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RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 1
Multifrequency tests of Dark Matter
Sources
Aldo MorselliINFN Roma Tor Vergata
FRASCATI WORKSHOP 2009, Silver Jubilee May 25-30, VulcanoRENATA REd NAcional Temática de Astropartículas , Alcala
Aldo MorselliINFN, Sezione di Roma 2 &
Università di Roma Tor Vergata
Search for Dark matter in the sky in the Fermi and Pamela era.
June 23 2009
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 2
Neutralino WIMPs
Assume χ present in the galactic halo• χ is its own antiparticle => can annihilate in galactic haloproducing gamma-rays, antiprotons, positrons….• Antimatter not produced in large quantities through standard processes(secondary production through p + p --> anti p + X)• So, any extra contribution from exotic sources (χ χ annihilation) is aninteresting signature• ie: χ χ --> anti p + X• Produced from (e. g.) χ χ --> q / g / gauge boson / Higgs boson andsubsequent decay and/ or hadronisation.
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 3
Antiproton/proton ratio 1997
Caprice coll.Astrophysics Journal,487, 415, 1997
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 4
MASS Matter Antimatter Space Spectrometer
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 5
MASS 89 the calorimeter
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 6MASS 89 flight
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 7MASS 89 flight
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 8MASS 89
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 9
PAMELA Payload for Antimatter Matter Exploration and
Light Nuclei Astrophysics
In orbit on June 15, 2006, on board of the DK1satellite by a Soyuz rocket from the Bajkonourlaunch site.First switch-on on June 21 2006From July 11 Pamela is in continuous datataking mode
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 10
Separating pfrom e-
Pamela
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 11
PAMELA:Cosmic-Ray Antiparticle
Measurements: Antiprotons
fd: Clumpiness factors neededto disentangle a neutralinoinduced component in theantiproton flux
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 [astro-ph/0502406]
an example in mSUGRA
f = the dark matter fractionconcentrated in clumpsd = the overdensity due to aclump with respect to the localhalo density
DSU06
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 12
• ~ 3 years fromPAMELA launch
• Launched in orbit onJune 15, 2006, on boardof the DK1 satellite by aSoyuz rocket from theBajkonour cosmodrom.
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 13
antip
roto
n / p
roto
n Antiproton-Proton Ratio
• PAMELA data, Nature [arxiv:0810.4994]
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 14
Antiproton-Proton Ratio
Diffuse and ConventionPropagation ModelUpper and lower bounds A.Lionetto, A.Morselli, V.ZdravkovicJCAP09 (2005) 010 [astro-ph/0502406]
• PAMELA data arxiv:0810.4994
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 15
PAMELA antiprotons and WIMP Detection
CMSSM
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 16
PAMELA antiprotons and WIMP Detection CMSSM
larger values of tg(B) gives larger signals both in antiprotons and gammas
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 17
Antiproton-Proton Ratio
Diffuse and ConventionPropagation ModelUpper and lower bounds A.Lionetto, A.Morselli, V.ZdravkovicJCAP09 (2005) 010 [astro-ph/0502406]
• PAMELA data arxiv:0810.4994
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 18
Propagation Equation for Cosmic Rays
convection velocity field that corresponds togalactic wind and it has a cylindrical symmetry,as the geometry of the galaxy. It’s z-componentis the only one different from zero and increaseslinearly with the distance from the galactic plane loss term: fragmentation
loss term: radioactive decaydiffusion coefficient is function of rigidity
diffusioncoefficient in theimpulse space,quasi-linear MHD:
primary spectra injection index
implemented in Galprop ( Strong &Moskalenko, available on the Web) [astro-ph/0502406]
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 19
Cosmic Ray Electron propagation modelsCosmic Ray Electron propagation modelsThey generally assume:• Power-law source spectrum
• Power-law diffusion coefficient (normalised to match CR nuclear data)• Continuos source distribution in the Galactic Disk
For E > 10 GeV solar modulation, re-acceleration, convection have negligible effects.Only synchrotron and IC energy losses matter. Under those conditions
!
Ne(E) " E
- # 0
!
D = D
0
E
E0
#
%
&
( )
!
