Aldo Morselli INFN Roma Tor Vergata 2 Feb 2013
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1 The Quest for Dark Matter Signals and the gamma-ray sky: the low energy window Aldo Morselli INFN Roma Tor Vergata 2 Feb 2013 Aspen 2013 Closing on Dark Matter 1!
2 many talks during this conferences: Dan Hooper: In my opinion, no single indirect detection experiment has more potential to constrain or discover dark matter than the Fermi Gamma Ray Space Telescope (FGST) Tim Linden: the importance of the galactic center But we need more data to discriminate between pulsar and Dark Matter Alex Drlica-Wagner Angular resolution of Fermi Lat Compared with optical telescopes 2!
3 Fermi Gamma-Ray Large Area Space Telescope Tracker 1.68 m! 84 cm! Grid Silicon Tracker tower! 18 planes of X Y silicon detectors + converters! 12 planes with 3% R.L. of W, 4 planes with 18% R.L! 2 planes without converters! DAQ Electronics ACD Anticoincidence Shield! Calorimeter Thermal Blanket ( 8.5 Rad.Length) 3!
4 How Fermi LAT detects gamma rays 4 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 " Incoming Conversion ( in e + /e - ) in W foils Incoming direction reconstruction by tracking the charged particles e + e - An anticoincidence detector around the telescope distinguishes gammarays from charged particles Energy measurement with e.m. calorimeter 4!
5 5!
6 6!
7 Elements of a pair-conversion telescope photons materialize into matter-antimatter pairs: E --> m e +c 2 + m e -c 2 electron and positron carry information about the direction, energy and polarization of the -ray (energy measurement) 7!
8 Elements of a pair-conversion telescope (more realistic scheme) photons materialize into matter-antimatter pairs: E --> m e +c 2 + m e -c 2 electron and positron carry information about the direction, energy and polarization of the -ray (energy measurement) 8!
9 6 projected angular distribution ( degrees) E(GeV) 0.15Xo(deg) 0.07Xo(deg) 0.05Xo(deg) projected angular distribution ( degrees) Multiple Scattering 0.15Xo(deg) 0.07Xo(deg) 0.05Xo(deg) E(GeV) E(GeV)! 9!
10 Multiple Scattering 50 10!
11 Fermi Instrument Response Function 11!
12 Fermi Instrument Response Function 12!
13 N s = number of photons from source N B = number of photons from background = solid angle around dth source A eff = Effective area ( Area* efficiency ) x = converter plane in radiation lengh Sensitivity depends on field of view Sensitivity number of depends on angular resolution 13!
14 good detector small converter plane large effective area (large geometric area and large total conversion efficiency ) large field of view 14!
15 1/E Sensitivity of -ray detectors! from here geometric angolar resolution GLAST thin section! GLAST (1 yr )! GLAST (5 yr )! MAGIC 2 (exp)! MAGIC (now)! ARGO! HAWC!!! A.Morselli.11-10! CTA! HESS! limited by statistics 15!
16 The Fermi LAT 2FGL Source Catalog August 4, 2008, to July 31, MeV to 100 GeV energy range 1873 sources 1095 AGN s 589 unidentified Fermi Coll. arxiv: !
17 The Fermi LAT 2FGL Inner Galactic Region August 4, 2008, to July 31, MeV to 100 GeV energy range Fermi Coll. ApJS (2012) 199, 31 arxiv: !
18 Spectrum (E> 400 MeV, 7 x7 region centered on the Galactic Center analyzed with binned likelihood analysis ) data (stat. error) preliminary best diffuse model and isotropic emission! 12 Fermi 1 year catalog sources V.Vitale, A.M. for the Fermi Coll. NIM A630 (2011) !
19 GC Residuals 7 x7 region centered on the Galactic Center 11 months of data, E >400 MeV, front-converting events analyzed with binned likelihood analysis )"! The systematic uncertainty of the effective area (blue area) of the LAT is ~10% at 100 MeV, decreasing to 5% at 560 MeV and increasing to 20% at 10 GeV! V.Vitale, A.M. for the Fermi Coll. NIM A630 (2011) !
