venice “ telescopes”, feb 22-25 tom weiler, vanderbilt university high-energy cosmic ray/...

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Venice “ Telescopes”, Feb 22-25 Tom Weiler, Vanderbilt University High-Energy Cosmic Ray/ Observatories, and What They Can Do for Us Tom Weiler Vanderbilt University

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Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

High-Energy

Cosmic Ray/ Observatories,

and What They Can Do for Us

Tom Weiler

Vanderbilt University

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Cosmic Photon- Proton-Spectra

Rad

io

CM

B

Vis

ible

-ra

ys

CERN/Fermilab

x-ra

ysUV

IRCosmic-rays

TeV

-w

all

(after Ressell & Turner ‘90)

hadron wall?

no wall a’tall

sunSN87a

NeutrinoIncognito

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

The Sun thru SuperK eyes:

No dark glasses required

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

1991 Fly’s Eye reports 3x1020 eV, with proton-like profile;

Akeno/AGASA Xpt begins

 mid-90sDUMAND prototype ended; Baikal continues

 90s SuperK neutrinos from the sun (directional astro)

 1996 AGASA reports event clustering within 2.50 ang. res’n

and: F(E 1020 eV) ~ 1/km2/century,

with shower diameter ~ 5km, N(e) ~ 1011

 2000 20 events at and above 1020 eV

 2001 HiRes withdraws 7 events; AGASA adds 6 (from z > 45o);

And the controversy has begun!

Importantly, Auger gets first “light”

 2002 AMANDA pushes to 1014 eV thru-Earth neutrinos

2005 IceCube sees first muon

 2005 Auger Observatory data expected

 2008 Extreme Universe Space Observatory (EUSO) ?

Timeline

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

2012, a hundred years since Victor Hess

Auger data digested

IceCube data digested(neutrinos are calorie-free)

Anita data on cosmogenics

Nestor/Antares 100 GeV point sources

EUSO extends Auger

GZK are history!Neutrino sky-maps are available in textbooks;

But, there is no consensus theory in sight for neutrino mass and mixing

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

CR Spectrum above a TeV

from Tom Gaisser

VLHC(100 TeV)2

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Highest Energy Event

The CR record energy is 3x1020 eV (0.3 ZeV). Found by Fly’s Eye a decade ago (they got lucky!). This is truly a macroscopic energy: 3x1020 eV = 50 Joules 

equivalent to a Roger Clemens fastball,a Tiger Woods tee shot,a Pete Sampras tennis serve,Or a speeding bullet.

 

(Also to 12 Calories, which heats a gram of water by 12oC)

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

3 x1020 eV = macroscopic 50 Joules

Clemens does this with 1027 nucleons;Nature does this with one nucleon, 1027 times better pitcher !

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Fly’s Eye 3x1020 eV event (1992)

100 billion e+e- pairs at xmax ~ 800 g/cm2

This longitudinal profile is consistent with a primary proton, but less so with a primary photon; Disfavors “local” top-down sources such as massive Particle DK, topo-defects,Z-bursts, etc.

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

AGASA Spectrum: EeV to ZeV

AGASA, July 2002

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

UHECR Mysteries-- acceleration mechanism above 10^18 eV

-- bottom-up: few nearby candidates for p&A (50Mpc horizon)

-- top-downgammas (5Mpc horizon) and neutrinos (no horizon)

-- is there a GZK suppression? (AGASA vs HiRes)

-- is there directional clustering of events? (AGASA vs HiRes)

-- is the crossover to Xgal at 2nd knee (10^18eV), or ankle (~10^19eV) ?

Neurtrino co-emission an important tool !!

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Greisen-Zatsepin-Kuzmin and the Cosmic-Ray Wall

-resonance

multi-pions

Photo-pion production off CMB

p+cmb p/n+

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

HiRes vs. AGASA UHE spectrum

discovery

opportunity

GZK recovery ?Z-burst uncovery ?

