Square Kilometre Array: World s Largest Radio Telescope Design and Science drivers
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1 Square Kilometre Array: World s Largest Radio Telescope Design and Science drivers Miroslava Dessauges Geneva Observatory, University of Geneva With my thanks to Philip Diamond (SKA director-general), Tyler Bourke (SKA organisation), Jeff Wagg (SKA project scientist) Footer text
2 SKA site selection Republic of South Africa Australia Exploring the Universe with the World s largest telescope
3 Karoo Radio Astronomy Reserve 500 km Exploring the Universe with the World s largest telescope
4 Murchison Radio Astronomy Observatory => km -2 Exploring the Universe with the World s largest telescope
5 SKA specifications Greatest Observatory for the coming decades 2 sites; 3 telescopes; one Observatory SKA-Mid ( GHz) : m dishes + 64 MeerKAT 12m dishes, RSA Frequency range: Phase 1 > 50 MHz 3 GHz Phase 2 > up to 15 GHz Cost-cap: 650M Construction for Phase 1: Early science for Phase 1: 2020 SKA-Low ( MHz): low-frequency dipoles, AUS SKA-Survey ( MHz): 60 15m dishes + 36 ASKAP 12m dishes, AUS Exploring the Universe with the World s largest telescope
6 Sensitivity comparison Exploring the Universe with the World s largest telescope
7 Survey speed comparison Exploring the Universe with the World s largest telescope
8 Angular Resolution (arcsec) Andrea Isella Ground based telescopes JVLA SMA CARMA/PBI Angular resolution comparison 10 Spitzer CCAT GBT SKA - mid 1 JWST 0.1 ALMA mas 0.1 mas 1 um 10 um 100 um 1 mm 1 cm 10 cm 1 m 300 THz 30 THz 3 THz 300 GHz 30 GHz 3 GHz 300 MHz Exploring the Universe with the World s largest telescope
9 Emerging themes for 21 st century astrophysics 20 th Century: We discovered our place in the Universe 21 st Century: We understand the Universe we inhabit Remaining major enigma SKA science drivers: Fundamental Forces and Particles Gravity Radio pulsar tests of General Relativity Gravitational Waves Dark Energy Magnetism Origin and evolution of Cosmic Magnetism Cosmic Origins Galaxies and the Universe Cosmic Dawn, Epoch of Reionization First Galaxies Galaxy Assembly and Evolution Stars, Planets, and Life Protoplanetary disks Biomolecules SETI SKA is a Physics Machine Exploring the Universe with the World s largest telescope
10 Cosmic Origins
11 Probing the early Universe with the 21 cm HI line Neutral Hydrogen 21 cm spin-flip transition provides probe of neutral intergalactic medium before and during formation of first stars/galaxies EoR Cosmic Dawn Dark Ages MHz T b (mk) = 1420 MHz/(1 + z) l = 21 cm (1 + z) Pritchard & Loeb (2010) z 100
12 Review by Mellema et al. (2013) HI surveys of the Cosmic Dawn and the Epoch of Reionization (EoR) Tomography to δt = 1 mk level on a few arcmin scales, required to map out HI temperature fluctuations in the IGM over cosmic time during the Cosmic Dawn and Epoch of Reionization Tomography to δt = 10 mk level over many arcmin scales, required to map out ionized bubbles during the Epoch of Reionization Studying the cosmic reionization using SKA will give new insights on both the nature of the primordial sources and the 3-D maps of HI distribution during the entire epoch of cosmic dawn and reionization at redshifts 6 < z < 27.
