMS is US Dept of Energy (DOE) led International Collaboration 16 Contries, 60 Instittes and 600 Physicists, 17 years USA FLORIDA A&M UNIV. FLORIDA STATE UNIVERSITY MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER TEXAS A&M UNIVERSITY UNIV. OF MARYLAND - DEPT OF PHYSICS YALE UNIVERSITY - NEW HAVEN MEXICO UNAM NETHERLANDS ESA-ESTEC NIKHEF NLR FRANCE GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE SPAIN CIEMAT - MADRID I.A.C. CANARIAS. PORTUGAL LAB. OF INSTRUM. LISBON DENMARK UNIV. OF AARHUS FINLAND HELSINKI UNIV. UNIV. OF TURKU ITALY ASI CARSO TRIESTE IROE FLORENCE INFN & UNIV. OF BOLOGNA INFN & UNIV. OF MILANO INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF SIENA GERMANY RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE ROMANIA ISS UNIV. OF BUCHAREST SWITZERLAND ETH-ZURICH UNIV. OF GENEVA RUSSIA I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. CHINA KOREA EWHA KYUNGPOOK NAT.UNIV. BISEE (Beijing) IEE (Beijing) IHEP (Beijing) NLAA (Beijing) SJTU (Shanghai) SEU (Nanjing) TAIWAN SYSU (Gangzho) SDU (Jinan) ACAD. SINICA (Taiwan) AIDC (Taiwan) CSIST (Taiwan) NCU (Chng Li) NCKU (Tainan) NCTU (Hsinch) NSPO (Hsinch) Z, P are measred independently by the Tracker, RICH, TOF and ECAL The detectors were bilt all over the world and assembled at CERN, near Geneva, Switzerland The Permanent Magnet: on the Shttle - AMS-01 and on ISS AMS-02 B Provides trigger Time of Flight (TOF) Measres the time of particles to ~ 150 picoseconds PMTs Scintillator PMTs Light Gides

5 PPC AMS2 (Lectre 10) 掃部輝機 PHYS 823 1

6 PPC Projects at A Glance Phys. Lett. B 505 (2001) 161 (Tevatron) Phys. Lett. B 538 (2002) 121 (Tevatron) Phys. Lett. B 611 (2005) 223 (ILC) Phys. Lett. B 618 (2005) 182 (ILC) 1 Lectre 3 Er. Phys. J. C46 (2006) 43 (LHC+ILC) Spersymmetry Parameter Analysis: SPA Convention and Project Phys. Lett. B 639 (2006) 46 (LHC) Phys. Lett. B 649 (2007) 73 (LHC) Phys. Rev. Lett. 100 (2008) (LHC) 2 Phys. Rev. D 79 (2009) (LHC) Phys. Rev. D 82 (2010) (LHC) 3 Phys. Lett. B 703 (2011) 475 ( BEST at LHC) Lectre 6 Lectre 9 Something is missing... 2

7 AMS 2 Alpha Magnetic Spectrometer on ISS Find how one can search for the dark matter annihilation. 3

8 Transition Radiation Detector: TRD Identify e +, reject P Transition Radiation Detector: TRD Identify e +, reject P Silicon Tracker: 200,000 Channels in 9 planes, resoltion 10 microns Ring Imaging CHerenkov (RICH) Reflector Particle Radiator NaF Detector RICH Detector Intensity Z 2 V detectors 10,880 photosensors Single Event displays from the Test beam E=158 GeV/n He Li C O Ca

9 Calorimeter (ECAL) 1mm Lead foil Z Y X 1mm Fibers e e Fiber direction X Y X Y X Y X Y X 9 sper layers provide 3D measrement of shower profile 50,000 fibers, mm, distribted niformly inside 1,200 lb of lead which provides a precision, 3-dimensional, 17X 0 measrement of the directions and energies of light rays and electrons p to 1 TeV Taiwan in AMS National Central University Academia Sinica the leading research instittion directly nder the Presidential Office National ChiaoTng University Chng-Shan Institte of Science and Technology the research arm of the Defense AIDC National Cheng Kng University National Space Organization the space agency of Taiwan Manfactre of AMS Electronics JSBC JIM-CAN JHIF JIM-AMSW&1553 JBU JIM-HRDL Taiwan collaborated closely with MIT, INFN, KIT in the design and prodction of the electronics system of the AMS detector: In total 775 boards and 48 crates. Space Qalification Test of AMS Electronics 4

10 Thermal Blanket installation on Electronics, 2009 AMS-02 Avionics & DAQ 19 AMS in the ESA Thermal Vacm Chamber, Noordwijk, the Netherlands Test at CERN AMS in accelerator test beam Feb 4-8 and Ag 8-20, km AMS 7 km 19 Janary 2010 CERN Accelerator Complex AMS in Test Beam 8-20 Ag 2010 N Test Beam Reslts N Velocity measred to an accracy of 1/1000 for 400 GeV protons N Bending Plane Residal (cm) e Energy Resoltion: 2.5-3% TRD: 400 GeV protons Energy

