gamma- rays from space anddipastro.astro.unipd.it/pizzella/glast/morselli_padova06.pdf · lars...

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 1

Aldo MorselliINFN, Sezione di Roma 2 &

Università di Roma Tor Vergata

Workshop on

Dark Matter

Università di

Padova

6 aprile 2006

Gamma-Raysfrom space andDark Matter


EGRET Map E> 100 MeV


Energy versus time for X and Gamma ray detectors


High galactic latitudes(!b=2 10-5 " cm-2 s-1 sr -1 (100 MeV/E)1.1). Cerenkov telescopes sensitivities

(Veritas, MAGIC, Whipple, Hess, Celeste, Stacee, Hegra) are for 50 hours of observations.Large field of

view detectors sensitivities (AGILE, GLAST, Milagro, ARGO, AMS) are for 1 year of observation.

Sensitivity of "-ray detectors


(1) Organize and schedule regular meetings of the group

(2) Review the list of anticipated papers and, with special attention to papers likelyto be generated from data obtained during the first year of operation. Also,identify any papers that the group can generate before launch.

GLAST SCIENCE GROUP: Dark Matter and exotic physics tasks:

GLAST LAT Science Groups

Catalogs

Diffuse (Galactic & Extragalactic) and Molecular Clouds

Blazars and Other AGNs

Pulsars, SNRs, and Plerions

Unidentified Sources, Population Studies, and Other Galaxies

Dark Matter and Exotic Physics

Gamma-Ray Bursts

Sources in the Solar System

Calibration and Analysis Methods

Multiwavelength Coordinating Group


Dark Matter and New PhysicsResponsibilities: Search for signatures of dark matter, extradimensions

(e.g. KK graviton decay), quantum gravity dispersion effects, etc.

Coordinators: Elliott Bloom Aldo Morselli

Members: 47 (Feb.06) (39 Aug. 05 )

Sergio Colafrancesco

Jan Conrad

Alessandro deAngelis

Joakim EdsjoPiergiorgio Fusco

Fabio Gargano

Stefano Germani

Nico Giglietto

Gary Godfrey

Sylvain Guiriec

Richard E. Hughes

Michael Kuss

Luca Latronico

Andrea Lionetto

Mario Nicola Mazziotta

Lester Miller

Alex Moiseev

Aldo Morselli

Igor Moskalenko

Eric Nuss

Takashi Ohsugi

Monica Pepe

Piergiorgio Picozza

Frederic Piron

Carlotta Pittori

Silvia RainòSteve Ritz

Eduardo do Couto e Silva

Tadayuki Takahashi

Lawrence L. Wai

Ping Wang

Brian Winer

Marcus Ziegler

Ted Baltz

Ronaldo Bellazzini

Bijan Berenji

Lars Bergstrom

Giovanni F. Bignami

Pasquale Blasi

Elliott Bloom

Anders W. Borgland

Toby Burnett

Giovanni Busetto

Per Carlson

Claudia Cecchi

James Chiang

Johann Cohen-Tanugi


DM&NP Meeting @ SLACPlace - ROB Redwood room, SLACTime - 28 February 2006, 5 -9:30 PM,

1. DM & NP Overview and Goals - Elliott Bloom,15 Min

2. Review of work - Aldo Morselli, 15 Min

3. The search for Milky Way halo substructure WIMP annihilations using the GLASTLAT - Larry Wai, 15 min

4. The search for Milky Way halo substructure WIMP annihilations using the GLASTLAT (continued) - Ping Wang, 15 min

5. Benchmak points for DM study in view of DC2 preparation - Eric Nuss, 15 min

6. A quick look at recent papers, especially about dwarf spheroids - Johann CohenTanui

7. Detecting with GLAST gamma rays coming from LKP annihilations in the context ofthe minimal UED models - Andrea Lionetto, 15 min 7:00 PM.

8. Uncertainties in the interpretation of the diffuse galactic gamma-ray emission -Igor Moskalenko, 15 min

slide in: http://people.roma2.infn.it/glast


Neutralino WIMPs

Assume # present in the galactic halo• # 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 --> p + X)• So, any extra contribution from exotic sources (# # annihilation) is aninteresting signature• ie: # # --> p + X• Produced from (e. g.) # # --> q / g / gauge boson / Higgs boson andsubsequent decay and/ or hadronisation.


Signal rate from Supersymmetry

governed by supersymmetric parameters

governed by halo distribution

gamma-ray flux from neutralino annihilation

J($):


• Galactic satellites

･ Galactic halo

･ Extra-galactic

･ Galactic center

Where should we look for WIMPs with GLAST?


