DARK MATTER SEARCHES WITH AMS-02 EXPERIMENT
|
|
- Peregrine Walsh
- 5 years ago
- Views:
Transcription
1 DARK MATTER SEARCHES WITH AMS-02 EXPERIMENT A.Malinin a, For AMS Collaboration IPST, University of Maryland, MD-20742, College Park, USA Abstract. The Alpha Magnetic Spectrometer (AMS), to be installed on the International Space Station, will provide data on cosmic radiations in a large range of rigidity from 0.5 GV up to 2 TV. The main physics goals in the astroparticle domain are the anti-matter and the dark matter searches. Observations and cosmology indicate that the Universe may include a large amount of unknown Dark Matter. It should be composed of non baryonic Weakly Interacting Massive Particles (WIMP). A good WIMP candidate being the lightest SUSY particle in R-parity conserving models. AMS offers a unique opportunity to study simultaneously SUSY dark matter in three decay channels from the neutralino annihilation: e +, anti-proton and gamma. The supersymmetric theory frame is considered together with alternative scenarios (extra dimensions). The expected flux sensitivities in 3 year exposure for the e + /e ratio, anti-proton and gamma yields as a function of energy are presented and compared to other direct and indirect searches. Introduction The first evidence for the existence of Dark Matter comes from the observation of rotation velocities across the spiral galaxies, derived from the variation in the red-shift. The rotation velocities rise rapidly from the galactic center, then remain almost constant to the outermost regions of a galaxy. The observations are consistent with the gravitation motion only if the matter in the Universe is mostly non luminous dark matter. The recent WMAP results [1] confirm that about 83% of the matter in the Universe exists in the form of cold Dark Matter (DM). The mystery of the Dark Matter remains unsolved. Many candidates such as massive neutrino, Universal Extra Dimensions Kaluza-Klein states and Super Symmetry theory (SUSY) heavy neutralinos were proposed. If Dark Matter, or a fraction of it, is non-baryonic and consists of almost noninteracting particles like neutralinos, it can be detected in cosmic rays through its annihilation into positrons or anti-protons, resulting in deviations (in case of anti-protons) or structures (in case of positrons) to be seen in the otherwise predictable cosmic ray spectra [2]. Considering the hypothesis of a possible clumpy DM, the expected fluxes of such primary positrons, γ-s or anti-protons may be enhanced [3] since the annihilation rate is proportional to the square DM density contrary to the direct DM searches which will suffer from a decreased probability for the Earth to be contained into an eventual DM clump. a malinin@mail.cern.ch
2 1 AMS-02 Instrument The Alpha Magnetic Spectrometer (AMS) is a particle physics experiment in space. Its initial space mission on board of the Space Shuttle Discovery (STS- 91) in June, 1998 confirmed the basic concept of the experiment [4]. During this short flight AMS measured of the GeV cosmic-ray fluxes over most of the Earth s surface [5 8], and provided the impetus to upgrade the instrument for the ISS 3 year mission (hereafter called AMS-02). These upgrades include among others a stronger, BL 2 = 0.9T superconducting magnet to achieve the maximal detectable rigidity of 1 TV (the rigidity resolution better than 2% up to 20 GV) in the Silicon Tracker, as well as the addition of a Transition Radiation Detector (TRD), a Ring Imaging Cherenkov (RICH) and an Electromagnetic Calorimeter (ECAL). The upgraded instrument will provide data on cosmic radiation in a large range of energy from a fraction of GeV to 3 TeV with very high accuracy and free from the atmospheric corrections needed for balloon-born measurements. Its main physics goals in the astroparticle domain are the Antimatter and the Dark Matter searches as well as the cosmic ray composition and propagation study. 2 AMS-02 Sensitivity for DM search The Monte Carlo study, based on the AMS-02 mathematical model, was performed to estimate the instrument sensitivity for the indirect DM search channels [9 13]. More than 10 9 events containing p +, He, e + and γ at different energies have been fully simulated [14 17] passing through the detector and then reconstructed. The results of the study in the anti-proton, e + and γ cannels are presented in the figures 1-9. The background rejection factors up to 10 6 necessary to extract the tiny anti-proton and e + signals were achieved by combining the redundant information from the TRD, RICH and ECAL detectors. The selection criteria were tuned and the resulting efficiencies were used to simulate the measured spectra. Comparison with the existing data demonstrates that the AMS-02 will have an adequate sensitivity to address the enhancement in the positron fraction measurement reported by HEAT [9, 10], simultaneously constraining the DM signal parameter space by combining the anti-proton, e + and γ channels [18]. The Galactic Center γ signal measurement by AMS-02 would provide 95% CL exclusion limits for several msugra models in 3 years.
3 Figure 1: The acceptance for the anti-proton signal including the selection efficiency. Figure 2: The background rejection factors for the anti-proton signal.
4 Figure 3: The simulated AMS-02 three year combined measurement of the cosmic p spectrum and the residual background (left plot). The comparison of the AMS-02 expected three year p spectrum measurement with existing data (right plot). Lines show different secondary anti-proton flux models. Figure 4: MC prediction for the AMS-02 positron energy reconstruction (left plot). The simulated AMS-02 three year combined measurement of the cosmic e + spectrum (right plot).
