126 ix 05 SLUO

Kavli Institute for Particle Astrophysics and Cosmology

SLUO Annual Meeting Sept 26 2005

Roger D. Blandford

KIPAC at 2+ years

Physics

Astronomy

Campus

SLAC

Theory

Experiment

NASA

DOE

NSF

326 ix 05 SLUO

KIPAC Membership* 4 new KIPAC faculty

– Abel, Allen, Blandford, Kahn (1/2 SLAC)

* 6 existing SLAC senior personnel– Bloom, Chen, Digel, Drell, Kamae, Madejski, Tajima+GLAST, LSST

* 9 existing campus senior personnel– Cabrera, Chen, Church, Gratta, Linde, Michelson, Petrosian, Romani, Wagoner

* 5 new senior research staff at SLAC – Craig, Gilmore, Marshall, Morris, Rasmussen

* 18 postdocs – + Carlsson, Cheung, Fuerst, Kazantzidis, Rapetti

* 23 students – participate

* 4 visitors* 3+ Administrators

– HEPL-KIPAC Christiansen

426 ix 05 SLUO

Recent Developments

* SLAC reorganization– PPA->PPA-KIPAC-> KIPAC-SLAC + GLAST ->ISOC+Physics || ||

KIPAC KIPAC-CAMPUS LAT

* Faculty searches– Senior Experimentalist– Junior Theorist

* New building preparations– Transition committee - Kamae + Wagoner

* Project roller-coaster– GLAST, LSST, SNAP, NuSTAR…

GLAST

526 ix 05 SLUO

Fred Kavli Building

Completion Jul 2006

Completion Jan 2006

Physics-Astrophysics Building

626 ix 05 SLUO

KIPAC Activities

* Regular Seminars– Alternate campus, SLAC

* Bi-weekly group meeting– Alternating– 40-80 attendees

* Four International Conferences* Public outreach* Joint activities with UCB, UCSC etc

– Postdoc-student organized

* Future activities– NuSTAR meeting– SLUO sponsored particle physics/astrophysics

726 ix 05 SLUO

The Science of KIPAC

* Particle Astrophysics– Black Holes, Neutron Stars, White Dwarfs…

– GRBs, magnetars, supernovae…

– Accretion disks and jets…

– Relativistic shocks, particle acceleration, UHECR…

– Solar Physics

* Cosmology – Dark energy, dark matter

– Gravitational lenses

– Clusters of galaxies and intergalactic medium

– Microwave background observations

– First stars, galaxy formation

– Supernovae

826 ix 05 SLUO

Theoretical Astrophysics and Cosmology

* Pulsar magnetospheres* Dark matter* Gravitational lensing* Clusters of Galaxies * Double pulsar* Gamma ray bursts* Dark energy* Particle acceleration* Ultra High Energy Cosmic Rays* Atomic Astrophysics* Computational Cosmology

926 ix 05 SLUO

KIPAC Observational Program

* KIPAC members very successful in getting observing time on HST, Chandra, XMM-Newton, Astro-E2, Swift, VLBA…

* Supernova research program on Hobby-Eberly Telescope - Joined Sloan survey project

* Multi-wavelength observations for GLAST- VIPS* Building experience with handling large

astronomical datasets to enable us to work in the LSST environment

1026 ix 05 SLUO

KIPAC Projects

NuSTARLaunch ~ 2009

LSSTFirst Light ~ 2012 SNAP

Launch ~ 2018Dark Energy and Matter

Cosmic Acceleratorsand Black Holes

Combining:•Physics and Astronomy•Theory and Experiment•SLAC and Campus•DOE, NASA and NSF

GLASTLaunch 2007

All Sky High Resolution

All SkyHigh

Resolution

1126 ix 05 SLUO

GLAST

1226 ix 05 SLUO

Supernova Acceleration Probe

* SNAP is designed to study dark energy by measuring the rate of expansof the Universe using supernovae and through determining the distortion of the images of distant galaxies. It is complementary to LSST, emphasizing small over large scale structure

* SNAP is a collaboration with LBL.* KIPAC will be responsible for

the Observatory Control Unit and the strong lensing science

* At present the timescale for SNAP is set by NASA and is unacceptably long.

Focal plane

Spacecraft

1326 ix 05 SLUO

NuSTAR: Nuclear Spectroscopic Telescope Array

NuSTAR Key Science Questions

High Energy X-ray optics: (Columbia, LLNL, Danish Space Center, KIPAC/SLAC).

Selected by NASA in January 2005 as one of two Small Explorers (120M$). Launch is scheduled for 2009. Now in an extended study phase with final launch confirmation in 2006.

NuSTAR Instrument & MissionBlack Holes: How are black holes distributed through the cosmos, and how do they influence the formation of structure? NuSTAR will perform a deep black hole survey.

Supernovae: How do stars explode and forge the elements that compose the Earth? NuSTAR will map supernova remnants.

Extreme Objects: What powers the most extreme active black holes? Contemporaneous observations of blazars detected by GLAST.

CdZnTe Detectors: (Caltech)

1426 ix 05 SLUO

Computational Astrophysics

* KIPAC plans to build up its infrastructure to work in LSST era - 30 Petabytes!