Ne(E) " E
- ( # 0 + $
2 +
1
2)
This is only for illustrative purposes. All models here have been computed with GALPROP accountingfor all effects !!
See http://galprop.stanford.edu/web_galprop/galprop_home.html
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 20
The situation before 2008The situation before 2008Electron + positron spectrumElectron + positron spectrum
Data were compatible with conventional large-scale Galactic models of CRs tuned to fitgamma-ray data and other observables
GALPROP model with γ0 = 2.54 ( δ = 0.33 )
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 21
Antiproton-Proton Ratio
Diffuse and ConventionPropagation ModelUpper and lower bounds A.Lionetto, A.Morselli, V.ZdravkovicJCAP09 (2005) 010 [astro-ph/0502406]
• PAMELA data arxiv:0810.4994
The conventionalGALPROP model with γ0 = 2.54 ( δ = 0.33 )
gives a satisfactorydescription of those data
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 22
2008: Results from ATIC and HESS2008: Results from ATIC and HESS
Data clearly call for major changes to the conventional model:Nearby sources (e.g. pulsar) or dark matter annihilation/decay models have been proposedto explain those data
GALPROP model with γ0 = 2.54 ( δ = 0.33 )
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 23
2009: PAMELA results2009: PAMELA results
conventional GALPROP model γ0 = 2.54 ( δ = 0.33 )Secondary positrons only !
e+/(e+ + e-) ∝ E - γp + γ0 - δ γp: proton source power-indexIt improves only adopting very soft electron spectra (high γ0 )
E< 10 Gev, probably solar modulation effect
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 24
1. arXiv:0901.3474 Cosmic Ray Positrons from Cosmic Strings Robert Brandenberger, Yi-Fu Cai, Wei Xue, Xinmin Zhang2. arXiv:0901.2556 Positrons and antiprotons from inert doublet model dark matter Emmanuel Nezri, Michel H.G. Tytgat,
Gilles Vertongen3. arXiv:0901.1520 On the cosmic electron/positron excesses and the knee of the cosmic rays - a key to the 50 years' puzzle?
Hong-Bo Hu, Qiang Yuan, Bo Wang, Chao Fan , Jian-Li Zhang , Xiao-Jun Bi4. arXiv:0812.4851 A Gamma-Ray Burst for Cosmic-Ray Positrons with a Spectral Cutoff and LineKunihito Ioka5. arXiv:0812.4555 Is the PAMELA Positron Excess Winos? Phill Grajek, Gordon Kane, Dan Phalen, Aaron Pierce, Scott
Watson6. arXiv:0812.4457 Dissecting Pamela (and ATIC) with Occam's Razor: existing, well-known Pulsars naturally account for
the "anomalous" Cosmic-Ray Electron and Positron Data Stefano Profumo7. arXiv:0812.4272 Study of positrons from cosmic rays interactions and cold dark matter annihilations in the galactic
environment Roberto A. Lineros thesis8. arXiv:0812.3895 Gamma-ray and Radio Constraints of High Positron Rate Dark Matter Models Annihilating into New
Light Particles Lars Bergstrom, Gianfranco Bertone, Torsten Bringmann, Joakim Edsjo, Marco Taoso9. arXiv:0812.2102 A Relativistic Electron-Positron Outflow from a Tepid FireballKatsuaki Asano, Fumio Takahara10. arXiv:0812.0219 Neutrino Signals from Annihilating/Decaying Dark Matter in the Light of Recent Measurements of
Cosmic Ray Electron/Positron Fluxes Junji Hisano, Masahiro Kawasaki, Kazunori Kohri, Kazunori Nakayama11. arXiv:0811.0477 High-energy Cosmic-Ray Positrons from Hidden-Gauge-Boson Dark Matter Chuan-Ren Chen,
Fuminobu Takahashi, T. T. Yanagida11. arXiv:0811.3526 Status of indirect searches in the PAMELA and Fermi era Aldo Morselli, Igor Moskalenko
some articles about the positron excess
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 25