The search for milky way halo substructure WIMPannihilations using the GLAST LAT

Dark matter calculationwith semi-analytic

method of Taylor &

Babul 2004, 2005

Background estimateusing EGRET above

1GeV (source

subtracted)

M=100GeV

<! v> = 2.3x10-26cm3s-1

Larry Wai and Ping Wang

on behalf of GLAST DM & Exotic Physics WG


Satellite mass distributions


Satellite distances


EGRET,E > 1GeV

Mayer-Hasselwander

et al, 1998

Integral data 20 x 20 field IBIS/ISGRI 20–40 keV


Poin source locationfor GLAST~ 5 arcmin

1 pixel ~ 5 arcmin

20 x 20 field IBIS/ISGRI 20–40 keV

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 1720 x 20 field IBIS/ISGRI 20–40 keV1 pixel ~ 5 arcmin

Poin source locationfor GLAST~ 5 arcmin

20 x 20 field EGRET, E > 1GeV


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, Nuc. Phys. 113B (2002) 213 [astro-ph/0211327]

Nb=1.82 1021

N#=8. 51 104

Typical N# values:NFW: N# = 104

Moore: N# = 9 106

Isotermal: N# = 3 101


~2 degrees aroundthe galactic center,2 years data

(Galprop)

(one example from DarkSusy)

GLAST Expectation & Susy models

A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astrop. Phys., 21, 267, 2004 [astro-ph/0305075]

Nb=1.82 1021

N#=8.51 104

Typical N# values:NFW: N# = 104

Moore: N# = 9 106


Annihilation channel W+W-

M# =80 GeV


Galactic Center

HESS SpectrumUnbroken power-law.

!Hard spectrum % = 2.2.

!No evidence for variability ona variety of time scales.

Consistent withSGR A* to 6’’ and slightly extended.

SGR A

Good agreement

between HESS and

MAGIC (large zenith

angle observation).

astro-ph/0512469


EGRET, GLAST, HESS

it might still bethat a DMcomponent could besingled out, e.g. theEGRET source (?):a DM source can fitthe EGRET data;GLAST woulddetect its spectraland angularsignatures andidentify withoutambiguity such DMsource!


EGRET, GLAST, HESS

HESS, extrapolation with & = 2.2

EGRET data

" from '0


region where

0.13 < (CDM.h2 < 1

GLAST sensitivity (5 )) for aneutralino density N# of 104 ina *(=10-5 sr region around thegalactic center in 5 years

Minimal Supersymmetric Standard Model with:A0 = 0, µ > 0, mt =174 GeV

Typical N# values for *(=10-5 sr :NFW: N# = 104

Moore: N# = 9 106


A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics 21, 267-285, 2004 [astro-ph/0305075]

Estimated reaches with GLAST

region where

0.09 < (CDM.h2 < 0.13

if GLAST do not see Supersymmetrythis region is excluded for a NFW halo mh0 <114.3 GeV GeV


region where

0.13 < (CDM.h2 < 1

GLAST sensitivity (5 )) for aneutralino density N# of 104

in a *(=10-5 sr region aroundthe galactic center in 5 years

Minimal SupersymmetricStandard Model with:A0 = 0, µ > 0, mt =174 GeV

Typical N# values for *(=10-5 sr :NFW: N# = 104

Moore: N# = 9 106


Estimated reaches with GLAST

region where

0.09 < (CDM.h2 < 0.13

if GLAST do not see Supersymmetrythis region is excluded for a NFW halo mh0 <114.3 GeV GeV

A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics 21, 267-285, 2004 [astro-ph/0305075]


LHC and Linear Collider

region where

0.13 < (CDM.h2 < 1


region where

0.09 < (CDM.h2 < 0.13

accelerator limits from hep-ph/0405210

LHC 100 fb-1

LC1000 100 fb-1

LC500 100 fb-1


mh0 <114.3 GeV

LHC

LC1000

LC500

region where

0.13 < (CDM.h2 < 1

GLAST sensitivity (5 )) for atruncated NFW in a *(=10-5 srregion around the galactic centerin 5 years. If GLAST does notsee Supersymmetry this regionis excluded for a NFW halo


region where

0.09 < (CDM.h2 < 0.13


LHC 100 fb-1

LC1000 100 fb-1

LC500 100 fb-1


mh0 <114.3 GeV

LHC

LC1000

LC500

m#=400 GeV

m#=100 GeV

m#=200 GeV

m#=200 GeV

region where

0.13 < (CDM.h2 < 1



region where

0.09 < (CDM.h2 < 0.13


LHC 100 fb-1

LC1000 100 fb-1

LC500 100 fb-1


region where

0.13 < (CDM.h2 < 1


region where

0.09 < (CDM.h2 < 0.13

LHC 100 fb-1

LC1000 100 fb-1

LC500 100 fb-1



LHC

LC1000

LC500

107

106

107

106


Kaluza-Klein Dark Matter in (minimal) UED

SM in D = 5 with 1 compactified extra-dimension

(over S1/!2 with S1 radius R)

