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 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) = w 0 + w 1 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) 97.6 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 J : 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 gas SKA

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 – Broad, thermal eMERLIN 1 – High resolution ATA 1 – ? Wide fields DSN 8, ? Telemetry LWA 0.03– Low freq window LOFAR 0.08 – EoR++ MWAd 0.1 – EoR+ PAPER 0.1 – EoR SKADS (europe) 0.1 – HI survey (aperture array) xNTD (Oz) 0.7 – HI survey (FPA) South Africa 0.7 – HI Survey (FPA) SKA-TDP (USA) 0.3 – Nd

Goal 4: Hubble constant through direct measurement: Water Maser Disks (Greenhill) Future 1% measures of CMB and related require 1% measure of H o for fully constrained cosmological parameters: covariance Water masers disks into the Hubble flow can provide direct measure of H o to 1% h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