5 Figure 5: The HEAT positron fraction data with an example of estimated 1 year AMS-02 measurement. Solid lines show one of the most favorable SUSY neutralino scenario and the standard LBM prediction. SUSY signal enhancement 100 (clumpy DM) is necessary to fit data. Figure 6: The integrated γ flux from the Galactic Center as a function of m χ for the NFW halo profile (left plot) and cuspy NFW halo (right plot) parameterizations with the standard set of parameters. The considered models are the msugra scheme, AMSB scenario and Kaluza-Klein Universal Extra Dimensions. The various selections were done by varying Ωh 2 cuts.
6 Figure 7: Combined example. The anti-proton flux as a function of kinetic energy, assuming 150 GeV SUSY neutralino mass (left plot) and 50 GeV Kaluza-Klein boson mass (right plot) for 3 years of AMS-02 data taking. Figure 8: Combined example. The positron flux as a function of energy, assuming 150 GeV SUSY neutralino mass (left plot) and 50 GeV Kaluza-Klein boson mass (right plot) for 3 years of AMS-02 data taking. Figure 9: Combined example. The γ flux as a function of energy, assuming 150 GeV SUSY neutralino mass (left plot) and 50 GeV Kaluza-Klein boson mass (right plot) for 3 years of AMS-02 data taking. IMBH associated DM clumps at different distance: 20 kpc (case 1) and 2 kpc (case 2) are shown.
7 Conclusions During the 3 year mission in space, AMS-02 will perform precise, high statistics cosmic ray measurements in the 1 GeV to few TeV energy range. It will allow to combine all indirect Dark Matter search channels, constraining the existing models and will have a high discovery potential of the Dark Matter signal. References [1] D.N.Spergel et al., ApJS, 148, 175 (2003). [2] I.V.Moskalenko and A.W.Strong, Adv.Space Res. 27, 717 (2001). [3] E.A.Baltz et al. Cosmic-ray positron excess and neutralino dark matter,phys.rev. D (2002). [4] G.M.Viertel, M.Capell, The Alpha Magnetic Spectrometer, Nucl.Inst.Meth. A 419, 295 (1998). [5] J.Alcaraz et al., Search for Antihelium in Cosmic Rays, Phys. Lett. B 461, 387 (2000). [6] J.Alcaraz et al., Protons in Near Earth Orbit, Phys.Lett. B 472, 215 (2000). [7] J.Alcaraz et al., Leptons in Near Earth Orbit, Phys.Lett. B 484, 10 (2000). [8] J.Alcaraz et al., Cosmic Protons, Phys.Lett. B 490, 27 (2000). [9] S.W.Barwick et al. (HEAT Collaboration), Measurements of the Cosmic-Ray Positron Fraction from 1 to 50 GeV, Astro-phys.J. 482, L191 (1997). [10] S.Coutu et al. (HEAT-pbar Collaboration), Positron Measurements with the HEAT-pbar Instrument, in (Proceedings of 27 th ICRC), [11] R.L.Golden et al., Observation of cosmic ray positrons in the region from 5 to 50 GeV, A&A 188, 145 (1987). [12] L.Bergstrom, J.Edsjo, P.Ullio, Cosmic Antiprotons as a Probe for Supersymmetric Dark Matter, Astro-phys.J. 526, 215 (1999). [13] D.Hooper, G.Kribs, Kaluza-Klein Dark Matter and the Positron Excess, Phys.Rev. D (2004) [14] R.Brun et al., GEANT 3, CERN/DD/EE/84-1, [15] S.Giani et al., GEANT 4 An Object-Oriented Toolkit for Simulation in HEP, CERN/LHCC/98-44, [16] V.Choutko, G.Lamanna, A.Malinin, (Trento II International Workshop on Matter Antimatter and Dark Matter Proceedings), Int.J.Mod.Phys. A 17, N12-13, 1817 (2002). [17] A.Jacholkowska, et al., An indirect dark matter search with diffuse gamma rays from the Galactic Centre with the Alpha Magnetic Spectrometer, arxiv:astro-ph/ , 23 May [18] S.Rosier-Lees in (Proceedings of 30 th ICRC), ID0618, Merida, 2007.
Indirect Search for Dark Matter with AMS-02
Indirect Search for Dark Matter with AMS-02 A. Malinin, UMD For the AMS Collaboration SUSY06, UC Irvine, June 14, 2006 Alpha Magnetic Spectrometer science The AMS is a particle physics experiment in space.
