An observatory for gamma rays In the MeV/GeV domain h ps ... · =Tracker - Double sided Si strip detectors (DSSDs) for excellent spectral resolu on and ﬁne 3-D posi on resolu on

AlessandroDeAngelisINFN&INAFPadova,Univ.Udine,LIP/ISTLisboaPadova,February28,2017

AnobservatoryforgammaraysIntheMeV/GeVdomain

h�p://eastrogam.iaps.inaf.it

h�ps://arxiv.org/abs/1611.02232(Exp.Astronomy,inpress)

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TheMeV/GeVdomain

  Worstcoveredpartoftheelectromagne�cspectrum(onlyafewtensofsteadysourcesdetectedsofarbetween0.2and30MeV)

  Manyobjectshavetheirpeakemissivityinthisrange(GRBs,blazars,pulsars...)  Bindingenergiesofatomicnucleifallinthisrange,whichthereforeisasimportant

forHEastronomyasop�calastronomyisforphenomenarelatedtoatomicphysics

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SPI

IBIS-ISGRI

IBIS-PICsIT

JEM-X

COMPTEL

EGRET

CTA North

CTA South

Fermi-LAT

LHAASO

HiSCORE

MAGIC VERITAS

Energy (MeV)

Sens

itivi

ty (e

rg cm

-2 s-1

)

/HESS

Thislackofdatareflectesintouncertain�esintheglobalphotonflux

A.DeAngelis,1ste-ASTROGAMWorkshop,Padova3

4CTA Athena E-ELT JWST ALMA SKA

eLISA -- Gravitational waves

Km3Net/IceCube-Gen2 - νν

e-ASTROGAM

Coresciencemo�va�on(willbeexploredindetailduringthisworkshop)

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1.  ProcessesattheheartoftheextremeUniverse(AGNs,GRBs,microquasars):prospectsfortheAstronomyofthe2030s  Mul�-wavelength,mul�-messengercoverage

ofthesky(withCTA,SKA,eLISA,νdetectors...),withspecialfocusontransientphenomena

2.Theoriginofhigh-energypar�clesandimpactongalaxyevolu�on,fromcosmicraystoan�ma�er3.NucleosynthesisandthechemicalenrichmentofourGalaxy

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e-ASTROGAM

SPI

IBIS-ISGRI

IBIS-PICsIT

JEM-X

COMPTEL

EGRET

CTA North

CTA South

Fermi-LAT

LHAASO

HiSCORE

MAGIC VERITAS

Energy (MeV)

Sens

itivi

ty (e

rg cm

-2 s-1

)

e-ASTROGAMscien�ficrequirements(seeVincent)1.  Achieveasensi�vitybe�erthanthatofINTEGRAL/CGRO/COMPTELbyafactorof

20-50-100intherange0.2-30MeV2.  Fullyexploitgamma-raypolariza�onforbothtransientandsteadysources3.  Improvesignificantlytheangularresolu�on(toreach,e.g.,∼10’at1GeV)4.  Achieveaverylargefieldofview(∼2.5sr)⇒efficientmonitoringoftheγ-raysky5.  Enablesub-millisecondtriggerandalertcapabilityfortransients


  Tracker-DoublesidedSistripdetectors(DSSDs)forexcellentspectralresolu�onandfine3-Dposi�onresolu�on(1m2,500µmthick,0.3Xointotal)  Calorimeter -High-Zmaterialforanefficientabsorp�onofthesca�eredphoton⇒CsI(Tl)scin�lla�oncrystalsreadoutbySidri�detectorsorphotomul�pliersforbestenergyresolu�on.8cm(4.3Xo)  An�coincidencedetectortovetocharged-par�cleinducedbackground⇒plas�cscin�llatorsreadoutbySiphotomul�pliers

θ

γSilicon tracker

Scintillator calorimeter

Plastic anti-coincidence detector

γ

e+ e-

Pair event Compton event

HowtomeasuregammaraysintheMeV-GeV?

  BestPSFinMeV-GeV–  Resolvesources

  CalorimetricmeasurementsofMeVlineswithhighresolu�on:–  Positrondetec�on(511keVline)–  Measurementsofisotopiccontents,withhighestsensi�vity–  HadroniccollisionsofLECRwithmolecularclouds

  Capabilityofmeasuringpolariza�on(marksComptoninterac�onsatthesourcesandmagne�cfields)  SEDresolu�onintheMeV/GeVrange:allowsto

reconstructthe“pionbump”,characteris�cofthedecayπο -> γγ andthusanindicatorofhadronicprocesses

Keyinstrumentcharacteris�cs:asummary


PKS 2149-306 (z = 2.345)   Howdoestheaccre�ondisk/jettransi�onoccuraroundsupermassiveblackholesinAGN?

