High Energy Messenger Workshop KICP, June Foteini Oikonomou
|
|
- Ethelbert Tucker
- 5 years ago
- Views:
Transcription
1 High Energy Messenger Workshop KICP, June Foteini Oikonomou! Anisotropies in the arrival directions of Ultra-High Energy Cosmic Rays: Current status and prospects with a next-generation instrument 1
2 Introduction!! 5 EeV protons: GZK Horizon ~ few hundred Mpc Deflections 3 in IGMF In the Galactic B-field ~ 2-4 Larger through Galactic centre Iron much larger deflections, ~ Z x proton Anisotropy expected for proton UHECRs! Uncertain composition complicates expectations -> one way to model it, introduce an isotropic background (large deflections) 2
3 Arrival directions of UHECRs observed by Auger UHECRs with E > 55 EeV detected until end 29 Protons E > 55 EeV, PSCz IRAS PSCz ~full sky ~ 1 galaxies, ~far-ir selected: excellent probe of star-formation activity Protons E > 55 EeV, 6dF Calculations take into account: proton energy losses galaxy weights as a function of redshift Auger exposure galaxy survey selection functions 2MASS 6dF ~full sky ~ 1 galaxies, ~near-ir selected: excellent probe of ellipticals, minimal dust extinction 3
4 Arrival directions of UHECRs observed by Auger UHECRs with E > 55 EeV detected until end 29 Protons E > 55 EeV, PSCz IRAS PSCz ~full sky ~ 1 galaxies, ~far-ir selected: excellent probe of star-formation activity Protons E > 55 EeV, 6dF Calculations take into account: proton energy losses galaxy weights as a function of redshift Auger exposure galaxy survey selection functions 2MASS 6dF ~full sky ~ 1 galaxies, ~near-ir selected: excellent probe of ellipticals, minimal dust extinction 3
5 Correlation with Large Scale Structure: 29 dataset: 69 events E > 55 EeV FO et al 213: JCAP5(213)15 PSCz 6dFGs isotropic LSS = 3 = isotropic LSS = 3 = 5 Frequency data Piso,PSCz = 7% PPSCz,proton,no deflections = 1% Frequency data Piso,6dF = 2% P6dF,proton,no deflections = 1% X 5 1 X ~ 1% uncertainty due to binning. 4
6 Correlation with Large Scale Structure: 29 dataset: 69 events E > 55 EeV FO et al 213: JCAP5(213)15 PSCz 6dFGs isotropic LSS = 3 = isotropic LSS = 3 = 5 Frequency data Piso,PSCz = 7% PPSCz,proton,no deflections = 1% Frequency data Piso,6dF = 2% P6dF,proton,no deflections = 1% X 5 1 X X = X i data N CR,i N iso,i N M,i N iso,i N iso,i LSS model isotropic expectation ~ 1% uncertainty due to binning. 4
7 Correlation with Large Scale Structure: Full set to April 214: 142 events E > 55 EeV (my analysis).12.1 PSCz isotropic LSS = dF isotropic LSS = 3 Frequency = 5 data Frequency = 5 data X X Piso,PSCz = 7% Piso,6dF = 1% PPSCz,protons,no deflections <.1% P6dF,protons,no deflections <.1% 5
8 The future: Will better statistics help? Objectives for next generation instrument: 1-3 x Auger annual exposure 1 x Auger FD annual exposure 4 EeV < E < 1 EeV 1-2 events/5 years JEM-EUSO Coll. 213-arXiv:
9 What type of clustering? 2 regimes Source Density:! Absence of significant number of multiplets in Auger data suggests a relatively large source number density! (cf. n gal 1-2 Mpc -3 ) Auger Coll 213, FO et al 213, Takami & Sato 29.. E > 1 EeV low source density 1-5 Mpc -3 anisotropy dominated by clustering around few sources (see e.g., Blaksley et al 13, D Orfeuil et al 214) horizon for ~ 5 EeV protons r 7
10 What type of clustering? 2 regimes Source Density:! Absence of significant number of multiplets in Auger data suggests a relatively large source number density! (cf. n gal 1-2 Mpc -3 ) Auger Coll 213, FO et al 213, Takami & Sato 29.. E > 1 EeV low source density 1-5 Mpc -3 E > 5 EeV low source density 1-4 Mpc -3 anisotropy dominated by clustering around few sources anisotropy imprinted by galaxy distribution (see e.g., Blaksley et al 13, D Orfeuil et al 214) horizon for ~ 5 EeV protons r 8
11 What type of clustering? 2 regimes Source Density:! Absence of significant number of multiplets in Auger data suggests a relatively large source number density! (cf. n gal 1-2 Mpc -3 ) Auger Coll 213, FO et al 213, Takami & Sato 29.. E > 1 EeV low source density 1-5 Mpc -3 E > 5 EeV low source density 1-4 Mpc -3 anisotropy dominated by clustering around few sources anisotropy imprinted by galaxy distribution (see e.g., Blaksley et al 13, D Orfeuil et al 214) horizon for ~ 5 EeV protons r 8
12 Modelling different UHECR source populations 5 EeV protons Unbiased (e.g.,grbs/pulsars) Linear (e.g.agn) Threshold (galaxy clusters) 1 EeV protons 9
