C.Carilli, AUI Board October 2006

• ISAC-run three year process: Quantified ‘experiments’ for future large area cm telescopes

• 50 chapters, 90 authors, 25% theorists

Cradle of Life: Terrestrial planet formation + astrobiology + SETI

Cosmic reionization and first light

HI + continuum survey: galaxy evolution and dark energy

Strong field tests of GR using pulsars

Cosmic magnetism: origin and evolution

Key Science Projects: (i) Address key questions, (ii) Unique role of radio, or complementary but critical, (iii) Excites broad community

KSP I: Cosmic magnetism -- Origin, Structure, Evolution

Experiment: All Sky Polarization/Rotation measure survey (σ

0.1 μJy at 1.4GHz) -- 2e7 RMs, spaced by ~ 90" (vs. 1500 currently)

Currently: 300 local pulsar RMs

SKA: 2e4 pulsars

2. Nearby galaxies Synchrotron+RMs: test dynamo models

3. Distant radio galaxies: Intercluster magnetic fields

4. Ly-a absorbers: galaxian magnetic field evolution over cosmic time

5. Cosmic web: the magnetized intergalactic medium

KSP II: Galaxy evolution and dark energy

Experiment: All sky HI line + continuum survey -- 1e9 Galaxies in HI out to z=1.5

Goal 1: Galaxy evolution – conversion gas to stars

1e4/deg^2 in HI to z=0.5 to 1.5

Goal 2: SKA as Dark Energy Machine

DE EoS: w = P/ = -1? Func(z)?

Baryon Oscillations + Weak lensing:

Evolution of LSS -- ‘standard ruler’

w(z) = w0 + w1 z

SKA: variance limited

SKA: measure w(z) to few %

KSP III: Study of Cosmic reionization and first light

The last unexplored phase of cosmic evolution (0.1 to 1Gyr after BB)

z=12 (109MHz) 9 7.6

Experiment: Imaging 3D ‘tomography’ of IGM in HI 21cm line

“Richest of all cosmological data sets”

1e9 M_sun in dust, 1e10 M_sun in mol. gas =>

Hyper luminous IR galaxy (FIR =1e13 L_sun): SFR = 1e3 M_sun/yr ?

Coeval formation of SMBH/galaxy?

Dust formation by massive stars?

Break-down of M- relation at high z?

J1148 VLA: CO 3-2 at 45GHz

1”

SDSS J1148+5251: Observing first light at radio wavelengths

z=6.42; t_univ=0.87 Gyr

Fan +

Early enrichment of heavy elements (z_sf > 8)

Integration times: hours to days on HLIRGs

50K

Complementarity

AGN, star formation

Low order mol. lines

Mol. Gas, dust

Stars, ionized gasSKA

KSP IV: Gravity Beyond Einstein

Experiment: 2e4 Galactic pulsars

Strong field GR tests using pulsar-black hole binaries

Pulsar Timing Array: most sensitive gravity wave detector

for SMBH binaries

KSP V: Cradle of life

• Terrestrial planet formation: disks and gaps on sub-AU scales (complementary with ALMA).

• Prebiotic large molecules (abiotic amino acids)

• Search for Extraterrestrial Intelligence: leakage radiation (interstellar TV)

• All require sensitivity: A/T >= 1e4 m^2/K

• Most require frequencies >= 10 GHz

• Many require > 1deg^2 FoV at 1.4 GHz

• Some require > 1000 km baselines

• A few require multibeaming

END

Pathfinders

Freq (GHz) Year Focus

• EVLA I 0.3 – 50 2012 Broad, thermal

• eMERLIN 1 – 30 2010 High resolution

• ATA 1 – 10 2008? Wide fields

• DSN 8, 32 2010? Telemetry

• LWA 0.03–0.08 2009 Low freq window

• LOFAR 0.08 – 0.3 2009 EoR++

• MWAd 0.1 – 0.3 2009 EoR+

• PAPER 0.1 – 0.2 2008 EoR

• SKADS (europe) 0.1 – 25 2015++ HI survey (aperture array)

• xNTD (Oz) 0.7 – 1.4 2010 HI survey (FPA)

• South Africa 0.7 – 1.4 2010 HI Survey (FPA)

• SKA-TDP (USA) 0.3 – 25 2010 Nd

Goal 4: Hubble constant through direct measurement: Water Maser Disks (Greenhill)• Future 1% measures of CMB and related require 1% measure of Ho for fully constrained cosmological parameters: covariance

• Water masers disks into the Hubble flow can provide direct measure of Ho to 1%

h

Rayleigh-Jeans curve implies thermal objects are a factor four stronger (in Jy) at 45GHz relative to 22 GHz

=> a 10% demonstrator becomes 40% of the SKA

10% demonstrator

Case for frequencies up to 45 GHz: Thermal objects