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?