13 Can we distinguish between astrophysical scenarios with anisotropy? FO, Kotera, Abdalla, in prep. Assume: 2º angular resolution JEM-EUSO detection efficiency (Adams et al 213) 3% energy resolution (Gaussian response) 5 years JEM-EUSO (optimistic) Frequency events E > 5 EeV n ~ 1-3 Mpc -3 1% protons isotropic! LSS/galaxy like! linear AGN like! thres cluster like.2 X = X i N CR,i N iso,i N M,i N iso,i 1 2 X UB N iso,i P(not iso LSS model)99.7% > 99.9% 1
14 Can we distinguish between astrophysical scenarios with anisotropy? FO, Kotera, Abdalla, in prep. Assume: 2º angular resolution JEM-EUSO detection efficiency (Adams et al 213) 3% energy resolution (Gaussian response) 5 years JEM-EUSO (optimistic) Frequency events E > 5 EeV 3 1% % isotropic protons n ~ 1-3 Mpc -3 isotropic! LSS/galaxy like! linear AGN like! thres cluster like.2 X = X i N CR,i N iso,i N M,i N iso,i X UB N P(not iso LSS model)99.7% > 99.9% 99% iso,i 1
15 Can we distinguish between astrophysical scenarios with anisotropy? FO, Kotera, Abdalla, in prep. Assume: 2º angular resolution JEM-EUSO detection efficiency (Adams et al 213) 3% energy resolution (Gaussian response) 5 years JEM-EUSO (optimistic) Frequency events E > 5 EeV 3 7 1% % isotropic protons n ~ 1-3 Mpc -3 isotropic! LSS/galaxy like! AGN linear like! cluster thres like X = X i N CR,i N iso,i N M,i N iso,i X UB N P(not iso LSS model)99.7% model)99% > 99.9% 7% 99% iso,i 1
16 Are we going to see anisotropy with JEM-EUSO? % of realisations with significant anisotropy % 99% 99.7% 21 events E > 5 EeV, n = 1 3 Mpc 3 99% CL unbiased (galaxy like)! linear (AGN like)! threshold (cluster like) Isotropic fraction 11
17 If we can determine the composition? % of realisations with a significant anisotropy signal Proton fraction events, E>5 EeV, n ~ 1-2 Mpc -3 (galaxy like)! unbiased (AGN like)! linear (cluster like) threshold Number of detected protons % CL 12
18 Distinguish between bias models? 21 events, E>5 EeV, n ~ 1-2 Mpc -3 % of realisations with a significant anisotropy signal Proton fraction Number of detected protons P(not Linear Biased) P(not Unbiased Linear) P(not Unbiased Biased) 99% CL 99.7% 13
19 Conclusions Auger (my analysis): ~2σ anisotropy hints - look out for new Auger publication soon. Next generation instrument (~2 events): Clustering of events around a few sources or: Clustering of source distribution (lower E and/or higher number density): 4% proton composition, >4 protons -> statistically significant anisotropy 1 protons: distinguish different astrophysical scenarios High statistics will help whatever the source number density and threshold energy Distinguishing p/heavy elements would help 14
20 Conclusions Auger (my analysis): ~2σ anisotropy hints - look out for new Auger publication soon. Next generation instrument (~2 events): Clustering of events around a few sources or: Clustering of source distribution (lower E and/or higher number density): 4% proton composition, >4 protons -> statistically significant anisotropy 1 protons: distinguish different astrophysical scenarios High statistics will help whatever the source number density and threshold energy Distinguishing p/heavy elements would help 14
Study of the arrival directions of ultra-high-energy cosmic rays detected by the Pierre Auger Observatory
Study of the arrival directions of ultra-high-energy cosmic rays detected by the Pierre Auger Observatory Piera L. Ghia*, for the Pierre Auger Collaboration * IFSI/INAF Torino, Italy, & IPN/CNRS Orsay,
More informationUHECRs sources and the Auger data
UHECRs sources and the Auger data M. Kachelrieß Institutt for fysikk, NTNU Trondheim, Norway I review the evidence for a correlation of the arrival directions of UHECRs observed by the Pierre Auger Observatory
More informationUHECR autocorrelation function after Auger
UHECR autocorrelation function after Auger Pasquale D. Serpico based on work in collaboration with A. Cuoco, S. Hannestad,, T. Haugbølle,, M. Kachelrieß (arxiv:0709.2712; arxiv:0809.4003 :0809.4003) SOCoR
More informationA few grams of matter in a bright world
A few grams of matter in a bright world Benjamin Rouillé d Orfeuil (LAL) Fellow Collaborators: D. Allard, C. Lachaud & E. Parizot (APC) A. V. Olinto (University of Chicago) February 12 th 2013 LAL All
More informationP. Tinyakov 1 TELESCOPE ARRAY: LATEST RESULTS. P. Tinyakov. for the Telescope Array Collaboration. Telescope Array detector. Spectrum.
