Subir Sarkar
|
|
- Byron Harrell
- 5 years ago
- Views:
Transcription
1 Trinity 2016 Oxford ² The universe observed ² Relativistic world models ² Reconstructing the thermal history ² Big bang nucleosynthesis ² Dark matter: astrophysical observations ² Dark matter: relic particles ² Dark matter: direct detection ² Dark matter: indirect detection ² Cosmic rays in the Galaxy ² Antimatter in cosmic rays ² Ultrahigh energy cosmic rays ² High energy cosmic neutrinos ² The early universe: constraints on new physics ² The early universe: baryo/leptogenesis ² The early universe: inflation & the primordial density perturbation ² Cosmic microwave background & large-scale structure Subir Sarkar
2 Particularly interesting (to high energy physicists) because of the PAMELA anomaly PAMELA has measured the positron fraction: (Gast & Schael, ICRC 09) Anomaly excess above astrophysical background Source of anomaly: Dark matter? Pulsars? Supernova remnants?
3 confirmed by AMS-02
4 resulting in a bold claim The new results from AMS on the positron fraction published in Physical Review Letters show that items (1)-(4) highlighted in Figure 3 have been unambiguously resolved, yielding observations of a new phenomenon. They are consistent with a dark-matter particle (neutralino) of mass on the order of 1 TeV. To determine if the observed new phenomenon is from dark matter or from astrophysical sources such as pulsars, AMS is now making measurements to determine the rate of decrease of the positron fraction beyond the turning point (item 5), as well as to determine the antiproton fraction...
5 However e lose energy readily during propagation, so only nearby sources dominate at such high energies the usual background calculation is then irrelevant Delhaye et al, A&A 501:821,2009 ' yr 1TeV E 1 TeV 100 GeV 10 GeV 1 GeV 100 MeV Kobayashi et al, ApJ 601:340,2004 Might there be primary sources of e + (with a hard spectrum) in our Galactic neighbourhood?
6 This is not the first time an anomalous excess over background has been seen The inclusive jet differential cross section has been measured for jet transverse energies, E T, from 15 to 440 GeV, in the pseudorapidity region 0.1 η 0.7. The results are based on 19.5 pb -1 of data collected by the CDF Collaboration at the Fermilab Tevatron collider. The data are compared with QCD predictions for various sets of parton distribution functions. The cross section for jets with E T > 200 GeV is significantly higher than current predictions based on O(α s3 ) perturbative QCD calculations. Various possible explanations for the high-e T excess are discussed. Abe et al, PRL 77:438,1996 it turned out to be a mis-estimation of the QCD background not new physics!
7 What particle physicists have learnt through experience (UA1 monojets, NuTeV anomaly, CDF high E T excess, ) Yesterday s discovery is today s calibration and tomorrow s background! Richard Feynman Val Telegdi is also now a major issue for astroparticle physics viz. just how well do we know the astrophysical background for signals of apparently new particle physics?
8 A nearby cosmic ray accelerator?. Rise in e + fraction could be due to secondaries being produced during acceleration which are then accelerated along with the primaries (Blasi, PRL 103:051104,2009)... generic feature of a stochastic acceleration process, if τ 1 è2 < τ acc (Cowsik 1979, Eichler 1979) This component naturally has a harder spectrum and fits PAMELA/AMS-02 data (adjusting just one parameter) RXJ , HESS (age~3000 yr, d~0.8 kpc) Ahlers, Mertsch & Sarkar,PRD80:123017,2009
9 Diffusive (1 st -order Fermi) shock acceleration Flux: Conservation equation: density change acceleration convection injection Steady state: log f i.e. = 4 for strong shock (u 1 /u 2 = 4) log p
10 Diffusive (1 st -order Fermi) shock acceleration Acceleration determined by compression ratio: Solve transport equation: u f x = D 2 f x du dx p f p Solution for: f x f inj (p), lim x f where, f 0 (p) = p 0 dp p p p f inj (p ) + Cp As long as f inj (p) is softer than p at high energies: f(x, p) p
