Introduction to the demo Dark Matter Tool on the Web - - PowerPoint PPT Presentation

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Introduction to the demo Dark Matter Tool on the Web - - PowerPoint PPT Presentation

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TOOLS 2008 New physics and its background June 30 - July 4, 2008 MPI Munich, Germany Introduction to the demo Dark Matter Tool on the Web http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/ R. Lemrani, ILIAS-N3 Dark Matter Network /

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SLIDE 1

Introduction to the demo “Dark Matter Tool on the Web”

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

TOOLS 2008 New physics and its background June 30 - July 4, 2008 MPI Munich, Germany

  • R. Lemrani, ILIAS-N3 Dark Matter Network / CEA Saclay
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SLIDE 2

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

A word on ILIAS

Integrated Large Infrastructures for Astroparticle Science

European tool : I3 structure (Integrated Infrastructure Initiative) of FP6 Participants: 21 Contractors (70 laboratories), 14 European Countries Start date ; April 1st 2004 for 5 years Web site : ilias.in2p3.fr

Prime areas : Double Beta Decay, Dark Matter, Gravitational Waves Infrastructures : - Deep Underground Laboratories

  • Gravitational Wave Interferometers

“ … to produce a focused, coherent and integrated project to improve the existing infrastructures and their operation as well as to organise and structure the scientific community to prepare the best infrastructures for the future.”

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SLIDE 3

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

A word on ILIAS-N3 Dark Matter Network

Web site : http://ilias-darkmatter.uni-tuebingen.de/ Working groups

→ Input for ASPERA Roadmap

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SLIDE 4

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Web tool : Purpose

  • Build a web interface for dark matter calculations :

Expected spectra, limits extraction, …

  • Handling different detection techniques
  • Handling different theoretical assumptions
  • Cross check methods and codes
  • Available to the whole dark matter community
  • Allowing comparisons of experimental strategies

using the same theoretical inputs and varying them

Nothing to install. The calculations are done online with a web browser.

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SLIDE 5

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Homepage

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SLIDE 6

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

List of available pages

I will focuse on these 2 webpages

  • expected experimental signal for given WIMP
  • Deriving limits on WIMP-nucleon cross section

from experiments

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SLIDE 7

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Galactic Halo

ρ

=

= density

f(v) =

= velocity distribution

Nucleus

F = Nuclear form factor µ µ = WIMP-nucleus reduced mass

Detection q(E) = quenching ε(E) = efficiency r(E) = resolution

Direct Search for WIMPs

WIMP nature : ie Neutralino

σ = = WIMP-nucleus cross section (point-like) mχ

=

= WIMP mass

( (µ µ = = WIMP-nucleus reduced mass) dN dE = σ ρ 2µ 2µ2mχ F2 f(v) v dv

∫

Vesc Vmin(Er) X ε(E)/ q(E)⊗ r(E)

  • J. D. Lewin and P. F. Smith, Astropart. Phys. 6, (1996)87

Detection rate :

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SLIDE 8

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Experimental Spectra

Label of the produced figure WIMP mass (GeV) A of Target : defines nucleus form factor, WIMP-nucleon reduced mass Exposure (kg.days) : mass of detector x acquisition time WIMP-nucleon cross-section (pb) Add, Combine, reset

1 2 3 4 5 1 2 3 4 5

Default values are “standard” for galactic halo, nuclear form factors and recoil spectra are without experimental parameters

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SLIDE 9

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

  • Ex. : Dependence on WIMP Mass

Using ddmc tool (by J. Gascon, V. Sanglard and R.L.)

All parameters are entered in a form : The outputs are figures and tables

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SLIDE 10

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

How it works

When leaving the webpage or starting new figures the session is destroyed → before leaving copy the created figures and tables Input parameters PHP form

with a bit of Javascript for ergonomy

Shell script Root Physics program Session variables Temporary directory Results : figures, tables contains creates creates calls calls

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SLIDE 11

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Galactic Halo

ρ 0

0 = WIMP density (GeV/cm3)

V0

defines velocity distribution f(v) maxwellian

Galactic escape velocity Vesc= upper bound on integral dv f(v) v

∫

Vesc Vmin(Er)

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SLIDE 12

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Nuclear Form Factors

Two form factors function of A of target

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SLIDE 13

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Experimental Parameters

Experimental parameters default values : Quenching = 1 Resolution = 0 Efficiency = 1

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SLIDE 14

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Efficiency

Explained in next slide

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SLIDE 15

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Entering binned values

Nbins Bins edges Efficiencies

(Nbins+1 numbers) (Nbins numbers)

Example : 1 0 200 1 200 E eff 1 Example : 2 0 100 200 0.5 1 100 E eff 1 0.5 200

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SLIDE 16

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Quenching

Type : a) Lindhard parametrisation aEr

b

b) binned Type a) parameters a and b Type b) binned

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SLIDE 17

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Resolution

Type : a) parametrisation a+b√Er b) binned Type a) parameters a and b Type b) binned

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SLIDE 18

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Effect of resolution/quenching

Effect of resolution

Low resolution => flattens the spectra but worsens efficiency (discrimination)

quenching=0.36->0.3 An error on quenching estimation changes the recoil energy threshold

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SLIDE 19

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

LIMITS on WIMP-nucleon cross-section

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SLIDE 20

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

LIMITS on WIMP-nucleon cross-section

1 2 4 3 5

Method : 1. Poisson enter also number of Observed events

  • 2. Feldman-Cousins/Cousins-Highland

enter also number of Observed events and Expected background events and uncertainty on background (Feldman-Cousins for poisson process with a perfectly known background

Cousins-Highland if uncertainty on background)

  • 3. Enter directly predetermined limit on rate
  • 4. Yellin method : enter number of observed events

and their energy (uses optimal interval method)

2 2 4 3 2 2 5

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SLIDE 21

http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/

  • R. Lemrani, ILIAS N3 / CEA Saclay

TOOLS for the new physics and its background , June 30- July 4 2008, MPI, Munich, Germany

Demo

The webpage address is : http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/ Some examples can be found in : http://pisrv0.pit.physik.uni-tuebingen.de/darkmatter/examples.html All contributions, suggestions, cross-checks, feedback to enrich, improve the tool are very welcome