1 1 Université Libre de Bruxelles, Bruxelles, Belgium Telescope Outline Telescope Global distributions Hot spot Correlation with LSS Other searches Telescope UHECR experiments Telescope ARRAY COLLABORATION
More informationUltra-High Energy Cosmic Rays and Astrophysics. Hang Bae Kim Hanyang University Hangdang Workshop,
Ultra-High Energy Cosmic Rays and Astrophysics Hang Bae Kim Hanyang University Hangdang Workshop, 2012. 08. 22 Ultra High Energy Cosmic Rays Ultra High Energy Cosmic Ray (UHECR)» E 3 E & 10 18 ev Energy
More informationHigher Statistics UHECR observatories: a new era for a challenging astronomy
CRIS 2010 100 years of Cosmic Ray Physics: from Pioneering Experiments to Physics in Space 1 Higher Statistics UHECR observatories: a new era for a challenging astronomy Etienne Parizot APC University
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 informationThe AUGER Experiment. D. Martello Department of Physics University of Salento & INFN Lecce. D. Martello Dep. of Physics Univ. of Salento & INFN LECCE
The AUGER Experiment D. Martello Department of Physics University of Salento & INFN Lecce The Pierre Auger Collaboration Argentina Australia Bolivia Brazil Croatia Czech Rep. France Germany Italy Mexico
More informationSearches for cosmic ray anisotropies at ultra-high energies
Searches for cosmic ray anisotropies at ultra-high energies Haris Lyberis*, on behalf the Pierre Auger Collaboration * U n i v e r s i t é P a r i s V I I D e n i s d i d e r o t, P a r i s, F r a n c
More informationIntergalactic Magnetic Field and Arrival Direction of Ultra-High-Energy Protons
Intergalactic Magnetic Field and Arrival Direction of Ultra-High-Energy Protons Dongsu Ryu (Chungnam National U, Korea) Hyesung Kang (Pusan National U, Korea) Santabrata Das (Indian Institute of Technology
More informationThe Pierre Auger Observatory: on the arrival directions of the most energetic cosmic rays
The Pierre Auger Observatory: on the arrival directions of the most energetic cosmic rays Piera L. Ghia*, for the Pierre Auger Collaboration * IFSI/INAF Torino, Italy, & IPN/CNRS Orsay, France Outline
More informationOverview: UHECR spectrum and composition Arrival directions and magnetic field Method for search for UHE nuclei sources Application to the Auger data
Overview: UHECR spectrum and composition Arrival directions and magnetic field Method for search for UHE nuclei sources Application to the Auger data Acceleration of UHECR A.G.N. GRB Radio Galaxy Lobe
More informationP. Tinyakov 1,2 TELESCOPE ARRAY: LATEST RESULTS. P. Tinyakov. for the Telescope Array Collaboration. Telescope Array detector.
1,2 1 Université Libre de Bruxelles, Bruxelles, Belgium 2 Institute for Nuclear Research, Moscow, Russia Telescope Outline Telescope Telescope UHECR ground-based experiments Telescope ARRAY DETECTOR Telescope
More informationMulti-Messenger Astonomy with Cen A?
Multi-Messenger Astonomy with Cen A? Michael Kachelrieß NTNU, Trondheim [] Outline of the talk 1 Introduction 2 Dawn of charged particle astronomy? Expectations vs. Auger data Effects of cluster fields
More informationSearch for clustering of ultra high energy cosmic rays from the Pierre Auger Observatory
Nuclear Physics B (Proc. Suppl.) 190 (2009) 198 203 www.elsevierphysics.com Search for clustering of ultra high energy cosmic rays from the Pierre Auger Observatory Silvia Mollerach, for the Pierre Auger
More informationAnisotropy studies with the Pierre Auger Observatory
Anisotropy studies with the Pierre Auger Observatory Carla Macolino 1 for the Pierre Auger Collaboration 2 Full author list: http://www.auger.org/archive/authors_2011_05.html 1 Lab. de Physique Nucleaire
More informationStudies of Ultra High Energy Cosmic Rays with the Pierre Auger Observatory
Studies of Ultra High Energy Cosmic Rays with the Pierre Auger Observatory Universidade Federal do Rio de Janeiro, Brazil E-mail: haris@if.ufrj.br Aquiring data continuously from 004, the Pierre Auger
More informationArrival directions of the highest-energy cosmic rays detected by the Pierre Auger Observatory
Arrival directions of the highest-energy cosmic rays detected by the Pierre Auger Observatory a for the Pierre Auger Collaboration b a Instituto de Física, Universidade Federal do Rio de Janeiro, Brazil
More informationSERCH FOR LARGE-SCALE