11 DSA with secondary production Secondaries have same spectrum as primaries (Feynman): Only particles with are accelerated Bohm diffusion: Fraction of accelerated secondaries is Steady state spectrum: log n p 2 > p 1 è rising positron fraction! log p
12 Diffusion near shock front Ø Ø Diffusion coefficient not known a priori in neighbourhood of shock Bohm diffusion sets a limit: Ø Ø Ø Actual rate may be parametrised by: D = D Bohm /K B, K B = B 2 / B 2 Can try and determine diffusion rate from simulations (difficult!) So we fix K B by fitting to the Fermi e excess can then predict e + /(e + + e - ) for PAMELA/AMS-02, and other secondary-to-primary ratios (e.g B/C)
13 The downstream spectrum, integrated over SNR lifetime where is downstream volume Mertsch, Sarkar, Phys.Rev.D90,:061301(R),2014
14 It is not just the few (optically) observed SNRs which contribute to observed cosmic rays there must be many other hidden SNRs (if there are ~3 SN/century and cosmic rays diffuse in Galaxy for ~10 7 yr)!" ( 10 GeV 100 GeV Known!" ( Simulated!" ' 1 TeV H!" '?::2! =03*.>-!" &,*30 45!" % A07- EF #! B4>.C+ ='&D$ &D( ;!%( ;<!G& ;<!""' 84/9: ,*30 45!" %!" $!" $!"# $%&%'() %! *+"#"!&,)#!" #!"!!!" )*+,-./0 12/!"# $%&%'() %! *+"#"!&,)#!" #!"!!!" )*+,-./0 12/ Ahlers, Mertsch & Sarkar,PRD80:123017,2009
15 Statistical distribution of SNRs in our neighbourhood %&'() "# "$ # $!#!"$!"#!"#!"$!# $ # "$ "# %&'() Case & Bhattacharya, ApJ 504:761,1998 $! #" #! "!! " #! #" $! $" Draw source positions from this distribution Inject e - & e + normalized to observables (HESS ) Propagate to Earth accounting for synchrotron and inverse-compton scattering energy losses Confront total e - +e + flux at Earth with Fermi data The best fit to data is closest to real distribution Ahlers, Mertsch, Sarkar,PRD80:123017,2009
16 Parameters of the Monte Carlo Di usion Model D cm 2 s 1 from GCR nuclear 0.6 secondary-to-primary ratios L 3 kpc b GeV 1 s 1 CMB, IBL and B energy densities Source Distribution t max yr from E min 3.3 GeV SNR 10 4 yr from observations N from number of observed SNRs Source Model R 0 e GeV 1 fit to e flux at 10 GeV 2.4 average -ray spectral index E max 20 TeV typical -ray maximum energy E cut 20 TeV DSA theory R GeV 1 -rays K B 15 free parameter (for fixed ) Ahlers, Mertsch & Sarkar, PRD80:123017,2009
17 Normalising the source spectra Cassiopeia A, HESS Normalisation of primary : fit absolute flux at low energies Normalisation of secondary : Source Other name(s) J E max d Q [(cm 2 s TeV) 1 ] [TeV] [kpc] [(s TeV) 1 ] HESS J RX J (Vela Junior) 2.1 ± ± 2 > HESS J RCW 86, SN 185 (?) 2.54 ± ± HESS J CTB 37B, G ± ± HESS J RX J , G ± ± ± HESS J CTB 37A 2.30 ± ± HESS J G ± ± HESS J a W 28, GRO J ± ± HESS J b W 30, G ± HESS J W 41, G ± MAGIC J IC ± Cassiopeia A 2.4 ± ± J Monoceros 2.53 ± ± 0.17 N/A Mean Mean, excluding sources with > Mean, excluding sources with > Ahlers, Mertsch & Sarkar, PRD80:123017,2009
18 Fitting the e + + e - flux The propagated primary e - spectrum is much too steep to match the Fermi LAT data... but the accelerated secondary e + + e - component has a harder spectrum so does fit the bump! Ahlers, Mertsch & Sarkar, PRD80:123017,2009
19 The postdicted positron fraction 1 Standard Solar modulation Charge-sign dependent Solar modulation Positron fraction 10 1 PAMELA Ahlers, Mertsch, Sarkar, PRD80:123017, Energy GeV
20 Nearby pulsars as source of. Highly magnetized, fast spinning neutron stars -rays and electron/positron pairs produced along the magnetic axis Spectrum speculated to be harder than background from propagation:
21 Combination of Galactic contribution and two nearby pulsars, Geminga (157 pc) and B (290 pc), can fit PAMELA excess (and perhaps also Fermi bump) Hooper, Blasi & Serpico, JCAP 01:025,2009 However ~40% of rotational energy must be released as energetic e + plausible? Fermi should detect expected anisotropy towards B in ~5 years?
