Future experiments in space and on ground for the search of Dark Matter with gamma-rays
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1 Future experiments in space and on ground for the search of Dark Matter with gamma-rays Aldo Morselli INFN Roma Tor Vergata IBS-MultiDark Joint Focus Program: WIPMs and Axions IBS-CTPU, Korea October, 2014 Aldo Morselli, INFN Roma Tor Vergata! 1!
2 The Low Energy frontier Aldo Morselli, INFN Roma Tor Vergata! 2!
3 History of GALACTIC CENTER observations Indirect Search for Dark Matter from the center of the Milky Way with the Fermi-Large Area Telescope Vincenzo Vitale, Aldo Morselli, the Fermi/LAT Collaboration Proceedings of the 2009 Fermi Symposium, 6 pages, econf Proceedings C arxiv: Search for Dark Matter with Fermi Large Area Telescope: the Galactic Center V.Vitale, A.Morselli, the Fermi/LAT Collaboration Nuclear Instruments and Methods in Physics Research A 630 (2011) (Available online 23 June 2010) Dark Matter Annihilation in The Galactic Center As Seen by the Fermi Gamma Ray Space Telescope Dan Hooper, Lisa Goodenough. (21 March 2011 ). 21 pp. Published in Phys.Lett. B697 (2011) On The Origin Of The Gamma Rays From The Galactic Center Dan Hooper, Tim Linden. Oct pp. Published in Phys.Rev. D84 (2011) Detection of a Gamma-Ray Source in the Galactic Center Consistent with Extended Emission from Dark Matter Annihilation and Concentrated Astrophysical Emission Kevork N. Abazajian, Manoj Kaplinghat (UC, Irvine). Jul pp. Published in Phys.Rev. D86 (2012) Dark Matter and Pulsar Model Constraints from Galactic Center Fermi-LAT Gamma Ray Observations Chris Gordon, Oscar Macías (Canterbury U.). Jun 24, pp. Published in Phys.Rev. D88 (2013) The Characterization of the Gamma-Ray Signal from the Central Milky Way: A Compelling Case for Annihilating Dark Matter Tansu Daylan, Douglas P. Finkbeiner, Dan Hooper, Tim Linden, Stephen K. N. Portillo, Nicholas L. Rodd, Tracy R. Slatyer. Feb 26, pp. e-print: arxiv: [astro-ph.he] Aldo Morselli, INFN Roma Tor Vergata! 3!
4 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.Morselli, Fermi Coll. NIM A630 (2011) 147, arxiv: Aldo Morselli, INFN Roma Tor Vergata! 4!
5 ARE WE SEEING DARK MATTER WITH THE FERMI-LAT IN A REGION AROUND THE MILKY WAY CENTER? Maybe yes, but we can t be sure as far as we don t understand the background at the level needed for disentangle a DM-induced γ-ray flux in this interesting region. New experiment at energies below 100 MeV is needed Aldo Morselli, INFN Roma Tor Vergata! 5!
6 Constraints from the inner Galaxy 3 σ upper limits on the annihilation cross-section for different channels and halo profiles No assumption on background very robust result Gomez-Vargas et al. JCAP 10 (2013) 029 arxiv: Aldo Morselli, INFN Roma Tor Vergata! 6!
7 Low energy lines limits and implications for gravitino dark matter in the µνssm excluded Excluded region JCAP accepted,[arxiv: ] Aldo Morselli, INFN Roma Tor Vergata! 7!
8 New Low Energy Line Search But this Analysis is Systematics Limited Modeling effective area background emission not masking known point sources: because the broad PSF of the LAT at low energies. Excluded region To improve the search a better energy and angular resolution at low energies is needed Aldo Morselli, INFN Roma Tor Vergata! 8!
9 Differential yield for each annihilation channel Quite distinctive spectrum (no power-law) solid lines are the total yields, while the dashed lines are components not due to π 0 decays WIMP mass=200gev! A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, 267, 2004 [astro-ph/ ]! Aldo Morselli, INFN Roma Tor Vergata! 9!
10 Differential yield for b bar for different neutralino mass Low energy range is very important also for high mass neutralino search neutralino mass A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, , 2004 [astro-ph/ ]! Aldo Morselli, INFN Roma Tor Vergata! 10!
11 Aldo Morselli, INFN Roma Tor Vergata! 11!
12 Aldo Morselli, INFN Roma Tor Vergata! 12!
13 Elements of a pair-conversion telescope photons materialize into matter-antimatter pairs: E γ --> m e +c 2 + m e -c 2 electron and positron carry information about the direction, energy and polarization of the γ-ray (energy measurement) Aldo Morselli, INFN Roma Tor Vergata! 13!
14 Interaction of photons with matter Fractional energy loss for e + and e - in lead Photon total cross sections Pair x/x 0 Prob Int Aldo Morselli, INFN Roma Tor Vergata! 14!
