Cosmological Magnetic Fields Angela V. Olinto University of Chicago.

Cosmological Magnetic Fields

Angela V. Olinto

University of Chicago

Cosmological Fields?

Were there Magnetic Fields before recombination?



If yes:

how were primordial Magnetic fields created?

What role have they played since?



If yes: how were primordial Magnetic fields

created? PHASE TRANSITIONS

What role have they played since?Star FormationSeed DynamosStructure Formation…



How would we know?

Were there Magnetic Fields before galaxies formed?

Lyman- forest - intermediate scales

Are there large scale Magnetic Fields today?

Extra Galactic Magnetic Fields

Constraints from Faraday Rotation to distant Quasars in an Inhomogeneous Universe (Burles, Blasi, A.O. ‘98)

variance increases - non-gaussian tail

Median| from z = 0 to 2.5, bh2 = 0.02

BHubble 10-9 G (Ly- forest)

BHubble 2 10-8 G (homogeneous)

B50Mpc 6 10-9 G (Ly- forest)

B50Mpc 10-7 G (homogeneous)

BJ 10-8 G (Ly- forest)

BJ 10-6 G (homogeneous)


Where there Magnetic Fields before recombination?

How would we know?

Were there Magnetic Fields before galaxies formed?

Lyman- forest - intermediate scales




How would we know?


Yes - in clusters of galaxies (M ~ 1015 Msolar )B can reach 10-6 Gauss (Kronberg et al)

equi-partition with gas dynamics

What about in emptier regions?

EHE Cosmic Rays should point!

after S. Swordy

B

pRgyro = 0.11 Mpc E20/ZBG

1kpc

B<10 nGR>11 Mpc

EHE Cosmic Rays should point!

Magnetic Fields less effective at EHEs (~ 1020 eV):

Simulations CDM LSS + MFs BExtraGal ~ <10 nG D. Grasso (ICRC03)

AGASA clusters constraints Bgal

G. Medina-Tanco (ICRC03)

Isola, Lemoine, Sigl ‘02

Presented 3 oral + 2 posters:

11 Super-GZK events

Small Scale Clustering

Constraints on Composition

- protons at UHEs.

AGASAAkeno Giant Air Shower

Array

111 scintillators + 27 muon det.

AGASA

Composition: K. Shinozaki et al. ICRC03

Muon density E0 ≥1019eV ≤36º

Fe frac. (@90% CL): < 35% (1019 –1019.5 eV), < 76% (E>1019.5eV)

Akeno 1km2 : Hayashida et al. ’95

Haverah Park: Ave et al. ’03

Volcano Ranch: Dova et al. ICRC03

HiRes: Archbold et al. ICRC03 AGASA

Gamma-ray fraction upper limits (@90%CL)

34% (>1019eV) (/p<0.45)

56% (>1019.5eV) (/p<1.27)

AGASA

Small Scale Clustering M. Teshima et al. ICRC03

1 triplet + 6 doublets (2 triplets + 6 doublets with looser cut)

Clustering for E ~1019eV and ~5x1019eV,

Ratio of Cluster/All increases with E up to 5x1019eV

Above GZK energy (5x1019eV) statistics too small

No significant time self-correlation

Angular Correlations

Log E>19.6Log E>19.4

Log E>19.2Log E>19.0

2D-Correlation Map in (ΔlII ,ΔbII )

Log E >19.0eV, 3. 4σ Log E >19.2eV, 3. 0σ

Log E >19.4eV, 2.0σ Log E >19.6eV, 4.4σΔΔllIIII

ΔΔbbIIII

Polarizationstudies will limit B gal and B Xgal

Polarization

Energy spectrum of Cluster eventsE -1.8±0.5

Cluster Component

AGASA

11 events with E > 1020 eV M. Takeda et al. ICRC03

AGASA systematic errors ~ 18%

QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.

Flu

x *

E3

The High Resolution Fly’s Eye (HiRes)

Air fluorescence detectors HiRes 1 - 21 mirrors HiRes 2 - 42 mirrors Dugway (Utah) start ‘97HR1 ‘99HR2

Pioneers of Fluorescence Technique (8 oral + 4 posters)

No Super-GZK flux

No Small Scale Clustering

Composition ChangeHiRes 2HiRes 1

Thanks to D. Bergman

Systematic off-set

systematic errorsin by hand…

•30% in order to reconcile low energy data (1018.5-1019.5

eV)

•15% within limits allowed by both collaborations

AGASA -15% HiRes +15%

best fit slope: 2.6number of events above 1020eV:

no GZK @ 1.5 sigmanumber of events above 1020eV:

GZK cutoff

DDM, Blasi, Olinto 2003DDM, Blasi, Olinto 2003

DeMarco et al (ICRC03)

