UHECRPropaga-on+RelatedPhysics
UHECRPropaga-onAndrewTaylor
AndrewTaylor
CosmicRayInterac-onsInterac-ons
p γ
R =2m2
p
E2p
Z1
✏2dN�
d✏
Z 4Ep✏/mp
0kp�✏
0�p�(Ep, ✏0)d✏0
2
e+e+
e-
π
Mostimportantenergylosses
CosmicRayInterac-onsInterac-ons
γN
R =2m2
N
E2N
Z1
✏2dN�
d✏
Z 4EN✏/mN
0kN�✏
0�N�(EN, ✏0)d✏0
3
p
Assump-onsonSourcePopula-on
dN
dVC/ (1+ z)n
EZ,max
= (Z/26)⇥EFe,max
dN
dE/ E�↵
exp[�E/EZ,max
]
z < zmax
n = �6, �3, 0, 3
4
Note-magne-cfieldhorizoneffectsareneglectedinthefollowing.Thisamountstoassuming:ie.thesourcedistribu-onmaybeapproximatedtobespa-allycon-nuous(alsonote,presenceoftHtermcomesfromtemporallycon-nuousassump-on)
ds < (ctH�scat)1/2
MCMCLikelihoodScan:Spectral+Composi-onFits
n=3evolu-onresult
L(fp, fHe, fN, fSi,Emax,↵) / exp(��2/2)
0.01
0.1
1
10
100
1000
17.5 18 18.5 19 19.5 20 20.5
E2 dN
/dE
[eV
cm-2
s-1
sr-1
]
log10 Energy [eV]
EFe, max=1020.2 eV
α=0.6
A=1-2A=3-6
A=7-19A=20-39A=40-56
650
700
750
800
850
17.5 18 18.5 19 19.5 20 20.5
<Xm
ax>
[g c
m-2
]
log10 Energy [eV]
protons
Iron
Auger 2014
10
20
30
40
50
60
70
80
17.5 18 18.5 19 19.5 20 20.5
RM
S(X m
ax) [
g cm
-2]
log10 Energy [eV]
protons
Iron
Auger 2014
5
MCMCLikelihoodScan:“SoE”SpectraSolu-ons
0.01
0.1
1
10
100
1000
17.5 18 18.5 19 19.5 20 20.5
E2 dN
/dE
[eV
cm-2
s-1
sr-1
]
log10 Energy [eV]
EFe, max=1020.5 eV
α=1.8
A=1-2A=3-6
A=7-19A=20-39A=40-56
!"#$
!%$$
!%#$
!&$$
!&#$
!'%(# !'& !'&(# !') !')(# !*$ !*$(#
+,-./0!12!3-4*5
672'$!89:;2<!1:=5!
>;7?79@
A;79
BC2:;!*$'D
!"#
!$#
!%#
!&#
!'#
!(#
!)#
!*#
!")+' !"* !"*+' !", !",+' !$# !$#+'
-./012345!67!82
9$:
;<7"#!=>?@7A!6?B:!
C@<D<>E
F@<>
GH7?@!$#"&
n=-6evolu-onresult
L(fp, fHe, fN, fSi,Emax,↵) / exp(��2/2)
6
MCMCResultsTable
Hardspectrapreferredforsourceevolu-onfollowingthatoftheSFR
FlaUerspectrapreferredfornega-vesourceevolu-on
7
Similarconclusionarrivestobyothers(eg.ADDREF.TOKAMPERTETAL.)