22 What about the antiproton-to-proton ratio? Blasi & Serpico, PRL 103:081103,2009 Bohm-like ISM ISM+B term Total Dark matter ( ) p- /p Pulsars Acceleration of secondaries 1e-05 B term A term Kinetic Energy, T [GeV] Secondary acceleration model predicts rise beyond 100 GeV will be tested soon by AMS-02 (if we see this then pulsars are ruled out)
23 Can solve problem analytically but more complicated than for since energy losses must now be included Transport equation: with boundary condition: Solution: Mertsch & Sarkar, PRL 103:081104,2009
24 Nuclear secondary-to-primary Ratios Dark matter Pulsars Acceleration of secondaries (TBD) S/P If we see this rise convincingly, then both dark matter and pulsar origin models would be ruled out! Ti Fe ratio Since nuclei are accelerated in the same sources, the ratio of secondaries to primaries (e.g. B/C or Ti/Fe) must also rise with energy beyond ~100 GeV spallation during propagation only spallation during acceleration as well our fit ATIC-2 Zatsepin et al., arxiv: energy per nucleon GeV Mertsch & Sarkar, PRL 103:081104,2009
25 We fit the AMS-02 p, He fluxes to fix the spectral indices and normalisation, and the e - flux (in accordance with radio data) E 3 J e,e 3 J e + [GeV 2 m 2 s 1 sr 1 ] e (AMS-02) e + (AMS-02) R max = 10 3 GV R max = GV R max = 10 4 GV kinetic Energy E [GeV] E 2.7 Jp, E 2.7 JHe [(GeV/n) 1.7 m 2 s 1 sr 1 ] 10 4 p (AMS-02) He (AMS-02) 10 3 R max = 10 3 GV R max = GV R max = 10 4 GV kinetic Energy E [GeV/n] Mertsch, Sarkar, Phys.Rev.D90: ,2014
26 positron fraction B/C 10 1 R max = 10 3 GV R max = GV R max = 10 4 GV kinetic Energy E [GeV] R max = 10 3 GV R max = GV R max = 10 4 GV AMS-02 CREAM TRACER (AMS-02) kinetic Energy E [GeV/n] pbar/p We can then predict secondary to primary ratios the only free parameter is the maximum energy of the cosmic accelerator (taken to be 1, 3, 10 TeV for illustration) Measurements of B/C and by AMS-02 at higher energies then calibrate/test our model (PAMELA) R max = 10 3 GV R max = 10 4 GV kinetic Energy E [GeV] R max = GV Mertsch, Sarkar, Phys.Rev.D90: (R),2014
27 and here are our predictions confronted with the latest AMS-02 data Looks like the cutoff is closer to ~500 GV? 10 3 (PAMELA) pbar/p B/C R max = 10 4 GV kinetic Energy E [GeV] R max = 10 3 GV R max = GV R max = 10 4 GV R max = 10 3 GV R max = GV AMS-02 CREAM TRACER kinetic Energy E [GeV/n] Mertsch, Sarkar, Phys.Rev.D90, (R),2014
28 Summary AMS-02 confirms the rising positron fraction in cosmic rays (first observed by PAMELA) and this has been interpreted as due to the annihilation of ~TeV mass dark matter particles But the claim is seriously undermined by uncertainties in the modelling of the astrophysical foreground/background These uncertainties must be quantified through a better understanding of the conventional physics before claims for new physics are made (just as establishing new phenomena in the lab depends on precise knowledge of SM processes) this is increasingly important as we come to rely on astroparticle arguments to motivate BSM physics (in the absence of signals at the LHC)
Evidence of Stochastic Acceleration of Secondary. Antiprotons by Supernova Remnants! Ilias Cholis, 08/09/2017
C [ ] -4 Evidence of Stochastic Acceleration of Secondary 2.2 1.0 2.0 1.8 1.6 1.4 1.2 C k p p Φ /Φ ratio fit Antiprotons by Supernova Remnants! 0.8 0.6 0.4 0.2 0.0-6 - 1 k [ GV ] -1 AMS-02 PAMELA Fermi
More information² The universe observed ² Relativistic world models ² Reconstructing the thermal history ² Big bang nucleosynthesis ² Dark matter: astrophysical
² The universe observed ² Relativistic world models ² Reconstructing the thermal history ² Big bang nucleosynthesis ² Dark matter: astrophysical observations ² Dark matter: relic particles ² Dark matter:
More informationAstrophysical issues in the cosmic ray e spectra: Have we seen dark matter annihilation?
Astrophysical issues +/ in the cosmic ray e spectra: Have we seen dark matter annihilation? Julien Lavalle Department of Theoretical Physics University of Torino and INFN Collab: Torino: R. Lineros, F.