15 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)! Aldo Morselli, INFN Roma Tor Vergata! 15!
16 Multiple Scattering 50 Aldo Morselli, INFN Roma Tor Vergata! 16!
17 Elements of a pair-conversion telescope (more realistic scheme) photons materialize into matter-antimatter pairs: E γ --> m e +c 2 + m e -c 2 electron and positron carry information about the direction, energy and polarization of the γ-ray (energy measurement) Aldo Morselli, INFN Roma Tor Vergata! 17!
18 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' Aldo Morselli, INFN Roma Tor Vergata! 18!
19 Gamma-light Simulation Aldo Morselli, INFN Roma Tor Vergata! 19!
20 Power~ 400 W Weight Tracker ~110 Kg Weight Calorimeter ~60 Kg Total weight ~ 600 Kg Gamma-light payload Aldo Morselli, INFN Roma Tor Vergata! 20!
21 GAMMA-LIGHT satellite launch configurations for the PSLV and VEGA a companion satellite similar to G-LIGHT can be accomodated. Aldo Morselli, INFN Roma Tor Vergata! 21!
22 Gamma-Light Point Spread Function (angular resolution) AGILE! 30 0! GAMMA-LIGHT! 30 0! Fermi LAT! ( Front + Back)! Fermi LAT! front P7v6! A.Morselli et al., Nuclear Physics B Proc. Supp (2013) [arxiv: ]! Aldo Morselli, INFN Roma Tor Vergata! 22!
23 Effective area Fermi LAT! ( Front + Back)! Fermi LAT! ( Front)! GAMMA-LIGHT 30 0! AGILE 30 0! COMPTEL Kalman reconstruction, assumed bkg rejection eff A.Morselli et al., Nuclear Physics B Proc. Supp (2013) [arxiv: ]!! Aldo Morselli, INFN Roma Tor Vergata! 23!
24 AGILE! Fermi LAT! ( Front)! GAMMA-LIGHT! Fermi LAT! ( Front+Back)! Flux Sensitivity A.Morselli et al., Nuclear Physics B Proc. Supp (2013) [arxiv: ]!! Aldo Morselli, INFN Roma Tor Vergata! 24!
25 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 Aldo Morselli, INFN Roma Tor Vergata! 25!
26 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. Aldo Morselli, INFN Roma Tor Vergata! 26!
27 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; Aldo Morselli, INFN Roma Tor Vergata! 27!
28 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. Aldo Morselli, INFN Roma Tor Vergata! 28!
29 ESA$M&4$Call$ quite$different$from$previous$medium&sized$mission$ Calls$(Solar$Orbiter,$EUCLID,$PLATO);$ total$esa$budget:$450$meuro.$ guidelines$for$an$ ESA&only $mission:$ Payload$mass:$300$kg;$ total$spacecrap$mass:$800$kg.$ Aldo Morselli, INFN Roma Tor Vergata! 29!
30 ESA$M&4$Call$ idea$of$$ marriage $with$a$compton$telescope$ sensitve$in$the$range$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$200$kev$ $10$ MeV.$ $ possible$merging$with$the$astro&mev$group.$ $ Science,$Instrument,$Community.$ # Aldo Morselli, INFN Roma Tor Vergata! 30!
31 the$ MeV&GeV $concept$ range$$200$kev$ $100$MeV:$new$window.$ $ sensitvity$(contnuum$and$lines)$be[er$than$integral,$ COMPTEL,$AGILE$and$FERMI$by$a$factor$10&20.$ $ Two$opTons$under$consideraTons:$ One$single$instrument$for$Compton$and$pair$ Two$instruments$on$board$the$same$spacecraP$ # Aldo Morselli, INFN Roma Tor Vergata! 31!
32 Gamma-MeV scheme Difference: DSSD planes 100 µm pitch each ~0.016 X 0 -~0.012 X 0 AC Tot~ 1 X cm 2 Xo Calorimiter height of a plane 1.3 cm 50 cm 50 cm DSSD= Double Side Silicon Detectors Compton'sca+ering'and'pair'produc2on'telescope' 9.5 cm 100 µm pitch Aldo Morselli, INFN Roma Tor Vergata! 32!
33 Double Side Silicon Detector DSSD Even (odd) sensors, on the n-side, are coupled to decrease the numbers of readout channels Aldo Morselli, INFN Roma Tor Vergata! 33!
34 Concept of Compton Gamma-Ray Imaging Gamma rays interact several times with detector via Compton interaction (e.g. until it is stopped by the photo-electrical effect) Measuring positions and energies of individual interactions enables to determine pathway of gamma ray in detector (tracking) Energies and positions of first two interactions define cone of incident angles (electron path is not measured) Cones are projected on plane or sphere (one circle per event) for 2D or into cube (one cone per event) for 3D imaging 3 components critical for Compton imaging: Position Resolution (distance between first two interactions) Energy Resolution (energy deposition/ scattering angle) Intrinsic Electron Momentum (scattering angle, gamma-ray energy) Aldo Morselli, INFN Roma Tor Vergata! 34!
