NASA Technical Reports Server (NTRS) 20130013643: Status of the GAMMA-400 Project

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AdvancesinSpaceResearch51(2013)297–300
www.elsevier.com/locate/asr
Status of the GAMMA-400 project
A.M. Galpera,b, O. Adrianic, R.L. Aptekard, I.V. Arkhangelskajab, A.I. Arkhangelskiyb,
M. Boezioe, V. Bonvicinie, K.A. Boyarchukf, Yu.V. Gusakova, M.O. Farberb,
M.I. Fradkina, V.A. Kachanovg, V.A. Kaplinb, M.D. Kheymitsb, A.A. Leonovb,
F. Longoe, P. Maestroh, P. Marrocchesih, E.P. Mazetsd, E. Mocchiuttie, A.A. Moiseevi,
N. Moric, I. Moskalenkoj, P.Yu. Naumovb, P. Papinic, P. Picozzak, V.G. Rodinl
M.F. Runtsob, R. Sparvolik, P. Spillantinic, S.I. Suchkova, M. Tavanim, N.P. Topchieva,⇑,
A. Vacchie, E. Vannuccinic, Yu.T. Yurkinb, N. Zampae, V.G. Zverevb
aLebedevPhysicalInstitute,RussianAcademyofSciences–Leninskiipr.53,RU-119991Moscow,Russia
bNationalResearchNuclearUniversityMEPhI–Kashirskoesh.31,RU-115409Moscow,Russia
cIstitutoNazionalediFisicaNucleare,SezionediFirenzeandPhysicsDepartmentofUniversityofFlorence,ViaSansone1,
I-50019SestoFiorentino(Firenze),Italy
dIoffePhysicalTechnicalInstitute,RussianAcademyofSciences–ul.Polytekhnicheskaya26,RU-194021St.Petersburg,Russia
eIstitutoNazionalediFisicaNucleare,SezionediTrieste–Padriciano99,I-34012Trieste,Italy
fOpenJointStockCompany“ResearchInstituteforElectromechanics”–ul.Panfilova11,RU-143502Istra,Moscowregion,Russia
gInstituteforHighEnergyPhysics–ul.Pobedy1,RU-142281Protvino,Moscowregion,Russia
hIstitutoNazionalediFisicaNucleare,SezionediPisaandPhysicsDepartmentofUniversityosSiena,ViaRoma56,I-53100Siena,Italy
iNASAGoddardSpaceFlightCenterandCRESST/UniversityofMaryland,Greenbelt,Maryland20771,USA
jHansenExperimentalPhysicsLaboratoryandKavliInstituteforParticleAstrophysicsandCosmology,StanfordUniversity,Stanford,CA94305,USA
kIstitutoNazionalediFisicaNucleare,SezionediRoma2andPhysicsDepartmentofUniversityofRome“TorVergata”–ViadellaRicercaScientifica1,
I-00133Rome,Italy
lSpaceResearchInstitute,RussianAcademyofSciences–ul.Profsoyuznaya84/32,RU-117997Moscow,Russia
mIstitutoNazionalediAstrofisica–IASFandPhysicsDepartmentofUniversityofRome“TorVergata”,ViadellaRicercaScientifica1,I-00133Rome,Italy
Availableonline8February2012
Abstract
Thepreliminarydesignofthenewspacegamma-raytelescopeGAMMA-400fortheenergyrange100MeV–3TeVispresented.The
angularresolutionoftheinstrument,1–2(cid:2)atEc(cid:2)100MeVand(cid:2)0.01(cid:2)atEc>100GeV,itsenergyresolution(cid:2)1%atEc>100GeV,
andtheprotonrejectionfactor(cid:2)106areoptimizedtoaddressabroadrangeofsciencetopics,suchassearchforsignaturesofdarkmat-
ter,studiesofGalacticandextragalacticgamma-raysources,Galacticandextragalacticdiffuseemission,gamma-raybursts,aswellas
high-precision measurementsofspectraofcosmic-ray electrons, positrons,and nuclei.
(cid:3)2012COSPAR. PublishedbyElsevier Ltd.Allrights reserved.