SERCH FOR LARGE-SCALE Université Libre de Bruxelles (ULB) Brussels SNOWPAC 23-28 March, 2010 Matter tracer model: generic model of CRs under the assumptions: nearly straight propagation typical deflections
More informationThe Pierre Auger Observatory Status - First Results - Plans
The Pierre Auger Observatory Status - First Results - Plans Andreas Haungs for the Pierre Auger Collaboration Forschungszentrum Karlsruhe Germany haungs@ik.fzk.de Andreas Haungs Pierre Auger Observatory
More informationIs the search for the origin of the Highest Energy Cosmic Rays over? Alan Watson University of Leeds, England
Colloquium, University of Virginia: 18 April 2008 Is the search for the origin of the Highest Energy Cosmic Rays over? Alan Watson University of Leeds, England a.a.watson@leeds.ac.uk 1 OVERVIEW Why there
More informationUltra High Energy Cosmic Rays What we have learnt from. HiRes and Auger. Andreas Zech Observatoire de Paris (Meudon) / LUTh
Ultra High Energy Cosmic Rays What we have learnt from HiRes and Auger Andreas Zech Observatoire de Paris (Meudon) / LUTh École de Chalonge, Paris, Outline The physics of Ultra-High Energy Cosmic Rays
More informationThe influence of the observatory latitude on the study of ultra high energy cosmic rays
Prepared for submission to JCAP arxiv:1703.01529v1 [astro-ph.he] 4 Mar 2017 The influence of the observatory latitude on the study of ultra high energy cosmic rays Rita C. dos Anjos, a,b,1 Vitor de Souza
More informationUHE Cosmic Rays in the Auger Era
Vulcano Workshop 2010 - May, 23-29, 2010 UHE Cosmic Rays in the Auger Era Sergio Petrera, L'Aquila University email: sergio.petrera@aquila.infn.it Vulcano Workshop 2010 - May, 23-29, 2010 UHE Cosmic Rays
More informationPoS(ICRC2017)548. Telescope Array anisotropy summary
Telescope Array anisotropy summary M. Fukushima 1,2, D. Ikeda 1, D. Ivanov 3, K. Kawata 1, E. Kido 1, J.P. Lundquist 3, J.N. Matthews 3, T. Nonaka 1, T. Okuda 4, G. Rubtsov 5, H. Sagawa 1, N. Sakurai 6,
More informationDetection of Ultra-high energy neutrinos The First Light of the high energy neutrino astronomy
Detection of Ultra-high energy neutrinos The First Light of the high energy neutrino astronomy Shigeru Yoshida Department of Physics Chiba University the 1 st discovery of the PeV ν Bert Physical Review
More informationRECENT RESULTS FROM THE PIERRE AUGER OBSERVATORY
RECENT RESULTS FROM THE PIERRE AUGER OBSERVATORY (Neutrino 2008, Christchurch, NZ) Esteban Roulet (Bariloche) the Auger Collaboration: 17 countries, ~100 Institutions, ~400 scientists Argentina, Australia,
More informationOVERVIEW OF THE RESULTS
VIIIth International Workshop on the Dark Side of the Universe, Buzios STUDY OF THE ULTRA HIGH ENERGY COSMIC RAYS WITH THE AUGER DATA OVERVIEW OF THE RESULTS H. Lyberis on behalf of the Pierre Auger Collaboration
More informationarxiv: v2 [astro-ph.he] 1 Aug 2014
Mon. Not. R. Astron. Soc., 1 (214) Printed th March 217 (MN LATEX style file v2.2) A Bayesian self-clustering analysis of the highest energy cosmic rays detected by the Pierre Auger Observatory Alexander
More informationAn Auger Observatory View of Centaurus A
An Auger Observatory View of Centaurus A Roger Clay, University of Adelaide based on work particularly done with: Bruce Dawson, Adelaide Jose Bellido, Adelaide Ben Whelan, Adelaide and the Auger Collaboration
More informationSecondary particles generated in propagation neutrinos gamma rays
th INT, Seattle, 20 Feb 2008 Ultra High Energy Extragalactic Cosmic Rays: Propagation Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware Energy loss processes protons
More informationDetection of Ultra-high energy neutrinos The First Light of the high energy neutrino astronomy
Detection of Ultra-high energy neutrinos The First Light of the high energy neutrino astronomy Shigeru Yoshida Department of Physics Chiba University black hole radiation enveloping black hole The highest
More informationPoS(ICRC2015)326. TA anisotropy summary
1, M. Fukushima 2,3, D. Ikeda 2, D. Ivanov 4, K. Kawata 2, E. Kido 2, J.N. Matthews 4, S. Nagataki 5, T.Nonaka 2, T. Okuda 6, G. Rubtsov 7, H. Sagawa 2, N. Sakurai 8, B.T. Stokes 4, M. Takeda 2, R. Takeishi
More informationStudy of Two Metrics for Anisotropy in the Highest Energy Cosmic Rays
Study of Two in the Highest Energy Cosmic Rays John D. Hague, B. R. Becker, L. Cazon, M. S. Gold, J. A. J. Matthews University of New Mexico Department of Physics and Astronomy jhague@unm.edu The Impact
More informationUltra-High Energy AstroParticles!