More informationCosmic ray electrons from here and there (the Galactic scale)
Cosmic ray electrons from here and there (the Galactic scale) Julien Lavalle Department of Theoretical Physics Torino University and INFN Outline: (i) local electrons (ii) comments on synchrotron [based
More informationGamma-ray and neutrino diffuse emissions of the Galaxy above the TeV
Gamma-ray and neutrino diffuse emissions of the Galaxy above the TeV (with spatial dependent CR transport) D. Grasso (INFN, Pisa) with D. Gaggero, A. Marinelli, A. Urbano, M. Valli IceCube recent results
More informationGamma rays from supernova remnants in clumpy environments.! Stefano Gabici APC, Paris
Gamma rays from supernova remnants in clumpy environments!! Stefano Gabici APC, Paris Overview of the talk Galactic cosmic rays Gamma rays from supernova remnants Hadronic or leptonic? The role of gas
More informationAntimatter from Supernova Remnants
Antimatter from Supernova Remnants Michael Kachelrieß NTNU, Trondheim with S. Ostapchenko, R. Tomàs - PAMELA anomaly )) )+ φ(e + ) / (φ(e + 0.4 0.3 0.2 Positron fraction φ(e 0.1 0.02 Muller & Tang 1987
More informationAstro2020 Science White Paper Prospects for the detection of synchrotron halos around middle-age pulsars
Astro2020 Science White Paper Prospects for the detection of synchrotron halos around middle-age pulsars Thematic Areas: Planetary Systems Star and Planet Formation Formation and Evolution of Compact Objects
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 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 informationHigh and low energy puzzles in the AMS-02 positron fraction results
High and low energy puzzles in the AMS-02 positron fraction results Dario Grasso (INFN, Pisa) D. Gaggero (SISSA), L.Maccione (MPI, Munich), C. Evoli(DESY), G. Di Bernardo (Göteborg) AMS-02 positron fraction
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 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 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 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 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 informationProduction of Secondary Cosmic Rays in Supernova Remnants
Production of Secondary Cosmic Rays in Supernova Remnants E. G. Berezhko, Yu. G. Shafer Institute of Cosmophysical Research and Aeronomy, 31 Lenin Ave., 677891 Yakutsk, Russia E-mail: ksenofon@ikfia.sbras.ru
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 informationWhite dwarf pulsar as Possible Cosmic Ray Electron-Positron Factories
White dwarf pulsar as Possible Cosmic Ray Electron-Positron Factories 2010 7/9 Kazumi Kashiyama (Kyoto University) Kunihito Ioka & Norita Kawanaka (KEK) arxiv:1009.1141 (submitted to PRD) http://www.nasa.gov/centers/goddard/news/topstory/2007/whitedwarf_pulsar.html
More informationSupernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
More information99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park
99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park #5 How do Cosmic Rays gain their energy? I. Acceleration mechanism of CR
More informationThe High-Energy Interstellar Medium
The High-Energy Interstellar Medium Andy Strong MPE Garching on behalf of Fermi-LAT collaboration Cosmic Ray Interactions: Bridging High and Low Energy Astrophysics Lorentz Centre Workshop March 14-18
More informationPERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY. Paolo Lipari Vulcano 27 may 2006
PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY Paolo Lipari Vulcano 27 may 2006 High Energy Neutrino Astrophysics will CERTAINLY become an essential field in a New Multi-Messenger Astrophysics What is
More informationAntimatter spectra from a time-dependent modeling of supernova remnants
Journal of Physics: Conference Series Antimatter spectra from a time-dependent modeling of supernova remnants To cite this article: M Kachelrieß et al 2010 J. Phys.: Conf. Ser. 259 012092 View the article
More informationFermi: Highlights of GeV Gamma-ray Astronomy
Fermi: Highlights of GeV Gamma-ray Astronomy Dave Thompson NASA GSFC On behalf of the Fermi Gamma-ray Space Telescope Large Area Telescope Collaboration Neutrino Oscillation Workshop Otranto, Lecce, Italy
More informationCosmic Pevatrons in the Galaxy
Cosmic Pevatrons in the Galaxy Jonathan Arons UC Berkeley Cosmic Rays Acceleration in Supernova Remnants Pulsar Wind Nebulae Cosmic rays Cronin, 1999, RMP, 71, S165 J(E) = AE! p, p " 2.7,1GeV < E
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 informationCosmic Ray Excess From Multi-Component Dark Matter
Cosmic Ray Excess From Multi-Component Dark Matter Da Huang Physics Department, NTHU @ LeCosPA PRD89, 055021(2014) [arxiv: 1312.0366] PRD91, 095006 (2015) [arxiv: 1411.4450] Mod. Phys. Lett. A 30 (2015)