Keywords: Cosmicrays;Gammarays;Electrons;Positrons;Nuclei
1. Introduction cosmic rays (CRs), their acceleration, and propagation in
the Galaxy and intergalactic space remain open. Energetic
OnehundredyearsafterHess’discoveryoftheradiation CR particles when interacting with matter and radiation
comingfromspace,themainquestionsabouttheoriginof fields produce gamma-ray emission and, therefore, studies
ofgamma-raysources and diffuse emission provideimpor-
⇑ Correspondingauthor. tant clues to the origin and propagation of cosmic rays. A
E-mailaddress:[email protected](N.P.Topchiev). large number of outstanding problems in physics and
0273-1177/$36.00(cid:3)2012COSPAR.PublishedbyElsevierLtd.Allrightsreserved.
doi:10.1016/j.asr.2012.01.019
298 A.M.Galperetal./AdvancesinSpaceResearch51(2013)297–300
astrophysicsareconnectedwithstudiesofCRsandassoci- Beischer et al., 2009). A search for a fine structure in the
atedgamma-rayemission. Amongthemostpressingissues spectra of high-energy CR electrons-positrons and nuclei
are the nature of the dark matter, particle acceleration in is another important direction to pursue.
Galacticandcosmologicalshocks,theoriginofextragalac-
ticdiffuseemission,CRsinothergalaxiesandtherolethey
2. The GAMMA-400 gamma-ray telescope
play in galactic evolution, studies of the Galactic Center
and local Galactic environment, CR propagation in the
2.1. The GAMMA-400 performance
heliosphere, as well as many others.
The last years were rich in new breakthroughs and dis-
GAMMA-400 is designed to address scientific chal-
coveries thanks to the combined efforts of many very suc-
lenges and will detect gamma rays in the energy range
cessful space missions, such as PAMELA (Picozza et al.,
100MeV–3TeV with an angular resolution of 1–2(cid:2) at
2007), AGILE (Tavani et al., 2009), and Fermi-LAT
Ec(cid:2)100MeVand(cid:2)0.01(cid:2)atEc>100GeV,anenergyres-
(Atwood et al., 2009); balloon-borne missions, such as
olution of (cid:2)1% at Ec>100GeV, and an effective area of
ATIC (Guzik et al., 2004), CREAM (Seo et al., 2004),
(cid:2)4000cm2 at Ec=100GeV. The instrument will also be
andBESS(Yamamotoetal.,2007);aswellasground-based
used to detect electrons (positrons) in the energy range
gamma-ray telescopes, such as MILAGRO (Atkins et al.,
1–3000GeVwithaprotonrejectionfactor(cid:2)106andnuclei
2004),H.E.S.S.(Aharonianetal.,2004),VERITAS(Weekes
in the energy range 250GeV/nucleon to 1015eV/nucleon.
et al., 2010), and MAGIC (Aleksic´ et al., 2010). Among
The total mass of the instrument is 2600kg with power
them are the new measurements of CR electrons-positrons
consumption of (cid:2)2000W and a telemetry downlink capa-
by PAMELA (Adriani et al., 2009), Fermi-LAT (Abdo
bility of 100Gbyte/day. Together with GAMMA-400, the
etal.,2009a),H.E.S.S.(Aharonianetal.,2009),andATIC
space observatory will include the KONUS-FG gamma-
(Chang et al., 2008); antiprotons by BESS (Mitchell et al.,
ray burst monitor (Aptekar et al., 2009) and a star sensor
2005) and PAMELA (Adriani et al., 2011a); and a discov-
for determining the GAMMA-400 axes with accuracy of
eryofthebreakinthespectraofCRnucleibyATIC(Panov
approximately 500.
et al., 2009), CREAM (Yoon et al., 2011), and PAMELA
The GAMMA-400 physical scheme is shown in Fig. 1.