Ultra-High Energy AstroParticles! Angela V. Olinto The University of Chicago ICFA 2008 International Committee for! Future Accelerators! Ancient Accelerators!! Ancient Accelerators!! from 10 3 to 10 9
More informationCharged-particle and gamma-ray astronomy: deciphering charged messages from the world s most powerful
Charged-particle and gamma-ray astronomy: deciphering charged messages from the world s most powerful Charged-particle astronomy coming of age How it is done The sources The signals What we have learned
More informationUltraHigh Energy Cosmic Rays Corrected for Galaxy Magnetic Field Models: FRIs & BL Lacs (Galactic Plane sources?)
UltraHigh Energy Cosmic Rays Corrected for Galaxy Magnetic Field Models: FRIs & BL Lacs (Galactic Plane sources?) Neil M. Nagar U. de Concepción, Chile Nagar & Matulich 2008, A&A, 488, 879 Nagar & Matulich,
More informationCosmogenic neutrinos II
Cosmogenic neutrinos II Dependence of fluxes on the cosmic ray injection spectra and the cosmological evolution of the cosmic ray sources Expectations from the cosmic ray spectrum measured by the Auger
More informationRecent results from the Pierre Auger Observatory
Recent results from the Pierre Auger Observatory Esteban Roulet, for the Pierre Auger Collaboration CONICET, Centro Atómico Bariloche, Bustillo 9500, Bariloche, 8400, Argentina E-mail: roulet@cab.cnea.gov.ar
More informationExtensive Air Showers and Particle Physics Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware
Extensive Air Showers and Particle Physics Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware Extensive air showers are the cascades that develop in the atmosphere
More informationUHE Cosmic Rays and Neutrinos with the Pierre Auger Observatory
UHE Cosmic Rays and Neutrinos with the Pierre Auger Observatory Gonzalo Parente Bermúdez Universidade de Santiago de Compostela & IGFAE for the Pierre Auger Collaboration Particle Physics and Cosmology
More informationTHE PIERRE AUGER OBSERVATORY: STATUS AND RECENT RESULTS
SF2A 2006 D. Barret, F. Casoli, T. Contini, G. Lagache, A. Lecavelier, and L. Pagani (eds) THE PIERRE AUGER OBSERVATORY: STATUS AND RECENT RESULTS Serguei Vorobiov (for the Pierre Auger Collaboration)
More informationCross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background
Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background Masato Shirasaki (Univ. of Tokyo) with Shunsaku Horiuchi (UCI), Naoki Yoshida (Univ. of Tokyo, IPMU) Extragalactic Gamma-Ray Background
More informationUltra-High Energy Cosmic Rays and the GeV-TeV Diffuse Gamma-Ray Flux
The 4th International Workshop on The Highest Energy Cosmic Rays and Their Sources INR, Moscow May 20-22, 2008 Ultra-High Energy Cosmic Rays and the GeV-TeV Diffuse Gamma-Ray Flux Oleg Kalashev* (INR RAS)
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 informationShort review and prospects of radio detection of high-energy cosmic rays. Andreas Haungs
Short review and prospects of radio detection of high-energy cosmic rays 1 To understand the sources of cosmic rays we need to know their arrival direction energy and mass we need large statistics large
More informationUltra- high energy cosmic rays
Ultra- high energy cosmic rays Tiina Suomijärvi Institut de Physique Nucléaire Université Paris Sud, Orsay, IN2P3/CNRS, France Atélier CTA, IAP, Paris, 30-31 June 2014 Outline Pierre Auger Observatory:
More informationUltrahigh Energy Cosmic Rays propagation II
Ultrahigh Energy Cosmic Rays propagation II The March 6th lecture discussed the energy loss processes of protons, nuclei and gamma rays in interactions with the microwave background. Today I will give
More informationarxiv: v1 [astro-ph.he] 18 Oct 2009
draft of October 19, 2009 arxiv:0910.3361v1 [astro-ph.he] 18 Oct 2009 Intergalactic Magnetic Field and Arrival Direction of Ultra-High-Energy Protons Dongsu Ryu 1,4, Santabrata Das 2, and Hyesung Kang
More informationULTRA HIGH ENERGY COSMIC RAYS
ULTRA HIGH ENERGY COSMIC RAYS Carla Bonifazi Instituto de Física Universidade Federal do Rio de Janeiro Dark Side Of The Universe 2012 Buzios Brazil Outline Introduction UHECRs Detection Recent Progress
More informationMultiscale Autocorrelation Function: a new approach to anisotropy studies
