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The Gamma-400 MISSION

The Gamma-400 MISSION. Valter Bonvicini INFN – Trieste, Italy On behalf of the Gamma-400 Collaboration Workshop on Recent Developments in Astronuclear and Astroparticle Physics International Centre for Theoretical Physics (ICTP) – Trieste, Italy – November 19 – 23, 2012. Outline.

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The Gamma-400 MISSION

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  1. The Gamma-400 MISSION ValterBonvicini INFN – Trieste, Italy On behalf of the Gamma-400 Collaboration Workshop on Recent Developments in Astronuclear and Astroparticle Physics International Centre for Theoretical Physics (ICTP) – Trieste, Italy – November 19 – 23, 2012

  2. Outline • Introduction • Gamma-400 mission: • “Baseline” (original Russian project) • Italian proposal • Gamma-400 physics potential • Photons • Electrons • Nuclei • Conclusions V. Bonvicini - INFN Trieste

  3. Gamma-400 Collaboration • Lebedev Physical Institute (leading organization) • National Research Nuclear University MEPhI • Ioffe Physical Technical Institute • Open Join Stock Company “Research Institute for Electromechanics” (Istra) • Institute for High Energy Physics (Protvino) • Space Research Institute • IstitutoNazionale di FisicaNucleare (INFN), Italy • IstitutoNazionale di Astrofisica, INAF, Italy • NASA Goddard SFC/University of Maryland, USA • Kavli Institute/Stanford University, USA V. Bonvicini - INFN Trieste

  4. Gamma-400 Collaboration • Expressed interest from Sweden, France, Spain, other U.S. groups • Interest from the TeV community (CTA, Hofmann) • Open to all contributions and possible collaborations V. Bonvicini - INFN Trieste

  5. The Gamma-400 project • Mission is approved by ROSCOSMOS (launch currently scheduled by November 2018) • Gamma-400: • Scientific payload mass: 2600 kg • Power budget: 2000 W • Telemetry downlink capability: 100 GB/day • Lifetime: 10 years • Orbit (initial parameters): apogee 300000 km, perigee 500 km, orbital period 7 days, inclination 51.8 ° • Gamma-400 will be installed onboard the platform “Navigator” manufactured by Lavochkin V. Bonvicini - INFN Trieste

  6. Gamma-400 orbit V. Bonvicini - INFN Trieste

  7. Gamma-400 “baseline” • Original Russian design focused on: • High energy gamma-rays (10 GeV- 3 TeV) • High energy electrons (e- and e+) • Science objectives (from Russian proposal): • “To study the nature and features of weakly interacting massive particles, from which the dark matter consists” • “To study the nature and features of variable gamma-ray activity of astrophysical objects from stars to galactic clusters” • “To study the mechanisms of generation, acceleration, propagation, and interaction of cosmic rays in galactic and intergalactic spaces” V. Bonvicini - INFN Trieste

  8. Gamma-400 “baseline” V. Bonvicini - INFN Trieste

  9. Gamma-400: Italian proposal • Availability for a revision of the design that could enhance the performance and science capability of the project • Gamma-400: a multi-purpose mission (photons@ high- and low-energies, electrons, nuclei) • Revised design of the converter/tracker • Breakthrough angular resolution (3-4 times better than Fermi-LAT @ 1 GeV) • Improved sensitivity • Homogeneous and isotropic calorimeter ( 40 X0 and 2 I)with optimal energy resolution and particle discrimination • Electron/positron detection beyond TeV energies • Nuclei detection up to 1015eV (“knee”) • Nuclei identification capability (dE/dx measurement) with Silicon pad detectors • Trigger with TOF capabilities (“smart” AC) V. Bonvicini - INFN Trieste

  10. Gamma-400: Italian proposal A/C TRACKER Silicon Array Time-of_Flight CALO V. Bonvicini - INFN Trieste

  11. Converter/Tracker • The parameters that mainly affect the angular resolution of silicon-based Trackers in the AGILE and Fermi-LAT configurations are: • The thickness X0 of each plane (multiple scattering) • The spacing (lever arm) between planes • The pitch of the strips and the thickness of the Si sensors • The read-out approach (analog or binary) • Event filtering, event topology and noise V. Bonvicini - INFN Trieste

