Michael Kachelrieß NTNU, Trondheimweb.phys.ntnu.no/~mika/nbi14.pdf · Introduction Outline of the talk 1 Introduction 2 IceCube events implications 3 Astrophysical sources point

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Astrophysical neutrinos

Michael Kachelrieß

NTNU, Trondheim

Introduction

Outline of the talk

1 Introduction

2 IceCube events

◮ implications

3 Astrophysical sources

◮ point sources versus diffuse flux

◮ Galactic sources versus extragalactic

4 PeV dark matter

5 Summary

Michael Kachelrieß (NTNU Trondheim) Astrophysical neutrinos NBI 2014 2 / 31

Introduction

Outline of the talk

1 Introduction

2 IceCube events

◮ implications

◮ or better speculations. . .




4 PeV dark matter

5 Summary


Introduction

Outline of the talk

1 Introduction

2 IceCube events

◮ implications





4 PeV dark matter

5 Summary


Introduction

Outline of the talk

1 Introduction

2 IceCube events

◮ implications





4 PeV dark matter

5 Summary


Introduction

Outline of the talk

1 Introduction

2 IceCube events

◮ implications





4 PeV dark matter

5 Summary


Introduction

The CR–γ–ν connection:

HE neutrinos and photons are unavoidable byproducts of HECRs

astrophysical models, cosmogenic flux:◮ ratio Iν/Ip determined by nuclear composition of UHECRs and source

evolution◮ ratio Eν/Eγ determined by isospin


Introduction





astrophysical models, direct flux:◮ strongly model dependent fluxes: unknown target density, . . .


Introduction






top-down DM models:◮ large fluxes with Iν ≫ Ip

◮ ratio Iν/Ip fixed by fragmentation


Introduction






top-down DM models:◮ large fluxes with Iν ≫ Ip

◮ ratio Iν/Ip fixed by fragmentation

prizes to win:◮ astronomy above 100 TeV◮ identification of CR sources◮ determination galactic–extragalactic transition of CRs◮ test/discover new particle physics


Introduction

What is the bonus of HE neutrino astronomy?astronomy with VHE photons restricted to few Mpc:

10

12

14

16

18

20

22

Gpc100Mpc10MpcMpc100kpc10kpckpc

log1

0(E

/eV

)

photon horizon γγ → e+e− CMB

IR

radio


Introduction

What is the bonus of HE neutrino astronomy?astronomy with VHE photons restricted to few Mpc:

10

12

14

16

18

20

22


log1

0(E

/eV

)


IR

radio

ambiguity: leptonic/hadronic origin


Introduction

HE neutrino astronomy vs UHECRs?

10

12

14

16

18

20

22


log1

0(E

/eV

)proton horizon


IR

Virgo ⇓


Introduction

HE neutrino astronomy vs UHECRs?

10

12

14

16

18

20

22


log1

0(E

/eV

)proton horizon


IR

Virgo ⇓

◮ large statistics of UHECRs, well-suited horizon scale

◮ but no conclusive evidence that qB is small enough


Introduction

What is the bonus of HE neutrino astronomy?Neutrino astronomy:

large λν but also “large” uncertainty 〈δϑ〉 >∼ 0.1◦ − 1◦


Introduction



small event numbers: <∼ 1/yr for PAO or ICECUBE

103

102

10

1

10-1

1022102110201019101810171016

j(E)

E2 [e

V c

m-2

s-1

sr-1

]

E [eV]

WB

max

0.2

CR flux

⇒ identification of steady sources challenging


Introduction



small event numbers: <∼ 1/yr for PAO or ICECUBE

103

102

10

1

10-1

1022102110201019101810171016

j(E)

E2 [e

V c

m-2

s-1

sr-1

]

E [eV]

WB

max

0.2

CR flux

⇒ identification of steady sources challenging

correlation with AGN flares, GRBs

which AGNs? GeV/TeV photon sources?


