Aldo Morselli, INFN & Università di Roma Tor Vergata, 1 Andrea Lionetto INFN, Sezione di Roma 2 & Università di Roma Tor Vergata.

Slides:



Advertisements
Similar presentations
5th May 2010Fergus Wilson, RAL1 Experimental Particle Physics PHYS6011 Looking for Higgs and SUSY at the LHC or...what can you get for $10,000,000,000.
Advertisements

5th May 2011Fergus Wilson, RAL1 Experimental Particle Physics PHYS6011 Looking for Higgs and SUSY at the LHC or...what can you get for $10,000,000,000.
Astronomical Solutions to Galactic Dark Matter Will Sutherland Institute of Astronomy, Cambridge.
Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, 1 Aldo Morselli Andrea Lionetto Vladimir Zdravkovic.
SUSY Higgs with Non-perturbative effects Yukihiro Mimura (National Taiwan University) Based on PLB718 (2013) Collaboration with N. Haba, K. Kaneta,
Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, 1 Aldo Morselli INFN, Sezione di Roma 2 & Università.
Measurement of Relic Density at the LHC1 Bhaskar Dutta Texas A&M University Bhaskar Dutta Texas A&M University Measurement of Relic Density at the LHC.
Gennaro Corcella 1, Simonetta Gentile 2 1. Laboratori Nazionali di Frascati, INFN 2. Università di Roma, La Sapienza, INFN Phenomenology of new neutral.
INDIRECT DARK MATTER SEARCHES WITH HESS J-F Glicenstein IRFU/CEA-Saclay on behalf of the HESS collaboration.
Dark Matter Annihilation in the Milky Way Halo Shunsaku Horiuchi (Tokyo) Hasan Yuksel (Ohio State) John Beacom (Ohio State) Shin’ichiro Ando (Caltech)
L.S.Stark 1, M.Doro 2, H.Bartko 3, A.Biland 1, M.Gaug 2, S.Lombardi 2, M.Mariotti 2, F.Prada 4, M.Sanchez-Conde 4, F.Zandanel 2 (for the MAGIC Collaboration*)
Intro to neutralino dark matter Pearl Sandick University of Minnesota.
Dark Matter Explanation For e^\pm Excesses In Cosmic Ray Xiao-Gang He CHEP, PKU and Physics, NTU.
Searching for Dark Matter
Annihilating Dark Matter Nicole Bell The University of Melbourne with John Beacom (Ohio State) Gianfranco Bertone (Paris, Inst. Astrophys.) and Gregory.
1 Search for Dark Matter Galactic Satellites with Fermi-LAT Ping Wang KIPAC-SLAC, Stanford University Representing the Fermi LAT Collaboration.
SLAC, June 23 rd Dark Matter in Galactic Gamma Rays Marcus Ziegler Santa Cruz Institute for Particle Physics Gamma-ray Large Area Space Telescope.
Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 1 Novel Searches for Dark Matter with Neutrino Telescopes.
Larry Wai SLAC Representing the GLAST LAT Collaboration Dark Matter and New Physics working group KIPAC-SLAC GLAST Physics: Dark Matter and New Physics.
The positron excess and supersymmetric dark matter Joakim Edsjö Stockholm University
The LC and the Cosmos: Connections in Supersymmetry Jonathan Feng UC Irvine Arlington LC Workshop January 2003.
The LC and the Cosmos: Connections in Supersymmetry Jonathan Feng UC Irvine American Linear Collider Physics Group Seminar 20 February 2003.
Enhancement of Line Gamma Ray Signature from Bino-like Dark Matter Annihilation due to CP Violation Yoshio Sato (Saitama University/Technical University.
Mia Schelke, Ph.D. Student The University of Stockholm, Sweden Cosmo 03.
Significant enhancement of Bino-like dark matter annihilation cross section due to CP violation Yoshio Sato (Saitama University) Collaborated with Shigeki.
SUSY Dark Matter Collider – direct – indirect search bridge. Sabine Kraml Laboratoire de Physique Subatomique et de Cosmologie Grenoble, France ● 43. Rencontres.
The Dark Side of the Universe What is dark matter? Who cares?
High-energy electrons, pulsars, and dark matter Martin Pohl.
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 1 Report from Italy A. Morselli, A. Lionetto, A. Cesarini, F.Fucito, P.Ullio* INFN,
Singlet Dark Matter, Type II Seesaw and Cosmic Ray Signals Nobuchika Okada Miami Fort Fauderdale, Dec , 2009 University of Alabama, Tuscaloosa.
The Universe  What do we know about it  age: 14.6 billion years  Evolved from Big Bang  chemical composition  Structures.
