Marc Kamionkowski- New Views of Cosmology and the Microworld

8/3/2019 Marc Kamionkowski- New Views of Cosmology and the Microworld

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New Views ofNew Views ofNew Views ofNew Views ofNew Views ofNew Views ofNew Views ofNew Views ofNew Views of

Cosmology and thCosmology and thCosmology and thCosmology and thCosmology and thCosmology and thCosmology and thCosmology and thCosmology and th

MicroworldMicroworldMicroworldMicroworldMicroworldMicroworldMicroworldMicroworldMicroworld

arc am on ows

(Caltech)

SLAC Summer InstituAugust 16, 2002


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Topics in Particle Astrophysics andI. Dark matter and relic particles

II. Gamma rays and x rays(GLAST, STACE

III. The CMB and inflationIV. Structure formation, cosmological par

dark energy. Ultrahigh energy cosmic rays

I. Gravitational radiationII. Neutrino astrophysics

III. Early universe and tests of fundamen

brane worlds and large extra dime

(see, e.g., Akerib, Carroll, MK, Ritz,of P4 Working Group at Snowm

hepph/0201178


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Funda

Forc

100 GeV 101516

GeV

strong

EM

weak

gravity

????

electroweak

GUT

Energy


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Astrophysics/cosmology and

advances in fundamental physics;

Keplers and Newtons laws

Discovery of helium

Serendipitous discovery of positrons, muons in

Big bang nucleosynthesis and number of light

Cosmological constraints to stable neutrino mSolar and atmospheric neutrinos and neutrino

Astrophysical verifications of general relativity

Eddington and bending of light

expansion of Universe

pulsar timing and gravitational waves


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Physics with astrophysical

neutrino masses and mixi

solar and atmospheric ne

SuperK


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I. The Cosmic Microwav

Background and Infl


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Geometry

Hubbleconstant

Jungman, MK, Kosows


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esults!!!Netterfield et al. (BOOMERanG) astroph/0104460 (also fro


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Current results:

show that Universe is flat

determine primordial seeds for large scal

independently verify big bang nucleosyntconfirm existence of nonbaryonic dark m

suggest 70% of total energy density is so

negative pressure dark energy (espe

combined with dynamical measurem

matter density of 30%)Physics is simple and peak structure is distincti

so most results (especially for geomet

...show is not over!! What we have seen so far

iceberg; MAP and Planck will improve precismeasurements by order of magnitude.


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Th

ebigbang!!!

Nuc

leosynthesis:

n+p

H,

D,

He,L

i

SecoT~M

q

uarksn,p

103 sec

T~100 MeV

elec

troweakEM

,weak

109 sec

T~100 GeV

quantumg

ravity,strings???

10

43

secT~ 1019 GeV

1036 sec

T~ 1016 GeV

GUT

electrowea

k,s

trong??

10

22

secT~ 1012 GeV

PQsymmetrybreaking??

SU

SYbreaking??

INFLATION


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CMB tests of inflation:

Recent CMB shows are on right trackWhat next? Determine energy scale o

Inflation robustly predicts gravitation

background with amplitude proportof energy scale of inflation (Abbott&W

Detection of inflationary gravitational wav

through CMB polarization can providgun" for inflation at GUT scale.

(MK, Kosowsky, Stebbins 1997; Seljak,Zald


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Gr

avitationalW

aveAmplitud

e

(Energyscale

ofinflation)

2


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Gravitational waves: Another probe of the inflato

GW amplitude h()

C

W


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Brief aside: CMB detection of Brief aside: CMB detection of

violation from Planck scale phviolation from Planck scale ph

(Lue, Wang, MK, 1999)

Certain cross correlations between temperat

polarization components can arise only if pa

FF~

RR

Two examples: Rolling scala

with P,T viol

to EM

P,T violating couplingto gravity can produce

preponderance of right

versus left handed GWs


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II. Large scale structure and

Inflatonpotential

Ma

spe


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Galaxy megasurveys now mapping

mass distribution over huge volumes (2


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Forecast

SDSS

Power

Spectrum

CD

Mo

h=0.5

h=0.2

(as

bia


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Dodelson et al. (SDSS Collaboration) ApJ (2


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Cosmic Shear

First detection (by several indgroups) of "cosmic shear", weagravitational lensing due to

large scale mass inhomogenei

Probes largescale distributio

rather than ofgalaxies.

...and mapping of dark matter aro

has become routine.


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Possible, e.g.


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Inflation: What Else??

Inflation distribution of primdensity perturbations is

Can be checked with CMB mapssurveys, weak lensing, cluster

abundances, abundances of

highredshift objects, clusterproperties....