12. arXiv:0811.0250 Cosmic-Ray Positron from Superparticle Dark Matter and the PAMELA Anomaly Koji Ishiwata, ShigekiMatsumoto, Takeo Moroi13. arXiv:0810.5344 The PAMELA Positron Excess from Annihilations into a Light Boson Ilias Cholis, Douglas P. Finkbeiner, LisaGoodenough, Neal Weiner14. arXiv:0810.4846 Possible causes of a rise with energy of the cosmic ray positron fraction Pasquale Dario Serpico15. arXiv:0810.2784 TeV Gamma Rays from Geminga and the Origin of the GeV Positron Excess Hasan Yuksel , Matthew D. KistlerTodor Stanev16. arXiv:0810.1892 Positron/Gamma-Ray Signatures of Dark Matter Annihilation and Big-Bang Nucleosynthesis Junji Hisano, MasahiroKawasaki, Kazunori Kohri, Kazunori Nakayama17. arXiv:0810.1527 Pulsars as the Sources of High Energy Cosmic Ray Positrons Dan Hooper, Pasquale Blasi, Pasquale Dario Serpico18. arXiv:0809.5268 Galactic secondary positron flux at the Earth T. Delahaye, F. Donato , N. Fornengo , J. Lavalle , R. Lineros , P. Salati ,R. Taillet ,19. arXiv:0809.2601 Two dark matter components in N_{DM}MSSM and dark matter extension of the minimal supersymmetricstandard model and the high energy positron spectrum in PAMELA/HEAT data Ji-Haeng Huh, Jihn E. Kim, Bumseok Kyae20. arXiv:0809.2491 On the 511 keV emission line of positron annihilation in the Milky Way N. Prantzos22. arXiv:0809.0792 Gamma rays and positrons from a decaying hidden gauge boson Chuan-Ren Chen, Fuminobu Takahashi, T. T.Yanagida23. arXiv:0808.3867 Minimal Dark Matter predictions and the PAMELA positron excessMarco Cirelli, Alessandro Strumia24. arXiv:0808.3725 New Positron Spectral Features from Supersymmetric Dark Matter - a Way to Explain the PAMELA Data?LarsBergstrom, Torsten Bringmann, Joakim Edsjo
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 2611 June 2008
~ 1 year from Fermi launch
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 27
The Galactic Diffuse Emission•Spectra shown formid-latitude range→ GeV excess inthis region of thesky is notconfirmed.•Sources are notsubtracted but area minor component.•LAT errors aredominated bysystematicuncertainties andare currentlyestimated to be~10% → this ispreliminary.
Fermi LAT
Fermi Coll. , to appear soon
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 28
2009: Fermi-LAT diffuse gamma-ray spectrum first measurements2009: Fermi-LAT diffuse gamma-ray spectrum first measurementsEGRET GeV excess wasnot observed ⇒Conventional models(based on the locallymeasured CR fluxes) canbe used
The conventional modelwithγ0 = 2.54 ( δ = 0.33 )gives a satisfactorydescription of Fermi-LATgamma-ray data
Conventional model areweakly affected by smallchanges in the electronspectrum.
Fermi Coll. , to appear soon PRELIMINARY
Fermi LAT dataTotal
π0 decay
IC
Bremsstrahlung
Isotropic component
Sources
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 29
2009: Fermi-LAT diffuse gamma-ray spectrum first measurements2009: Fermi-LAT diffuse gamma-ray spectrum first measurements
see: Gamma-ray detection from gravitino dark matter decay in the µνSSM arXiv:0906.368
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 30
gamma-ray spectrum for an example of gravitino dark matterdecay in the mid-latitude range
• 100≤ |b| ≤ 200
Gamma-ray detection from gravitino dark matter decay in the µνSSM arXiv:0906.368
Carlos Muñoz
yesterday
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 31
Fermi-LAT CRE data vs the conventional Fermi-LAT CRE data vs the conventional pre-Fermipre-Fermi model model
Although the feature @~600 GeV measured by ATIC is not confirmedSome changes are still needed respect to the pre-Fermi conventional model
Fermi Coll., PRL 102, 181101 (2009) [arXiv:0905.0025] 4/5/09
GALPROP model with γ0 = 2.54 ( δ = 0.33 )
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 32
(
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 33
How Fermi LAT detects gamma rays4 x 4 array of identical towers with:• Precision Si-strip tracker (TKR)
– With W converter foils• Hodoscopic CsI calorimeter (CAL)• DAQ and Power supply box
An anticoincidence detectoraround the telescope distinguishes gamma-rays from charged particles
γ
e+ e-
Conversion(γ in e+/e-)in W foils
Incoming γ
Incoming directionreconstruction bytracking thecharged particles