More informationAntimatter and DM search in space with AMS Introduction. 2 Cosmology with Cosmic Rays
Antimatter and DM search in space with AMS-02 Francesca R. Spada Istituto Nazionale di Fisica Nucleare Piazzale Aldo Moro, 5 I-00185, Rome, ITALY 1 Introduction AMS-02 is a space-borne magnetic spectrometer
More informationPHY326/426 Dark Matter and the Universe. Dr. Vitaly Kudryavtsev F9b, Tel.:
PHY326/426 Dark Matter and the Universe Dr. Vitaly Kudryavtsev F9b, Tel.: 0114 2224531 v.kudryavtsev@sheffield.ac.uk Indirect searches for dark matter WIMPs Dr. Vitaly Kudryavtsev Dark Matter and the Universe
More informationDark Matter Searches with AMS-02. AMS: Alpha Magnetic Spectrometer
Dark Matter Searches with AMS-02 AMS: Alpha Magnetic Spectrometer 2007/2008 Wim de Boer on behalf of the AMS collaboration University of Karlsruhe July, 20. 2004 COSPAR, Paris, W. de Boer, Univ. Karlsruhe
More informationDetection and measurement of gamma rays with the AMS-02 detector
Detection and measurement of gamma rays with the AMS-02 detector Simonetta Gentile Dipartimento di Fisica, Università La Sapienza, Sez. I.N.F.N., Roma, Piazza A.Moro 2, 00183, Roma (Italy) Email: simonetta.gentile@roma1.infn.it
More informationCosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity
Cosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity Masaki Asano The Graduate University for Advanced Studies Collaborated with Shigeki Matsumoto Nobuchika Okada Yasuhiro
More informationCosmic Ray Physics with the Alpha Magnetic Spectrometer
Cosmic Ray Physics with the Alpha Magnetic Spectrometer Università di Roma La Sapienza, INFN on behalf of AMS Collaboration Outline Introduction AMS02 Spectrometer Cosmic Rays: origin & propagations: Dominant
More informationDetection and measurement of gamma rays with the AMS-02 detector
Detection and measurement of gamma rays with the AMS-02 detector Simonetta Gentile Dipartimento di Fisica, Università La Sapienza, Sez. I.N.F.N., Roma, Piazza A.Moro 2, 00183, Roma (Italy) Email: simonetta.gentile@roma1.infn.it
More informationSearch for exotic process with space experiments
Search for exotic process with space experiments Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata Rencontres de Moriond, Very High Energy Phenomena in the Universe Les Arc, 20-27
More informationNew results from the AMS experiment on the International Space Station. Henning Gast RWTH Aachen
New results from the AMS experiment on the International Space Station Henning Gast RWTH Aachen 1 Questions to AMS-02: Are there galaxies made of anti-matter in the Universe? What is the nature of Dark
More informationThe Alpha Magnetic Spectrometer on the International Space Station
The Alpha Magnetic Spectrometer on the International Space Station Ignacio Sevilla 1 on behalf of the AMS Collaboration CIEMAT, Centro de Investigaciones Energéticas Medioambientales y Tecnológicas, Av.
More informationThe Search for Dark Matter. Jim Musser
The Search for Dark Matter Jim Musser Composition of the Universe Dark Matter There is an emerging consensus that the Universe is made of of roughly 70% Dark Energy, (see Stu s talk), 25% Dark Matter,
More informationM. Lattanzi. 12 th Marcel Grossmann Meeting Paris, 17 July 2009
M. Lattanzi ICRA and Dip. di Fisica - Università di Roma La Sapienza In collaboration with L. Pieri (IAP, Paris) and J. Silk (Oxford) Based on ML, Silk, PRD 79, 083523 (2009) and Pieri, ML, Silk, MNRAS
More informationDIETRICH MÜLLER University of Chicago SLAC SUMMER INSTITUTE 2011
SEARCHES FOR ANTIMATTER DIETRICH MÜLLER University of Chicago SLAC SUMMER INSTITUTE 2011 OUTLINE Early History Baryon Asymmetry of the Universe? Current Limits on Antimatter Nuclei from Distant Galaxies
More informationChapter 6.2: space based cosmic ray experiments. A. Zech, Instrumentation in High Energy Astrophysics
Chapter 6.2: space based cosmic ray experiments 1 A bit of history... space based experiments 1912-1950: first observations of the cosmic ray flux with detectors onboard balloons and air-planes. 1950s/60s:
More informationIndirect Dark Matter Detection
Indirect Dark Matter Detection Martin Stüer 11.06.2010 Contents 1. Theoretical Considerations 2. PAMELA 3. Fermi Large Area Telescope 4. IceCube 5. Summary Indirect Dark Matter Detection 1 1. Theoretical
More informationDark matter in split extended supersymmetry
Dark matter in split extended supersymmetry Vienna 2 nd December 2006 Alessio Provenza (SISSA/ISAS) based on AP, M. Quiros (IFAE) and P. Ullio (SISSA/ISAS) hep ph/0609059 Dark matter: experimental clues
More informationDark Matter. Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET)
Dark Matter Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET) 1 Dark Matter 1933 r. - Fritz Zwicky, COMA cluster. Rotation
More informationProject Paper May 13, A Selection of Dark Matter Candidates
A688R Holly Sheets Project Paper May 13, 2008 A Selection of Dark Matter Candidates Dark matter was first introduced as a solution to the unexpected shape of our galactic rotation curve; instead of showing
More informationSpectra of Cosmic Rays
Spectra of Cosmic Rays Flux of relativistic charged particles [nearly exactly isotropic] Particle density Power-Law Energy spectra Exponent (p, Nuclei) : Why power laws? (constraint on the dynamics of
More informationCurrent and Future balloon and space experiments L. Derome (LPSC Grenoble) Tango, May 4-6th, 2009