(Adriani et al., 2011b). In gamma rays – spectra of diffuse
The basic idea of the instrument was outlined in earlier
Galactic and extragalactic emission by EGRET (Hunter
publications (Dogiel et al., 1988; Ginzburg et al., 2007,
etal.,1997;Sreekumaretal.,1998)andFermi-LAT(Abdo
2009a,b), but the design is being improved (Galper et al.,
et al., 2009b); 270 Galactic and extragalactic gamma-ray
2011a,b,c) using the results of the current space missions
sources with energies up to 20GeV by EGRET (Hartman
Fermi-LAT andAGILE. Gamma-400 consists of scintilla-
et al., 1999), approximately 50 sources up to 50GeV by
tion anticoincidence top and lateral detectors (AC), con-
AGILE (Pittori et al., 2009), and nearly 1850 sources up
verter-tracker (C) with approximately 25 layers of double
to100GeVbyFermi-LAT(Abdoetal.,2011);aboutahun-
(x,y) silicon strip coordinate detectors (pitch 0.1mm)
dred sources of TeV photons by H.E.S.S. (Tibolla et al.,
2009), VERITAS (Holder et al., 2011), MAGIC (Cortina
et al., 2011), and MILAGRO (Smith et al., 2010).These
exciting recent developments show that we have just
touched the tip of the iceberg and even more exciting dis-
coveriesare still awaiting us.
Furtherobservationswithimprovedangularandenergy
resolutions in high-energy gamma-ray range are necessary
to address the following issues: study unidentified sources
which are one third of discovered gamma-ray sources
(Abdo et al., 2011), including detailed investigation of the
Galactic center, study sources for the energies more than
several tens GeV, where the energy ranges of Fermi and
ground-basedgamma-raytelescopesdonotoverlap(Abdo
et al., 2009c), study variability of many sources, study dif-
fuse gamma-ray emission for energies more than several
tens GeV, search for high-energy emission from gamma-
ray bursts and transient gamma-ray sources. The largely
unexplored energy range of several tens MeV – few hun-
dred MeV with only handful of observed sources has an
enormous discovery potential.
The diffuse gamma-ray emission above 100GeV
remainsunexploredandmayprovidesomecluestotheori-
gin of the dark matter (Abazajian and Harding, 2011; Fig.1. TheGAMMA-400physicalscheme.
A.M.Galperetal./AdvancesinSpaceResearch51(2013)297–300 299
interleaved with tungsten conversion foils, scintillation In the latter case, we use the four lateral detectors. Silicon
detectors (S1 and S2) of time-of-flight system (TOF), sili- arrays(atthetopandatthemiddle)areusedtodetermine
constripcoordinatedetectorCD1(pitch0.1mm),scintilla- the particle charge.
tion detectors S3 and S4, silicon arrays (silicon pad Using thick calorimeter ((cid:2)25X ) allows us to extend
0
detectors with 1(cid:3)1cm2 pixels), lateral detectors (LD) the energy range up to several TeV and to reach the
from the same Si arrays andtungsten planes, and calorim- energy resolution up to (cid:2)1% above 100GeV. The
eterfrom twoparts(CC1 andCC2).Theimagingcalorim- improvement in the angular resolution is achieved by
eter CC1 consists of 4 layers of double (x,y) silicon strip using CC1, which allows us to reconstruct the axis of
coordinate detectors (pitch 0.5mm) interleaved with tung- the cascade, together with the coordinates of the conver-
sten planes, and the electromagnetic calorimeter CC2 con- sion point in multilayer converter. This method allows
sistsofBGOcrystals.Thetotalconverter-trackerthickness us to reach the superior angular resolution of (cid:2)0.01(cid:2)
is (cid:2)1X (X is the radiation length). The thickness of CC1 above 100GeV.
0 0
and CC2 is 3X and 22X , respectively. The total calorim- The calorimeter scheme together with additional data
0 0
eter thickness is 25X and 1.2k (k is nuclear interaction from other detectors provides proton rejection factor up
0 0 0
length) in the vertical direction and 70X and 3.5k in the to(cid:2)106.Toincreasetheinstrumentefficiencyathighener-
0 0
lateral direction. giesandtoreducethedeadtimeofthetelescopeduetothe
Table1showsacomparisonofbasicparametersofspace- backsplashparticlesweusethetemporalandsegmentation
basedandground-basedinstruments:EGRET(Thompson methods.