More informationCosmic Accelerators. 2. Pulsars, Black Holes and Shock Waves. Roger Blandford KIPAC Stanford
Cosmic Accelerators 2. Pulsars, Black Holes and Shock Waves Roger Blandford KIPAC Stanford Particle Acceleration Unipolar Induction Stochastic Acceleration V ~ Ω Φ I ~ V / Z 0 Z 0 ~100Ω P ~ V I ~ V 2 /Z
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 informationParticle Acceleration in the Universe
Particle Acceleration in the Universe Hiroyasu Tajima Stanford Linear Accelerator Center Kavli Institute for Particle Astrophysics and Cosmology on behalf of SLAC GLAST team June 7, 2006 SLAC DOE HEP Program
More informationConstraints on cosmic-ray origin from gamma-ray observations of supernova remnants
Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants Marianne Lemoine-Goumard (CENBG, Université Bordeaux, CNRS-IN2P3, France) On behalf of the Fermi-LAT and HESS Collaborations
More informationQuest for New Physics
Stefano Profumo UC Santa Cruz Santa Cruz Institute for Particle Physics T.A.S.C. [Theoretical Astrophysics in Santa Cruz] Cosmic Rays and the Quest for New Physics Scineghe 2010, Trieste, Italy Thursday,
More informationCosmic-ray propagation in the light of the Myriad model
Cosmic-ray propagation in the light of the Myriad model Y. Genolini,, P. Serpico and R. Taillet LAPTh & Université Savoie Mont Blanc E-mail: genolini@lapth.cnrs.fr, salati@lapth.cnrs.fr A hardening of
More informationQuestions 1pc = 3 ly = km
Cosmic Rays Historical hints Primary Cosmic Rays: - Cosmic Ray Energy Spectrum - Composition - Origin and Propagation - The knee region and the ankle Secondary CRs: -shower development - interactions Detection:
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 informationReview of direct measurements of cosmic rays. Sources of Galactic cosmic rays APC, Paris - December 7-9, 2016
Review of direct measurements of cosmic rays Sources of Galactic cosmic rays APC, Paris - December 7-9, 2016 CR astrophуsics main problems Sources? - Accelerators? The basic paradigm of CR acceleration
More informationW.R. Webber. New Mexico State University, Astronomy Department, Las Cruces, NM 88003, USA
A Galactic Cosmic Ray Electron Spectrum at Energies from 2 MeV to 2 TeV That Fits Voyager 5-60 MeV Data at Low Energies and PAMELA and AMS-2 Data at 10 GeV Using an Electron Source Spectrum ~E -2.25 A
More informationTesting a DM explanation of the positron excess with the Inverse Compton scattering
Testing a DM explanation of the positron excess with the Inverse Compton scattering Gabrijela Zaharijaš Oskar Klein Center, Stockholm University Work with A. Sellerholm, L. Bergstrom, J. Edsjo on behalf
More informationAMS-02 Antiprotons Reloaded
AMS-02 Antiprotons Reloaded Rolf Kappl Bethe Center for Theoretical Physics & Physikalisches Institut der Universität Bonn based on RK, Annika Reinert, Martin Wolfgang Winkler JCAP 10 (2015) 034, arxiv:1506.04145
More informationThe 2 Icecube PeV events [A. ] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays IPM School, Tehran / 23
The 2 Icecube PeV events [A. Schuhkraft@NOW2012 ] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays IPM School, Tehran 2012 1 / 23 The 2 Icecube PeV events [A. Schuhkraft@NOW2012 ] Michael Kachelrieß (NTNU
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 information> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center!
> News < Anti-matter, dark matter measurement By measuring the cosmic rays (Mainly electron, positron, proton, anti-proton and light nuclei) AMS-02 will be launched onboard the Shuttle Endeavour On May
More informationa cosmic- ray propagation and gamma-ray code
GALPROP: a cosmic- ray propagation and gamma-ray code A. Strong, MPE Garching Tools for SUSY, Annecy, June 28 2006 The basis: cosmic-ray production & propagation in the Galaxy intergalactic space HALO
More informationCosmic Ray Transport (in the Galaxy) Luke Drury. Dublin Institute for Advanced Studies Institiúid Ard-Léinn Bhaile Átha Cliath
Cosmic Ray Transport (in the Galaxy) Luke Drury Dublin Institute for Advanced Studies Institiúid Ard-Léinn Bhaile Átha Cliath 1 A few disclaimers and preliminary remarks! Not my main field of research
More informationThe Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission
The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission 1 Outline Mainly from 2009 ApJ 697 1071 The Pair Conversion Telescope The Large Area Telescope Charged Background and Events
More informationCosmic Ray Astronomy. Qingling Ni
Cosmic Ray Astronomy Qingling Ni What is Cosmic Ray? Mainly charged particles: protons (hydrogen nuclei)+helium nuclei+heavier nuclei What s the origin of them? What happened during their propagation?