  12. Converter/Tracker • Homogeneous Si-W Tracker • 25 W/Si-x/Si-y planes • Thickness of each plane 0.03X0 • 4 towers ( 50 cm x 50 cm each) • Single-sided,  120 µm pitch • microstrip detectors • Each sensor  9.7 cm x 9.7 cm • Sensors arranged in ladders (5 • detectors/ladder) • Capacitive charge division readout • (1 strip every 2) • 5000 silicon detectors • 384000 readout channels V. Bonvicini - INFN Trieste

  13. Gamma-400 and Fermi: Aeff & PSF PSF Effective area Black line: Fermi front+back (PASS 7) Blue line: Fermi front (PASS 7) Red solid line: G-400 120 x 120 cm2 Red dashed line: G400 100 x 100 cm2 Black line: Fermi front (PASS 7) Blue line: Fermi front + back (PASS 7) Red line: Gamma-400 V. Bonvicini - INFN Trieste

  14. Gamma-400 sensitivity Galactic center Black line: Fermi front+back (PASS 7) Red solid line: G-400 120 x 120 cm2 Blue line: Fermi front (PASS 7) Red dashed line: G400 100 x 100 cm2 V. Bonvicini - INFN Trieste

  15. Gamma-400 sensitivity Galactic center Black line: Fermi front+back (PASS 7) Red solid line: G-400 120 x 120 cm2 Blue line: Fermi front (PASS 7) Red dashed line: G400 100 x 100 cm2 V. Bonvicini - INFN Trieste

  16. Gamma-400 sensitivity CTA CTA Black line: Fermi front+back (PASS 7) Red solid line: G-400 120 x 120 cm2 Blue line: Fermi front (PASS 7) Red dashed line: G400 100 x 100 cm2 V. Bonvicini - INFN Trieste

  17. Calorimeter • Homogeneous cubic calorimeter • Symmetric, to maximize GF • Total mass ~ 1600 kg • Very large dynamic range • Finely segmented in all directions • 1 RM x 1 RM x 1 RMCsI(Tl) cubic • crystals • Few mm gaps between crystals Detail of a calorimeter plane: Blue: crystals Grey: Al support Green: photodetectors Brown: readout cables V. Bonvicini - INFN Trieste

  18. Calorimeter details (* one Moliere radius) (** within a reduced perimeter of size (N-1)*L ) V. Bonvicini - INFN Trieste

  19. Calorimeter Small pre-prototype (18 cubes) read-out with CASIS ASICs assembled and tested in October 2012 at the CERN SPS. Data analysis is on-going, first results give S/N ~ 17 for 1-MIP signals! V. Bonvicini - INFN Trieste

  20. Calorimeter • Overall Geometrical Factor: 5 X (1.72 m2sr) = 8.5 m2sr • For electrons (1 TeV) with selection criteria allowing an efficiency of 33%: • Resolution 1% • GF 8.5 x 0.33 = 2.84 m2sr • For protonsallowing for an suitable shower development and containment: • Efficiency 44% corresponding to an effective GF = 3.75 m2sr • In absence of software and/or hardware compensation the energy resolution for protons is of about 33%. By applying those compensations simulations indicates that 16% is reachable. • Rejection power for protons when selecting electrons is >105 simulation work is ongoing. V. Bonvicini - INFN Trieste

  21. Calorimeter energy resolution • Protons 1 TeV Efficiency ~ 44% Energy resolution after software compensation: fit 68.7% prob. ~ 16% V. Bonvicini - INFN Trieste

  22. Calorimeter energy resolution • Electrons 1 TeV • Energy resolution: • RMS ~0.91% • fit68.7% prob. • ~ 0.69% Electrons from every direction (2), traversing the top calorimeter surface, with contained shower maximum V. Bonvicini - INFN Trieste

  23. Calorimeter energy resolution • Photons 100 GeV Gamma rays traversing the top detectors (AC) and the top calorimeter surface, with contained shower maximum • Energy resolution: • RMS~1.26% • fit68.7% prob. • ~ 0.87% V. Bonvicini - INFN Trieste

  24. Silicon Array Silicon large pixel (pads ~ 1.5 x 1.5 cm2)) detector V. Bonvicini - INFN Trieste

  25. Gamma-400: scientific goals • Gamma-400: a dual instrument • Proton/nuclei cosmic-rays up to the "knee“ whose spectrum and composition is to be studied with unprecedented detail up to 1 PeV/nucleon. • Cosmic-ray acceleration in SNR and galactic diffusion resolved with unprecedented detail in both space and spectra. • Excellent sensitivity to neutral pion emission below 200 MeV. • Gamma-rays from 30 MeV up to 300 GeVto be studied with substantial improvements concerning the angular and energy resolution, the broad-band sensitivity, and the continuous exposure of sources without Earth occultation • Electrons/positrons in the TeVenergy range and beyond, to be measured with much improved sensitivity compared with current space, balloon-borne and ground measurements; V. Bonvicini - INFN Trieste

  26. Scientific goals: DM Indirect search with gamma-rays • Ground-based Imaging Atmospheric Cherenkovtelescopes: • MAGIC, HESS, VERITAS, CTA, … • sensitive to g’s from 50 GeV – 50 TeV (>100 TeV for CTA) • Gamma-ray space telescopes: • EGRET, AGILE, Fermi/LAT, Gamma-400,… • sensitive to g’s 30 MeV - 300 GeV, excellent pointing, mapping capability • Signature: Mono-energetic -line from direct annihilation or continuum through annihilation into intermediate states • search in galactic dark matter halo, dwarf galaxies, galaxy clusters, galactic dark matter satellites, … V. Bonvicini - INFN Trieste

  27. Scientific goals: high-energy s + arXiv:1205.1045 arXiv:1206.1616 Gamma-400 ideal for looking for spectral DM-induced features, like searching for –ray lines! If Weniger is right, the 130 GeV line should be seen with 10  significance (L. Bergströmet al., arXiv:1207.6773v1 [hep-ph]) L. Bergström, , Stockholm 2012 V. Bonvicini - INFN Trieste

  28. Scientific goals: low-energy s Cosmic rays and low-energy s V. Bonvicini - INFN Trieste

  29. Scientific goals: dark matter and electrons V. Bonvicini - INFN Trieste

  30. Scientific goals: dark matter and electrons V. Bonvicini - INFN Trieste

  31. Electrons – counts estimation V. Bonvicini - INFN Trieste

  32. Scientific goals: nuclei V. Bonvicini - INFN Trieste

  33. Protons and He – counts estimation V. Bonvicini - INFN Trieste

  34. Conclusions • The Gamma-400 mission represents a unique opportunity to perform simultaneous measurements of photons, electrons and nuclei with unprecedented accuracy. • Gamma-400 can provide in-depth investigations on some of the most challenging physics items, such as DM search, CR origin, production and acceleration to the highest energies… • A TDR of the upgraded version of the instrument will be presented by mid 2013. • The launch is currently scheduled by November 2018. V. Bonvicini - INFN Trieste

  35. Back-up slides V. Bonvicini - INFN Trieste

  36. Russian vs. Italian design V. Bonvicini - INFN Trieste

  37. Tracker geometry V. Bonvicini - INFN Trieste

  38. Sensitivity – 48 hrs Galactic center Extragalactic Black line: Fermi front+back Blue line: Fermi front Red solid line: G-400 120 x 120 cm2 Red dashed line: G400 100 x 100 cm2 V. Bonvicini - INFN Trieste

  39. Sensitivity – 1 month Galactic center Extragalactic Black line: Fermi front+back Blue line: Fermi front Red solid line: G-400 120 x 120 cm2 Red dashed line: G400 100 x 100 cm2 V. Bonvicini - INFN Trieste

  40. Calorimeter summary V. Bonvicini - INFN Trieste

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