The Gamma-400 MISSION

THE GAMMA-400 MISSION

Valter BonviciniINFN – 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

V. Bonvicini - INFN Trieste 2

Outline

Introduction Gamma-400 mission:

“Baseline” (original Russian project) Italian proposal

Gamma-400 physics potential Photons Electrons Nuclei

Conclusions

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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

Istituto Nazionale di Fisica Nucleare (INFN), Italy

Istituto Nazionale di Astrofisica, INAF, Italy NASA Goddard SFC/University of Maryland, USA Kavli Institute/Stanford University, USA

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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

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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

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Gamma-400 orbit

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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”

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Gamma-400 “baseline”

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Gamma-ray energy range 10 – 3000 GeV

Multilayer converter Si-W, 11 layers, 100 x 100 cm2 , 0.84 X0

Calorimeter CC1 CsI-Si, 5 layers, 80 x 80 cm2, 3 X0

Calorimeter CC2 1024 BGO bars (25 x25 x 250 mm3), 80 x 80 cm2, 22

X0

Angular resolution (@ 100 GeV)

0.01 – 0.02°

Energy resolution (@ 100 GeV)

1 – 2%

Proton rejection 105


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 1015 eV (“knee”)

Nuclei identification capability (dE/dx measurement) with Silicon pad detectors

Trigger with TOF capabilities (“smart” AC)

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Gamma-400: Italian proposal

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CALO

TRACKERSilicon ArrayA/C

Time-of_Flight


Converter/Tracker

The parameters that mainly affect the angular resolution of silicon-based Trackers in the AGILE and Fermi-LAT configurations are:

1. The thickness X0 of each plane (multiple scattering)

2. The spacing (lever arm) between planes3. The pitch of the strips and the thickness of the

Si sensors4. The read-out approach (analog or binary)5. Event filtering, event topology and noise

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Converter/Tracker

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• 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


Gamma-400 and Fermi: Aeff & PSF

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Effective area PSF

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


Gamma-400 sensitivity

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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



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Galactic center



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CTA CTA


Calorimeter

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• 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 RM CsI(Tl) cubic crystals • Few mm gaps between crystals

Detail of a calorimeter plane:Blue: crystalsGrey: Al supportGreen: photodetectorsBrown: readout cables


Calorimeter details

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Cubes Cubes Cubes Cubes

NNN 202020 202019 212118 323232

L (cm) 3.6* 3.6* 3.6* 2.2

Crystal volume (cm3)

46.7 46.7 46.7 10.6

Gap (cm) 0.3 0.4 0.3 0.3

Mass (Kg) 1683 1599 1578 1574

N.Crystals 8000 7600 7497 32768

Size (cm3) 78.078.078.0 80.080.076.0 81.981.981.9

80.080.080.0

Depth (R.L.) “ (I.L.)

3939391.81.81.8

3939371.81.81.7

4141331.91.91.6

3838381.81.81.8

Planar GF (m2sr)(fiducial**)

1.721.721.72 1.811.721.72 1.911.531.53

1.891.891.89(* one Moliere radius)(** within a reduced perimeter of size (N-1)*L )


Calorimeter

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Small pre-prototype (18 cubes)read-out with CASIS ASICs assembled and tested in October2012 at the CERN SPS.

Data analysis is on-going, first resultsgive S/N ~ 17 for 1-MIP signals!


Calorimeter

Overall Geometrical Factor: 5 X (1.72 m2 sr) = 8.5 m2 sr For electrons (1 TeV) with selection criteria allowing an

efficiency of 33%: Resolution 1% GF 8.5 x 0.33 = 2.84 m2 sr

For protons allowing for an suitable shower development and containment: Efficiency 44% corresponding to an effective GF = 3.75 m2 sr 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.

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Calorimeter energy resolution

Protons 1 TeV

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Efficiency ~ 44%Energy resolution

after software compensation:

fit 68.7% prob.

~ 16%



Electrons 1 TeV

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Energy resolution:

•RMS ~0.91%

• fit68.7% prob.

~ 0.69%

Electrons from every direction (2), traversing the top calorimeter surface, with contained shower maximum



Photons 100 GeV

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Energy resolution:•RMS ~1.26%• fit68.7% prob. ~ 0.87%

Gamma rays traversing the top detectors (AC) and the top calorimeter surface, with contained shower maximum


Silicon Array

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Silicon large pixel (pads ~ 1.5 x 1.5 cm2)) detector


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 GeV to 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 TeV energy range and beyond, to be measured with much improved sensitivity compared with current space, balloon-borne and ground measurements;

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Scientific goals: DM Indirect search with gamma-rays

Ground-based Imaging Atmospheric Cherenkov telescopes: 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, …

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Scientific goals: high-energy s

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arXiv:1205.1045arXiv:1206.1616

+

Gamma-400 ideal for looking for spectral DM-inducedfeatures, like searching for –ray lines! If Weniger is right, the 130 GeV line should be seen with 10 significance (L. Bergström et al., arXiv:1207.6773v1 [hep-ph])

L. Bergström, , Stockholm 2012


Scientific goals: low-energy s

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Cosmic rays and low-energy s


Scientific goals: dark matter and electrons

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Electrons – counts estimation

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Scientific goals: nuclei

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Protons and He – counts estimation

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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.

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Back-up slides

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Russian vs. Italian design

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Tracker geometry

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Sensitivity – 48 hrs

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Galactic center Extragalactic

Black line: Fermi front+backBlue line: Fermi frontRed solid line: G-400 120 x 120 cm2



Sensitivity – 1 month

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Black line: Fermi front+backBlue line: Fermi frontRed solid line: G-400 120 x 120 cm2


Galactic center Extragalactic


Calorimeter summary

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The Gamma-400 MISSION

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