  AreBLLacssourcesofUHECRsandhigh-energyneutrinos?

  Launchofultra-rela�vis�cjetsinGRBs?Ejectacomposi�on,radia�onprocesses?

  Canshort-dura�onGRBsbeunequivocallyassociatedtogravita�onalwavesignals?

ü  Withitswidefieldofview,unprecedentedsensi�vityoveralargespectralband,andexcep�onalcapacityforpolarimetry,e-ASTROGAMwillgiveaccesstoavarietyofextremetransientphenomena

e-ASTROGAMcoresciencetopic#1


Rela�vis�cjets;flares


MeVblazars;cosmologyatzupto4.5


Gamma-raybursts;thenewAstronomy  Thresholdat30keVusingtheCalorimeter  200GRB/yeardetected

–  Localizedwithin0.1-1deg,andtheinforma�oncanbeprocessedonboard

–  42GRBs/yearwithadetectablepolariza�onfrac�onof20%

  Possibledetec�onofelectromagne�ccounterpartsofimpulsiveGWevents–  MeVlikelytobethethreshold(Patricellietal.2016)–  Possibleassocia�onsGRB/GW

  MeVgoodtargetalsoforthecounterpartsofneutrinobursts


  Whataretheenergydistribu�onsandfluxesofCRsproducedinsupernovaremnantsandpropaga�ngintheinterstellarmedium?

  Whatistheroleoflow-energyCRs?

  WhataretheoriginsoftheFermiBubblesandthe511keVemissionfromtheGalaxy’sbulge?

ü  e-ASTROGAMwillenableadetailedspectro-imagingofthevarioushigh-energycomponents,thankstoitssensi�vityandangularresolu�onintheMeV-GeVrangesignificantlyimprovedoverpreviousmissions

e-ASTROGAMcoresciencetopic#2

An�ma�erandDarkMa�er  Uniquesensi�vitytothe511-keVline  Sensi�vitytomanyclassicalpositronsources:canconstrainthe

contribu�onfromnearbypulsarsinthepositronexcessseenbyPAMELA/AMS-02

  TheMeVregionisthemissingingredienttodeterminethephotonbackgroundfromtheInnerGalaxy:clarifyifthereisaphotonexcess(whichmightbeduetoDM,newpar�cles)

  TheMeVregioniswherethebulkofphotonsfromWIMPsbelow100GeVisexpected

  Insomemodels,MeVdarkma�er–  PlusAxions,ALPs:

  Sensi�vitytophotonsemi�edbySNe(Meyeretal.2016)  Sensi�vitytophoton/ALPoscilla�ons(Roncadellietal.2011;Hooperetal.2009)


0 50 100 150 2000

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0 50 100 150 200Time past explosion [days]

0

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56C

o 12

38 k

eV li

ne fl

ux [1

0−4 p

h cm

−2 s

−1] W7 (Chandrasekhar−Deflagration)

He−DetonationMerger DetonationPulsating Delayed DetonationSuperluminous He−DetonationSPI DataSPI Exposure

e-ASTROGAM

SN 2014J

847

  Howdothermonuclearandcore-collapseSNeexplode?Howarecosmicisotopescreatedinstarsanddistributedintheinterstellarmedium?

missions,e-ASTROGAMshouldallowustofinallyunderstandtheprogenitorsystem(s)andexplosionmechanism(s)ofTypeIaSNe(56Ni,56Co),thedynamicsofcorecollapseinmassivestarexplosions(56Co,57Co),andthehistoryofrecentSNeintheMilkyWay(44Ti,60Fe...)

ü  Witharemarkableimprovementinγγ-raylinesensi�vityoverprevious

(adapted from Diehl et al. 2015)

e-ASTROGAMcoresciencetopic#3(today)


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e-ASTROGAM

3FGL catalog

Energy (MeV)

E2 × d

N/d

E (e

rg c

m-2

s-1)

  Over2/3ofthe3033sourcesfromthe3rdFermiLATCatalog(3FGL)havepower-lawspectra(Eγ>100MeV)steeperthanEγ

-2,implyingthattheirpeakenergyoutputisbelow100MeV

  Theseincludesabout1100(candidate)blazarsandmorethan720unassociatedsources

  Mostofthesesourceswillbedetectedbye-ASTROGAM⇒largediscoveryspacefornewsourcesandsourceclasses

e-ASTROGAMdiscoveryspace

  DiffuseGalac�cgamma-raybackground  Pulsarsandmillisecondpulsarsbothisolatedandinbinaries,

whose(pulsedorunpulsed)emissionwillbeobservableinaspectralrangerichininforma�ontodiscriminatebetweendifferentpar�cleaccelera�onmodels