20 DM in the galactic center? arxiv: ! 20!
21 Milky Way Dark Matter Profiles All profiles are normalized to the local density 0.3 GeV cm 3 at the Sun s location r 8.5 kpc A.Lapi et al. arxiv: ! 21!
22 Different spatial behaviour for decaying or annihilating dark matter The angular profile of the gamma-ray signal is shown, as function of the angle to the centre of the galaxy for a Navarro-Frenk-White (NFW) halo distribution for decaying DM, solid (red) line, compared to the case of self-annihilating DM, dashed (blue) line 22!
23 Differential yield for each annihilation channel WIMP mass=200gev! A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, 267, 2004 [astro-ph/ ]! 23!
24 Differential yield for b bar neutralino mass A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, , 2004 [astro-ph/ ]! 24!
25 Gamma-light scheme 40+1 x-y planes 100 µm pitch each ~0.025 X 0 AC Tot~ 1 X cm height of a plane 1.3 cm 2 Xo Calorimiter 50 cm 50 cm 9.5 cm 100 µm pitch Compton'sca+ering'and'pair'produc2on'telescope' 25!
26 ESA'Call'for'Small'Missions:'June,'2012' Gamma-light payload Power~ 400 W Weight~600 Kg 26!
27 GAMMA-LIGHT satellite launch configurations for the PSLV and VEGA a companion satellite similar to G-LIGHT can be accomodated. 27!
28 Gamma-light Participants INAF Italian Institute of Astrophysics (INAF), Italy! INFN Italian Institute of Nuclear Physics, Italy! ASDC ASI Science Data Center, Italy! SRC PAS Space Research Center of Polish Academy of Sciences, Poland! NCAC Nicolaus Copernicus Astronomical Center, Warsaw, Poland! UBA University of Barcelona, Spain! DTU Space, Denmark! UIB University of Bergen, Norway! TOV University of Rome Tor Vergata, Italy! TUR University of Turin, Italy! YAL Yale University, USA! SAP University of Rome "La Sapienza, Italy! IFT-UAM Universidad Autonoma de Madrid, Spain! USAL University of Salamanca, Spain! TRI University of Trieste, Italy! ENEA, Italy! 28!
29 G-LIGHT Simulation Compton interaction of a 10 MeV photon producing a low-energy single-track electron, and depositing energy in the Calorimeter for a 30 0 incidence 29!
30 Gamma-light Simulation 30!
31 Effective area Fermi LAT! ( Front + Back)! Fermi LAT! ( Front)! GAMMA-LIGHT! 30 0! AGILE! 30 0! COMPTEL Kalman reconstruction, assumed bkg rejection eff !
32 PSF (68% containment radius) AGILE! 30 0! GAMMA-LIGHT! 30 0! Fermi LAT! ( Front + Back)! Fermi LAT! front P7v6! 32!
33 AGILE! Fermi LAT! ( Front)! GAMMA-LIGHT! Fermi LAT! ( Front+Back)! Flux Sensitivity 33!
34 Flux Sensitivity AGILE! GAMMA-LIGHT! Fermi LAT! ( Front)! Fermi LAT! ( Front+Back)! 34!
35 Astrophysics Objectives of GAMMA-LIGHT 1. Search of Dark Matter gamma-ray signatures in the Galaxy and in particular in the Galactic Center region; 2. Resolving the Galactic Center region in gamma-rays: the central BH region, GeV and TeV sources, nebulae, compact sources, SNRs; 3. Resolving the diffuse emission in the Galactic plane, relation with cosmic-ray propagation, star forming regions in the Galactic plane; extending the cosmic-ray propagation and emission properties of the "Fermi bubbles" to the lowest energies below 100 MeV; 4. Resolving spatially and spectrally SNRs and addressing the origin and propagation of cosmic- rays; 5. Polarization studies of gamma-ray sources; 35!