HiRes

Composition: J. Mathews et al. ICRC03

HiRes Stereo: unchanging, light composition above 1018 eVStereo HiRes and HiRes Prototype-MIA consistent in overlap region

HiRes Prototype-MIA Hybrid changing composition (Heavy to Light) between 1017 and 1018 eV

No significant information near GZK region yetCome back to 29th ICRC

10 31

10 32

10 33

10 100 1000

Energy (in EeV)

Φ

(E)

× E3 (∝EeV-1cm-2s

-1sr-1)

no magnetic field

(with uniform sources from 10 to 1000 Mpc)

fully magnetized universe(B = 300 nG)

2 Mpc / 15 Mpc

5 Mpc / 30 Mpc

GZK cut-off is model and B dependent…

E. Parizot et al. ICRC03

Magnetized Local

Super-Cluster -

better fit to spectrum(Blasi, A.O. ‘99)

Are the sources Astrophysical or New Physics?

Super Heavy

Dark Matter Relics in the Dark Halo

of our Galaxy

Cosmic StringsPulsar,AGNBL Lacs - some correlation

Anisostropic UHECRs -BL-Lacs correlation

Accounting for deflection by Galactic MF correlation improves for charged +1 particles Tinyakov and Tkachev ’01b, 02

Time to get the Heavy Artillery

Auger & EUSO

DDM, Blasi, Olinto 2003

Auger South

EUSO


2 Giant AirShower Arrays

South – Argentina Funded North – Not Funded Yet

1600 particle detectors over 3000 km2

+ 4 Fluorescence Detectors

Will Measure Direction, Energy, & Composition of

~ 60 events/yr E > 1020eV~ 6000 events/yr E > 1019eV

> 250 scientists from 19 countries

J. Cronin and T. Yamamoto

QuickTime™ and aGIF decompressor

are needed to see this picture.

Pierre Auger Project3000 km2 - 1600 water tank array

Auger

South



130 tanks on +40 EA



Complete Calibration from Atmosphere to Telescope

LASERSLIDARSTelescope and Mirrors Calibs…

Fluorescence Telescopes



Inclined showerstop view in shower plane

Great Resource forAsymmetry of Showers M. T. Dova et al ICRC03

which lead to novel

Composition Studies M. Ave et al ICRC03

J. Cronin

Hybrid detector can reach 1018eV for Clustering studies

A. Kravtsov

Matter and Galaxies

N - Super Galactic PlaneS - see through Galactic Center

A. Kravtsov

Matter Distribution

Auger N and S can measure Large Scale Structure +Small Scale Clustering

Number of sources ~ 2(blue or red)

N 2 x N

Statistics improve by 2

Overlap region (purple)

L L/ 2 R 21/4 x R N 23/4 x N

P. Sommers ‘03

Gas + DMKravtsov, Klypin & Hoffman ‘01

Sigl, Miniati & Enßlin, ‘03

G 10 B 7 - obs =

observer position

UHECRs isotropization (?)

MAP OF DEFLECTIONSaround “Virgo” cluster

Preliminary results

Significant deflections are obtained only when UHECRs cross a rich cluster of galaxies at a distance < few Mpc’s

In the filaments, where

deflections in filaments are neglibible

MF strength around the local group is

UHECRs are not isotropized !!

100 10 )/( gas ÷≅ρδρ

G 10 B 8 - <

G 10 8 - <<

Dolag, Grasso et al 03

Concluding

UHECRs can map Magnetic Fields in Intergalactic Medium ( B ~ 1 - 10 nG) and the Galaxy (polarization).

Need complete simulations +

Better UHECR data

Watch for Auger S + N

MSPH simulations of MFs in rich clusters

MSPH (Magnetic-SPH) simulations implement the SPH (Smoothed Particle Hydrodynamics) strategy by adding MHD equations (Faraday equation) SPH:

N-BOBY SIMULATIONS of DM + GAS + MAGNETIC FIELDS Initial conditions ( z ~ 20) : density fluctuation field compatible with -CDM +

seed magnetic field

MAGNETIC FIELD AMPLIFICATION:

(frozen-in field)

+ non-linear MHD amplification due to the presence of shocks and turbulence

2/3 gas el B ρσ ∝⇒∞≅

Dolag, Bartelmann & Lesch, ‘99, ‘02

Predictions for -CDM

G 10 0.5 B : 12 -0 ×=low

G 10 2.5 B : 12 -0 ×=mediumG 10 1 B : 11 -

0 ×=highDolag, Baterlmann & Lesch ’02

G 10 1 B 10 5 11 - 0

13 - ×<<×

The memory of the initial MF geometrical structure is lost

They succeed to reproduce observations if

RMs

B(R)

Deflections induced by the smooth component of the cosmic MF:

G 10 B E

eV 10

Mpc 1

l

Mpc 1000

d Z0.25 11 -

0

192/1

C

2/1

o <⎟⎟⎠

⎞⎜⎜⎝

⎛⎟⎟⎠

⎞⎜⎜⎝

⎛⎟⎟⎠

⎞⎜⎜⎝

⎛<

This is consistent with the UHECRs – BL-Lacs correlation !

are below experimental sensitivity if Mpc 100 l C <

Probability to cross a rich cluster outside the LSC for a CR coming from d < 1000 Mpc: 0.1 P cross <

Deflections have to be dominated by EGMF in the local universe

It is consistent with hints of anisotropies in the UHECRs – BL-Lacs correlation

Constrained MSPH simulation of the LSC

The goal is to produce a realistic map of MF in the LSC

Initial conditions on density fluctuations are constrained so that the simulated smoothed density field is equal to that inferred from observations

Kolatt ’96Mathis et al. ‘01

dark matter only ( IRAS survey)

Conclusions

MSPH simulations account for observed EGMF in rich clusters without requiring a strong smooth component in the IGM

The “maximal” EGMF compatible with observations give rise to significant UHECR deflections only when they cross or skim clusterized regions

This is consistent with the claimed UHECR-BL Lacs correlation

MSPH constrained simulations will provide soon maps of UHECR deflections to be compared with data from high statistics experiments they will allow a more reliable source identificationprovide a deeper insight on the nature of cosmological magnetic fields

Preliminary results suggest that UHECR astronomy may be possible

The BL-Lacs – UHECR Connection

Small angle clustering: Very likely, sources of UHECR are pointlike !

● Correlation with -ray-loud BL-Lacs:

Tinyakov & Tkachev ’01a

5 - chance 10P <

4 - chance 10P <

Accounting for deflection by MF in the Galaxy correlation improves for charged +1 particles Tinyakov and Tkachev ’01b

Implications for the EGMF

AGASA angular resolution : 2.5 degd(z = 0.082) = 351 (70/h) Mpc E = 4.09 E 19 eV

2/1

C

10 -

l

kpc 100G 10 2 B ⎟⎟

⎠

⎞⎜⎜⎝

⎛×<

See also Berezinsky, Gazizov and Grigoreva ’02 Blasi & De Marco, ‘03 Tinyakov & Tkachev ’01c

AGASA multiplets

simulations withpoint sources

B=0 resol.=2.5º =2.6 m=0

E > 4 1019 eV - 57 events

10-5 Mpc-3

Blasi, DDM 2003, AP in press

AUGER multiplets E > 1020 eV - 70 events in 5 yrs

EUSO multiplets E > 1020 eV - 180-360 events in 3 yrs

10-5 sources/Mpc3 from AGASA Small Scale Anisotropy w/ large uncertainties. Auger & EUSO will greatly reduce the uncertainties.


HiRes

Small Scale Clustering - Monocular J. Belz et al. ICRC03

No significant clustering seen yet.“Bananas are harder than circles…”Flux upper limits of on point sources with E > 1018.5 eV Cygnus X-3 Dipole limit: Gal. Center, Centaurus A, M-87

HiRes-I Monocular Data, E > 1019.5 eV

HiRes-I Monocular Data, E > 1018.5 eV

Upper limit of 4 doublets (90% c.l.) in HiRes-I monocular dataset.

HiRes

Small Scale Clustering - Stereo C. Finley et al. ICRC03

No significant clustering seen yet.

Two-point correlation for HiRes Stereo Events

> 1019 eV

RMS fluctuations

Extra Galactic Magnetic Fields UHE CR + Gamma Rays

Secondary Photon spectrum modified by EGMFs via synchrotron losses of e+e- in EM cascade (Lee, A.O., Sigl ‘95)

BEG ~ 10-9 - 10-11 G

Extra Galactic Magnetic Fields & UHECRs

Monte Carlo for Propagation with EGMF Time Delay, Deflection Angle(Lemoine, A.O., Sigl, Schramm’97, Sigl, Lemoine, A.O.’97)

E ~ 20 yr (D/10Mpc)2 (E/10EeV)-2 (B/10-11 G)2 (lc/1 Mpc)

E ~ 0.02o (D/10Mpc)-1/2 (E/1yr)1/2

Need 10 events/cluster

Auger

Most Recent Exposures

Thanks to HiRes and AGASA Collaborations

Too Low Statistics for clear GZK or no-GZK determination

AGASA HiResEmax=1021.5 eV

number of events above 1020eV:no GZK @ 2.5 sigma

number of events above 1020eV:GZK cutoff

DDM, Blasi, Olinto 2003, AP in pressDDM, Blasi, Olinto 2003, AP in press


Cosmological Magnetic Fields Angela V. Olinto University of Chicago.

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