Univ. Tübingen Present and future Dark Matter searches by HESS...

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A. Jacholkowska, Fermilab 10/05/07 MPI Kernphysik, Heidelberg Humboldt Univ. Berlin Ruhr-Univ. Bochum Univ. Hamburg LSW Heidelberg Univ. Tübingen Ecole Polytechnique, Palaiseau APC Paris Univ. Paris VI-VII Paris Observatory, Meudon LAPP Annecy LAOG Grenoble LPTA Montpellier CEA Saclay CESR Toulouse Durham Univ. Dublin Inst. for Adv. Studies Charles Univ., Prague Yerewan Physics Inst. North-West Univ., Potchefstroom Univ. of Namibia, Windhoek Present and future Dark Matter Present and future Dark Matter searches by HESS experiment searches by HESS experiment Hunt for Dark Matter Symposium Hunt for Dark Matter Symposium Fermilab Fermilab , May 10 , May 10 - - 12, 2007 12, 2007 Agnieszka Agnieszka Jacholkowska Jacholkowska on behalf of HESS on behalf of HESS LPTA Montpellier LPTA Montpellier

Transcript of Univ. Tübingen Present and future Dark Matter searches by HESS...

Page 1: Univ. Tübingen Present and future Dark Matter searches by HESS …conferences.fnal.gov/dmwksp/Talks/Jacholkowska_Fermilab... · 2015. 12. 2. · Present and future Dark Matter searches

A. Jacholkowska, Fermilab 10/05/07

MPI Kernphysik, HeidelbergHumboldt Univ. BerlinRuhr-Univ. BochumUniv. HamburgLSW HeidelbergUniv. TübingenEcole Polytechnique, PalaiseauAPC ParisUniv. Paris VI-VIIParis Observatory, MeudonLAPP AnnecyLAOG GrenobleLPTA MontpellierCEA SaclayCESR ToulouseDurham Univ.Dublin Inst. for Adv. StudiesCharles Univ., PragueYerewan Physics Inst.North-West Univ., PotchefstroomUniv. of Namibia, Windhoek

Present and future Dark MatterPresent and future Dark Mattersearches by HESS experimentsearches by HESS experiment

Hunt for Dark Matter SymposiumHunt for Dark Matter SymposiumFermilabFermilab, May 10, May 10--12, 200712, 2007

AgnieszkaAgnieszka JacholkowskaJacholkowska on behalf of HESSon behalf of HESSLPTA MontpellierLPTA Montpellier

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A. Jacholkowska, Fermilab 10/05/07

OUTLINE

HESS experiment and source observations

Results from the Galactic Centre

Analysis of Sagittarius Dwarf data and preliminary results

Prospects for HESS2

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A. Jacholkowska, Fermilab 10/05/07

Four telescopes, 107 m2 mirror area each

960 PMT cameras, field of view 5o

Observation in moonless nights, ~1000 h / year

Each night several objects are tracked and ~300 images recorded per second

First analysis (almost) online in the same night on PC cluster in Namibia

Final analysis and calibration in Europe

Energy threshold:~ 100 GeV

Sensitivity:1% Crab in 25 h

HESS experiment

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A. Jacholkowska, Fermilab 10/05/07

HESS: principle of detection

Stereoscopy (2-4) telescopes:reconstruction of direction andenergy of the particle

Angular resolution: ~ 0.1o

Energy resolution: ~ 15%

Analysis of the images:allows disciminationbetween γ / hadron/ muon

HESS II (2008): add 596m2 mirror in the centre→ Ethr ~ 20 GeV

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A. Jacholkowska, Fermilab 10/05/07

γ flux from DM annihilation

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A. Jacholkowska, Fermilab 10/05/07

Sources & astrophysical uncertainties

Halo density profiles parameterizationsIsothermal, Navarro-Frenk-White, Moore, …

Uncertainties on flux predictionsabove 102 !

DM sources observed by HESS:Galactic CentreGlobular Clusters – M15, Ω-centauris,…Milky Way satellites – dwarf spheroidals, LMC, SMC other galaxies - M31, M87

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A. Jacholkowska, Fermilab 10/05/07

Galactic Centre region

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A. Jacholkowska, Fermilab 10/05/07

HESS: Galactic Centre

Galactic Centre is a verycrowded region in all wave-lengths

Point-like sky map

Diffuse part

White contours:molecular cloud emission(CS rays)

Sgr A*

SNR G 0.9+0.1

~3500 diffuse γSig= 14.6σ

EGRET non-identifiédsources

Sgr B

HESS, NATURE, vol.439, p.695, 2006

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A. Jacholkowska, Fermilab 10/05/07

HESSJ1745-290: morphology

Diffuse component: 16%Source size: 0.12°

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A. Jacholkowska, Fermilab 10/05/07