  PWNe,forwhiche-ASTROGAMwillobtaincrucialdataonpar�cleaccelera�onandpropaga�on

  Magnetars  Galac�ccompactbinaries,includingNSandBHswhose

spectraltransi�onsandoutburstswillbemonitored  Interstellarshocks  Propaga�onovercosmologicaldistances(LIV,ALPs,…)  Novae  Solarflaresandterrestrialgamma-rayflashes

e-ASTROGAMObservatoryscience


SolarSystemSupermassiveBlackHoles

RadioGalaxiesBlazarsFSRQs

BLLacs Other/Unknown RadioLobesCentralEngine

SgrA*

Uniden�fiedSolarFlares

Terrestrialγ-RayFlashes Gamma-RaySourceClassesGamma-RayBursts

Short

Long

MilkyWay

Superbubbles

MolecularClouds

Star-formingRegions

StellarObjects

Pulsars

>1000 sources expected with e-ASTROGAM

Magnetosphericemission

PulsarWindNebulae

StarburstGalaxies

BinarySystems

Novae

InterstellarMedium

SupernovaeCore-collapse

SupernovaRemnants

ThermonuclearGlobularClusters

SatelliteGalaxies

Magnetars

BlackHoleBinaries

NeutronStarbinaries

CollidingWindsGalaxy’sBulge

VincentTa�scheff GANIL 10February2017

~350collaboratorsfromins�tu�onsin19countrieswithanofficialendorsement

Thee-ASTROGAMCollabora�on


Thee-ASTROGAMCollabora�on(attheproposal�me)

INFN, INAF, U. Padova, U. & Polit. Bari, U. Roma Tor Vergata, U. Siena, U. Udine, U. Trieste

CSNSM, APC, CEA/Irfu, IPNO, LLR, CENBG, LUPM, IRAP

U. Mainz, KIT/IPE, U. Tübingen, U. Erlangen, RWTH Aachen, U. Potsdam, U. Würzburg, MPE

DPNC UniGe, ISDC, Univ. Geneva, PSI

ICE (CSIC-IEEC), IMB-CNM (CSIC), IFAE-BIST, Univ. Barcelona, CLPU & Univ. Salamanca

KTH and Univ. Stockholm

CzechTechnicalUniv.,Prague;University of Coimbra, LIP and IST Lisboa; Univ.Sofia

DTU Copenhagen

Univ. College Dublin, Dublin City Univ.

Space Research Center of PAS Warsaw

NASA GSFC, NRL, Clemson Univ., Washington Univ., Yale Univ., Univ. Maryland, UC Berkeley

Ioffe Institute, St. Petersburg

University of Tokyo

CBPF Rio de Janeiro

Principalinves�gator:AlessandroDeAngelis,INFN/INAFPadova,U.Udine,Italy;LIP/IST,PortugalCo-I:VincentTa�scheff–CSNSM(CNRS/IN2P3)Paris,France;Univ.ParisSud

Endorsementsfromna�onalagencies/delega�onstoESA

  ASI(Italy)  CNES(France)  DLR(Germany)  (Switzerland)  SwedishNa�onalSpaceBoard(Sweden)  Na�onalSpaceAgency/DTU(Denmark)  SpanishResearchAgency(Spain)  PolishSpaceAgency  FCT(Portugal)  NASA(US)


Theinterna�onalscenario

  TheAll-skyMediumEnergyGamma-rayObservatoryAMEGO,asimilarprojectfromNASA,startedevalua�oninDec2016  PIisJulieMcEnery,NASAGSFC(theoldFermiteam);severale-ASTROGAMcollaboratorsareco-I  Ifapproved,launchin2028


  Padova,Feb28(startat12h)/Mar1-2(endonMar2at14h)  Setupateamforawhitebook(withAMEGO?)  Contributedtalks&postersonmul�messengerastrophysics

Firste-ASTROGAMScienceWorkshop


Peopletocontacthereforanyques�ons(logis�cs,etc.)

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  SandraCALORE(secretary)

  ElenaPAVAN(secretary)

  LucaFOFFANO(scien�ficsecretary)

Whoneedsashu�letotheairportonThursdaya�ernoon?

Summary


  ThealmostunexploredMeV/GeVgamma-raybandisoneoftherichestenergydomainsofastrophysics

  e-ASTROGAMcanfillthegapandbeanessen�alobservatorytostudytheextremetransientskyintheeraofastronomy’snewmessengers

  Thee-ASTROGAMpayloadisinnova�veinmanyrespects,butthetechnologyisready

  WeshouldelaborateonthesciencewithafutureMeV/GeVinstrument,toreinforcethescien�ficcase.Whitebook!

Documents

An observatory for gamma rays In the MeV/GeV domain h ps ... · =Tracker - Double sided Si strip detectors (DSSDs) for excellent spectral resolu on and ﬁne 3-D posi on resolu on