11 The ltra-precision of the AMS detector enables it to measre the particles with accracy of: 1- The coordinates: to 10 microns (10 millionths of a yard) 2- The travel time: 100 ps (one-tenth of a billionth of a second) 3- The velocity: to an accracy of 1 in 1000 It will also, simltaneosly, measre all cosmic ray atomic nclei to an energy of a trillion electron-volts. Test reslts from accelerator r-1 m -2 sr -1 GeV -1 ) Nclear Charge Z AMS will measre cosmic ray spectra for nclei, for energies from 100 MeV to 2 TeV with 1% accracy over the 11-year solar cycle. Example of AMS physics: 1. Search for the Dark matter : e X p X We look for excess in the e + and p spectrm. case 1 e + /(e + + e - ) I.Cholis et al, arxiv: v3 m m m m = = = = AMS search for DM: 1. Large acceptance and long dration 2. e+/p ~ 10-6 We present for stdies based on for models to highlight AMS sensitivity AMS-02 (18 Yrs) m =800 GeV m =400 GeV m =200 GeV e + /( e + + e ) M. Agilar et al., Phys. Lett. B 646 (2007) Berwick, S. W. et al., Astrophys. J. 482 (1997) L191-L194 O. Adriani et al., Natre 458 (2009) I.Cholis et al, astro-ph 30 Apr 2009 e + Energy [GeV] e + Energy (GeV) case 2 L.Bergstrom et al, PRL 103 (2009) AMS-02 (18 Yrs) e + Energy [GeV] Kalza-Klein Bosons are also Dark Matter candidates case 3 Edardo Pontón and Lisa Randall 10-1 Positron fraction e + /(e + + e - ) sdm_500_18yb 10-2 TeV Scale Singlet Dark Matter Fig.5 AMS-02 (18 yrs) arxiv: v2 [hep-ph] 20 Jan Fig GeV e + Energy (GeV)

12 case 4: DM signal from p P. Brn, Phys.Rev.D76:083506, 2007 and private commnication 10-3 AMS-02 (18 yrs) AMS on ISS Physics of AMS (2): Search for Antimatter Universe The Universe began with the Big Bang p/p From a Model of Cosmic Ray collisions From Dark Matter (M = 840 GeV) Collisions (cannot be seen at LHC) After the Big Bang there mst have been eqal amonts of matter and antimatter p Kinetic Energy (GeV) AMS on the Space Station for 20 years will search for the existence of antimatter to the edge of the niverse Physics of AMS (3) Search for New Matter in the Universe Jack Sandweiss, Yale University There are six types of Qarks fond in accelerators (, d, s, c, b, t). All matter on Earth is made ot of only two types (, d) of qarks. Strangelets are new types of matter composed of three types of qarks (, d, s) which shold exist in the cosmos. AMS-02 (18 Yrs) Carbon Ncles Z/A ~ 0.5 d n p d d d d d d d d d d d d d d d d d Strangelet Z/A ~ 0.1 d s d d s s s s s d d d d d d s s s d s d d d AMS will provide a definitive search for this new type of matter. E. Witten, Phys. Rev. D, (1984) 34 AMS-02 measrement of Strangelets based on the candidate measred with AMS-01 strangelets = 5x10-10 (cm 2 s sr) -1 Z/A = Z/A Search limit down to 2x10-12 (cm 2 s sr) -1

13 Identifying Sorces with AMS 1 AMS Physics example Stdy of high energy (0.1 GeV 1 TeV) diffse gammas T.Prodanovi c et al., astro-ph/ v1 22 Mar 2006 Space Experiments Grond Experiments EGRET e e P 7-8 P+ Tracker 9 AMS-02 E E+ Uniqe constraints P + = E + = P = E + The diffse gamma-ray spectrm of the Galactic plane 40 o < 1 < 100 o, b < 5 o 26 Agst: U.S. Air Force C-5 transported AMS to KSC The Lanch and Installation of AMS Mark E. Kelly (Captain, USN) Gregory H. Johnson (Colonel, USAF, Ret.) E. M. Mike Fincke (Colonel, USAF) Roberto Vittori (Italian Air Force Colonel) Andrew J. Festel (Ph.D.) Gregory Errol Chamitoff (Ph.D.) AMS Ready for Installation in Endeavor s Payload Bay, Ag. 28, 2010

14 AMS Ready for Lanch in Endeavor s Payload Bay Closing Endeavor s Payload Bay Doors April 26, 2011 May 16, 08:56 AM Pnching throgh the other side of the clods Endeavor approaching ISS May 18, 2011

15 Endeavor approaching ISS with Soyz in foregrond May 18, 2011 Endeavor approaching ISS May 18, 2011 AMS abot to be picked p by the shttle robotic arm AMS in transit, picked p by the ISS robotic arm AMS on the ISS trss. May 19, 2011