Every SM field (bulk field) possess a KK tower

1-loop level computation shows that the LKP is well

approximated by the first KK mode of the hypercharge

gauge boson B(1)a

A.Lionetto, J.Cohen-Tanugi, E.Nuss

on behalf of GLAST DM & Exotic Physics WG

aReference papers: Servant, Tait Nucl.Phys.B650:391- 419,2003,

Bergstrom et al. Phys.Rev.Lett.94:131301,2005


> Whole sky 'realistic' simulation (Data Challenge2 Instrument Response Function)

> One Year observations, 30 deg radius FOV Galactic Center centered

GLAST simulations

Dark Matter NFW profile,

mB(1)

~ 500 GeV

Diffuse background based on

GALPROP code

(Point source substracted)


Comparison between

different

spectral shapes

primary and

secondary

contribution

mSUGRA

and E-2 spectra

vs

LKP

･Detecting with GLAST gamma rays coming from LKP annihilations inthe context of the minimal UED models


Preliminary computation indicates that, in the energy rangeE" > 5 GeV, GLAST could detect "-rays from GC via LKPannihilations with moderate boost factors

Connection with ground based Cherenkov arrays (continuum and gamma ray lines) is needed to disantangle KK signal fromstandard astrophysical signal (~ E-2 spectra)


region where 0.13 < (CDM.h2 < 0.3

MSSMEstimated reaches with GLAST and Pamela

region where 0.09 < (CDM.h2 < 0.13

Clumpiness factors fd needed todisentangle a neutralino inducedcomponent in the antiproton fluxwith PAMELA (#2>1.8) that stillgive a good fit of the presentdata.

Equi-clumpiness factor density inrespect to a NFW

Equi-neutralino mass lines

GLAST sensitivity (5 )) for aneutralino density N# of 104

NFW in a *(=10-5 sr regionaround the galactic center

same but for N# of 105

(clumpines factor 10 )

astro-ph/0502406 and astro-ph/0305075


Pamelain Samara,Russia 4/09/05


PAMELA scientific program

energy range particles/3 years

Antiproton flux 80 MeV - 190 GeV >3 104

Positron flux 50 MeV – 270 GeV >3 105

Electron flux up to 400 GeV 6 106

Proton flux up to 700 GeV 3 108

Electron/positron flux up to 2 TeVLight Nuclei (up to Z=6) up to 200 GeV/n He/Be/C: 4 107/4/5

AntiNuclei search (sensitivity of 3 10-8 in He/He)

" Unprecedented Statistics and new Energy Range in Cosmic Rays

Actual limits: antip&positrons + 40 GeV

PAMELA is a magnetic spectrometer which will fly on a Russian satellite by Fall 2005.Its scientific scope is the measurement of the antiproton and positron spectra up to fewhundred GeV, of the proton and electron spectra up to 700 GeV and that of light nuclei.


PAMELA @ Baikonur 28/03/06


The Satellite: Resurs DK1- Soyuz-TM Launcher

from Baikonur

- Launch in 2005

- Lifetime >3 years

- PAMELA mounted insidea Pressurized Container,attached to Satellite

- Earth-Observation-Satellite


GLAST

GLASTScheme

Gamma-Ray

Large Area Space

Telescope


The GLAST Participating InstitutionsItalian Team Institutions INFN - Instituto Nazionale di Fisica Nucleare and Universities of Bari, Perugia, Pisa, Roma2, Trieste, Udine ASI - Italian Space Agency IASF- Milano, RomaAmerican Team Institutions

SU-HEPL Stanford University, Hanson Experimental Physics Laboratory , , SU-SLAC Stanford Linear Accelerator Center, Particle Astrophysics group GSFC-NASA-LHEA Goddard Space Flight Center, Laboratory for High Energy Astrophysics NRL - U. S. Naval Research Laboratory, E. O. Hulburt Center for Space Research, X-ray and gamma-ray branches UCSC- SCIPP University of California at Santa Cruz, Santa Cruz Institute of Particle Physics SSU- California State University at Sonoma, Department of Physics & Astronomy , WUStL-Washington University, St. Louis UW- University of Washington , TAMUK- Texas A&M University-Kingsville, Ohio State UniversityJapanese Team Institutions University of Tokyo ICRR - Institute for Cosmic-Ray Research ISAS- Institute for Space and Astronautical Science Hiroshima UniversityFrench Team Institutions CEA/DAPNIA Commissariat à l'Energie Atomique, Département d'Astrophysique,

de physique des Particules, de physique Nucliaire et de l'Instrumentation Associée, CEA, Saclay IN2P3 Institut National de Physique Nucléaire et de Physique des Particules, IN2P3 IN2P3/LPNHE-X Laboratoire de Physique Nucléaire des Hautes Energies de l'École Polytechnique IN2P3/PCC Laboratoire de Physique Corpusculaire et Cosmologie, Collège de France IN2P3/CENBG Centre d'études nucléaires de Bordeaux GradignanSwedish Team Institutions KTHRoyal Institute of Technology Stockholms Universitet

total US

Collaboration members: 161 75

Members: 77 43

Affiliated Sci. 67 28

Postdocs: 17 4


Summary of GLAST physic itemsCosmic Diffuse Background

Origin is still a mystery for gamma rays

Is there a truly diffuse cosmological component?