Multiscale Autocorrelation Function: a new approach to anisotropy studies Manlio De Domenico 12, H. Lyberis 34 1 Laboratory for Complex Systems, Scuola Superiore di Catania, Catania, Italy 2 Istituto Nazionale
More informationUltra High Energy Cosmic Rays: Observations and Analysis
Ultra High Energy Cosmic Rays: Observations and Analysis NOT A NEW PROBLEM, STILL UNSOLVED John Linsley (PRL 10 (1963) 146) reports on the detection in Vulcano Ranch of an air shower of energy above 1020
More information(High-Energy) Cosmic Rays
APPEC Town Meeting Roadmap ( Considerations ) Discussion (High-Energy) Cosmic Rays Paris, 6-7 April 2016 Andreas Haungs Karlsruhe Institute of Technology Petr Tinyakov Université Libre de Bruxelles petr.tiniakov@ulb.ac.be
More informationMass Composition Study at the Pierre Auger Observatory
OBSERVATORY Mass Composition Study at the Pierre Auger Observatory Laura Collica for the Auger Milano Group 4.04.2013, Astrosiesta INAF Milano 1 Outline The physics: The UHECR spectrum Extensive Air Showers
More informationWORKSHOP PRESENTATIONS
KICP workshop, 2014 June 9-11, 2014 Chicago, IL WORKSHOP PRESENTATIONS http://kicp.uchicago.edu/ http://www.uchicago.edu/ The Kavli Institute for Cosmological Physics (KICP) at the University of Chicago
More informationWORKSHOP PROGRAM. High-Energy Messengers: Connecting the Non-Thermal Extragalactic Backgrounds KICP workshop, June 9-11, 2014 Chicago, IL
KICP workshop, 2014 June 9-11, 2014 Chicago, IL WORKSHOP PROGRAM http://kicp.uchicago.edu/ http://www.uchicago.edu/ The (KICP) at the University of Chicago is hosting a workshop this summer on the origin
More informationNeutrino Astronomy fast-forward
Neutrino Astronomy fast-forward Marek Kowalski (DESY & Humboldt University Berlin) TeVPA 2017, Columbus, Ohio Credit: M. Wolf/NSF The promised land The Universe is opaque to EM radiation for ¼ of the spectrum,
More informationarxiv:astro-ph/ v2 26 Aug 2004
Ultra-High Energy Cosmic Ray Probes of Large Scale Structure and Magnetic Fields Günter Sigl a,b, Francesco Miniati c, Torsten A. Enßlin c a GReCO, Institut d Astrophysique de Paris, C.N.R.S., 98 bis boulevard
More informationLecture 11: SDSS Sources at Other Wavelengths: From X rays to radio. Astr 598: Astronomy with SDSS
Astr 598: Astronomy with SDSS Spring Quarter 4, University of Washington, Željko Ivezić Lecture : SDSS Sources at Other Wavelengths: From X rays to radio Large Surveys at Many Wavelengths SDSS: UV-IR five-band
More informationWhite Paper on Ultra-High Energy Cosmic Rays
White Paper on Ultra-High Energy Cosmic Rays Corresponding author: A. V. Olinto 1, (olinto@kicp.uchicago.edu) Co-Authors: J. H. Adams 2, C. D. Dermer 3, J.F. Krizmanic 4, J.W. Mitchell 4, P. Sommers 5,
More informationSEARCHES OF VERY HIGH ENERGY NEUTRINOS. Esteban Roulet CONICET, Centro Atómico Bariloche
SEARCHES OF VERY HIGH ENERGY NEUTRINOS Esteban Roulet CONICET, Centro Atómico Bariloche THE NEUTRINO SKY THE ENERGETIC UNIVERSE multimessenger astronomy γ ν p γ rays (Fermi) ν (Amanda) UHE Cosmic rays
More informationULTRA-HIGH ENERGY COSMIC RAYS
ULTRA-HIGH ENERGY COSMIC RAYS P. Tinyakov Université Libre de Bruxelles (ULB), Brussels Odense Winter School, October 2012 Outline 1 Introduction 2 Extensive airshowers 3 Detection methods Surface Detectors
More informationThe Pierre Auger Observatory in 2007
The Pierre Auger Observatory in 2007 Henryk Wilczyński 1 for the Pierre Auger Collaboration 2 1 Institute of Nuclear Physics PAN, Kraków, Poland 2 Pierre Auger Observatory, Malargüe, Mendoza, Argentina
More informationProbing the extragalactic cosmic rays origin with gamma-ray and neutrino backgrounds
Probing the extragalactic cosmic rays origin with gamma-ray and neutrino backgrounds Denis Allard laboratoire Astroparticule et Cosmologie (APC, CNRS/Paris 7) in collaboration with Noemie Globus, E. Parizot,
More informationOn the GCR/EGCR transition and UHECR origin
UHECR 2014 13 15 October 2014 / Springdale (Utah; USA) On the GCR/EGCR transition and UHECR origin Etienne Parizot 1, Noémie Globus 2 & Denis Allard 1 1. APC Université Paris Diderot France 2. Tel Aviv
More informationChapter 1 Introduction. Particle Astrophysics & Cosmology SS
Chapter 1 Introduction Particle Astrophysics & Cosmology SS 2008 1 Ptolemäus (85 165 b.c.) Kopernicus (1473 1543) Kepler (1571 1630) Newton (1643 1727) Kant (1724 1630) Herschel (1738 1822) Einstein (1917)
