Appendix E: Intro to the Banff Feb06 Annual Meeting

See the body of the text, Section 3.2, for an introduction to this introduction. The slides were taken from the Planning Meeting summary (with small updates) associated with the C&G Annual Meeting in Mont Tremblant in March 2005

Notes on slides: The proposed C&G components and some of the questions being addressed are shown in the second slide.

The dark matter abundance has gone down to ~0.2 with WMAP3 and the dark energy up to ~0.7

Not all of the experiments shown in the timelines will go (e.g. Constellation X may fall victim to NASA funding problems for fundamental science missions.

CIAR Cosmology & Gravity ProgramThe Cosmic Quest for Fundamental Physics

12 fellows (all but 3 new/repatriated Cdns) 1 institute fellow

6 scholars (all new/repatriated Cdns)

all in Canada (UVic, UBC, UofA, McMaster, PI, UofT, CITA, Queens, McGill)

22 Associates US, UK (4), Canada (3, incl 2 ex-fellows)

7 Board Members (treated as associates for interaction)US (4), Germany (1), Canada (2)

+ 47 PDFs, 51 grad students (+ undergrads) in Canada

Physical cosmology

Early universe physics & Inflation

Dark matter, Dark Energy probes

Cosmic Microwave Background

Redshifted 21 cm

Galaxy formation & properties

Large scale structure

Weak lensing, z-surveys

Supernovae

Clusters in CMB, optical, X

String theory

branes & compactified extra dimensions

the landscape

“environmental selection” anthropic

emergence of space/time

Strong Gravity

Strings

Early Universe

Black holes

HEA

High Energy Astrophysics

neutron stars

Black holes

High energy cosmic rays

Magnetars, double pulsars

Particle Astrophysics

Experiment

SNOlab, LHC

Numerical relativity

colliding black holes in 3D

Gravity Waves

dm = 0.25± 0.03dm = 0.25± 0.03

de = 0.70± 0.03de = 0.70± 0.03

b = 0.045 ± 0.005b = 0.045 ± 0.005

2003

2004

2005

2006

2007

2008

Polarbear(300 bolometers) California

SPT+(1000 bolometers) South Pole

ACT+(3000 bolometers) Chile

Planck(84 bolometers)

HEMTs L2

CMBpol

Quiet1Quiet2Bicep

QUaD

CBI ongoing to Sept’05+

WMAP ongoing to 20092017

(1000 HEMTs) Chile

Spider

Clover

Boom03

DASI

CAPMAP

(1856 bolometer LDB)EBEXEBEX

2003

2004

2005

2006

2007

2008

SZA(Interferometer) California

APEX(~400 bolometers) Chile

SPT(1000 bolometers) South Pole

ACT(3000 bolometers) Chile

Planck(84 bolometers)

HEMTs L2

CMBpol

ALMA(Interferometer) Chile

(12000 bolometers)SCUBA2

Quiet2CBI2 Jun06 to Apr’07+

Acbar to Jan’06+

2017

(1000 HEMTs) Chile

Clover

AMI

GBT

JCMT, Hawaii

2003

2004

2005

2006

2007

2008

SZ/ PVmeasure: SZA, APEX, GBT, AMI, ACT. SPT, Planck, ALMA

Pan-STARRS

LSST

JDEM DUNESpace

CFHT-Legacy ongoing to 08 (165 spec, 700 in can) ~400+ SN/5yrCFHT-Legacy ongoing to 08 (165 spec, 700 in can) ~400+ SN/5yr

SN1: Oct04 ~100 @ z ~ .3-.7

~ 10 @ z ~ 1-1.5 ~30

SN1: Oct04 ~100 @ z ~ .3-.7

~ 10 @ z ~ 1-1.5 ~30

CLUSTER/GROUP system in the Cosmic WebCLUSTER/GROUP system in the Cosmic Web

2015

ESSENCE ongoing to 06+ ~150 SN/5yrESSENCE ongoing to 06+ ~150 SN/5yr

WEAK LENSING:WEAK LENSING:

CFHT-Legacy ongoing to 08 (first great results 05) 140 sq degCFHT-Legacy ongoing to 08 (first great results 05) 140 sq degDeep Lens Survey ongoing 28 sq degDeep Lens Survey ongoing 28 sq deg

Oct04: RCS1 53 sq deg, Virmos-Descart 11 sq deg +Oct04: RCS1 53 sq deg, Virmos-Descart 11 sq deg +

RCS2 ongoing 1000 sq deg RCS2 ongoing 1000 sq degKIDS (960 sq deg), UKIDS KIDS (960 sq deg), UKIDS

SDSS ongoingSDSS ongoing

Optical: RCS, RCS2, SDSS + ongoing Optical: RCS, RCS2, SDSS + ongoing Large Optical Surveys for SZ tomography (DES, .)

Large Optical Surveys for SZ tomography (DES, .)

LISA 2013

LISA 2013

LIGO2

2008-12

LIGO2

2008-12

LIGO1LIGO1

Galaxy Formation Developments Timeline

2007

Photometric Surveys:VISTA, UKIRT, VST, etc

Submillimeter:SHADES, BLAST,

SCUBA2, ..

HST, Spitzer, GALEX, XMM,

CHANDRA,..

2005

Spectroscopic Surveys:

VIRMOS, KAOS, FMOS, WFMOS, ..

2003

TMT?ELT?

OWL?SKA?

LOFARSCUBA

Millennium Run10.077.960.000 particles

Max-Planck Institut für Astrophysik

Springel et al. (2004)

Semi- analytic machinery

Tully- Fisher relation

Galaxy colors

Star formation history

Luminosity function

Galaxy morphologies

Morphology density relation

Evolution to high redshift

Clustering properties

Radiative gas cooling

Morphological evolution

Dark matter merging

history tree

Feedback

Metal enrichment

Spectrophotometric evolution

Star formation

Pre

dic

tio

ns

Inp

ut p

hysic

s

SEMIANALYTIC

OB

SE

RV

AT

ION

ST

HE

OR

Y

SPH+Nbody

2005 2010

? Constellation X

High Energy AstrophysicsChandra

XMM-Newton

RXTE

HETE2

SWIFT

ASTROE2

Astrosat

Agile

GLAST

NuSTAR

Integral

XEUS

2005 2010 2015

Radio Astrophysics

Arecibo/ALFA EVLA

CLAR(?)Green Bank Telescope ALMA

CBI2, VSA, AMI

LOFAR

GMRT, India

Astroparticle Experiment Timeline

• 2004 TeV gamma ray astronomy – now• 2006/07 onwards multi-messenger astronomy

– 1019 eV cosmic rays in 2006– neutrinos (IceCube) in 2010

• 2007 SNOLAB space available– next-generation dark matter searches 2008/09– exploration of neutrino properties 2008/09

• double beta decay• neutrino-matter interactions• “new physics” – neutrino physics is the only “beyond the

Standard Model”

Direct Measurements of Dark Matter

From Angel Morales

The Top 10 Galaxy Formation Puzzles

(in no particular order)

• 1) What is the origin of the characteristic mass of galaxies?

• 2) Why does the CDM halo mass function differ so drastically from the galaxy luminosity function:– Why does the luminosity function cutoff exponentially?– What sets the faint end slope?

• 4) Why are big galaxies old and small ones young?• 5) Is the spatial distribution of dark matter within

galaxies consistent with CDM halos?

The Top 10 Galaxy Formation Puzzles

• 6) When did the first luminous objects form and what are their descendants?– What/When/How did the universe reionize?

• 7) Where are all the baryons at low-z?• 8) How prevalent are galactic winds and what is

the role of Active Galactic Nuclei?• 9) How much star formation is obscured?• 10) How did supermassive black holes form and

how do they relate to the formation of stars?