Current and Future balloon and space experiments L. Derome (LPSC Grenoble) Tango, May 4-6th, 2009 L. Derome, Tango, May 4-6th 2009 1 Plan I will focus on: Future experiments which are going to measure
More informationPAMELA from Dark Matter Annihilations to Vector Leptons
PAMELA from Dark Matter Annihilations to Vector Leptons phalendj@umich.edu With Aaron Pierce and Neal Weiner University of Michigan LHC and Dark Matter Workshop 2009 University of Michigan Outline PAMELA
More informationGeV to Multi-TeV Cosmic Rays: AMS-02 Status and Future Prospects
: AMS-02 Status and Future Prospects DPNC and Center for Astroparticle Physics (CAP Genève) Université de Genève E-mail: martin.pohl@cern.ch Due to recent observations, there is a renewed interest in GeV
More informationEnhancement of Antimatter Signals from Dark Matter Annihilation
Enhancement of Antimatter Signals from Dark Matter Annihilation around Intermediate Mass Black Holes Pierre Brun Laboratoire d Annecy-le-vieux de Physique des Particules CNRS/IN2P3/Université de Savoie
More informationSUPPLEMENTARY INFORMATION
1. Selecting electrons in ATIC ATIC is a calorimetric instrument and, as such, relies upon the difference in the development of the cascades (showers) initiated by protons and electrons. Moreover, the
More informationKaluza-Klein Dark Matter
Kaluza-Klein Dark Matter Hsin-Chia Cheng UC Davis Pre-SUSY06 Workshop Complementary between Dark Matter Searches and Collider Experiments Introduction Dark matter is the best evidence for physics beyond
More informationPoS(IDM2010)013. Antiproton and Electron Measurements and Dark Matter Searches in Cosmic Rays. Piergiorgio Picozza.
Antiproton and Electron Measurements and Dark Matter Searches in Cosmic Rays University of Rome Tor Vergata and INFN, Rome, Italy E-mail: piergiorgio.picozza@roma2.infn.it Roberta Sparvoli University of
More informationRare Components in Cosmic Rays with AMS-02
Rare Components in Cosmic Rays with AMS-02 TAUP Sendai Sep.07 IEKP - Andreas Sabellek Universität (TH) for the AMS Collaboration The AMS Project: History and Future 1998 2008 again ready for launch AMS-01
More informationPrecision measurements of nuclear CR energy spectra and composition with the AMS-02 experiment
Journal of Physics: Conference Series PAPER OPEN ACCESS Precision measurements of nuclear CR energy spectra and composition with the AMS-02 experiment To cite this article: E Fiandrini 2016 J. Phys.: Conf.
More informationAntimatter in Space. Mirko Boezio INFN Trieste, Italy. PPC Torino July 14 th 2010
Antimatter in Space Mirko Boezio INFN Trieste, Italy PPC 2010 - Torino July 14 th 2010 Astrophysics and Cosmology compelling Issues Apparent absence of cosmological Antimatter Nature of the Dark Matter
More informationPayload for Antimatter Matter Exploration and Light-nuclei Astrophysics. PAMELA MissioN 17 December 2010 Prepared by FatiH KAYA
Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics PAMELA MissioN 17 December 2010 Prepared by FatiH KAYA Astropartical Physics İssue To inform. What Powered the Big Bang? Inflation
More informationHigh-energy Gamma Rays detection with the AMS-02 electromagnetic calorimeter. F. Pilo for the AMS-02 ECAL Group INFN Sezione di Pisa, Italy
Frascati Physics Series Vol. 58 (2014) Frontier Objects in Astrophysics and Particle Physics May 18-24, 2014 High-energy Gamma Rays detection with the AMS-02 electromagnetic calorimeter F. Pilo for the
More informationJustin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration
Measurement of the cosmic ray positron spectrum with the Fermi LAT using the Earth s magnetic field Justin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration International Cosmic Ray
More informationAntiproton Flux and Antiproton-to-Proton Flux Ratio in Primary Cosmic Rays Measured with AMS on the Space Station
Antiroton Flux and Antiroton-to-Proton Flux Ratio in Primary Cosmic Rays Measured with AMS on the Sace Station Andreas Bachlechner on behalf of the AMS collaboration 3 07.08.017 von TeVPA 017, Columbus
More informationDark matter and LHC: complementarities and limitations
Dark matter and LHC: complementarities and limitations,1,2, F. Mahmoudi 1,2,3, A. Arbey 1,2,3, M. Boudaud 4 1 Univ Lyon, Univ Lyon 1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574,
More informationProperties of Elementary Particle Fluxes in Cosmic Rays. TeVPA Aug. 7, Yuan-Hann Chang National Central University, Taiwan
Properties of Elementary Particle Fluxes in Cosmic Rays TeVPA Aug. 7, 2017 Yuan-Hann Chang National Central University, Taiwan Elementary Particles in Space There are hundreds of different kinds of charged
More informationSearching for Dark Matter Annihilation from Milky Way Dwarf Spheroidal Galaxies. Present status and future prospects
Searching for Dark Matter Annihilation from Milky Way Dwarf Spheroidal Galaxies. Present status and future prospects Aldo Morselli INFN Roma Tor Vergata CTA in the quest for Dark Matter and exotic phenomena
More informationDark matter searches and prospects at the ATLAS experiment
Dark matter searches and prospects at the ATLAS experiment Wendy Taylor (York University) for the ATLAS Collaboration TeVPA 2017 Columbus, Ohio, USA August 7-11, 2017 Dark Matter at ATLAS Use 13 TeV proton-proton
More informationAntimatter and dark matter: lessons from ballooning.