Icecube events

Icecube: 2 events presented at Neutrino 20122 cascade events close to Emin = 1015 eV, bg = 0.14

Two events passed the selection criteria

8

Run119316-Event36556705 Jan 3rd 2012 NPE 9.628x104

Number of Optical Sensors 312

Run118545-Event63733662 August 9th 2011 NPE 6.9928x104

Number of Optical Sensors 354

CC/NC interactions in the detector

MC

2 events / 672.7 days - background (atm. m + conventional atm. n) expectation 0.14 events

preliminary p-value: 0.0094 (2.36s)


Icecube events

Icecube: prompt neutrino analysis [A. Schukraft, NOW2012 ]

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Icecube events


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Icecube events


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Icecube events

IceCube events


Icecube events

IceCube events: specifications for candidate sources

28 events with ∼ 10 bg: flukes are possible. . .

flux is large, close to◮ Waxman-Bahcall estimate◮ cascade limit


Icecube events




anisotropies◮ event cluster around GC, enhancement close to Galactic plane?⇒ mainly Galactic origin


Icecube events





CR energies Ep ∼ 20Eν ⇒ few×1016 eV◮ high for Galactic CRs◮ lowish for cosmogenic, AGN, GRB


Icecube events





CR energies Ep ∼ 20Eν ⇒ few×1016 eV◮ high for Galactic CRs◮ lowish for cosmogenic, AGN, GRB

flavor ratio consistent with 1:1:1


Astrophysical sources

Astrophysical sources of high-energy neutrinos

Galactic sources:

Galactic plane and bulge

SNR

Sun

hypernova, GRB

micro-quasar

. . .

Extragalactic sources:

diffuse flux from normal/starburst galaxies

cosmogenic neutrinos

diffuse flux from AGN

GRB

single AGN


Astrophysical sources Galactic point sources

Galactic CRs: KASCADE-Grande 2013

primary energy E/eV

1510

1610 1710

1810

)1

.5 e

V-1

s-1

sr

-2 / (

m2

.5 E

dif

f. f

lux

dJ

/dE

·

1510

1610

1710

Akeno (J.Phys.G18(1992)423)AGASA (ICRC 2003)HiResI (PRL100(2008)101101)HiResII (PRL100(2008)101101)AUGER (arXiv:1107:4809)AUGER AMIGA infill (ICRC 2011)

EAS-TOP (Astrop.Phys.10(1999)1)Tibet-III, QGSJET 01 (ApJ678(2008)1165)GAMMA (ICRC 2011)IceTop (arXiv:1202.3039v1)TUNKA-133 (ICRC 2011)Yakutsk (NewJ.Phys11(2008)065008)KASCADE-Grande, QGSJET II (Astrop.Phys.36(2012)183)

KASCADE-Grande, all-part., QGSJET II (this work)KASCADE-Grande, light (p), QGSJET II (this work)KASCADE-Grande, medium (He+C+Si), QGSJET II (this work)KASCADE-Grande, heavy (Fe), QGSJET II (this work)

KASCADE, all-part., QGSJET II (see Appendix A)KASCADE, light (p), QGSJET II (see Appendix A)

KASCADE, medium (He+C+Si), QGSJET II (see Appendix A)KASCADE, heavy (Fe), QGSJET II (see Appendix A)



Galactic sources

at low energies:

◮ many sources, large confinement times



Galactic sources

at low energies:


⇒ average CR sea plus few recent sources



Galactic sources

at low energies:



close to the knee:

◮ CRs in PeV range spread fast

◮ few extreme sources



Galactic sources

at low energies:



close to the knee:

◮ CRs in PeV range spread fast

◮ few extreme sources

⇒ inhomogenous CR sea, extended sources

⇒ no clear distinction between point sourcesvs. Galactic bulge + plane cases



E = 100 TeV → 1 PeV → 10 PeV t = 500 yr ↓ 2000 yr ↓ 7000 yr

S S S

S S S

S S

0 0.2 0.4 0.6 0.8 1

S



Point source in gamma-ray

source HESS J1825-137 [Neronov, Semikoz, Tchernin ’13 ]

0.00100

0.00150

0.00200

0.00250

0.00300

0.00350

0.00400

0.00450

0.00500

0.00550

0.00600

180.000225.000270.000315.000 0.00045.00090.000135.000

-90.000

-60.000

-30.000

0.00

0

30.000

60.000

90.000

Kookaburra region

HESS J1632 region

Galactic Center

HESS J1825 region

Cygnus region

Vela region

Crab



Gamma-ray point sourcesflux from HESS J1825-137, GC and GP



(Isotropic) photon limits

101 102 103 104

Eγ [TeV]

10−10

10−9

10−8

10−7

10−6

10−5

10−4

E2J

γ[G

eVcm

−2

s−1

sr−

1]

8.5kpc

20kpc

30kpc

GRAPES-3

UMC

HEGRA

EAS-TOP

IC-40 (γ)

KASCADE

GAMMA

CASA-MIA

[Ahlers, Murase ’13 ]


Astrophysical sources CR sea interactions in bulge and plane

Galactic plane

gas is concentrated as n(z) ∼ n0 exp[−(z|/z12)2] with z12 ∼ 0.2 kpc

n0 decreases with ρ – events at GAC?