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 informationThe Highest Energy Cosmic Rays
The Highest Energy Cosmic Rays Angela V. Olinto Department of Astronomy & Astrophysics, Kavli Institute of Cosmological Physics The University of Chicago, 5640 S. Ellis Ave, Chicago, IL 60637, USA olinto@oddjob.uchicago.edu
More informationarxiv:astro-ph/ v1 28 Oct 2004
Highest Energy Cosmic Rays Angela V. Olinto arxiv:astro-ph/0410685v1 28 Oct 2004 Department of Astronomy & Astrophysics, Kavli Institute of Cosmological Physics The University of Chicago, 5640 S. Ellis
More informationDr Carolyn Devereux - Daphne Jackson Fellow Dr Jim Geach Prof. Martin Hardcastle. Centre for Astrophysics Research University of Hertfordshire, UK
Millennium simulation of the cosmic web MEASUREMENTS OF THE LINEAR BIAS OF RADIO GALAXIES USING CMB LENSING FROM PLANCK Dr Carolyn Devereux - Daphne Jackson Fellow Dr Jim Geach Prof. Martin Hardcastle
More informationExperimental Constraints to high energy hadronic interaction models using the Pierre Auger Observatory part-i
Experimental Constraints to high energy hadronic interaction models using the Pierre Auger Observatory part-i (cosmic rays, the Auger detectors, event reconstruction, observations) Jose Bellido QCD @ Cosmic
More informationSEARCH FOR POINT-LIKE SOURCES OF COSMIC RAYS WITH ENERGIES ABOVE. Malina Aurelia Kirn
SEARCH FOR POINT-LIKE SOURCES OF COSMIC RAYS WITH ENERGIES ABOVE 10 18.5 ev IN THE HIRES I MONOCULAR DATASET by Malina Aurelia Kirn A thesis submitted in partial fulfillment of the requirements for the
More informationDES Galaxy Clusters x Planck SZ Map. ASTR 448 Kuang Wei Nov 27
DES Galaxy Clusters x Planck SZ Map ASTR 448 Kuang Wei Nov 27 Origin of Thermal Sunyaev-Zel'dovich (tsz) Effect Inverse Compton Scattering Figure Courtesy to J. Carlstrom Observables of tsz Effect Decrease
More informationRecent Results of the Observatory Pierre Auger. João R. T. de Mello Neto Instituto de Física Universidade Federal do Rio de Janeiro
Recent Results of the Observatory Pierre Auger João R. T. de Mello Neto Instituto de Física Universidade Federal do Rio de Janeiro S. Tomé e Príncipe, September 2009 Outline Cosmic ray detection and the
More informationConstraints and Signals from the Diffuse Gamma Ray and X-ray Backgrounds
Constraints and Signals from the Diffuse Gamma Ray and X-ray Backgrounds Kevork Abazajian University of California, Irvine!! KICP High-Energy Messengers Workshop June 10, 2014 The Diffuse Gamma Ray Background
More informationSignal Model vs. Observed γ-ray Sky
Signal Model vs. Observed γ-ray Sky Springel+, Nature (2008) Two main dark matter signal components: 1. galactocentric diffuse 2. small structures Observed sky modeled with bremsstrahlung π 0 decay up-scattered
More informationPossible sources of very energetic neutrinos. Active Galactic Nuclei
Possible sources of very energetic neutrinos Active Galactic Nuclei 1 What might we learn from astrophysical neutrinos? Neutrinos not attenuated/absorbed Information about central engines of astrophysical
More informationUltra High Energy Cosmic Rays. Malina Kirn March 1, 2007 Experimental Gravitation & Astrophysics
Ultra High Energy Cosmic Rays Malina Kirn March 1, 2007 Experimental Gravitation & Astrophysics Outline Cosmic Rays What are UHECR? GZK Effect Why study UHECR? Pillars of Research Energy Spectrum Composition
More informationUltrahigh Energy cosmic rays II
Ultrahigh Energy cosmic rays II Today we will discuss the new data on UHECR presented during the last couple of years by the Auger observatory in Argentina. These data do not match previous analyses and
More informationA Multimessenger Neutrino Point Source Search with IceCube
A Multimessenger Neutrino Point Source Search with IceCube Mădălina Chera FLC Group Meeting 04.10.2010 Mădălina Chera Overview 1 Introduction to UHE Cosmic Rays and Neutrino Astrophysics; 2 Motivation
More informationResults from the Telescope Array Experiment
Results from the Telescope Array Experiment Hiroyuki Sagawa (ICRR, University of Tokyo) for the Telescope Array Collaboration @ AlbaNova University Center on 2011.08.1 2011/08/1 H. Sagawa @ 7th TeVPA in
More informationMeasurement of Anisotropy and Search for UHECR Sources