Energy measurementwith e.m.calorimeter
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 34
How Fermi LAT detects electronsTrigger and downlink
• LAT triggers on (almost)every particle that crossesthe LAT– ~ 2.2 kHz trigger rate
• On board processingremoves many chargedparticles events– But keeps events with more
that 20 GeV of depositedenergy in the CAL
– ~ 400 Hz downlink rate• Only ~1 Hz are good γ-rays
Electron identification• The challenge is identifying
the good electrons amongthe proton background– Rejection power of 103 –
104 required– Can not separate electrons
from positrons
ACD identifiescharged particles
Incoming Electron
Main trackpointing to thehit ACD tile
Same tracking andenergyreconstructionalgorithms usedfor γ-rays
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 35
Event topology
• TKR: clean main track with extra-clusters very close to the track
• CAL: clean EM shower profile, notfully contained
• ACD: few hits in conjunction withthe track
• TKR: small number of extraclusters around main track
• CAL: large and asymmetric showerprofile
• ACD: large energy deposit per tile
A candidate electron (recon energy 844 GeV)
A candidate hadron (raw energy > 800 GeV)
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 36
Reconstruction of the mostprobable value for the eventenergy:- based on calibration of theresponse of each of 1536calorimeter crystals- energy reconstruction isoptimized for each event-calorimeter imaging capabilityis heavily used for fittingshower profile --tested at CERN beams up to280 GeV with the LATCalibration Unit
Very good agreementbetween shower profile inbeam test data (red) andMonte Carlo (black)
Energy reconstruction
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 37
)
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 38
Models 0 and 1 account for CR re-acceleration in the ISM, while 2 is a plain-diffusionmodel. All models assume γ0 = 1.6 below 4 GeV.
γ0 = 2.42 (δ = 0.33 - with reacceleration): red line γ0 = 2.33 (δ = 0.6 - plain diffusion): blue line
• γ0 = 2.54 ( δ = 0.33 )
Cosmic Ray Electron propagation modelsCosmic Ray Electron propagation models
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 39
Numerical models of propagation of CR electrons can be tuned to fit Fermi dataassuming an harder injection index:Problems: These tuned models are in tension with low-energy and HESS data (no big problems with gamma-ray data - work in progress)
γ0 = 2.42 (δ = 0.33 - with reacceleration): red line γ0 = 2.33 (δ = 0.6 - plain diffusion): blue line
A simple interpretation of Fermi-LAT CRE spectrumA simple interpretation of Fermi-LAT CRE spectrum
• γ0 = 2.54 ( δ = 0.33 )
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 40
Fermi-LAT & HESS CRE dataFermi-LAT & HESS CRE datavs the conventional vs the conventional pre-Fermipre-Fermi model model
problem of the model with HESS @ E> 2 TeV γ0 = 2.54 ( δ = 0.33 )
cutoff in the CRE source spectrum or breakdown of the source spatial continuity?
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 41
NatureMLP+BDTD(+data, no pre-sampler,improved knowledge of detectors)
statistics improved by ~2.5 ÷ 3
GALPROP
Positron fraction, new analysis May 09
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 42
Primary electrons in Cosmic Rays
• Now, ~45 years laterPAMELA excess inpositron fraction
and Fermi results on the electron+positron
spectrum unavoidably testifies
the presence of primarypositrons in CRs
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 43
which are the sourcessources of theof theprimary positrons ?
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 44
Pulsars as sources of ePulsars as sources of e-/+-/+ pairs pairs
Crab Pulsar Wind Nebula (PWN)
e± pairs are produced in themagnetosphere and accelerated by theelectric fields and/or the pulsar wind.