Detecting dark matter annihilation at the ground EAS detectors X.J. Bi (IHEP)
Overview of indirect dark matter detection Jae Ho HEO Theoretical High Energy group Yonsei University 2012 Jindo Workshop, Sep
Direct and Indirect Dark Matter Detection in Models with a Well-Tempered Neutralino Eun-Kyung Park Florida State University in collaboration with H. Baer.
Dark Matter Particle Physics View Dmitri Kazakov JINR/ITEP Outline DM candidates Direct DM Search Indirect DM Search Possible Manifestations DM Profile.
DARK MATTER CANDIDATES Cody Carr, Minh Nguyen December 9 th, 2014.
Search for Gamma Rays from LKP Dark Matter in the UED framework with GLAST a E.Nuss b, J.Cohen-Tanugi c and A.Lionetto d on behalf of GLAST DM & Exotic.
Dark matter in split extended supersymmetry in collaboration with M. Quiros (IFAE) and P. Ullio (SISSA/ISAS) Alessio Provenza (SISSA/ISAS) Newport Beach.
The Origin and Acceleration of Cosmic Rays in Clusters of Galaxies HWANG, Chorng-Yuan 黃崇源 Graduate Institute of Astronomy NCU Taiwan.
Low scale supergravity mediation in brane world scenario and hidden sector phenomenology Phys.Rev.D74:055005,2006 ( arXiv: hep-ph/ ) ACFA07 in Beijing:
Lake Louise - February Detection & Measurement of gamma rays in the AMS-02 Detector J. Bolmont - LPTA - IN2P3/CNRS Montpellier - France.
Gamma rays annihilated from substructures of the Milky Way and Quintessino dark matter Bi Xiao-Jun Institute of High Energy Physics, Chinese Academy of.
Summary of indirect detection of neutralino dark matter Joakim Edsjö Stockholm University
1 Additional observable evidences of possible new physics Lecture from the course “Introduction to Cosmoparticle Physics”
Analysis methods for Milky Way dark matter halo detection Aaron Sander 1, Larry Wai 2, Brian Winer 1, Richard Hughes 1, and Igor Moskalenko 2 1 Department.
中国科学院高能物理研究所 INSTITUTE OF HIGH ENERGY PHYSICS Constraints on the cross-section of dark matter annihilation from Fermi observation of M31 Zhengwei Li Payload.
DARK MATTER & GALACTIC ROTATION 2012 ASTRO SUMMER SCHOOL.
Collider searchIndirect Detection Direct Detection.
Anisotropies in the gamma-ray sky Fiorenza Donato Torino University & INFN, Italy Workshop on High-Energy Messengers: connecting the non-thermal Extragalctic.
Indirect Detection Of Dark Matter
CONSTRAINED MSSM AND RECENT ASTROPHYSICAL DATA Alexey Gladyshev (JINR, Dubna & ITEP, Moscow) SEMINAR AT KEK THEORY GROUP November 1, 2004.
Gennaro Corcella 1, Simonetta Gentile 2 1. Laboratori Nazionali di Frascati, INFN 2. Università di Roma, La Sapienza, INFN Z’production at LHC in an extended.
Type II Seesaw Portal and PAMELA/Fermi LAT Signals Toshifumi Yamada Sokendai, KEK In collaboration with Ilia Gogoladze, Qaisar Shafi (Univ. of Delaware)
STAU CLIC Ilkay Turk Cakir Turkish Atomic Energy Authority with co-authors O. Cakir, J. Ellis, Z. Kirca with the contributions from A. De Roeck,
Keegan Stoner Columbia High School. dark matter Obeying Inverse Square Law Outer stars orbit too fast what we should seewhat we actually see.
DARK MATTER Fisica delle Astroparticelle Piergiorgio Picozza a.a
Elba -- June 7, 2006 Collaboration Meeting 1 CDF Melisa Rossi -- Udine University On behalf of the Multilepton Group CDF Collaboration Meeting.
Topics on Dark Matter Annihilation
Indirect dark matter search with the balloon-borne PEBS detector
An interesting candidate?
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata
Imaging Dark Matter with the Pamela Experiment
Dark Matter in Galactic Gamma Rays
Dark Matter Subhalos in the Fermi First Source Catalog
Topics in Higgs Portal Dark Matter
Dark Matter Phenomenology of the GUT-less CMSSM
Neutral and charged Higgsino as carriers of residual SUSY effects.
朱守华, 北京大学物理学院.
Indirect detection of dark matter
Evidence for WIMP Dark Matter
Presentation transcript:

Aldo Morselli, INFN & Università di Roma Tor Vergata, 1 Andrea Lionetto INFN, Sezione di Roma 2 & Università di Roma Tor Vergata Dark Activities ASI Workshop, Frascati 3 Luglio 2007

Dark Matter really exist ? = M + = ~ 0.73 M ~ 0.27 CDM ~ 0.23 b ~ 0.04 HDM, < 0.01 { Concordance model CDM ~ 6 b

color image from the Magellan images of the merging cluster 1E kpc Chandra image of the cluster weak lensing reconstruction NEWS: Dark Matter really exist ? astro-ph/ Due to the collision of two clusters, the dissipationless stellar component and the fluid-likeX-ray emitting plasma are spatially segregated

Dark Matter Ring around Galaxy Cluster CL M.Jee et al.,arXiv: high-speed line-of-sight collision of two massive clusters ~ 1-2 Gyr ago

Aldo Morselli, INFN & Università di Roma Tor Vergata, 5

6 1% Stars 7% Gas in vir. structures 7% WH Gas in IGM 85% DARK MATTER Baryons Non-baryonic An Inventory of Matter in the Universe So, what is Dark Matter?

Aldo Morselli, INFN & Università di Roma Tor Vergata, 7

8 Particle Physics after Big Bang

Supersymmetry Particle Sparticle For unbroken supersymmetry there is a mass degeneracy Sparticle have not be found at accelerators so far Supersymmetry is broken Supersymmetry breaking schemes: gravity-mediated scenarios Gauge mediated scenarios Anomaly mediated scenarios

Running couplings

Neutralino WIMPs Assume c are present in the galactic halo c Majorana particle => can annihilate in pairs in the galactic halo producing gamma-rays, antiprotons, positrons…. Antimatter not produced in large quantities through standard processes (secondary production through p + p --> p + X) So, any extra contribution from exotic sources (c c annihilation) is an interesting signature ie: c c --> p + X Produced from (e. g.) c c --> q / g / gauge boson / Higgs boson and subsequent decay and/ or hadronisation.

PAMELA Payload for Antimatter Matter Exploration and Light Nuclei Astrophysics In orbit on June 15, 2006, on board of the DK1 satellite by a Soyuz rocket from the Bajkonour launch site. First switch-on on June From July 11 Pamela is in continuous data taking mode

Aldo Morselli, INFN & Università di Roma Tor Vergata, 13 PAMELA

Aldo Morselli, INFN & Università di Roma Tor Vergata, 14 PAMELA: Cosmic-Ray Antiparticle Measurements: Antiprotons fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton ux A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [astro-ph/ ] an example in mSUGRA f = the dark matter fraction concentrated in clumps d = the overdensity due to a clump with respect to the local halo density

Aldo Morselli, INFN & Università di Roma Tor Vergata, 15 PAMELA: Cosmic-Ray Antiparticle Measurements: Antiprotons contribution background totalMSSM fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton ux A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [ astro-ph/ ]

Where should we look for WIMPs with GLAST? Galactic center Galactic satellites Galactic halo Extra-galactic

Aldo Morselli, INFN & Università di Roma Tor Vergata, 17 Sun Galactic Center

Signal rate from Supersymmetry governed by supersymmetric parameters governed by halo distribution gamma-ray flux from neutralino annihilation J( ):

Model independent results for the GC Assume a truncated NFW profile Assume a dominant annihilation channel (good assumption except for + - ) Differential yield for each annihilation channel WIMP mass=200GeV figure from: A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, , June 2004 [astro-ph/ ]

Aldo Morselli, INFN & Università di Roma Tor Vergata, 20 neutralino mass Differential yield for b bar

Aldo Morselli, INFN & Università di Roma Tor Vergata, 21 EGRET data & Susy models ~2 degrees around the galactic center EGRET data Annihilation channel W + W - M =80.3 GeV background model(Galprop) WIMP annihilation (DarkSusy) Total Contribution A.Morselli, A. Lionetto, A. Cesarini, F. Fucito, P. Ullio, astro-ph/ N b = N = Typical N values: NFW: N = 10 4 Moore: N = Isotermal: N =

Aldo Morselli, INFN & Università di Roma Tor Vergata, 22 ~2 degrees around the galactic center, 2 years data (Galprop) (one example from DarkSusy) GLAST Expectation & Susy models astro-ph/ A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, , June 2004 [astro-ph/ ] N b = N = Typical N values: NFW: N = 10 4 Moore: N = Isotermal: N = Annihilation channel W + W - M =80 GeV

Model independent results for the GC 3 Max background Min background

Aldo Morselli, INFN & Università di Roma Tor Vergata, 24 EGRET, E > 1GeV Mayer- Hasselwander et al, 1998 Integral data 2 0 x 2 0 field IBIS/ISGRI 20–40 keV

Aldo Morselli, INFN & Università di Roma Tor Vergata, 25 1 pixel ~ 5 arcmin 2 0 x 2 0 field IBIS/ISGRI 20–40 keV Point source location for GLAST~ 5 arcmin

Galactic Center HESS and MAGIC Spectrum Unbroken power-law. Hard spectrum = 2.2. No evidence for variability on a variety of time scales. Consistent with SGR A* to 6 and slightly extended. SGR A Good agreement between HESS and MAGIC (large zenith angle observation). astro-ph/

Aldo Morselli, INFN & Università di Roma Tor Vergata, 27 EGRET, GLAST, HESS, MAGIC it might still be that a DM component could be singled out, e.g. the EGRET source (?): a DM source can fit the EGRET data; GLAST would detect its spectral and angular signatures and identify without ambiguity such DM source!