FlysEye event goes here

Auger (EUSO) reach 70 (103) better

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Auger update – February05

-- 12 of 24 FD’s operational (50%)

-- 650 (of 1600) tank’s operational (40%)

-- 100,000 events within 60deg vertical

-- data set Jan04-Mar05 to publish at ICRC Aug05,

with AGASA-equivalent exposure

-- site inaugural celebration Nov05

-- all 24 FDs end of 05

-- all 1600 SDs July06

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Auger Rates

Auger Events/yr:

spectrum above 10^19 eV above 10^20 above 3 10^20 above 5 10^20 above 10^21

E -̂2 2000 200 70 40 20

E -̂2.7 2000 40 7 2 to 3 0.7

E -̂3 2000 20 2 0.8 0.2

EUSO comparison:

EUSO FOV ~ (230 km)2 ~ 70 (instantaneous)Auger FOV (30 km)2

x 15% EUSO duty cycle ~ 10 (averaged)

But EUSO energy threshold ~ n x 1019 eV, versus Auger threshold ~ 1018 eV.

No GZK

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

AGASA hot-spots -- Data

red: E > 4 1019 eVgreen: E > 1020 eV

Cluster Component~ E -1.8±0.5

Neutrinos will point better

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

AGASA hot-spots -- numbersWithin 2.5 degree circles,AGASA identifies six doublet, one triplet,Out of 57 events;

Opening the angle to just 2.6 degrees,AGASA identifies seven doublets, two triplets;

Haverah Park contributes two more paired events in AGASA directions.

NOT corroborated by HiRes.

Source number ~ N12/2N2 ~ 270 to 50%,

weighting with GZK suppression, ~ 10-5 /Mpc3for source density

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

“Essentially Guaranteed” High-Energy Galactic Neutrino Flux

cn = 10 kpc (En / EeV)and

E/ En ~ Q / mn ~ 0.8 x 10-3

E ~ PeV, for En ~ EeV

AGHW2004

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

AMANDA, RICE, Anita, and IceCube:neutrinos as ice-art

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

AMANDA/IceCube event

and coming in the Mediterranean: Nestor, Antares

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

“More Guaranteed”

Icecube atmos background in 1o circle is just 1.5events/yr, 3.5 events offers 95% CL detection in 1 yr;

Calculated signal is 4 /yr and 16 e+ showers/yr.

Conclude that in a few years, IceCube attains 5discovery sensitivity for Fe n e providing “smoking ice” for GP neutron hypothesis.

Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher !

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Galactic Plane -beam, pure anti-e at source

Serpico and kachelreiss, 2005

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Xgal proton flux – Berezinsky et alMass-composition data (HiRes 2002)

Xgal proton dominance begins at 1018 eV, not 1019 eV !F ~ 50 x Waxman-Bahcall AMANDA/RICE/EAS-sensitive !!

(AGHW, 2004)

Theory threshold for p2.7Kpe+e- and data (knee) are at 1017.6 eV.

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

AMANDA to 100 TeV

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Xgal proton fit huge flux

is pion energy/CR energy at source (1 for WB “limit”);z is cosmic evolution factor, 0.6 (no) to 3.0 (SFR)

WB fluxes

low Xgal dominance flux,with no evolution

AGHW, hep-ph/04010003,And in prog, w/ A. Ringwald

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Galaxy Distribution 7-21 Mpc

Visible from the northern site

Auger Skies

Galaxy Distribution 7-21 MpcVisible from the southern site

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Centaurus A (3.4 Mpc South)

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Auger neutrons form Cen-A

Since cn = 0.9 Mpc E20,

Neutron survival probability from Cen-A = e –3.8/E

20

= 2% at 1020 eV= 15% at 2 1020 eV= 1/e at 3.8 1020 eV

Maybe 2 evts/yr at Auger, more at EUSO,with Glennys’ flux (Farrar-Piran)

Anchordoqui, Goldberg, TJW;PRL2001

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Size mattersEUSO ~ 300 x AGASA ~ 15 x AugerEUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger

Exposure

1

10

100

1000

10000

Year

Expo

sure AGASA

HiResAugerEUSO

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Extreme Universe Space Observatory

2009 EUSO onboard the ISS (Or Not!)

2012 Hundredth anniversary of Hess

– EUSO finishes three-year data-taking

 

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

“clear moonless nights”

Blackout_14aug03.jpeg

Or New York State power blackout

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Orbiting Wide-angle Lens (OWL)

3000 events/year above 1020eV

and UHE Neutrinos!