Column density of gas

[Evoli, Grasso, Maccione ’07 ]



Diffuse ν flux from Galactic plane

[Evoli, Grasso, Maccione ’07 ]

averaged over 1,2,5 degrees


Astrophysical sources Diffuse extragalactic flux

Diffuse ν flux from normal and starburst galaxies

103

105

107

109

1011

10−9

10−8

10−7

10−6

10−5

Eν [GeV]

E2 ν Φ

ν [G

eV/c

m2 s

sr]

0.1 km2

1 km2

WB Bound

Star Bursts

AMANDA( νµ); Baikal(νe)

Atmospheric→← GZK

[Loeb, Waxman ’06 ]


Astrophysical sources Diffuse extragalactic flux

Diffuse ν flux from normal and starburst galaxies

103

105

107

109

1011

10−9

10−8

10−7

10−6

10−5

Eν [GeV]

E2 ν Φ

ν [G

eV/c

m2 s

sr]

0.1 km2

1 km2

WB Bound

Star Bursts

AMANDA( νµ); Baikal(νe)

Atmospheric→← GZK

[Loeb, Waxman ’06 ]

too optimistic?◮ fraction of starbust galaxies?◮ all calorimetric?


Astrophysical sources Cosmogenic neutrinos

Reminder: The photon horizon

10

12

14

16

18

20

22


log1

0(E

/eV

)


IR

radio


Astrophysical sources Cascade spectrum

Development of the elmag. cascade:



Development of the elmag. cascade:

analytical estimate: [Strong ’74, Berezinsky, Smirnov ’75 ]

Jγ(E) =

K(E/εX)−3/2 at E ≤ εX

K(E/εX)−2 at εX ≤ E ≤ εa

0 at E > εa

three regimes:◮ Thomson cooling:

Eγ =4

3

εbbE2

e

m2e

≈ 100 MeV

(

Ee

1TeV

)2

◮ plateau region: ICS Eγ ∼ Ee

◮ above pair-creation threshold smin = 4Eγεbb = 4m2

e:

flux exponentially suppressed



Fermi limit for cosmogenic neutrinos: [Berezinsky et al. ’10, Ahlers et al. ’10,. . . ]

E, eV1810 1910 2010 2110

-1st

er-1

sec

-2m2

J(E

) eV

3E

2310

2410

2510eV; m=021=10

max=2; Emaxz

HiRes II HiRes I

p

iνΣ

2.7

2.0

2.7

2.0

2.0

2.7



Fermi limit for cosmogenic neutrinos: [Berezinsky et al. ’10, . . . ]

0 1 2 3 4 5 610-8

10-7

10-6

10-5

10-4

cas(m

), eV

/cm

3 5

5

6

6

4

4

2

m

5.8x10-7

Emax=1021eV

2

g=2.6g=2.0

n(z)L(z) ∝ (1 + z)m , zmax



Fermi limit for cosmogenic neutrinos: [Berezinsky et al. ’10, . . . ]

1016 1017 1018 1019 1020 1021 102210-1

100

101

102

103

104

105

106

1021

1020

IceCube 5yr tilted

2.0

RICE

Auger diff.

E-2 cascade

ANITA

E2 J(

E), e

Vcm

-2s-1

sr-1

E, eV

ANITA-liteAuger

2.6

nadirJEM-EUSOBAIKAL

e =

1022

m=3


Astrophysical sources Gamma-Ray Burst

IceCube limit on GRBs

215 optically detected GRBs stacked


Astrophysical sources Gamma-Ray Burst

IceCube limit on GRBs

215 optically detected GRBs stacked

10

4

10

5

10

6

10

7

Neutrino Energy (GeV)

10

-9

10

-8

E

2

Φ

ν

(GeV cm

−2

s

−1

sr

−1

)

Waxman & BahcallIC40 limitIC40 Guetta et al.IC40+59 Combined limitIC40+59 Guetta et al.