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 45
The CRE spectrum accounting for nearby pulsars (d < 1 The CRE spectrum accounting for nearby pulsars (d < 1 kpckpc))
This particular model assumes: 40% e± conversion efficiency for each pulsar pulsar spectral index Γ = 1.7 Ecut = 1 TeV . Delay = 60 kyr
Rescaled conventional pre- FermiGCRE model by 0.95 @ 100 GeV γ0 = 2.54 ( δ = 0.33 )
Analytically computed spectrausing the same diffusion param. asfor the GCRE model
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 46
the positron ratio accounting for nearby pulsars (d < 1 the positron ratio accounting for nearby pulsars (d < 1 kpckpc))
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 47
What if we randomly vary the pulsar parametersrelevant for e+e- production?
(injection spectrum, e+e- production efficiency, PWN “trapping” time)
Under reasonable assumptions, electron/positron emission from pulsarsoffers a viable interpretation of Fermi CRE data which isalso consistent with the HESS and Pamela results.
[arXiv:0905.0636]
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 48
The Pulsing γ-ray Sky
Pulsesat1/10thtruerate
33 gamma-ray and radio pulsars (including nine ms psrs)33 gamma-ray and radio pulsars (including nine ms psrs)
16 gamma-ray only pulsars16 gamma-ray only pulsars
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 49
Predictions for the CRE spectrum from two specific dark mattermodels
( spectrum should be folded withthe Fermi energy resolution)
[arXiv:0905.0636]
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 50
Pure e+e- Modelsthe dark matterpair annihilationalways yields apair ofmonochromatice+e-, withinjection energiesequal to the massof theannihilating darkmatter particle
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 51
Lepto-philic Models
here we assume ademocratic darkmatter pair-annihilationbranching ratiointo each chargedlepton species:1/3 into e+e-, 1/3into µ+ µ- and 1/3into τ+ τ- Heretoo antiprotonsare not producedin dark matterpair annihilation.
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 52
Super-heavy Models (ann. in gauge bosons)
Super-heavy dark mattermodels: antiprotons canbe suppressed below thePAMELA measured fluxif the dark matterparticle is heavy (i.e. inthe multi-TeV massrange), and pairannihilates e.g. in weakinteraction gauge bosons.Models with super-heavydark matter can havethe right thermal relicabundance, e.g. in thecontext of the minimalsupersymmetricextension of theStandard Model
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 53
electron + positron expected anisotropy in thedirections of Monogem and Geminga
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 54
Where should we look for Dark Matterwith FERMI ?
• Galactic center• Galactic satellites• Galactic halo• Extra-galactic
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 55
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 56
EGRET data & Susy models
~2 degrees around the galactic center
EGRET data
Annihilation channel W+W-
Mχ =80.3 GeV
background model(Galprop)WIMP annihilation (DarkSusy)Total Contribution
A.Morselli, A. Lionetto, A. Cesarini, F. Fucito, P. Ullio, astro-ph/0211327
Nb=1.82 1021
Nχ=8. 51 104
Typical Nχ values:NFW: Nχ = 104
Moore: Nχ = 9 106
Isotermal: Nχ = 3 101
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 57
~2 degrees aroundthe galactic center,2 years data
(Galprop)(one example from DarkSusy)
Fermi Expectation & Susy models
astro-ph/0305075A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, 267-285, June 2004 [astro-ph/0305075]
Nb=1.82 1021
Nχ=8.51 104
Typical Nχ values:NFW: Nχ = 104
Moore: Nχ = 9 106
Isotermal: Nχ = 3 101
Annihilation channel W+W-
Mχ =80 GeV
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 58
Differentialyield for each
annihilationchannel
WIMP mass=200GeV
A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, 267, 2004 [astro-ph/0305075]
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 59
neutralino mass
Differential yieldfor b bar
A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, 267-285, 2004 [astro-ph/0305075]
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 60
Model independent results for the GC
5 years ofoperations,truncated NFW
after the FermiGalactic DiffuseEmission data
upated from arXiv:0806.2911
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 61
above EGRET observation
mWimp (GeV/c2)
< σ
v >
( 10
-26 c
m3 s
-1 )
channel bb at 3 σ, Moore profile
Not detectable by Fermi
detectable by GLAST( conventional and optimized GALPROP models assumptions)
detectable by Fermi
Model independent results for the Sagittarius Dwarft
after the FermiGalactic DiffuseEmission data
upated fromarXiv:0806.2911
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 62
Fermi and LHC WIMP Detection Sensitivity
Fermi sensitivity in five years for a Navarro Frank and White (NFW) halo profile arXiv:0811.3526
Fermi
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 63
Fermi, PAMELA and LHC WIMP Detection Sensitivity
Fermi sensitivity in five years for a Navarro Frank and White (NFW) halo profile
arX
iv:0
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RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 64
Optimized diffuse background and a 5σ line signal at 200 GeV
Optimized diffuse background
5σ signal at 200 GeV
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 65
con: conventional Galactic background model opt: Optimized Galactic background model
arXiv:0806.2911
5σ sensitivity contours to line signal (5 years)
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 66
•213th AAS Meeting — Long Beach, CA.