HESSJ1745-290: spectrum

fit " only dark matter "

fit " dark matter+ bckg power law "

Data 2003/2004:

− Power Law Spectrum (Eth > 160 GeV)Γ=2.25±0.04±0.10

− Exponential cut-off limit Ecut > 9 TeV (95% CL)

− Diffuse emission included

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A. Jacholkowska, Fermilab 10/05/07

HESS: Galactic Centre• Strong point-like source (0.1°) detected - HESSJ1745-290at the position of Sgr A* with spectral index Γ ~ 2.2

• Important Diffuse emission associated with molecularclouds spread over whole region with similar spectral index

• No line emission observed

• Need of uncomfortably high masses of neutralino or Kaluza-Klein particles

• Contribution of Dark Matter below 10% cannot be excluded→ constraints on <σv> ~ 10-24 cm3/s with NFW profile

HESS will re-observe Galactic Centre with low energythreshold in phase II

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A. Jacholkowska, Fermilab 10/05/07

Sagittarius Dwarf and Canis Major

Canis Major dw

30 kpc

Sgr dw

LMC

SMCCarina dw

Sculptor dw

Fornax dw

Draco dw

Sextans dw

Ursa Minor dw

Important factors:

Mdark ~ 107 MoM/L ~100Distance: 25 & 8 kpc

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A. Jacholkowska, Fermilab 10/05/07

03.0~75.05.0~2.01.0~GC

Draco

GC

CMaj

GC

Sgr

φφ

φφ

φφ

−−

Evans,Ferrer,Sarkar PRD 69 123501 (2004)

For a given particle model, dφ/dE depends only on <J>

3.7~12~11~GC

Draco

GC

CMaj

GC

Sgr

φφ

φφ

φφ

NFW halo:

Halo with core:

Dwarf Spheroidals: γ flux predictions

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A. Jacholkowska, Fermilab 10/05/07

Sagittarius Dwarf and M54

M54

Majewski et al. (2003) Monaco et al., astro-ph/0411107

“nucleated dwarf galaxy”

Sagittarius radial profile

Almost all mass < 1.5 pc→ search for a point-like source

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A. Jacholkowska, Fermilab 10/05/07

No significant γ-ray excess → limit on flux:

Sagittarius Dwarf: observation results

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A. Jacholkowska, Fermilab 10/05/07

Modeling Sgr Dwarf halo profile

2 popular halo profiles:

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A. Jacholkowska, Fermilab 10/05/07

Sgr Dwarf: constraints on Neutralino DM

pMSSM models with low Ωrelic

excluded in case of the cored profile

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A. Jacholkowska, Fermilab 10/05/07

Sgr Dwarf: constraints on Kaluza–Klein DM

Some KK models with Ωrelic compatiblewith WMAP are excluded in case of the cored profile

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A. Jacholkowska, Fermilab 10/05/07

Complementarity: LHC / Indirect searches

Assumption: dark matter is composed predominantly by SUSY or ExtraDim stable particles (and H2)

• LHC (>2007) will provide:- indications for masses and BRs of new particles- will favor some classes of models

• Exotic interpretation of the annihilation signal: is degenerate with respect to various models of SUSY or Kaluza-Klein type

• Potential of LHC experiments is limited in some domains of the parameter space (large tanβ, Focus Point, ..) where annihilation flux prediction are most optimistic!

→ common interest for model dependent/independent studies

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A. Jacholkowska, Fermilab 10/05/07

HESS phase II and LHC

LPTA: A. Jacholkowska, JL. Kneur E. Moulin G. Moultaka, E. NussATLAS: S. Asai, T. Lari, G. Polesello, D. Tovey, M. White, Z. Yang

Studies in the Focus Point regions (ATLAS-HESS collaborators)scan with IsaSugra (DarkSusy) simulation —> Φγ, Ωrelic, Nevt (ATLAS)

HESS II (Eth > 20 GeV): 5σ sensitivityfor 50 hrs

100 fb-1: 3-body leptonicdecays

Page 21: Univ. Tübingen Present and future Dark Matter searches by HESS …conferences.fnal.gov/dmwksp/Talks/Jacholkowska_Fermilab... · 2015. 12. 2. · Present and future Dark Matter searches

A. Jacholkowska, Fermilab 10/05/07

No exotic signal from HESS observations of the Galactic Centre which is not a « smoking gun » for dark matterdetection as populated by various types of the standardastrophysical sources

Sagittarius et Canis Major galaxies are potential targets of interestdue to the high M/L ratio and quiet astrophysical environment

First results from 11 hrs of observations Sagittarius Dwarf galaxy show no signal and allow to reject few SUSY & KK models with low Ωrelic and for a cored DM density profile

From 2008 HESS II will start taking data with ~20 GeV thresholdallowing to probe low mass neutralino range with improvedsensitivity and first indications from LHC!

Summary