Secondary(Guaranteed)Gamma-RayFluxesFrom>1018.6eVUHECRComponent
0.01
0.1
1
10
100
1000
17.5 18 18.5 19 19.5 20 20.5
E2 dN
/dE
[eV
cm-2
s-1
sr-1
]
log10 Energy [eV]
EFe, max=1020.5 eV
α=1.8
A=1-2A=3-6
A=7-19A=20-39A=40-56
n=-6evolu-onresult
0.01
0.1
1
10
100
1000
17.5 18 18.5 19 19.5 20 20.5
E2 dN
/dE
[eV
cm-2
s-1
sr-1
]
log10 Energy [eV]
EFe, max=1020.2 eV
α=0.6
A=1-2A=3-6
A=7-19A=20-39A=40-56
n=3evolu-onresult
8
IGRB(EGBwithresolvedpointssourcesremoved)
107 108 109 1010 1011 1012 1013 1014
E [eV]
10�1
100
101
102
103
E2 J
[eV
cm�
2s�
1sr�
1 ]
Fermin = 0 / proton onlyn = 3 / mixedn = 0 / mixedn =�3 / mixedn =�6 / mixed
n=3to-6evolu-onscenariosgiverisetobetween40%and12%ofFermilimit
Tayloretal.2015(1505.06090)
0.01
0.1
1
10
100
1000
10000
17 17.5 18 18.5 19 19.5 20 20.5
EFe, max=1020.50eV
α=2.0
E2 dN
/dE
[eV
cm-2
s-1
sr-1
]
log10 Energy [eV]
A=1-2A=3-6
A=7-19A=20-39A=40-56
n=3to-6evolu-onscenariosgiverisetobetween100%and40%ofFermilimit
99
DominantSourceatSub-AnkleEnergies
TheIsotropicGamma-RayBackground
Lisan-etal.2016(1606.04101)Zechlinetal.2016(1605.04256)
dN
dS/ S�↵
I =
ZSdN
dSdS
Arepeatofthisanalysisbyothergroupshavegiven:68+9-8%and81+52-19%
Energy [MeV]210 310 410 510
]-1 s
r-1
s-2
dN
/dE
[MeV
cm
2 E
-610
-510
-410
-310
Total EGB
IGRB
°Resolved sources, |b|>20
IGRB - Abdo et al. 2010
10
UsingPhotonFluctua-onAnalysis,theFermicollabora-onpushedafactorof~10belowthe2FHLsensi-vity
Lat.Cut+Gal.ForegroundRemoval….+RemovalofRes.Blazars….+RemovalofUnres.Blazars
Blazarsexplainintotality86+16-14%ofthe>50GeVEGB
TheOriginofProtonsAbovetheSecondKnee
11
Note-IGRBcontribu-onfromcascadelossesratherindependentofsourcespectra
SFRevolu-onscenario noevolu-onscenario
Liuetal.2016(1603.03223)
S-llNon-Blazar&StarburstGalaxyContribu-onsNotRemoved
12
10-6
10-5
10-4
10-3
10-2
101 102 103 104 105 106
E2 d
N/d
E [
Me
V/c
m2/s
/sr]
Eγ [MeV]
1-σ Lr,core-Lγ and N1-σ Lr,core-Lγ and N (k=1)
Lr,core-Lγ best fitLr,core-Lγ best fit Cascade
Lr,core-Lγ best fit TotLr,tot-Lγ
Fermi IGRBFermi IGRB fit
Fermi IGRB
DiMauroetal.2013(1304.0908)
RadioGalaxycontribu-onsarees-matedtomakeupasignificantfrac-onoftheremainingIGRB.
Ackermannetal.2012(1206.1346)
Contribu-onfromlowerenergy(<10PeV)CRsinstarburstgalaxies
13
TheOriginofProtonsBelowtheAnkleSourcesat120Mpc
Ifonly1%ofEGBcomesfromsub-ankleUHECR(presentlimitis14%),wewillbeforcedtolookextremelylocallyfortheirsources
G(r, t) / e(�r2/(4Dt))
(4⇡Dt)3/2
Recallthatthediffusivepropagatoris
SteadyStateSpectrumFluxfromSourceis
n / 1/Dr
SourceofCosmicRaysBelowtheAnkle?
UHECRPropaga-onAndrewTaylorAbramowskietal.2016(1603.07730)
nCR
r
/ r�1
Particle Acceleration in Centers of Galaxies (within the Central Molecular Zone)
tacc = ⌘Rlar
c�2
Rlar =�
⌘RMaximumenergy
(Hillascriterion)
Rlar(E,B) =
✓E
1 PeV
◆✓100 µG
B
◆0.01 pc
Eichleretal.2016(1604.05721)Notehowever
tesc. =R2
⌘cRlar
AndrewTaylor
Diagram taken from Ferrari -1998
For
O’Sullivanetal2009(0903.1259)
2.8kpc
VLAMap
Preliminary
�scat. ⇡ 10�1
Emax
⇡ 1018eV
tacc ⇡ 0.1 Myr
Example Candidate Local Sources HESS-NewResultsfromCenA!
Bsc ⇡ 30 µG
RLar(1018eV p) ⇡ 30 pc
GW/EM170817asanEfficientAcceleratorWhatcanwelearnfromMWLmeasurements?
AbsenceofbreakinsynchrotronemissionspectrumuptoX-rayenergiesconstraint
Accelera-onwithinremnant-mescaleconstraint(tacc<100days)
B < 2 mG
…alterna-vely,synchrotronemilngelectronsmaybealways“fresh”,ortheinjec-onspectrumfromthesourcemaybeveryhardandtheelectronsobservedcooled
B > 0.02 mG
Rogriguesetal.2018(1806.01624)
10�8 10�4 100 104 108 1012 10161031
1033
1035
1037
1039
1041
1043
1045
E�dL
/dE
�(e
rgs�
1)
5 daysB = 30 mG H.E.S.S
10�8 10�4 100 104 108 1012 1016
E� (eV)
1031
1033
1035
1037
1039
1041
1043
1045
E�dL
/dE
�(e
rgs�
1)
110 daysB = 2 mG
Synchrotron (Emaxe = EX�ray
e )
Synchrotron (Emaxe = Esynch cuto↵
e )
Inverse Compton (Emaxe = EX�ray
e )
Inverse Compton (Emaxe = Esynch cuto↵
e )
Thermal component
10�8 10�4 100 104 108 1012 1016
E� (eV)
1031
1033
1035
1037
1039
1041
1043
1045
110 daysB = 10 G
InverseComptonsynchrotron
Kimuraetal.2018(1807.03290)
10�8 10�4 100 104 108 1012 1016
E� (eV)
1029
1031
1033
1035
1037
1039
1041
1043
1045
E�dL
/dE
�(e
rgs�
1)
5 daysH.E.S.S.
upper lim.