16 Data from the 1 st few mintes 20 GeV proton Data from the 1 st few mintes 42 GeV/c Carbon The AMS probes the fndamental physics in the search for the Dark matter and antimatter in the niverse. The AMS provides precise measrement of the cosmic ray spectra over a large energy range and extended period of time. We are excitingly waiting for new phenomena that have not yet been predicted. Thank yo Realization of AMS 1. Strong endorsement of the AMS science from reviews by the world s leading scientists 2. Unanimos spport from the US Senate and Hose 3. Major worldwide spport from: Veto System rejects random cosmic rays NASA DOE MIT ESA and CERN FRANCE CNRS SPAIN CIEMAT GERMANY DLR RWTH-I ITALY INFN ASI SWITZERLAND ETH NSF CHINA Academy of Science Ministry of Science NLAA Shandong Gangdong Jiangs TAIWAN ACAD. SINICA CSIST Measred veto efficiency better than

17 Silicon Tracker Cosmic Ray Measrements Showing Maximim Measrable Energy of 2.2 TeV Events * TeV AMS with Spercondcting Magnet AMS with Permanent Magnet 10 mil pitch Provides coordinate resoltion of 10 microns 1/Energy Experimental work on Antimatter in the Universe Dark Matter at high energies with large acceptance and long dration and e + /p ~ 10-6 Direct search Search for Baryogenesis Model of I. Cholis et al, arxiv: v3 New CP BELLE BaBar (sin 2 = consistent with SM) FNAL KTeV (Re( / ) = ( )*10-4 ) CERN NA-48 CDF, D0 Proton decay Sper K ( p > 6.6 * years ) e + /(e + + e - ) m = 100 m = 200 m = 400 m = 800 m =200 GeV AMS-02 m =400 GeV m =800 GeV AMS Increase in sensitivity: x Increase in energy to ~TeV LHC-b ATLAS CMS e + Energy (GeV) y06k299a The Origin of Dark Matter Cosmic Rays: protons, electrons, Helim Collision of Cosmic Rays will prodce e+ ~ 90% of Matter in the Universe is not visible and is called Dark Matter A Galaxy as seen by telescope If we cold see Dark Matter in the Galaxy Search for the origin of Dark Matter: Collisions of Dark Matter will prodce additional e+ These characteristics of additional e+ can be measred very accrately by AMS

18 The leading candidate for Dark Matter is a SUSY netralino ( 0 ) Collisions of 0 will prodce excess in the spectra of e + different from known cosmic ray collisions e + /( e + + e ) M. Agilar et al., Phys. Lett. B 646 (2007) Berwick, S. W. et al., Astrophys. J. 482 (1997) L191-L194 O. Adriani et al., Natre 458 (2009) I.Cholis et al, astro-ph 30 Apr 2009 AMS-02 (3 Yrs) e + Energy [GeV] AMS-02 (18 Yrs) Experimental work on Antimatter in the Universe Crrently, minimal direct searches Assmption: Antimatter does not exist. Search for explanations Major experiments worldwide over the last 40 years, inclding 2 dedicated accelerators No explanation fond Assmption: Antimatter exists. Search for its existence AMS on ISS Increase in sensitivity: x Increase in energy to ~TeV e + /( e + + e ) m 0 = 200 GeV e + Energy [GeV] e + Energy [GeV] The new Large Hadron Collider (LHC) will contine this search Mirko Boezio, Commissione II, 2010/04/2 Facility Original prpose, Expert Opinion Discovery with Precision Instrment 30 GeV Proton Accelerator CERN 30 GeV Proton Accelerator Brookhaven (1960 s) (1960 s) Nclear force Nclear force Netral Crrents 2 types of netrinos Break down of time reversal symmetry New form of matter 400 GeV Proton Accelerator (1970 s) Netrino physics 5th and 6th types of qark FNAL Electron Positron Collider Qark inside protons (1970 s) Properties of 4th type of qark SLAC Spear qantm electricity 3rd kind of electrons Electron Positron Collider PETRA (1980 s) 6th kind of qark Glon Large Undergrond Cave (2000) Sper Kamiokande Proton life time Netrino has mass Hbble Space Telescope AMS on ISS (1990 s) Galactic srvey Dark Matter, Antimatter, Strangelets, Crvatre of the niverse, dark energy Exploring a new territory with a precision instrment is the key to discovery.? Fndamental Science on the International Space Station Two types of cosmic rays in space 1- Light rays have been measred (e.g., COBE, HUBBLE, INTEGRAL, FERMI, HERSCHEL, WMAP, PLANCK,.) for over 50 years. Fndamental discoveries have been made. 2- Charged cosmic rays: A nearly nexplored region in science. A magnetic spectrometer (AMS) on ISS is the only way to provide long dration (20 years), high precision measrements of charged cosmic rays. AMS