35 Concept of Compton Gamma-Ray Imaging Polarization The differential Klein-Nishina cross-section for Compton scattering contains a strong dependence on the polarisation of the incident γ-ray photon. Scattered photons are emitted preferentially perpendicular to the direction of the electric field vector of the incoming photon. The strongest azimuthal modulation in the distribution of scattered photons will be for the lowest γ-ray energies and scatter angles of deg. This makes a Compton telescope with a calorimeter covering a large solid angle a unique polarimeter. Aldo Morselli, INFN Roma Tor Vergata! 35!
36 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 Work in progress. Please join us if you are interested Aldo Morselli, INFN Roma Tor Vergata! 36!
37 The High Energy frontier Aldo Morselli, INFN Roma Tor Vergata! 37!
38 New projects in space Gamma-400 launch foreseen by end MeV 3 TeV, an approved Russian γ-ray satellite. Energy resolution (100 GeV) 1 %. Effective area 0.4 m2. Angular resolution (100 GeV) Science with Gamma-400 Workshop DAMPE: Satellite of similar performance as Gamma-400. An approved Chinese γ-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 Aldo Morselli, INFN Roma Tor Vergata! 38!
39 DAMPE and HERD Gamma-ray Sensitivity Aldo Morselli, INFN Roma Tor Vergata! 39!
40 CTA Aldo Morselli, INFN Roma Tor Vergata! 40!
41 Design for operation up to 30 years Prototypes: First science: 2017 Completion (?): 2020 Aldo Morselli, INFN Roma Tor Vergata! 41!
42 CTA SENSITIVITY (IN UNITS OF CRAB FLUX) FOR DETECTION IN EACH 0.2-DECADE ENERGY BAND Aldo Morselli, INFN Roma Tor Vergata! 42!
43 Dwarf Spheroidal Galaxies upper-limits Segue 1! CTA array B 100 h! Segue 1! CTA array B 100 h! Fermi 2 years! Fermi 2 years! Fermi 10 years! Fermi 10 years! Fermi 10 years 30 dsphs! Fornax Cluster! Fornax CTA Cluster! array B 100 h! CTA array B 100 h! Galactic Halo CTA! array B 100 h! Galactic Halo CTA array B 100 h! Update of Doro et al. arxiv: Aldo Morselli, INFN Roma Tor Vergata! 43!
44 HAWC Gamma Ray Observatory Site selected in August 2013 start of operations HAWC-100 HAWC inauguration March 2015 Volcán Sierra Negra, central Mexico latitude 19o North altitude 4,100 m asl Aldo Morselli, INFN Roma Tor Vergata! 44!
45 LHAASO Aldo Morselli, INFN Roma Tor Vergata! 45!
46 Status of LHAASO LHAASO has been included in the roadmap of the infrastructure construction for basic science in a short term (5 years). Total 16 projects are included. The local government has approved the LHAASO site last month. A ceremony of signing the LHAASO-MOU by the CAS president and Sichuan governor is tentatively scheduled on June 5th. Engineering arrays at scales of 1%-10% of the full project. Steps ahead: environment impact evaluation, feasibility reviewing, TDR reviewing Aldo Morselli, INFN Roma Tor Vergata! 46!
47 LHAASO International Coll. is growing France, Italy Russia, Thailand Aldo Morselli, INFN Roma Tor Vergata! 47!
48 LHAASO Aldo Morselli, INFN Roma Tor Vergata! 48!
49 Sensitivity of present and future experiments Aldo Morselli, INFN Roma Tor Vergata! 49!
50 LHAASO and Dark Matter Search A.Morselli 2014! Hawc Segue 1! LHAASO Segue 1! update of arxiv: Aldo Morselli, INFN Roma Tor Vergata! 50!
51 LHAASO CTA and HAWC and Dark Matter Search update of arxiv: , arxiv: Aldo Morselli, INFN Roma Tor Vergata! 51!
52 DM limit improvement estimate in 10 years with the composite likelihood approach ( ) 10 years of data instead of 2(5x) 30 dsphs (3x) (supposing that the new optical surveys will find new dsph) -10% from spatial extension (source extension increases the signal region at high energy E > 10 GeV, M > 200 GeV ) There are many assumptions in this prediction Doesn t deal with a possible detections. Aldo Morselli, INFN Roma Tor Vergata! 52!
53 LHAASO CTA and HAWC and Dark Matter Search Caveat: 30 dsphs (3x) (supposing that the new optical surveys will find new dsph) -10% from spatial extension (source extension increases the signal region at high energy There are many assumptions in this prediction Doesn t deal with a possible detections. update of arxiv: , arxiv: Aldo Morselli, INFN Roma Tor Vergata! 53!
54 Conclusions Thank you! Aldo Morselli, INFN Roma Tor Vergata! 54!
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