2 mG
10�8 10�4 100 104 108 1012 1016
E� (eV)
1029
1031
1033
1035
1037
1039
1041
1043
1045
110 days H.E.S.S.50 h
0.2mG
2 G
20 mG
Synchrotron Inverse Compton Thermal component Data
5 20 40 60 80 100
t (days)
1015
1016
1017
1018
1019
Em
ax
p(e
V)
Knee
Ankle2 G
20 mG
2 mG
Conclusions
• Anega-vesourceevolu-onallowsforanE-2typespectratoexplainCRabovetheankle(eg.theevolu-onobservedforHBLblazars)
• Theposi-veevolu-onofaseparatesourceclass,canaccountforsubAnkleextragalac-ccosmicrays(whichagainallowanE-2typespectraforthiscomponent)
• Anewes-ma-onofthediffusegamma-raybackgroundlimitexcludesposi-veevolu-onscenariosforthesesub-anklecosmicrays.
• Othersourcesofthediffusegamma-raybackgroundremaintoberemoved-
UHECRcanonlybeasmallcontributortothisbackground
• NewinputonthecandidatesforCRsourcesbelowtheanklearecomingfromrecentnon-thermalobserva-onsofthelocalUniverse!
18
ExtraSlides
UHECRPropaga-onAndrewTaylor
AnAlterna-veInterpreta-onoftheNega-veSourceEvolu-onResult
Athighenergies,thenega-veevolu-onscenarioshelpresolveboth:• “hardspectrum”• “IGRBover-produc-on”problems.Alterna-vely,thesescenariosmaysimplybeencapsula-ngthefactthatwe’vealocaldominantsourceandourlocalvalueforUHECRiswellabovethe“sealevel”!
20
150 pcs 50 pcs
Galac-cCenterPevatron
UHECRPropaga-onAndrewTaylor
HighSpectralPeakedBlazarEvolu-on
Fromastro-ph/1310.0006(Ajelloetal.2014)
• Reminder:Blazar->BLLac(FR1)->HSP• SupportsideathatFSRQ(gasaccre-ng)AGNevolveintoBLLac(gasstarved)AGN
n=-6evolu-onresult
ArchetypalHSPexampleMrk501
22
DoesaSeparateClassofExtragalac-cSourceDominateatSub-AnkleEnergies?
0.01
0.1
1
10
100
1000
10000
17 17.5 18 18.5 19 19.5 20 20.5
EFe, max=1020.50eV
α=2.0
E2 dN
/dE
[eV
cm-2
s-1
sr-1
]
log10 Energy [eV]
A=1-2A=3-6
A=7-19A=20-39A=40-56
Nega-veevolu-on(HSP)
Posi-veevolu-on(ISP+LSP)
23
AnkleEnergy
Binaryneutron-starmergers
• FirstproofthatBinaryNSmergersareprogenitorsofshortGRBs
• Jetemission– Internalshocksinjet→par-cleaccelera-on– HardX-rayandsougamma-rayproduc-on
– Timescalesof(0.1–2)seconds
• MergerEjecta-givesrisetolate-me(10-150day)non-thermalemission
Expectedelectromagne-cemission
(Baiok&Rezzolla2017,pre-GW170817)AndrewTaylor
How Far is the Nearest Source?
Silicon- L<60 Mpc
Iron- L<80 Mpc
Taylor et al. 2011 (1107.2055)
25
Fargion et al. 2015 (1412.1573)
AndrewTaylor
De Marco et al. 2006 (0603615)
Energy [TeV]4−10 3−10 2−10 1−10 1 10
]-1
s-2
[e
rg c
m2
E×Fl
ux
13−10
12−10
Fermi-LAT Pass 8
Fermi-LAT 3FGL
H.E.S.S. 2017
H.E.S.S. 2012
NGC 253: Gamma-Ray Spectrum
Docosmicrayprotonsdumpalltheirenergywithinthesource,oraresomefrac-onofthemabletoescape?
Gamma-Ray Spectral Coverage- very good energy information L�(GeV) ⇡ 1040 erg s�1
Couldbelargerscalediffuseemissionmissed
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