205 Preliminary Fermi LAT Bright Sources
Crosses mark source locations, in Galactic coordinates.
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 67
205 Preliminary LAT Bright Sources -
Some Information
• EGRET on the Compton Observatory found fewer than 30 sources above10 σ in its lifetime.
• Typical 95% error radius is less than 10 arcmin. For the brightestsources, it is less than 3 arcmin. Improvements are expected.
• About 1/3 of the sources show definite evidence of variability.
• More than 30 pulsars are identified by gamma-ray pulsations.
• Over half the sources are associated positionally with blazars. Some ofthese are firmly identified as blazars by correlated multiwavelengthvariability.
• Over 40 sources have no obvious associations with known gamma-rayemitting types of astrophysical objects.
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 68
A galactic dark matter halo
Gustavo Yepes
yesterday
work with
Beatriz Cañadas
in Roma
Detecting dark matter substructure with Fermi
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 69
Dwarf spheroidal galaxies (dSph) :promising targets for DM detection
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 70
Dwarf spheroidal galaxies (dSph) :promising targets for DM detection
• dSphs are the most DM dominated systems known in the• Universe with very high M/L ratios.• ➢Many of them (at least 6) closer than 100 kpc to the GC (e.g.• Draco, Umi, Sagittarius and new SDSS dwarfs).• ➢SDSS [only ¼ of the sky covered] already double the number of• dSphs these last years• ➢Most of them are expected to be free from any other• astrophysical gamma source.• ✔ Low content in gas and dust.
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 71
Dwarf Spheroidal Galaxies upper-limits
Fermi-LAT 3-months data preliminary results
)
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 72
Annihilation cross-section upper-limits in Dwarf Spheroidal Galaxies
Grey area: power-law upper-limitsLines: DMFit upper- limits
Fermi-LAT 3-months data preliminary results
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 73
New Data is Forthcoming• PAMELA & FERMI (GLAST) (taking data in space);• ATIC-4 (had successful balloon flight,under analysis);• CREST (new balloon payload under development);• AMS-02 (launch date TBD);• CALET (proposed for ISS);• ECAL (proposed balloon experiment).
Electron Spectrum:
Positron / Electron Separation: PAMELA & AMS-02
R.García
later
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 74
the positron ratiothe positron ratio
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 75
The CRE spectrum measured by Fermi-LAT is significantlyharder than previously thought on the basis of previous data
Conclusion:
Adopting the presence of an extra e± primary componentwith ~ 1.7 spectral index and Ecut ~ 1 TeV allow toconsistently interpret Fermi-LAT CRE data (improving thefit ), HESS and PAMELA
Such extra-component can be originated by pulsars for areasonable choice of relevant parameters
•Improved analysis and complementary observations•(CRE anisotropy, spectrum and angular distribution of diffuse γ,DM sources search in γ) are required to possibly discriminate theright scenario.
•or by annihilating dark matter for model with MDM ≈ 1 TeV
In September 2009 Fermi data will be open to the communityYou are all invited to join !
RENATA REd NAcional Temática de Astropartículas, Alcala, June 23 2009 Aldo Morselli, INFN Roma Tor Vergata 76
γ0 = 2.42 (δ = 0.33 - with reacceleration): red line γ0 = 2.33 (δ = 0.6 - plain diffusion): blue line
Fermi-LAT CRE spectrumFermi-LAT CRE spectrum
γ0 = 2.54 ( δ = 0.33 )
thank you for the attention !