UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2...

26
UHECR Propaga-on + Related Physics UHECR Propaga-on Andrew Taylor Andrew Taylor

Transcript of UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2...

Page 1: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

UHECRPropaga-on+RelatedPhysics

UHECRPropaga-onAndrewTaylor

AndrewTaylor

Page 2: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

Page 3: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

CosmicRayInterac-onsInterac-ons

γN

R =2m2

N

E2N

Z1

✏2dN�

d✏

Z 4EN✏/mN

0kN�✏

0�N�(EN, ✏0)d✏0

3

p

Page 4: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

Page 5: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

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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

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MCMCResultsTable

Hardspectrapreferredforsourceevolu-onfollowingthatoftheSFR

FlaUerspectrapreferredfornega-vesourceevolu-on

7

Similarconclusionarrivestobyothers(eg.ADDREF.TOKAMPERTETAL.)

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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)

Page 9: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

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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

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TheOriginofProtonsAbovetheSecondKnee

11

Note-IGRBcontribu-onfromcascadelossesratherindependentofsourcespectra

SFRevolu-onscenario noevolu-onscenario

Liuetal.2016(1603.03223)

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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

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13

TheOriginofProtonsBelowtheAnkleSourcesat120Mpc

Ifonly1%ofEGBcomesfromsub-ankleUHECR(presentlimitis14%),wewillbeforcedtolookextremelylocallyfortheirsources

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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

Page 15: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

Page 16: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

Page 17: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

Page 18: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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!

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ExtraSlides

UHECRPropaga-onAndrewTaylor

Page 20: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

AnAlterna-veInterpreta-onoftheNega-veSourceEvolu-onResult

Athighenergies,thenega-veevolu-onscenarioshelpresolveboth:•  “hardspectrum”•  “IGRBover-produc-on”problems.Alterna-vely,thesescenariosmaysimplybeencapsula-ngthefactthatwe’vealocaldominantsourceandourlocalvalueforUHECRiswellabovethe“sealevel”!

20

Page 21: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

150 pcs 50 pcs

Galac-cCenterPevatron

UHECRPropaga-onAndrewTaylor

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HighSpectralPeakedBlazarEvolu-on

Fromastro-ph/1310.0006(Ajelloetal.2014)

• Reminder:Blazar->BLLac(FR1)->HSP• SupportsideathatFSRQ(gasaccre-ng)AGNevolveintoBLLac(gasstarved)AGN

n=-6evolu-onresult

ArchetypalHSPexampleMrk501

22

Page 23: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

Page 24: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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

Page 25: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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)

Page 26: UHECR Propaga-on + Related Physics · Cosmic Ray Interac-ons Interac-ons p γ R = 2m2 p E2 p Z 1 2 dN d Z 4E p /mp 0 k p 0 p (E p, 0)d 0 2 e+ e- π Most important energy losses

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