13 The billion galaxy survey through HI emission HI galaxy counts Duffy et al. (2012) semi-analytic + N-body simulations galaxies with <z> galaxies with <z> 2 > redshift surveys > large scale structures up to z ~ 5 > HI mass density cosmic evolution Ω HI (z) > galaxy kinematics = dynamical masses > precision cosmology
14 Fundamental Forces and Particles
15 Dark Energy equation of state Universe s composition: 5% of Baryonic Matter 27% of Dark Matter (unknown nature) 68% of Dark Energy (unknown nature) The Universe is accelerating: Dark Energy must counteract/surpass the gravitational attraction caused by Baryonic and Dark Matter. The rate and speed of the formation of galaxy clusters thus is partly due to the balance between gravitational attraction and repulsion induced by Dark Energy. The measure of this rate and speed is a measure of the strength of Dark Energy. Constraining Dark Energy equation of state with: 1. redshift-resolved Baryon Acoustic Oscillation measurements at different z previous surveys: SDSS galaxies with <z> 0.1; BOSS galaxies with <z> 0.57; WigglesZ galaxies with <z> weak gravitational lensing measurements of cosmic shear
16 Systematic survey for pulsars in the Milky Way Cordes et al. (2004); Kramer et al. (2004); Smits et al. (2008) Objective ~ normal pulsars ~ 100 relativistic binaries first pulsars in Galactic Centre first extragalactic pulsars Timing precision is expected to increase by factor ~100 Rare and exotic pulsars and binary systems: including PSR-BH systems! Current estimates are that ~50% of entire Galactic population in reach of SKA
17 Tests of gravity in strong gravitational fields Test General Relativity in strong field regime Direct detection of gravitational waves Pulsar arrival times affected by low-frequency gravitational waves correlated across the sky Tests of GR in strong field regime via: Neutron Star White Dwarf binaries Neutron Star Neutron Star binaries Neutron Star Black Hole binaries In a Pulsar Timing Array (PTA) pulsars act as arms of a cosmic GW detector Sensitive to nhz waves, complementary to LIGO/LISA
18 Cosmic magnetism: rotation measure grid Access to galactic magnetic fields through the measure of the Faraday Rotation induced on the polarization vector of radio waves propagating through magnetized plasma. SKA objectives Derive the large-scale structure of the Galactic magnetic field (and how it got there) RMs are accumulated all along the line of sight > measure the RM signature of clusters and the cosmic web Study the structure of the jets and lobes for extragalactic sources, and how magnetic fields in these sources evolve with redshift
19 Cradle of life Glycine NH 2 CH 2 COOH Holy grail of prebiotic astrochemistry detection of an amino acid in the gas phase Firm detections in meteorites and comets ((Ehrenfreundet al. 2001; Elsila et al. 2009) Not (yet) detected in the ISM Cold cores and disks frozen onto dust grains?
20 Cradle of life Glycine NH 2 CH 2 COOH SKA simulations of the Glycine observations: Glycine lines detected with S/N > 3 in 8 hours with SKA1-MID (model dependent!)
21 More SKA science Exploring the Universe with the World s largest telescope
22 SKA members Australia Canada China Germany Italy Netherlands New Zealand South Africa Sweden UK India Others? Spain, Portugal, Japan, Brasil all interested. USA, but no money. 1M Euros buy in, plus % contributions based on GDP
23 SKA and Switzerland? Astronomers from UniGe, EPFL, and ETHZ have coordinated to reply to the Call for Applications for New Research Infrastructures of National Relevance of January 2014 with the aim to be involved and contribute in the SKA project to the level of at least 50M Euros scattered over more than a decade.
24 Science Phase II : 2024 Phase I : 2020 SKA in a nutshell 250,000 element Low Frequency Aperture Array 96 survey enabled dishes (incl. 36 ASKAP) 254 dishes (incl. 64 MeerKat) >250,000 element Low Frequency Aperture Array Mid Frequency Aperture Array 2500 dishes Cosmic Dawn & Reionzation Cosmology & Pulsars Cosmic Magnetism Cradle of Life Galaxy Evolution Exoplanets Exploration of the Unknown 50 MHz 100 MHz 1 GHz 10 GHz
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If you want to learn more about us, contact us or show up here, we are glad to give you a tour of CENTRA's facilities.
The Multidisciplinar Centre for Astrophysics (CENTRA) is a scientific research centre in IST, with a team in Universidade do Algarve (UAlg) and collaborators at the Universidade da Beira Interior (UBI).
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