Prog. Theor. Exp. Phys. 2015, 00000 (29 pages) DOI: 10.1093/ptep/0000000000 Measurement of Anisotropy and Search for UHECR Sources O. Deligny 1, K. Kawata 2, and P. Tinyakov 3 arxiv:1702.07209v1 [astro-ph.he]
More informationCosmic Rays and Bayesian Computations
Cosmic Rays and Bayesian Computations David Ruppert Cornell University Dec 5, 2011 The Research Team Collaborators Kunlaya Soiaporn, Graduate Student, ORIE Tom Loredo, Research Associate and PI, Astronomy
More informationResults from the Pierre Auger Observatory. Paul Sommers, Penn State August 7, 2008, SSI
Results from the Pierre Auger Observatory Paul Sommers, Penn State August 7, 2008, SSI The Cosmic Ray Energy Spectrum Non-thermal, approximate power law, up to about 3x10 20 ev (possibly higher) 1 EeV
More informationReceived 2002 October 5; accepted 2002 December 10
The Astrophysical Journal, 586:1211 1231, 2003 April 1 # 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A. SMALL-SCALE CLUSTERING IN THE ISOTROPIC ARRIVAL DISTRIBUTION OF
More informationRecent results on UHECRs from the Pierre Auger Observatory. Olivier Deligny (IPN Orsay), on behalf the Pierre Auger Collaboration
Recent results on UHECRs from the Pierre Auger Observatory Olivier Deligny (IPN Orsay), on behalf the Pierre Auger Collaboration LHAASO Workshop, Beijing, Feb. 2011 1 UHE Detectors 2 With time, gain not
More informationContents Findings and Results
Contents 2 Findings and Results 31 2.1 Findings and Results Summary............................ 31 2.2 STACEE Finding and Results............................. 32 2.2.1 Gamma-ray Pulsars: PSR1951+32......................
More informationA Bayesian analysis of correlation between AGNs and ultra high energy cosmic rays detected by the Telescope Array Experiment
A Bayesian analysis of correlation between AGNs and ultra high energy cosmic rays detected by the Telescope Array Experiment Department of Physics, Yonsei University, Seoul, Korea E-mail: wrcho@yonsei.ac.kr
More informationPEV NEUTRINOS FROM THE PROPAGATION OF ULTRA-HIGH ENERGY COSMIC RAYS. Esteban Roulet CONICET, Bariloche, Argentina
PEV NEUTRINOS FROM THE PROPAGATION OF ULTRA-HIGH ENERGY COSMIC RAYS Esteban Roulet CONICET, Bariloche, Argentina THE ENERGETIC UNIVERSE multi-messenger astronomy γ ν p γ rays neutrinos Fermi Amanda UHE
More informationAir Shower Measurements from PeV to EeV
Air Shower Measurements from PeV to EeV Andreas Haungs haungs@ik.fzk.de James L. Pinfold August 2006 TeV workshop Madison, US Andreas Haungs 1 Cosmic Rays around the knee(s) EeV PeV Knee 2 nd Knee? Ralph
More informationFrontiers: Ultra High Energy Cosmic Rays
Frontiers: Ultra High Energy Cosmic Rays We now focus on cosmic rays with almost unimaginable energies: 10 19 ev and beyond. The very highest energy cosmic rays have energies in excess of 50 Joules(!),
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 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 informationUltra-High Energy Cosmic Rays & Neutrinos above the Terascale
Ultra-High Energy Cosmic Rays & Neutrinos above the Terascale Angela V. Olinto A&A, KICP, EFI The University of Chicago Nature sends 10 20 ev particles QuickTime and a YUV420 codec decompressor are needed
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 informationElisaBete de Gouveia Dal Pino (IAG-USP) On behalf of the CTA Collaboration
ElisaBete de Gouveia Dal Pino (IAG-USP) On behalf of the CTA Collaboration UFES,Vitoria, 8 de Outubro, 2018 TeV sky today (~212 sources, 62 unidentified) tevcat.uchicago.edu/ Supernovae Pulsar wind neb.
More informationExperimental High-Energy Astroparticle Physics
KIT University of the State of Baden-Württemberg and National Research Center of the Helmholtz Association Experimental High-Energy Astroparticle Physics Andreas Haungs haungs@kit.edu 3 Content: 1. Introduction
More informationStatus KASCADE-Grande. April 2007 Aspen workshop on cosmic ray physics Andreas Haungs 1
Status KASCADE-Grande April 2007 Aspen workshop on cosmic ray physics Andreas Haungs 1 Cosmic Rays around the knee(s) Astrophysical questions for this energy range: (1 st ) knee Knee position Composition
More informationCosmological Evolution of Blazars
Cosmological Evolution of Blazars Chuck Dermer Naval Research Laboratory The impact of high energy astrophysics experiments on cosmological physics Kavli Institute for Cosmological Physics University of
More information