10

-1

10

0

E

2

F

ν

(GeV cm

−2

)


Astrophysical sources AGN

Flux from a single AGN: Cen A+ 2 events correlated with Cen A within 3.1◦

+ more events close-by [Gorbunov et al. ’07, Fargione ’08, Rachen ’08 ]

+ general correlation with AGN



Flux from a single AGN: Cen A+ 2 events correlated with Cen A within 3.1◦

+ more events close-by [Gorbunov et al. ’07, Fargione ’08, Rachen ’08 ]

+ general correlation with AGN

− confusion with LSS?− no confirmation by HiRes− tension to PAO chemical composition− Emax for most AGN (incl. Cen A) high enough?



Acceleration close to the core: α = 2

initial protonsfinal protons

totalneutrinosγ

γ

HESS

FERMI

PAO

8 10 12 14 16 18 2014

15

16

17

18

19

log10(E/eV)

log10

(E2 Φ

/eV km

-2 yr-1 )



Acceleration close to the core: α = 2

initial protonsfinal protons

totalneutrinosγ

γ

HESS

FERMI

PAO

8 10 12 14 16 18 2014

15

16

17

18

19

log10(E/eV)

log10

(E2 Φ

/eV km

-2 yr-1 )

compatible with HESS and Fermi

GeV emission may be of e/m origin(electron synchrotron/ICS)



Diffuse flux from AGN - normalized to Cen A

assume Cen A is a “typical source” with injection spectrum j(E)

diffuse flux from all Cen A-like sources

Φdiff(E) =cn0

4π

∫

∞

0

dz

∣

∣

∣

∣

dt

dz

∣

∣

∣

∣

dE0(E, z)

dEε(z)j(E0) ,

enhancement between O(10) (no evolution) and O(100) (strongevolution) [Koers, Tinyakov (’08) ]

Halzen, O’Murchadha (’08): all FR-I radio galaxies: 5 events/yr






Φdiff(E) =cn0

4π

∫

∞

0

dz

∣

∣

∣

∣

dt

dz

∣

∣

∣

∣

dE0(E, z)

dEε(z)j(E0) ,








Φdiff(E) =cn0

4π

∫

∞

0

dz

∣

∣

∣

∣

dt

dz

∣

∣

∣

∣

dE0(E, z)

dEε(z)j(E0) ,




PeV dark matter

Signatures of SHDM decays

flat spectra dE/E1.9 up to mX/2

E3J(E

)/m

−2s−

1eV

2

E/eV

1e+23

1e+24

1e+25

1e+26

1e+18 1e+19 1e+20 1e+21


PeV dark matter



composition: γ/p ≫ 1, large neutrino fluxes, no nuclei

threshold energy [eV]

1910 2010

ph

oto

n f

ract

ion

−210

−110

1

threshold energy [eV]

1910 2010

phot

on fr

actio

n

−210

−110

1

SHDM

SHDM’

TD

Z Burst

GZK

HP HP

A1

A1 A2

AY

Y

Y

Auger SD

Auger SD

Auger SD

Auger HYB


PeV dark matter



composition: γ/p ≫ 1, large neutrino fluxes, no nuclei

galactic anisotropy:

0 20 401

10

NFW

1020 eV 6x1019 eV 3x1019 eV 1019 ev


PeV dark matter

PeV dark matter

DM ® ΝeΝ e H15%L, bb H85%L

DM ® ΝeΝ e H12%L, cc H88%L

DM ® e-e+ H40%L, qq H60%L

1 10 102 103

10-11

10-10

EΝ HTeVL

EΝ2 dJ�d

EΝHT

eVcm-

2s-

1sr-

1 L

[Esmaili, Serpico ’13 ]


PeV dark matter

PeV dark matter

102 103

0.1

1

10

EΝ HTeVL

even

ts�b

in

DM ® ΝΝ , qqE-2 spec.

data

[Esmaili, Serpico ’13 ]


PeV dark matter

Summary

1 excess towards GC, consistent with γ-ray data

⇒ at least partly Galactic origin

2 enhancement towards Galactic plane:

◮ gas too narrow, flux too low

3 some tension with (Northern) γ-ray limits

4 extragalactic: (only additional?) isotropic component,diffuse, difficult to identify

5 PeV dark matter: angular distibution follows DM profile


PeV dark matter

Summary









PeV dark matter

Summary









PeV dark matter

Summary









PeV dark matter

Summary









PeV dark matter

Summary









Documents

Michael Kachelrieß NTNU, Trondheimweb.phys.ntnu.no/~mika/nbi14.pdf · Introduction Outline of the talk 1 Introduction 2 IceCube events implications 3 Astrophysical sources point