36 Astrophysics Objectives of GAMMA-LIGHT (cont.) 6. Detection of soft gamma-ray pulsars in the range MeV, and pulsar wind nebulae studies; 7. Detection of compact objects, microquasars, relativistic jets in the range 10 MeV - 1 GeV resolving the issue of hadronic vs. leptonic jets for a variety of sources (e.g., Cyg X-3); 8. Detection and localization of transients and exotic sources with much improved sensitivity;detection of Crab Nebula gammaray flares with excellent sensitivity down to 10 MeV; 9. Blazar studies down to 10 MeV, excellent positioning resolving source confusion; 10. GRB excellent capability in the range 10 MeV - 5 GeV; sub-millisecond timing capability in the range MeV. 36!
37 Extragalactic Sources, Blazars, MeV Blazars Multi-epoch SEDs of the FSRQ 3C454.3 G-LIGHT will allow us to investigate daily (or sub-daily) SEDs during gamma-ray super- flares. The 5-sigma G-LIGHT differential sensitivity (purple line) is computed for an integration time of 48 hours 37!
38 SNRs and the Origin and Propagation of CRs Bremsstrahlung GAMMA-LIGHT! sensitivity! neutral pion decay gamma-ray spectrum of SNRs W44. The red curve shows the expected GAMMA-LIGHT sensitivity for a 1-year effective time integration. 38!
39 Earth Studies Objectives of GAMMA-LIGHT: Terrestrial Gamma-Ray Flashes Fermi GBM 12xNaI! GAMMA-LIGHT CAL! Fermi GBM! 2xBGO! AGILE! GAMMA-LIGHT TRK! RHESSI! 39!
40 Earth Studies Objectives of GAMMA-LIGHT: Terrestrial Gamma-Ray Flashes G-LIGHT will fill this observational gap and contribute to TGF science with the following points: 1) detection of Terrestrial Gamma-Ray Flashes (TGFs) with extended energy range and imaging capability obtained by a new strategy for Earth albedo background rejection; 2) correlating high-energy TGFs with local and global meteorological data, addressing local climate and Climate Change issues; 3) studying the impact of TGFs and "high-energy"-tgfs for the atmospheric chemistry and particle transport including gammaray and neutron generation and atmospheric propagation to the ground; 4) maintaining an updated TGF archive, available to ESA and meteorological institutions. 40!
41 41!
42 INFN and the Cherenkov Telescope Array!! The future in VHE gamma ray astrophysics: 42!
![V Agile E*F(>E) [ TeV/cm 2 s] Agile, Fermi, Argo, Hawk: 1 year Magic, Hess, Veritas, CTA: 50h E 10-11 10-12 Fermi Magic-II Argo Hawc Crab 10%](/docs-images/82/86958305/images/43-2.jpg "Crab Hess/Veritas E 10-13 Far universe Pulsars Fundamental physics 10-14 CTA Cosmic rays 1% Crab at the knee 10 100 1000 10 4 10 5 E [GeV] 43!")
43 V Agile E*F(>E) [ TeV/cm 2 s] Agile, Fermi, Argo, Hawk: 1 year Magic, Hess, Veritas, CTA: 50h E Fermi Magic-II Argo Hawc Crab 10% Crab Hess/Veritas E Far universe Pulsars Fundamental physics CTA Cosmic rays 1% Crab at the knee E [GeV] 43! 43!
44 Future Experiments GAMMA-400, 100 MeV 3 TeV, an approved Russian -ray satellite. Planned launch Energy resolution (100 GeV) 1 %. Effective area 0.4 m2. Angular resolution (100 GeV) DAMPE: Satellite of similar performance. An approved Chinese -ray satellite. Planned launch HERD: Instrument on the planned Chinese Space Station. Energy resolution (100 GeV) 1 %. Effective area 1-2 m2. Angular resolution (100 GeV) Planned launch around !
45 Gamma-400 May be a merging with GAMMA-LIGHT? 45!
46 thank you for the attention 46!
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