Model independent results for the GC 3 Max background Min background Excluded by HESS and MAGIC

Satellites Optimistic case: 70 counts signal, 43 counts background within 1.5 deg of clump center 55-days GLAST in-orbit counts map (E>1GeV) Galactic Center 30-deg latitude Larry Wai et al. for the DM&NP Working Group

The search for milky way halo substructure WIMP annihilations using the GLAST LAT Dark matter calculation with semi-analytic method of Taylor & Babul 2004, 2005 Background estimate using EGRET above 1GeV (source subtracted) M=100GeV = 2.3x cm 3 s -1

GLAST sensitivity map for the identification of point sources of Dark Matter annihilation G.Bertone et al. astro-ph/

Cosmological Wimp annihiliation spectrum

spectral fits of simulated DM point sources

Supersymmetry introduces free parameters: In the MSSM, with Grand Unification assumptions, the masses and couplings of the SUSY particles as well as their production cross sections, are entirely described once 5 parameters are fixed: M 1/2 the common mass of supersymmetric partners of gauge fields (gauginos) m 0 the common mass for scalar fermions at the GUT scale m the higgs mixing parameters that appears in the neutralino and chargino mass matrices A is the proportionality factor between the supersymmetry breaking trilinear couplings and theYukawa couplings tan b = v 2 / v 1 = / the ratio between the two vacuum expectation values of the Higgs fields

GLAST limits no electroweak symmetry breaking WMAP 3 allowed region (95% C.L) tg( )=55, sign( )=+1 3 σ Sensitivity plot for for GLAST for a truncated (NFW) halo profile mSUGRA Sensitivity plot for 5 years observation of mSUGRA for GLAST for tan( b )=55. GLAST 3 σ sensitivity is shown at the blue line and below for truncated NFW halo profile

3 σ Sensitivity plot for for GLAST for a truncated (NFW) halo profile tg( )=55, sign( )=+1 equi neutralino mass curves GLAST limits no electroweak symmetry breaking WMAP 3 allowed region (95% C.L) m =400 GeV m =200 GeV m =300 GeV mSUGRA Sensitivity plot for 5 years observation of mSUGRA for GLAST for tan( b )=55. GLAST 3 σ sensitivity is shown at the blue line and below for truncated NFW halo profile

LHC limits 100 fb -1 LC500 GLAST limits LC1000 limits PAMELA Limits boost factor 10 accelerator 100 fb -1 from H.Baer et al., hep-ph/ GLAST, PAMELA, LHC, LC Sensitivities to Dark Matter Search mSUGRA Sensitivity plot for 5 years observation of mSUGRA for GLAST for tg(b)=55 and for other experiments. GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile

Aldo Morselli, INFN & Università di Roma Tor Vergata, 38 no electroweak symmetry breaking LHC limits LC1000 limits LCC2 m h 0 < GeV WMAP 3 3 allowed region GLAST limits tg( )=10, sign( )=+1 LC500 Sensitivity plot for observation of mSUGRA for a number of accelerator experiments and GLAST for tan( b )=10. GLAST 5 σ sensitivity is shown at the blue line and below a for truncated Navarro Frank and White (NFW) halo profile LCC2 from E.Baltz et al. hep- ph/ mSUGRA

no electroweak symmetry breaking tg( )=60, sign( )=+1 WMAP 3 5 allowed region GLAST 5 limits 5 years of data 5 σ Sensitivity plot for for GLAST for a truncated NFW halo profile mSUGRA Sensitivity plot for observation of mSUGRA for GLAST for tan( )=60. GLAST 5 σ sensitivity is shown at the blue line and below a for truncated NFW halo profile

the end

Aldo Morselli, INFN & Università di Roma Tor Vergata, x 2 0 field IBIS/ISGRI 20–40 keV1 pixel ~ 5 arcmin Point source location for GLAST~ 5 arcmin 2 0 x 2 0 field EGRET, E > 1GeV

Aldo Morselli, INFN & Università di Roma Tor Vergata, 42

Aldo Morselli, INFN & Università di Roma Tor Vergata, 44

you need a factor ~ with respect to the standard mSugra scenario Conclusion: GLAST limits for clumpiness factor 10