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

On to

Neutrinos

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Neutrinos versus Cosmic-Rays and Photons

s come from central engines

- near Rs of massive BHs

- even from dense “hidden” sources

cf. s vs. s from the sun

s not affected by cosmic radiation(except for annihilation resonance)

s not bent by magnetic fields- enables neutrino astronomy

Also, besides Energy and Direction, ’s carry flavor

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

The “Learned Plot” – merits of cosmic L/E

Oscillation phase is ( Lm2 / 4 E

Figureparameterizedby m2 / (eV)2

Nature’s miracles:L/E, m, nmatter

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

The cosmic flavor-mixing theorem

If theta32 is maximal (it is),And if Re(Ue3) is minimal (it is),

Then and equilibrate;

Further, if initial e flux is 1/3

(as from pion-muon decay chain),Then all three flavors equilibrate.

e:: = 1 : 1 : 1 at Earth

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Democracy Broken:

1. Galactic -beam

2. Source dynamics

3. decay (15 minutes of fame)

4. Vacuum resonance(MaVaNs, LIV vector)

5. Pseudo-Dirac oscillations

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

decay (via majoron emission)P(survive)= e –t/ = e –(L/E)(m/

0)

Beacom, Bell, Hooper, Pakvasa, TJW, PRL2003

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

diagnostic of astro-engines:pp vs. p

The process e+e-- W-- is resonant at 6.4 PeV;

IceCube will have flavor ID, and E/E of 25%,and so can measure On-Res/Off-Res ratio.

pp make nearly equal , with P/Pp ~ 0.6 ::e:e = 2:2:1:1 flavor democracy, e = 1/6 total

p via + make +, with P/Pp ~ 0.25 e = 1:1:1 (no e) e = 1/15 total

IceCube can resolve this (AGHW, hep-ph/0410003)

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Sources:

 Bottom-Up “Zevatrons” - givens Cosmogenics ~1019 eV·     AGNs·     GRBs·     Hidden vs. Transparent (the thick/thin debate)  Top-Down “EE-trons” - pure speculation·     Topological Defects·     Wimpzillas, M ~H(post-inflation) ~1022 eV·     Msee-saw ~ 1023 eV

·     MGUT ~ 1025 eV

·     And even MPlanck ~ 1028 eV

  Other: - impure thoughts  Mirror-Matter mixing Multiverse Leakage (Brane-bridges)

Extreme Energy (EE) Neutrinos

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Model fluxes (Protheroe review 199X)

atmosphere

AGN

GRB GZK

pIsm

SMPs

TDs MGUT

GeV

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

EE Neutrinos are young

Liberated at T=Mev, t= 1 sec;But age depends on energy (Lorentz boost)

(Peter Minkowski)

Consider a 1020 eV neutrino.

Lorentz factor = 1021 for m = 0.1 eV.

Age of Uni is 1018 sec,

But age of is 1018/1021 sec = 1 millisecond !

And it doesn’t even see the stream of radiation rushing past it – untouched !

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Earth Absorption versus Neutrino Cross-Section

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Can’t Lose Thm for Space-based

Whatever the weak cross-section, get robust event rate from HAS or UAS!

and

Get measurement of neutrino cross-section(peak angle also gives )

A. Kusenko, TJWPRL2002

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Upward and Horizontal Air-shower Rates Versus Neutrino Cross-section

HAS

UAS

Kusenko, TJW, PRL2002

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Space-based HAS/UAS

with cirrus (12km) or high cumulus (4km) cloudsNo clouds

Sergio Palomares-Ruiz, TJW

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

HAS event rate is small

e.g. FCR at 1020 eV implies 10-2 events/yr;

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

View (Japanese) of Earth-Moon System – Radio Cherenkov

radio Cherenkov

This is literally GLUE Xpt,

is related to RICE and FORTE,and eventually, to SalSa

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Model Neutrino Fluxes and Future Limits

GLUE, RICE, Forte

,Auger, Anita, EUSO

From Eberle, AR, Song, TJW;Semikoz and Sigl

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Z-burst integrated rate (EUSO/yr) toward Virgo

Red = photonsBlue = protonsGreen = Gal bkgd

Venice “ Telescopes”, Feb 22-25Tom Weiler, Vanderbilt University

Whether you like protons or nuclei or gammas or neutrinos,this is an exceptional time to be a cosmic-ray physicist !

Hadron-rays:Auger and maybe EUSO should answer the mysteries

raised by AGASA.

Neutrino-rays:– now in the hands of theorists (speculation) and engineers (construction)-- soon in the hands of experimenters (real data)

Promise to reveal -- neutrino physics (cross-section, lifetime, pseudoDirac)-- extreme astrophysics (source dynamics, source environment)-- cosmology (CB, Omega‘s)

Next ten years will be critical, and, the deities/gods willing, most fruitful !

Summary: