International research project GALA: Monitoring of high energy gamma-ray astrophysical sources.

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International research project GALA: Monitoring of high energy gamma-ray astrophysical sources

Preface Several hundreds of point high-energy gamma ray astrophysical sources were discovered to date, but more then half of those sources are still not identified. Taking in to account that gamma-ray emission is associated mainly with active variable objects, the continuous monitoring of celestial sphere using the telescope with high angle and time resolutions allow to identify a noticeable part of known unidentified sources and to discover new high-energy gamma- ray sources. To realize the continuous monitoring of gamma-ray astrophysical sources it is proposed to develop wide-aperture gamma telescope GALA with high angle resolution in MeV energy range and install it as additional payload onboard Meteor-M satellite. Meteor-M is the Russian meteorological low polar orbit satellite designed by Russian Space firm VNIIEM.

GALA scientific objectives The main task of project GALA is continuous, during several years, monitoring of celestial sphere aimed for: Clarification the nature of unidentified point high-energy gamma-ray sources; search of new gamma-transients. Study of discovered gamma-ray pulsars; search the pulsed gamma-ray emission from unidentified sources. Search of high-energy gamma-radiation from galactic binaries and supernova remnants. Investigation of known Active Galactic Nuclei; search new extragalactic high- energy gamma-ray discrete sources. Study of diffuse high-energy gamma-ray emission. The additional scientific goal of GALA project: Study of cosmic ray isotope fluxes in MeV/n energy range in near-Earth space.

GALA instrument diagram Telescope systems: 1) Silicon tracker. Purpose:  -quantum conversion and e + e - pair detection. Structure: 16 detecting planes 400  400 mm each. Distance between planes – 20 mm. Each plane consists of two layers. First layer – active converter SN1-SN16 (Each of these views is the single-sided, AC- coupled, 500  m thick silicon strip detector with a readout ). Second layer - double-sided (X, Y), 300  m thick silicon microstrip detector S1-S16 with readout peach 250  m). 2) Anticoincidence. Purpose: Rejection of cosmic ray charged particles. Structure: CU – the upper anticoincidence detector CS1-CS4 – side anticoincidence detectors CD1-CD4, CD – down anticoincidence detectors

Trigger Gamma-ray trigger:, where Isotope trigger:

Main physical characteristics Characteristics EGRETGALA Energy range30 MeV - 30 GeV>10 MeV Field of view0.5 sr3 sr Angle resolution ~15  (30 MeV) 5.5  (100 MeV) 1.2  (1 GeV) 4.9  (30 MeV) 1.6  (100 MeV) 0.3  (1 GeV) Sensitive area1500 cm cm 2 Energy resolution10%30 % ( MeV) Dead time>100 ms<1 ms

Effective area

Field of view

Angular resolution

Sensitivity to point sources

Meteor-M satellite Main characteristics Orbit Circular, sun- synchronous Altitude835 km Inclination  Pointing configurationOrbital Pointing accuracy 0.1  PositioningBetter then 30 m Accuracy of onboard time synchronization with UT 2  s Satellite mass800 kg Payload mass320 kg Power1.4 kW Telemetry122 Mbit/s Satellite lifetimeMore then 5 years GALA

Telescope GALA onboard Meteor-M GALA overall dimensions 600  600  600 mm Instrument mass~100 kg Power consumption~150 W Mass memory2 Gbytes Required pointing accuracy 0.1  Required accuracy of onboard time synchronization with UT Better then 10  s GALA technical characteristics

Comparison between EGRET and GALA exposures EGRET Cycles: 1, 2, 3, 4 GALA 1 year of observations Units: 10 8 cm 2 s

GALA exposure for point source vs. time

Expected results of observations: Number of detected gamma-quanta with energy >30 MeV versus spectral index  of 3EG sources demonstrated very low time variability

Expected results of observations: Expected GALA count maps of Galactic center region

GALA collaboration Collaborators from Russian side: Moscow Engineering Physics Institute (State University) Sternberg Astronomical Institute (Moscow State University) Institute of Astronomy RAS Lebedev Physical Institute RAS All Russian Scientific and Research Institute of Electro mechanics (VNIIEM) Foreign collaborators: National Institute of Nuclear Physics (INFN), Italy