Supermassive BHs and AGNRemarkable objects that shine most brightly in gamma rays

Gamma rays probe central engine

Gamma rays probe jets

GRBsHigh-energy prompt and delayed emission not understoodEGRET provided only a glimpseQuantum gravity effects possible

Unidentified SourcesMystery has been with us for > 20 years

Third EGRET Catalog includes 170 unidentified sources

A new class of Galactic sources?

SNRs Site of CR acceleration E < 1015 eV (still unproven for nuclei!) Should see extended sources in gammas (from 'o

decay) to answer the question definitively

Pulsars Gemingas only shine in gamma regime

Uncover acceleration mechanisms

Understand beaming

Cosmology - AGNs Spectral roll-offs due to EBL are in GLAST range

GLAST can see to z > 4

Cosmology - Dark Matter PBHs, cosmic strings, WIMP annihilation all

predicted to shine in gamma rays


Current Collaboration Science Groups

1a. Catalog

Seth Digel (SU-SLAC); Isabelle Grenier (CEA/ Saclay)

1b. Diffuse (Galactic and Extragalactic) and Molecular Clouds

Seth Digel (SU-SLAC); Isabelle Grenier (CEA/ Saclay)

2. Blazars and Other AGNs –Paolo Giommi (ASI), Benoit Lott (Bordeaux)

3. Pulsars, SNRs, and Plerions - Roger Romani (Stanford); David Thompson (GSFC)

4. Unidentified Sources, Population Studies, and Other Galaxies Patrizia Caraveo (IASF ); Olaf Reimer (Stanford)

5. Dark Matter and New Physics - Elliott Bloom (SU-SLAC); Aldo Morselli (INFN–Rome)

6. Gamma-Ray Bursts - Jay Norris (GSFC); Nicola Omodei (INFN-Pisa)

7. Solar System Sources - Gerry Share (NRL)

8. Calibration and Analysis Methods - William Atwood (UCSC); Steve Ritz (GSFC)

9. Multiwavelength Coordination Group – Roger Blandford (SU – KIPAC); David Thompson (GSFC)

GLAST @ SLAC

12/16 Towers in the GRID on 7/10/05

16/16 Towers in the GRID on 20/10/05

GLAST @ SLAC

The LAT Tracker numbers

11500 sensors11500 sensors

360 trays360 trays

18 towers18 towers

~ 1M channels~ 1M channels

83 m83 m22 SiSi surface surface

> 240K functional test> 240K functional test

recorded in DBrecorded in DB

~ 30M strip tested~ 30M strip tested

(30 test/strip on average)(30 test/strip on average)

> 60 physicist and engineers involved> 60 physicist and engineers involved

in the in the italianitalian teams from INFN teams from INFN

(Trieste, (Trieste, UdineUdine, , PadovaPadova, Pisa, , Pisa, PerugiaPerugia,,

Roma2, Roma2, BariBari) in partnership with ASI) in partnership with ASI


Celebrations for the end of Tracker construction

52 attendees from INFN, ASI, SLAC, NASA,

italian industrial partners


GLAST mission status

November 2005 ACD on the LAT

> All elements of the GLAST mission have completed the fabrication phase and are well into integration.

> LAT, GBM, and spacecraft assembly complete by mid 2006.

> Delivery of the instruments for observatory integration spring/summer 2006.

> Observatory integration and test summer 2006 through summer CY07.

Short term activities for the collaboration :

> Data Challenge 2 : March->May 2006

> Beam tests at CERN in summer/autumn 2006


• August 2004Assembling of first tower completed

• Middle of October 2005Completion of the LAT – Environmental testing

• February 2006Delivery to NRL–

• August 2007Kennedy Space Flight Center

LAUNCH

GLAST Master Schedule

•November 2007

Science operation begins!

more info : http://people.roma2.infn.it/glast/


Through most of history, the cosmos has beenviewed as eternally tranquil


`

During the 20th century the quest to broaden our view of the

universe has shown us the vastness of the Universe and

revealed violent cosmic phenomena and mysteries


` ExploringNature’s

Highest EnergyProcesses

• AGILEJan. 2006

Launch

• GLAST:August 2007

launch

• AMS:2008 launch

• GILDA

gamma- rays from space anddipastro.astro.unipd.it/pizzella/glast/morselli_padova06.pdf · lars...

Documents