tasi 2008: particle astro, cosmic rays, tom weiler vanderbilt …€¦ · the cosmic ray timeline...

TASI 2008 Tom Weiler, Vanderbilt University

TASI 2008:

Particle Astro, Cosmic Rays, ...

Tom Weiler Vanderbilt University

TASI 2008 Tom Weiler, Vanderbilt University

Lecture I - Cosmic Ray Physics at Highest Energies

Many thanks to Gustavo Medina-Tanco, Luis Anchordoqui, Haim Goldberg,Masahiro Teshima, Etienne Parizot, and anyone else whose slides I have “borrowed”...

TASI 2008 Tom Weiler, Vanderbilt University

The Cosmic Ray Timeline1912 Hess (Austrian) balloons to 5km, his sparks increase; also sees no change during solar eclipse1929 Cloud chambers, and the birth of particle physics:

1933 Anderson’s positron; Kunze’s muon (Rostock) 1937 Anderson’s muon 1938 Auger’s remarkable PeV air-shower 1949-54 Fermi’s “Doppler” acceleration via magnetized shocks 1966 3K CMB discovered; GZK predict cutoff at 5x1019 eV (But Linsley already reported (PRL) event at 1020 eV)

1987 IMB/Kamiokande neutrinos from SN87a

TASI 2008 Tom Weiler, Vanderbilt University4

AUGER’s key discoveryAuger, in 1938, separated two particle counters by nearly a km high in the Swiss Alps (Jungfrau, near Bern). He discovered coincident signals. He calculated ETOT to be about 1015 eV.His inference was correct. His energy was 107 times the prior record event,And now thought to be typical of emission from a SN remnant.

TASI 2008 Tom Weiler, Vanderbilt University

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

Akeno/AGASA Xpt begins

mid-90s DUMAND taken off life-support; 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 θz > 45o);

And the controversy has begun!

Importantly, Auger gets first “light”

2002 AMANDA pushes to 1014 eV thru-Earth neutrinos

2005 Auger Observatory data expected

2008 Extreme Universe Space Observatory (EUSO) ?

TASI 2008 Tom Weiler, Vanderbilt University

Cosmic Photon- Proton-Spectra

hadron wall?

no wall a’tall

sun SN87aNeutrinoIncognito

TASI 2008 Tom Weiler, Vanderbilt University

Power-laws are definitely not thermal exponentials

TASI 2008 Tom Weiler, Vanderbilt University

Any particle Rx we will ever make, CERN and beyond, was done many times by CRs.

BB: CoM calculation

TASI 2008 Tom Weiler, Vanderbilt University

LHC is “safe”, because CRs say so:

arXiv:0806.3414

TASI 2008 Tom 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 !

You might say, Nature is Clemens on steroids.

TASI 2008 Tom Weiler, Vanderbilt University

CR Spectrum above a TeV

from Tom Gaisser

VLHC(100 TeV)2

TASI 2008 Tom 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)

TASI 2008 Tom Weiler, Vanderbilt University

Fly’s Eye 3x1020 eV event (1992)The Big One that didn’t get away !

This longitudinal profile is consistent with a primary proton, but not with a primary photon; Disfavors “local” top-down sources such as massive Particle DK, topo-defects,Z-bursts, etc.

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

Fluorescence detectors see real-time shower development

TASI 2008 Tom Weiler, Vanderbilt University

Inter-galactic space is not “nothing”:

TASI 2008 Tom Weiler, Vanderbilt University

Energy-losses on the Cosmic Radiation Background (CRadB)

Nuclear Photo-dissociation

GZK process

Berezinsky’s favorite and (e+e-) 2

TASI 2008 Tom Weiler, Vanderbilt University

HE Gamma-Ray mfp/attenuation

Double pair production has huge t-channel log at HE

TASI 2008 Tom Weiler, Vanderbilt University

Greisen-Zatsepin-Kuzmin, and the Cosmic-Ray Wall

Δ-resonance

multi-pions

Photo-pion production off CMB p+γcmb→ Δ →p/n+π

TASI 2008 Tom Weiler, Vanderbilt University

The “GZK sphere” :

Too generous, imho;AND, about the size of the BAO length !!

(Dan, let’s write.)

TASI 2008 Tom Weiler, Vanderbilt University

But AGASA Spectrum, pre-2003: EeV to ZeV

AGASA, July 2002

TASI 2008 Tom Weiler, Vanderbilt University

Super-GZK events - yes?would-------

(e.g., Z--bursts)

TASI 2008 Tom Weiler, Vanderbilt University

Super GZK events - no?

-- Auger has many more events above 1020 eV that do not make their stringent tank cuts;

-- one awaits the “GZK recovery”, due to nearby sources, or Z-bursts or TDs or SMHPs or ... (coming tomorrow)

.

TASI 2008 Tom Weiler, Vanderbilt University

Composition signatures: X-max, and muon richness

TASI 2008 Tom Weiler, Vanderbilt University

Energy determination/estimation

At AGASA, from lateral particle distribution:

TASI 2008 Tom Weiler, Vanderbilt University

Fluctuations, dangerous or no?

Unfortunately, fluctuations also mimic “Zoo”-events

TASI 2008 Tom Weiler, Vanderbilt University

EAS detector types:

TASI 2008 Tom Weiler, Vanderbilt University

Pierre Auger Observatory

TASI 2008 Tom Weiler, Vanderbilt University

GZK suppression established (more or less)

Feb 2008 Confirmed by Auger

TASI 2008 Tom Weiler, Vanderbilt University

Auger anisotropy:

TASI 2008 Tom 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

TASI 2008 Tom 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 /Mpc3 for source density

TASI 2008 Tom Weiler, Vanderbilt University

Size mattersEUSO ~ 300 x AGASA ~ 10 x AugerEUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger

TASI 2008 Tom Weiler, Vanderbilt University

JEM-EUSO: Extreme Universe Space Observatory

TASI 2008 Tom Weiler, Vanderbilt University

“clear moonless nights”

Or New York State power blackout

TASI 2008 Tom Weiler, Vanderbilt University

Orbiting Wide-angle Lens (OWL), or “Super-EUSO”

3000 events/year above 1019.7eV

and UHE Neutrinos!

TASI 2008 Tom Weiler, Vanderbilt University

Particle Astronomy ?

TASI 2008 Tom Weiler, Vanderbilt University

EUSO number count

TASI 2008 Tom Weiler, Vanderbilt University

Clustering with EUSO