Mem. S.A.It. Vol. 79, 823 c SAIt 2008 Memorie della Antimatter and dark matter: lessons from ballooning. P. Picozza and L. Marcelli INFN and Dept. of Physics, University of Rome Tor Vergata, Italy e-mail:
More informationEGRET Excess of diffuse Galactic Gamma Rays as a Trace of the Dark Matter Halo
EGRET Excess of diffuse Galactic Gamma Rays as a Trace of the Dark Matter Halo Indirect Search for Dark Matter W. de Boer 1, I. Gebauer 1, A.V. Gladyshev 2, D. Kazakov 2, C. Sander 1, V. Zhukov 1 1 Institut
More informationAMS : A Cosmic Ray Observatory
Nuclear Physics B (Proc. Suppl.) 150 (2006) 24 29 www.elsevierphysics.com AMS : A Cosmic Ray Observatory Jean-Pierre Vialle a for the AMS collaboration a Laboratoire d'annecy-le-vieux de Physique des Particules
More informationGALACTIC CENTER GEV GAMMA- RAY EXCESS FROM DARK MATTER WITH GAUGED LEPTON NUMBERS. Jongkuk Kim (SKKU) Based on Physics Letters B.
GALACTIC CENTER GEV GAMMA- RAY EXCESS FROM DARK MATTER WITH GAUGED LEPTON NUMBERS Jongkuk Kim (SKKU) Based on Physics Letters B. 752 (2016) 59-65 In collaboration with Jong Chul Park, Seong Chan Park The
More informationNeutrinos and DM (Galactic)
Neutrinos and DM (Galactic) ArXiv:0905.4764 ArXiv:0907.238 ArXiv: 0911.5188 ArXiv:0912.0512 Matt Buckley, Katherine Freese, Dan Hooper, Sourav K. Mandal, Hitoshi Murayama, and Pearl Sandick Basic Result
More informationThe Egret Excess, an Example of Combining Tools
The Egret Excess, an Example of Combining Tools Institut für Experimentelle Kernphysik, Universität Karlsruhe TOOLS 2006-26th - 28th June 2006 - Annecy Outline Spectral Fit to EGRET data Problems: Rotation
More informationAstroparticle Physics with IceCube
Astroparticle Physics with IceCube Nick van Eijndhoven nickve.nl@gmail.com http://w3.iihe.ac.be f or the IceCube collaboration Vrije Universiteit Brussel - IIHE(ULB-VUB) Pleinlaan 2, B-1050 Brussel, Belgium
More informationThe PAMELA Satellite Experiment: An Observatory in Space for Particles, Antiparticles and Nuclei in the Cosmic Rays
: An Observatory in Space for Particles, Antiparticles and Nuclei in the Cosmic Rays M. Ricci 1 on behalf of the PAMELA Collaboration INFN, Laboratori Nazionali di Frascati, Via Enrico Fermi 40, I-00044
More informationThe positron and antiproton fluxes in Cosmic Rays
The positron and antiproton fluxes in Cosmic Rays Paolo Lipari INFN Roma Sapienza Seminario Roma 28th february 2017 Preprint: astro-ph/1608.02018 Author: Paolo Lipari Interpretation of the cosmic ray positron
More informationDark Matter in the Universe
Dark Matter in the Universe NTNU Trondheim [] Experimental anomalies: WMAP haze: synchrotron radiation from the GC Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron
More informationTHE AMS RICH COUNTER
THE AMS RICH COUNTER G. BOUDOUL ISN Grenoble ISN-GRENOBLE 1 The AMS RICH collaboration: Bologna, Grenoble, Lisbon, Madrid, Maryland, Mexico 2 The AMS collaboration UNAM S.C.C. TING (MIT), PI 3 AMS Scientific
More informationMonthly Proton Flux. Solar modulation with AMS. Veronica Bindi, AMS Collaboration
Solar modulation with AMS Monthly Proton Flux Veronica Bindi, AMS Collaboration Physics and Astronomy Department University of Hawaii at Manoa Honolulu, Hawaii, US 1 AMS on the ISS May 19, 2011 and for
More informationSignals from Dark Matter Indirect Detection
Signals from Dark Matter Indirect Detection Indirect Search for Dark Matter Christian Sander Institut für Experimentelle Kernphysik, Universität Karlsruhe, Germany 2nd Symposium On Neutrinos and Dark Matter
More informationCosmic Antimatter. Stéphane. Coutu The Pennsylvania State University. 3 rd. Astrophysics Arequipa,, Peru August 28-29, 29, 2008
Cosmic Antimatter Stéphane Coutu The Pennsylvania State University 3 rd rd School on Cosmic Rays and Astrophysics Arequipa,, Peru August 28-29, 29, 2008 Outline Cosmic Rays Antimatter: Positrons, Antiprotons
More informationDARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1
DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark
More informationGamma-ray Astrophysics
Gamma-ray Astrophysics AGN Pulsar SNR GRB Radio Galaxy The very high energy -ray sky NEPPSR 25 Aug. 2004 Many thanks to Rene Ong at UCLA Guy Blaylock U. of Massachusetts Why gamma rays? Extragalactic Background
More informationPropagation in the Galaxy 2: electrons, positrons, antiprotons
Propagation in the Galaxy 2: electrons, positrons, antiprotons As we mentioned in the previous lecture the results of the propagation in the Galaxy depend on the particle interaction cross section. If
More informationCosmic Ray panorama. Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1
1912 1932 Cosmic Ray panorama http::// Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1 Pamela : < 0.1 evt year/gev Flux E α α 2.7 / 3.3 Statistical precision
More informationGalactic Cosmic Ray Propagation in the AMS 02 Era
Galactic Cosmic Ray Propagation in the AMS 02 Era I Science case 1. Galactic Cosmic Rays 2. AMS 02 II Collaboration LAPP/LAPTh/LPSC 1. Teams and context 2. Support asked for the project III Conclusions
More informationDark matter annihilations and decays after the AMS-02 positron measurements
Dark matter annihilations and decays after the AMS-02 positron measurements Anna S. Lamperstorfer Technische Universität München SISSA - International School for Advanced Studies of Trieste Workshop The
More informationMeasurement of the CR e+/e- ratio with ground-based instruments
Measurement of the CR e+/e- ratio with ground-based instruments Pierre Colin Max-Planck-Institut für Physik CR Moon shadow MPP retreat - 21 January 2014 Cosmic ray electrons Observation: Above the atmosphere:
More informationCollider Searches for Dark Matter
Collider Searches for Dark Matter AMELIA BRENNAN COEPP-CAASTRO WORKSHOP 1 ST MARCH 2013 Introduction Enough introductions to dark matter (see yesterday) Even though we don t know if DM interacts with SM,
More informationPrimary Cosmic Rays : what are we learning from AMS
Primary Cosmic Rays : what are we learning from AMS Roberto Battiston University and INFN-TIFPA of Trento HERD Workshop IHEP-Beijing December 2-3 2013 1 Agile Fermi PAMELA AMS Direct study of the HESS
More informationLimits on Antiprotons in Space from the Shadowing of Cosmic Rays by the Moon
Limits on Antiprotons in Space from the Shadowing of Cosmic Rays by the Moon Presented by: Yupeng Xu ( ETH Zürich / L3+C collaboration) PhD Students Seminar, PSI, October 1-2, 2003 The L3+C Experiment
More informationDARK MATTER ANNIHILATION AT THE GALACTIC CENTER?
Complementarity Between Dark Matter Searches and Collider Experiments, UC Irvine, June 11, 2006 DARK MATTER ANNIHILATION AT THE GALACTIC CENTER? Joel Primack University of California, Santa Cruz The Milky
More informationIndirect detection of Dark Matter with the ANTARES Neutrino Telescope
EPJ Web of Conferences 116, 04002 (2016) DOI: 10.1051/epjconf/201611604002 C Owned by the authors, published by EDP Sciences, 2016 Indirect detection of Dark Matter with the ANTARES Neutrino Telescope
More informationKaluza-Klein Theories - basic idea. Fig. from B. Greene, 00
Kaluza-Klein Theories - basic idea Fig. from B. Greene, 00 Kaluza-Klein Theories - basic idea mued mass spectrum Figure 3.2: (Taken from [46]). The full spectrum of the UED model at the first KK level,
More informationSIMULATION OF THE GAMMA-RAY GALACTIC DISTRIBUTION AS SEEN BY THE AMS-02
SIMULATION OF THE GAMMA-RAY GALACTIC DISTRIBUTION AS SEEN BY THE AMS-02 M. Mollá 1, J.Alcaraz 1, J.Berdugo 1, J.Bolmont 2, J.Casaus 1, E.Lanciotti 1, C.Mañá 1, C.Palomares 1, E.Sánchez 1, F.J.Rodríguez
More informationDark Energy vs. Dark Matter: Towards a unifying scalar field?
Dark Energy vs. Dark Matter: Towards a unifying scalar field? Alexandre ARBEY Centre de Recherche Astrophysique de Lyon Institut de Physique Nucléaire de Lyon, March 2nd, 2007. Introduction The Dark Stuff
More informationCarsten Rott. mps. ohio-state. edu. (for the IceCube Collaboration)
Searches for Dark Matter from the Galactic Halo with IceCube Carsten Rott carott @ mps. ohio-state. edu (for the IceCube Collaboration) Center for Cosmology and AstroParticle Physics (CCAPP) The Ohio State
More informationMICROPHYSICS AND THE DARK UNIVERSE
MICROPHYSICS AND THE DARK UNIVERSE Jonathan Feng University of California, Irvine CAP Congress 20 June 2007 20 June 07 Feng 1 WHAT IS THE UNIVERSE MADE OF? Recently there have been remarkable advances
More informationThe God particle at last? Astronomy Ireland, Oct 8 th, 2012
The God particle at last? Astronomy Ireland, Oct 8 th, 2012 Cormac O Raifeartaigh Waterford Institute of Technology CERN July 4 th 2012 (ATLAS and CMS ) A new particle of mass 125 GeV I The Higgs boson
More informationImplication of AMS-02 positron fraction measurement. Qiang Yuan
Implication of AMS-02 positron fraction measurement Qiang Yuan (yuanq@ihep.ac.cn) Institute of High Energy Physics, Chinese Academy of Sciences Collaborated with Xiaojun Bi, Guo-Ming Chen, Yi-Qing Guo,
More informationThe Lightest Higgs Boson and Relic Neutralino in the MSSM with CP Violation
The Lightest Higgs Boson and Relic Neutralino in the MSSM with CP Violation Stefano Scopel Korea Institute of Advanced Study (based on: J. S. Lee, S. Scopel, PRD75, 075001 (2007)) PPP7, Taipei, Taiwan,
More informationObservational Prospects for Quark Nugget Dark Matter
Observational Prospects for Quark Nugget Dark Matter Kyle Lawson University of British Columbia Partially based on material reviewed in http://arxiv.org/abs/1305.6318 Outline Baryogenesis (matter/antimatter
More informationObservability of gamma-ray spectral feature from Kaluza-Klein dark matter
Observability of gamma-ray spectral feature from Kaluza-Klein dark matter Satoshi Tsuchida 1 and Masaki Mori 2,a) 1 Department of Physics, Osaka City University, Osaka 558-8585, Japan 2 Department of Physical
More informationPreliminary results from gamma-ray observations with the CALorimeteric Electron Telescope (CALET)
Preliminary results from gamma-ray observations with the CALorimeteric Electron Telescope (CALET) Y.Asaoka for the CALET Collaboration RISE, Waseda University 2016/12/15 CTA-Japan Workshop The extreme
More informationDark Matter Models. Stephen West. and. Fellow\Lecturer. RHUL and RAL
Dark Matter Models Stephen West and Fellow\Lecturer RHUL and RAL Introduction Research Interests Important Experiments Dark Matter - explaining PAMELA and ATIC Some models to explain data Freeze out Sommerfeld
More informationDPG Sascha Caron (Freiburg)
DPG 2010 Sascha Caron (Freiburg) Outline 2 Reminder: Why is SUSY interesting? SUSY production at LHC LHC, ATLAS and CMS status What can we expect in the next 2 years? Summary SUSY Reminder 3 SUPERSYMMETRY
More information!"#$%&'$(")*&$+,)*$-"+./&'$0,1&'2&$23 $4 &/1',"3 $5 -,6$!0($789&'23 &+1$,"#$%&'$:(( ;'<#=$-'=$(1&#,+$()*,&/
!"#$%&'$(")*&$+,)*$-"+./&'$0,1&'2&$23 $4 &/1',"3 $5 -,6$!0($789&'23 &+1$,"#$%&'$:(( ;'
More informationan introduction What is it? Where do the lectures fit in?
AstroParticle Physics an introduction What is it? Where do the lectures fit in? What is AstroParticle Physics? covers a wide range of research at the intersection of particle physics : dark matter and
More informationThe Story of Wino Dark matter
The Story of Wino Dark matter Varun Vaidya Dept. of Physics, CMU DIS 2015 Based on the work with M. Baumgart and I. Rothstein, 1409.4415 (PRL) & 1412.8698 (JHEP) Evidence for dark matter Rotation curves
More informationDARK MATTERS. Jonathan Feng University of California, Irvine. 2 June 2005 UCSC Colloquium
DARK MATTERS Jonathan Feng University of California, Irvine 2 June 2005 UCSC Colloquium 2 June 05 Graphic: Feng N. Graf 1 WHAT IS THE UNIVERSE MADE OF? An age old question, but Recently there have been
More informationSearch for Astrophysical Neutrino Point Sources at Super-Kamiokande
Search for Astrophysical Neutrino Point Sources at Super-Kamiokande Yusuke Koshio for Super-K collaboration Kamioka, ICRR, Univ. of Tokyo LNGS, INFN Super-Kamiokande detector Recent results of search for
More informationRecent results from the LHCb experiment
Recent results from the LHCb experiment University of Cincinnati On behalf of the LHCb collaboration Brief intro to LHCb The Large Hadron Collider (LHC) proton-proton collisions NCTS Wksp. DM 2017, Shoufeng,
More informationDark Matter Decay and Cosmic Rays
Dark Matter Decay and Cosmic Rays Christoph Weniger Deutsches Elektronen Synchrotron DESY in collaboration with A. Ibarra, A. Ringwald and D. Tran see arxiv:0903.3625 (accepted by JCAP) and arxiv:0906.1571
More informationPoS(LHCPP2013)016. Dark Matter searches at LHC. R. Bellan Università degli Studi di Torino and INFN
Dark Matter searches at LHC R. Bellan Università degli Studi di Torino and INFN E-mail: riccardo.bellan@cern.ch U. De Sanctis Università degli Studi di Udine and INFN E-mail: umberto@cern.ch The origin
More informationDark Matter - II. Workshop Freudenstadt shedding (Cherenkov) light on dark matter. September 30, 2015
Dark Matter - II GRK 1694: Elementarteilchenphysik bei höchster Energie und höchster Präzision Workshop Freudenstadt 2015 September 30, 2015 Guido Guido Drexlin, Drexlin, Institut Institut für für für
More informationMeasuring Dark Matter Properties with High-Energy Colliders
Measuring Dark Matter Properties with High-Energy Colliders The Dark Matter Problem The energy density of the universe is mostly unidentified Baryons: 5% Dark Matter: 20% Dark Energy: 75% The dark matter
More informationDark Matter Electron Anisotropy: A universal upper limit
Seminari teorici del venerdì Enrico Borriello Università degli Studi di Napoli Federico II & INFN Sezione di Napoli Dark Matter Electron Anisotropy: A universal upper limit Based on Borriello, Maccione,
More informationNeutrinos as Probes. of Dark Matter. Hasan Yüksel The Ohio State University
Neutrinos as Probes of Dark Matter Institute for Gravitation and Cosmos, Inaugural Conference, Penn State University, August 9 - August 11, 2007 Hasan Yüksel The Ohio State University arxiv:0707.0196 [astro-ph]
More informationarxiv:hep-ph/ v2 9 Sep 2005
Indirect Signals from Dark Matter in Split Supersymmetry Asimina Arvanitaki and Peter W. Graham Institute for Theoretical Physics Department of Physics Stanford University Stanford, CA 94305 USA email:
More informationIndirect Searches for Gravitino Dark Matter
Indirect Searches for Gravitino Dark Matter Michael Grefe Departamento de Física Teórica Instituto de Física Teórica UAM/CSIC Universidad Autónoma de Madrid PLANCK 202 From the Planck Scale to the Electroweak
More informationNeutralino Dark Matter as the Source of the WMAP Haze
Neutralino Dark Matter as the Source of the WMAP Haze Gabriel Caceres Penn State University & Fermilab Based on work with Dan Hooper INT Summer School 2009 Dark Matter: The Evidence The Search Direct Detection
More informationFluxes of Galactic Cosmic Rays
Fluxes of Galactic Cosmic Rays sr s m - GeV Flux solar Modulation: Φ = 550 MV proton helium positron electron antiproton photon galdef 50080/60080 (γ) Status of Cosmic Ray Measurements: good agreement
More informationSilicon Detectors for the Search of Cosmic Antimatter and Dark Matter
Silicon Detectors for the Search of Cosmic Antimatter and Dark Matter Piergiorgio Picozza INFN and University of Rome Tor Vergata From e + /e - Colliders to High Energy Astrophysics Trieste, September
More informationThe electron spectrum from annihilation of Kaluza-Klein dark matter in the Galactic halo
The electron spectrum from annihilation of Kaluza-Klein dark matter in the Galactic halo Satoshi Tsuchida Affiliation: Department of Physical Sciences, Ritsumeikan University E-mail: rp005076@ed.ritsumei.ac.jp
More informationDeepCore and Galactic Center Dark Matter
2nd Low-Energy Neutrino Workshop (PSU July 1-2, 2010) DeepCore and Galactic Center Dark Matter Carsten Rott carott @ mps. ohio-state.nospamedu Center for Cosmology and AstroParticle Physics The Ohio State
More informationTopics. 1. Towards a unified picture of CRs production and propagation: 2. AMS-02 good candidates for Dark Matter space search
Nicolò Masi Bologna University and INFN - 31 May 2016 Topics 1. Towards a unified picture of CRs production and propagation: Astrophysical uncertainties with GALPROP Local Interstellar Spectra: AMS-02
More informationSearching for a Dark Matter Candidate at the Fermilab Tevatron
Searching for a Dark Matter Candidate at the Fermilab Tevatron Paul Geffert, Max Goncharov, Eunsin Lee, and David Toback Texas A&M SlavaKrutelyov now at UCSB Peter Wagner now at Penn 1 Outline What is
More informationThe AMS-02 Anticoincidence Counter
The AMS-02 Anticoincidence Counter, W. Karpinski, Th. Kirn, K. Lübelsmeyer, St. Schael, M. Wlochal on behalf of the AMS-02 Collaboration philip.doetinchem@rwth-aachen.de I. Phys. Inst. B, RWTH Aachen University
More informationExperimental review of high-energy e e + and p p spectra
Experimental review of high-energy e e + and p p spectra Luca Baldini INFN Pisa luca.baldini@pi.infn.it TeV Particle Astrophysics, July 15 2009 Outline Measurement of the singly charged component of the
More information