* KIPAC is partnering with SLAC computing services and LLNL

* Modeling the first stars in the Universe, gamma ray bursts and neutron stars

* Advanced visualization is the key to performing this science

* Educational Visualization Project

1526 ix 05 SLUO

KIPAC Goals (2005-)* Become a Leading International Center for Particle

Astrophysics and Cosmology– Local scientific forum for Stanford and Bay Area– Help prepare for GLAST Science in 2007– Build outstanding faculty; attract students, postdocs, visitors

* Participate in and complete major projects – LSST, SNAP,…– NuSTAR, QUaD, QUIET, PoGO, Constellation-X, EXIST…– Develop ideas and technology for new projects

* Develop Computing Infrastructure so as to;– Work productively in the LSST era– Attack major physics problems eg first stars, relativistic shock waves– Perform multi- scale, multi-dimensional simulations

Major concern is uncertainty of Federal Funding through DOE + NASA + NSF

1626 ix 05 SLUO

General Relativity

* General Relativity (Einstein 1915)– Singular “simple” theory of classical gravity

– G=8T

– Many, more elaborate alternatives

• Scalar tensor, bimetric, extra dimensions, PPN…

* Experimental Program– Classical tests

• Redshift, Mercury. Light deflection

– Modern tests

• Shapiro delay, gravitational radiation, EP, inverse square law...

GR/AE vindicated at level from 10-2 to 10-4!

1726 ix 05 SLUO

Cosmology

* Einstein 1916– G+g=8T - Cosmological Constant

• Vacuum energy: P=-

* Friedmann 1922• a(t) is scale factor ( =1 now)

0][

][

.3

4

2

3

3

22

ad

adP

constaa

B

Const. measurescurvature =0 when flat.

DARK

1826 ix 05 SLUO

Historically, was taken very seriously

* Lemaitre 1927 – Basic equations, relativistic growth of perturbations

* Eddington 1933– The universe is much bigger than particles; therefore there must a

cosmological lengthscale - -1/2

– “I would as soon think of reverting to Newtonian theory as of dropping the cosmical constant”

– “To drop the cosmical constant would knock the bottom out of space”

* Bondi 1948– CDM Universe

1926 ix 05 SLUO

Simple World Models only

– const– a ~ exp t – De Sitter Universe

* Matter only– ~ a-3

– a ~ t2/3 – Einstein - De Sitter Universe– Deceleration

* Matter plus – Singular “simple” theory – a ~ (sinh t)2/3

– CDM universe– Deceleration -> acceleration

t

13

2

a

aaj

2026 ix 05 SLUO

Cosmological Observations

* Kinematical– Cannot measure time accurately

– Instead measure d(a), where

– Observe objects of known size

• eg density fluctuations – at recombination when a ~ 10-3

now

then

now

then

a

dtd

za

1

1

2126 ix 05 SLUO

Microwave Background Observations

Hinshaw et al WMAP

* Measure spectrum of temperature fluctuations– Derive from scale-invariant initial conditions => inflation?

* Calculate linear size of peak; angle => distance

Universe Flat to ~ 2 percent

2226 ix 05 SLUO

Cosmological Observations

* Kinematical– Cannot measure time accurately

– Instead measure d(a), where

– Observe objects of known size

• eg density fluctuations – at recombination when a ~ 10-3

– Observe objects of known power

• eg supernovae– For a > 0.3

now

then

now

then

a

dtd

za

1

1

Perlmutter

2326 ix 05 SLUO

Cosmological Observations

* Dynamical– Newtonian physics in Universe

expanding at rate given by a(t)– Measure CMB fluctuation spectrum– Clusters of galaxies

– Growth of structure• Compare with CMB

4.0B

B

MM

X-rays +Lensing

Nuclear PhysicsTegmark et al

2426 ix 05 SLUO

CDM Dynamics* Positive perturbations grow

– Gravity vs expansion– Initial conditions when a~0.001 from CMB observations– Fluctuation spectrum has “simple,” scale-free form

• Linear perturbations evolve with time according to:

– Extend into nonlinear phase using simulations– Many uncertainties on short scales

03

4

3

]coth[8 t

2526 ix 05 SLUO

Standard Model of the Universe

* = const

=0.7nJm-3 =6 x 10-28 kg m-3

Equivalent to:

• 0.4 mG, 40 K, 1meV, 100, 3THz

• m ~mSUSY2/mP

• Extra dimensions…

* DM = 0.25nJm-3 Supersymmetric particle?

* = 0.05nJm-3

* Flat spatial geometry

All contemporary data consistent with CDM to 10-20%

2626 ix 05 SLUO

How do we study DE/DM at 1% level?* What physics must we explain?* CMB observations will improve* Kinematic Tests

– Distance to supernovae– Baryon oscillations– …

* Dynamical Tests– Weak gravitational lensing– Counting clusters of galaxies– …

* Only careful, well-planned

projects will be up to the task

Eisenstein et al

In US, a task force is making choices

2726 ix 05 SLUO

Summary

* After two plus years, KIPAC is on track* Tremendous support from Stanford community

– Two new faculty

– Two buildings

* Self-sustaining theory-phenomenology-observing group* Great progress in experimental projects

• GLAST

• LSST

• NuSTAR, SNAP, QUaD, Constellation-X, PoGO, EXO, CDMS3…..

* Computing challenge/opportunity