et al., 1993), AGILE (Tavani et al., 2009), Fermi (Atwood
etal.,2009),CALET(Toriietal.,2008),H.E.S.S.(Aharonian 3. Spacecraft
et al., 2007), MAGIC (Aleksic´ et al., 2010), VERITAS
(Weekes et al., 2010), and CTA (The CTA Consortium, The GAMMA-400 space observatory will be installed
2010).Asseenfromthetable,GAMMA-400willhavesupe- on the Navigator space service platform produced by
riorangularandenergyresolutions. Lavochkin Research and Production Association. Two
variants of orbit are possible: Lagrange point L and
2
2.2. Particle detection high-elliptical orbit. The initial high-elliptical orbital
parameters are: an apogee of 300 000km, a perigee of
The gamma rays are detected through the conversion 500km, and an inclination of 51.8(cid:2). The orbit period will
into the electron-positron pairs in the converter-tracker. be 7days. After approximately 230days GAMMA-400
The time-of-flight system, where detectors S1 and S2 are will leave the Earth’s radiation belts and the orbit will
separated by approximately 500mm, determines the direc- changefromhighlyellipticaltoapproximatelycircularwith
tion of the arriving particle. Silicon strip coordinate detec- median altitude of (cid:2)150000km.
tor together with the anticoincidence detectors located at
front and sides of the converter-tracker helps to identify (cid:4) We are planning to use three basic modes of
gamma rays. The electromagnetic cascade initiated by the observations:
electron-positron pair develops in CC1 and CC2 parts of (cid:4) All-sky gamma-ray monitoring in order to search for
the calorimeter. Additional scintillation detectors S3 and new sources and to monitor the discovered variable
S4 can detect cascade particles. sources;
When measuring from the top-down direction, we use (cid:4) Long-term monitoring of selected point sources;
thetwomaintriggeringsystems:(i)forgammaraysifthere (cid:4) Observations of the GeV emission from gamma-ray
is no AC signal, (ii) for electrons (positrons) and nuclei bursts and solar flares using a trigger from the
when the AC signal is present. KONUS-FG gamma-ray burst monitor. A specific
Electrons (positrons) and nuclei are also detected in the pointingcanalsobetriggeredbyotherspacecraftaswell
calorimeter when coming from the four lateral directions. as by ground-based telescopes.
Table1
Acomparisonofbasicparametersofspace-basedandground-basedinstruments.
Spaced-based Ground-based
EGRET AGILE Fermi CALET GAMMA- H.E.S.S. MAGIC VERITAS CTA
400
Energyrange,GeV 0.03–30 0.03–50 0.1– 10– 0.1–3000 >100 >50 >100 >10
300 10000
Angularresolution,deg 0.2 0.1 0.1 0.1 (cid:2)0.01 0.1 0.1 0.1 0.1
(Ec>100GeV) Ec(cid:2)0.5GeV Ec(cid:2)1GeV
Energyresolution,%(Ec>100GeV) 15 50 10 2 (cid:2)1 15 20 15 15
Ec(cid:2)0.5GeV Ec(cid:2)1GeV
300 A.M.Galperetal./AdvancesinSpaceResearch51(2013)297–300
4. Conclusion Dogiel, V.A., Fradkin, M.I., Kurnosova, L.V., et al. Some tasks of
observationalgamma-rayastronomyintheenergyrange5–400GeV.
SpaceScienceRev.49,215–226,1988.
At present, we consider a possibility to extend the
Galper,A.M.,Aptekar,R.L.,Arkhangelskaya,I.V.,etal.Thepossibilities
GAMMA-400 energy range down to approximately of simultaneous detection of gamma rays, cosmic-ray electrons and
30MeV. The launch of the GAMMA-400 space observa- positronson the GAMMA-400 spaceobservatory.Astrophys.Space
tory is planned in 2018. The expected mission duration is Sci.Trans.7,75–78,2011a.
Galper,A.M.,Aptekar,R.L.,Arkhangelskaya,I.V.,etal.GAMMA-400
longer than 7years.
spaceobservatory.NuovoCimento34C,71–75,2011b.
Galper,A.M.,Borisov,S.V.,Zverev,V.G.,etal.Methodforreconstructing
Acknowledgements thegamma-rayarrivaldirectionintheconverter+calorimetersystem.
BulletinoftheLebedevPhysicsInstitute38(7),191–197,2011c.
Ginzburg, V., Kaplin, V., Karakash, A., et al. Development of the
This work was supported by Space Council of the
GAMMA-400 gamma-ray telescope to record cosmic gamma rays
RussianAcademyofSciencesandtheRussianSpaceAgency. withenergiesupto1TeV.Cos.Res.45,449–451,2007.
Ginzburg, V., Kaplin, V., Runtso, M., et al. Advanced GAMMA-400
Gamma-Ray Telescope for Recording Cosmic Gamma Rays with
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