(e.g., Verde et al., 2


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Ra

fo


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III. Sup

an acce

Univers

Dark E

1998


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Courtesy P. Garnavich (Highz Supernova Se(results also from Supernova Cosmology Pr


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Quintessence:

V()

Spintessence:

(Boyle, MK,Caldwell 2001)


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Qu(sp)intessence! Other connections:

"Vacuum" is CPT and Lorentz violatinand may contain global charge

May drive baryogenesis and/or hide aCould rotate polarization of distant ra

if scalar field coupled to EMCan reproduce and generalize (e.g., to

quartic terms in potential) fuzzy cold

matter


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III. Particle Dark Matter S


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Earth

(r

density

r

r0=8 kpc

Veloc

distrib

With


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Particle dark matter cand

Weakly Interacting Massive

Particles (WIMPS).

e.g.,neutralinos

Axions

ma~104

v

cmh

sec/103

327

2


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WIMPsWIMPsThe relic density of a massive particle is about:

vh

1327

2 scm103

v OfWeak Interaction strength

the particle has to be coupled to SM particleThere is chance for detection:

Detection

direct

indirect

Ne

from

ano

cosm

WIMP candidate motivated by SUSY:

Lightest Neutralino, LSP in MSSM


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Particle dark matter

searches (axions

and SUSY particles)

See

dmtools.berkeley.edu


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Spin depende

WIMPproto

Spin dependent

WIMPneutron coupling

Ullio,


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Searches for SUSY dark m

Direct detection inlow background detectors

Indirect de

via energefrom LSP a

in Sun/Ea


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Detection of SUSY dark

Indirect detection via observation

gamma rays from LSP annihilatio

E.g., in GLAST, VER

Whipple, CELESTE,

Or via observation of exotic cospositrons or antiprotons (e.g., iPBAR, AMS....)


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Axionsearch (Livermore) (courtes

Scanned already Next year

Ac

wi

(~

ow ca

these h


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Self interacting dark ma

Cluster

galactichalo

Moore et a

also Klypin

ph/99012

Kaufmann

Guiderdon300 kpc


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Probably dont need self interactRequires very unusual particles

scattering cross sections 13 ordmagnitude bigger than annihila

Not really clear that self interac

improves agreement with obsMay be due to other exotic proc

Broken scale invariance in primpower spectrum (MK, Liddle 2

Absence of small scale structuremost likely due to prosaic astro

mechanism


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MK,Liddle (2000)


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IV. Tests of strongfield gravity:

Gravitational waves from stellar or

supermassive black holes (e.g., wit

X ray timing and spectroscopy from

disks around supermassive black h

(RXTE, Chandra, XMM, ConX,GL

other interesting tests with grav ra

can test whether gravitational wav

at speed of light (extra dimensionsmight not!!)


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Possible detection of effects

black hole spin on surro

spacetime!!!

P. Nandra


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Gravitational Radi

Orbiting and merging massive

objects emit gravitationalradiation

Two biggest experiments aimigravity waves:

LISA(spacebasLIGO(groundbased, under construction)

firstlock at Hanford

Oct 2000

4km


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Possible detection of cosmic

above GZK cutoff!!!(p + p + ) 30 pc for E

p 1020 eV,

but no obvious sourceswithin ~30 Mpc also no

dramatic cutoff inspectrum near 1020 eV.

HiRes also seeing events


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Ultrahighenergy cosmic rays:

Existence of cosmic rays aboveGreisenZatsepinKuzmin limit su

propagation of exotic particle and/

of topological defects or ultrama

particles. Interactions in atmospheinclude interesting QCD.


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UHE Cosmic Ray TecNitrogen Fluorescence

Air Shower

~0Ground ArrayAGASA

~3Fluor.OWL

8Fluor.Telescope

Array

7

( x2

Ground Array

+ Fluor.

Auger

~1Fluor.HiRes

Ef

[10TechniqueExperiment

OW

L


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More:

Astrophysical probes of large extra dimLorentz/CPT violation...

Astrophysical tests of general relativity (

Shapiro time delay, radio deflection

ranging...Theoretical ultrahigh energy physics: the

Universe as a laboratory for string t

PQ symmetry breaking, GUTs, SUSY

extra dimensions....


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Conclusions/Summar

Astrophysics and cosmology are often difficult

BUT, can in some cases provide real opportuni

to probe new physics not accessible with accel

Its a good time for cosmology and particle astrplenty of exciting discoveries and breakthroug

rich frontier; healthy interplay between theory

prospects for rapid order of magnitude experim

in many areas.


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Marc Kamionkowski- New Views of Cosmology and the Microworld