More informationUltra High Energy Cosmic Rays I
Ultra High Energy Cosmic Rays I John Linsley (PRL 10 (1963) 146) reports on the detection in Vulcano Ranch of an air shower of energy above 1020 ev. Problem: the microwave background radiation is discovered
More informationPulsar Wind Nebulae: A Multiwavelength Perspective
Pulsar Wind Nebulae: Collaborators: J. D. Gelfand T. Temim D. Castro S. M. LaMassa B. M. Gaensler J. P. Hughes S. Park D. J. Helfand O. C. de Jager A. Lemiere S. P. Reynolds S. Funk Y. Uchiyama A Multiwavelength
More informationA-Exam: e + e Cosmic Rays and the Fermi Large Array Telescope
A-Exam: e + e Cosmic Rays and the Fermi Large Array Telescope Walter Hopkins Physics Department, Cornell University. The Fermi Large Area Telescope is a particle detector in space with an effective collecting
More informationIndirect dark matter detection and the Galactic Center GeV Excess
Image Credit: Springel et al. 2008 Indirect dark matter detection and the Galactic Center GeV Excess Jennifer Siegal-Gaskins Caltech Image Credit: Springel et al. 2008 Jennifer Siegal-Gaskins Caltech Image
More informationAstroparticle Anomalies
Astroparticle Anomalies Current Hints of Possible Dark Matter Signals Sheldon Campbell University of California, Irvine What is this talk really about? Isn t discussion of low-significance anomalies just
More informationarxiv: v1 [astro-ph] 17 Nov 2008
Dark Matter Annihilation in the light of EGRET, HEAT, WMAP, INTEGRAL and ROSAT arxiv:0811.v1 [astro-ph 1 Nov 008 Institut für Experimentelle Kernphysik, Universiät Karlsruhe E-mail: gebauer@ekp.uni-karlsruhe.de
More informationImplications of recent cosmic ray results for ultrahigh energy neutrinos
Implications of recent cosmic ray results for ultrahigh energy neutrinos Subir Sarkar Neutrino 2008, Christchurch 31 May 2008 Cosmic rays have energies upto ~10 11 GeV and so must cosmic neutrinos knee
More informationRemnants and Pulsar Wind
High Energy Supernova Remnants and Pulsar Wind Nebulae F. Giordano Dipartimento Interateneo di Fisica and INFN Sez. Bari For the Fermi-LAT Collaboration Scineghe 2010 The Afterlife of a star IC443 Crab
More informationRecent Observations of Supernova Remnants
1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) 2 Contents Supernova Remnants
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 informationCosmic Rays in the Galaxy
1, Over View Cosmic Rays in the Galaxy Discovery : Legendary baloon flight of Victor Hess Observation of Cosmic Rays : Satellite, Balloon (Direct), Air shower (Indirect) Energy Spectrum of Cosmic Rays
More informationCosmic rays in the local interstellar medium
Cosmic rays in the local interstellar medium Igor V. Moskalenko Igor V. Moskalenko/NASA-GSFC 1 LMC (Magellanic Cloud Emission Nuclear Data-2004/09/28, Line Survey: Smith, Points) Santa Fe R - H G - [S
More informationGamma rays from Galactic pulsars: high- and lowlatitude
Francesca Calore Gamma rays from Galactic pulsars: high- and lowlatitude emission Conca Specchiulla, 8th September 2014 based on: F. Calore, M. Di Mauro & F. Donato, arxiv:1406.2706 F. Calore, I. Cholis
More informationCosmic Rays, Photons and Neutrinos
Cosmic Rays, Photons and Neutrinos Michael Kachelrieß NTNU, Trondheim [] Introduction Outline Plan of the lectures: Cosmic rays Galactic cosmic rays Basic observations Acceleration Supernova remnants Problems
More informationThe Inner Region of the Milky Way Galaxy in High Energy Gamma Rays
The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays Simona Murgia, SLAC-KIPAC for the Fermi LAT Collaboration UCLA Dark Matter 2012 Marina del Rey 22-24 February 2012 arxiv:0908.0195 Gamma
More informationNeutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002
Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002 n High Energy Astronomy Multi-Messanger Astronomy Cosmic Rays
More informationSearching for Dark Matter in the Galactic Center with Fermi LAT: Challenges
Searching for Dark Matter in the Galactic Center with Fermi LAT: Challenges Simona Murgia University of California, Irvine Debates on the Nature of Dark Matter Sackler 2014 19-22 May 2014 arxiv:0908.0195
More informationAntiparticle detection in space for dark matter search: the PAMELA experiment.
Antiparticle detection in space for dark matter search: the PAMELA experiment. Piergiorgio Picozza INFN and University of Rome Tor Vergata XCVI Congresso Nazionale della Società Italiana di Fisica Bologna
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 informationRadio Observations of TeV and GeV emitting Supernova Remnants
Radio Observations of TeV and GeV emitting Supernova Remnants Denis Leahy University of Calgary, Calgary, Alberta, Canada (collaborator Wenwu Tian, National Astronomical Observatories of China) outline
More informationFive Years of PAMELA in orbit
32nd International Cosmic Ray Conference, Beijing 2011 Five Years of PAMELA in orbit P. Picozza on behalf of PAMELA collaboration 1,2;1) 1 University of Rome Tor Vergata, Department of Physics, I-00133,
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 informationIndirect detection of decaying dark matter
Indirect detection of decaying dark matter Alejandro Ibarra Technical University of Munich Many thanks to Chiara Arina, Wilfried Buchmüller, Gianfranco Bertone, Laura Covi, Mathias Garny, Michael Grefe,
More informationShort Course on High Energy Astrophysics. Exploring the Nonthermal Universe with High Energy Gamma Rays
Short Course on High Energy Astrophysics Exploring the Nonthermal Universe with High Energy Gamma Rays Lecture 1: Introduction Felix Aharonian Dublin Institute for Advanced Studies, Dublin Max-Planck Institut
More informationActivités au LAPTh. G. Bélanger
Activités au LAPTh G. Bélanger Equipes / Research - Teams Fields, Strings and Symmetries (Math-Phys) L. Frappat, L.Gallot. E. Ragoucy, F. Thuillier, E. Sokatchev, P. Sorba Particle Physics Astroparticles
More informationRevue sur le rayonnement cosmique
Revue sur le rayonnement cosmique Vladimir Ptuskin IZMIRAN Galactic wind termination shock GRB N cr ~ 10-10 cm -3 - total number density w cr ~ 1.5 ev/cm 3 - energy density E max ~ 3x10 20 ev - max. detected
More informationPoS(ICRC2015)540. Uncertainties on propagation parameters: impact on the interpretation of the positron fraction
Uncertainties on propagation parameters: impact on the interpretation of the positron fraction Mathieu Boudaud a, Sandy Aupetit a, Sami Caroff b, Antje Putze a, Geneviève Bélanger a, a, Corine Goy b, Vincent
More informationParticle acceleration and pulsars
Meudon, nov. 2013 p. 1/17 Particle acceleration and pulsars Fabrice Mottez LUTH - Obs. Paris-Meudon - CNRS - Univ. Paris Diderot Meudon, nov. 2013 p. 2/17 Pulsars (PSR) and pulsar wind nebulae (PWNe) Mostly
More informationSubir Sarkar
Trinity 2016 Oxford ² The universe observed ² Relativistic world models ² Reconstructing the thermal history ² Big bang nucleosynthesis ² Dark matter: astrophysical observations ² Dark matter: relic particles
More informationA New View of the High-Energy γ-ray Sky with the Fermi Telescope
A New View of the High-Energy γ-ray Sky with the Fermi Telescope Aurelien Bouvier KIPAC/SLAC, Stanford University On behalf of the Fermi collaboration SNOWPAC, 2010 The Fermi observatory Launch: June 11
More informationSTATUS OF ULTRA HIGH ENERGY COSMIC RAYS
STATUS OF ULTRA HIGH ENERGY COSMIC RAYS Esteban Roulet (Bariloche) COSMO / CosPA 2010, Tokyo Power law flux stochastic (Fermi) acceleration in shocks cosmic ray flux Small fractional energy gain after
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 informationExtremely High Energy Neutrinos
Extremely High Energy Neutrinos A. Ringwald http://www.desy.de/ ringwald DESY 6 th National Astroparticle Physics Symposium February 3, 2006, Vrije Universiteit, Amsterdam, Netherlands Extremely high energy
More informationObservations of. Pulsar Wind Nebulae
Observations of Pulsar Wind Nebulae I. Injection Spectrum I. Late-Phase Evolution II. PWNe and Magnetars PWNe and Their SNRs PWN Shock Reverse Shock Forward Shock Pulsar Wind Pulsar Termination Shock PWN
More informationIndirect Dark Matter search in cosmic rays. F.S. Cafagna, INFN Bari
Indirect Dark Matter search in cosmic rays F.S. Cafagna, INFN Bari Indirect Dark Matter search in cosmic rays With PAMELA experiment An experimentalist point of view F.S. Cafagna, INFN Bari Why Anti(particle)matter
More informationInterstellar gamma rays. New insights from Fermi. Andy Strong. on behalf of Fermi-LAT collaboration. COSPAR Scientific Assembly, Bremen, July 2010
Interstellar gamma rays New insights from Fermi Andy Strong on behalf of Fermi-LAT collaboration COSPAR Scientific Assembly, Bremen, July 2010 Session E110: ' The next generation of ground-based Cerenkov
More informationDark Matter searches with astrophysics
Marco Taoso IPhT CEA-Saclay Dark Matter searches with astrophysics IAP 24 February 2013 The cosmological pie Non baryonic Dark Matter dominates the matter content of the Universe Motivation to search for
More informationCosmic Ray Studies with PAMELA Experiment
Cosmic Ray Studies with PAMELA Experiment Piergiorgio Picozza INFN and University of Rome Tor Vergata 14th Lomonosov Conference on Elementary Particle Physics MSU, Moscow August 19 25, 2009 PAMELA Payload
More informationIndirect Dark Matter constraints with radio observations
Indirect Dark Matter constraints with radio observations In collaboration with E.Borriello and G.Miele, University of Naples Federico II Alessandro Cuoco, Institute for Physics and Astronomy University
More informationDark Matter Annihilation, Cosmic Rays and Big-Bang Nucleosynthesis
Dark Matter Annihilation, Cosmic Rays and Big-Bang Nucleosynthesis Institute for Cosmic Ray Research, University of Tokyo Kazunori Nakayama J.Hisano, M.Kawasaki, K.Kohri and KN, arxiv:0810.1892 J.Hisano,
More informationMeasurement of CR anisotropies with the AMS detector on the ISS
Measurement of CR anisotropies with the AMS detector on the ISS J. Casaus ( CIEMAT Spain ) on behalf of the AMS Collaboration Origin of excess of positrons Positron fraction shows an excess above 10 GeV
More informationSupernova Remnants and GLAST
SLAC-PUB-14797 Supernova Remnants and GLAST Patrick Slane Harvard-Smithsonian Center for Astrophysics Abstract. It has long been speculated that supernova remnants represent a major source of cosmic rays
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 informationCosmic Rays. Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon
Cosmic Rays Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon Nobel Prize in 1936 Origin of high energy cosmic rays is still not completely understood
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 informationEnergy Spectrum of all Electrons and Positron Fraction
Energy Spectrum of all Electrons and Positron Fraction Dr. Rena Majumdar Department of Physics Bhairab Ganguly College Kolkata-56, India renabkp021@gmail.com Abstract The absolute differential energy spectrum
More informationSources: acceleration and composition. Luke Drury Dublin Institute for Advanced Studies
Sources: acceleration and composition Luke Drury Dublin Institute for Advanced Studies Hope to survey... Current status of shock acceleration theory from an astrophysical (mainly cosmic-ray origin) perspective...
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 information1939 Baade&Zwicky 1949 Fermi 1977 (Krymski; Axford; Bell; Blandford & Ostriker
46 1939 Baade&Zwicky 1949 Fermi 1977 (Krymski; Axford; Bell; Blandford & Ostriker From Aharonian et al. 2011 From Letessier-Sevon & Stanev 2011 Fermi 2-year sky map Outline 1. 2. 3. 4. knee ankle (b)
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 informationProton/Helium spectral anomaly and other signatures of diffusive shock acceleration/propagation in/from SNR
Proton/Helium spectral anomaly and other signatures of diffusive shock acceleration/propagation in/from SNR M. Malkov CASS/UCSD Collaborators: P. Diamond, R. Sagdeev 1 Supernova Remnant Shocks- Cosmic
More informationCosmic-ray energy spectrum around the knee
Cosmic-ray energy spectrum around the knee M. SHIBATA Department of Physics, Yokohama National University, Yokohama, 240-8501, Japan Interesting global and fine structures of cosmic-ray energy spectrum
More informationH.E.S.S. Unidentified Gamma-ray Sources in a Pulsar Wind Nebula Scenario And HESS J
H.E.S.S. Unidentified Gamma-ray Sources in a Pulsar Wind Nebula Scenario And HESS J1303-631 Matthew Dalton Humboldt University at Berlin For the H.E.S.S. Collaboration TeV Particle Astrophysics, Paris.
More information