1 The Square Kilometre Array Exploring the Universe with the world s largest radio telescope
3 THE SQUARE KILOMETRE ARRAY 01 In the 20th century, we discovered our place in the Universe. Our telescopes have revealed an expanding Universe with billions of galaxies, each filled with stars of all sizes and temperatures, along with black holes, neutron stars, planets and gas clouds. The Square Kilometre Array f The largest and most sensitive radio telescope in the world Members of the SKA Science and Engineering Committee. (Credit: Colin Greenwood) In the 20th century, we discovered our place in the Universe. Our telescopes have revealed an expanding Universe with billions of galaxies, each filled with stars of all sizes and temperatures, along with black holes, neutron stars, planets and gas clouds. In the 21st century, we now seek to understand the complete evolution of our Universe and its constituents. To attack these fundamental questions, a new generation of astronomical facilities is needed with a revolutionary new radio telescope, the Square Kilometre Array, playing a crucial role. Recent, innovative technological developments in both computing and radio frequency devices have made it possible and affordable for the SKA to be built by With an unprecedented large radio wave collecting area, the SKA will be 50 times more sensitive, and be able to survey the sky times faster, than any imaging radio telescope array previously built. By observing a large volume of the Universe, over much of cosmic time, the SKA will answer many of the fundamental questions we are asking now, and many more that we do not yet know to ask.
4 Radio Sky Radio astronomy has produced some of the greatest discoveries of the 20th century. Central to these discoveries have been innovations in technology pushing the observational frontiers of sensitivity as well as spatial, temporal and spectral resolution. One such innovation in technology - radio interferometry - was awarded a Nobel Prize for Physics. The SKA will carry on this tradition of innovation by combining fundamental developments in radio frequency technology, information technology and high-performance computing. The SKA will be the world s premier imaging and surveying telescope with a combination of unprecedented versatility and sensitivity that will open up new windows of discovery. RELATIVE SENSITIVITY 1,000, ,000 10,000 1, RADIO TELESCOPE SENSITIVITY SKA 13 EVLA 12 E-MERLIN 11 GBT 10 GMRT 09 VLA 08 ATCA 07 ARECIBO 06 WSRT 05 EFFELSBERG 04 PARKES 03 JODRELL BANK 02 DWINGELOO 01 REBER YEAR n The galaxies M81 and M82 seen in optical (above top) and radio (above) light. Only the radio observations reveal the interaction between the two galaxies in the form of a gigantic stream of gas. (Credit: KNPO, NRAO) n Sensitivity of the SKA compared to that of other major radio telescopes at time of construction. j The sky seen at optical wavelengths (far left), at a radio frequency of 408 MHz (middle) and at the frequency of emission of neutral hydrogen, MHz (right). (Credit: Axel Mellinger/NASA SkyView, G. Haslam/MPIfR, J. Dickey/NASA SkyView)
5 THE SQUARE KILOMETRE ARRAY 03 RADIO EMISSION Introduction f The SKA - A revolution in Astronomy CORRELATOR ASTRONOMICAL IMAGES RADIO CROSS-POWER SPECTRA PRECISE POSITIONS OF THE RADIO SOURCES PRECISE ANTENNA LOCATIONS RADIO EMISSION n An aperture synthesis telescope consists of many independent receiving elements whose signals are combined at a central processing site forming a high-resolution image of the observed object. RADIO EMISSION n With multiple fields-of-view provided by phased array technology many astronomers can use the SKA telescope at the same time. (Credit: M. Kramer) The SKA will be an aperture synthesis instrument. Signals from separated antennas will be combined digitally to produce a telescope with a diameter equal to the largest antenna separation - more than 3000 km. This will give an extremely high angular resolution, so that the SKA will continue radio astronomy s tradition to produce the sharpest pictures of the sky. The SKA will also have a very large field-of-view (FOV). The goal is an FOV at low frequencies below 1 GHz of 200 square degrees, and an FOV of more than 1 square degree (about 5 full moons) at higher frequencies. One exciting development being explored is the use of phased array technology to provide multiple FOVs. This would dramatically increase the survey speed of the SKA or enable multiple users to observe different pieces of the sky simultaneously. The goal of achieving a large sky coverage with multiple FOVs is a major driver of the challenging signal processing and computing specifications for the SKA. The combination of a very large FOV with enormous sensitivity and diverse operation modes means that the SKA will provide a revolution in the way that we explore the Universe.
6 The SKA Program is a collaboration between institutions in 20 countries including Australia, Brazil, Canada, China, France, Germany, India, Italy, Japan, Korea, The Netherlands, New Zealand, Poland, Portugal, Russia, South Africa, Spain, Sweden, United Kingdom and the United States.
7 THE SQUARE KILOMETRE ARRAY 05 The SKA Program The collaboration is led by an international steering committee and a jointly funded SKA Program Development Office. TIMELINE 2024 FULL OPERATION 2019 FIRST ASTRONOMICAL OBSERVATIONS 2016 INITIAL CONSTRUCTION DETAILED DESIGN AND PRODUCTION ENGINEERING SITE SELECTION FUNDING APPROVAL FOR INITIAL (10% SKA) CONSTRUCTION. ESTABLISH SKA ORGANISATION SYSTEM DESIGN AND COSTING 2006 SHORTLISTING OF SUITABLE SITES 1991 SKA CONCEPT The SKA will: [ Be the largest radio telescope in the world. [ Revolutionise our understanding of the Universe and the laws of fundamental physics. [ Have 50 times the sensitivity and 100 times the survey speed of current imaging instruments. [ Extend to at least 3000 km from the central core region. [ Have half the total collecting area of each antenna type concentrated in three central cores each 5 km in diameter. [ Have life span of at least 50 years. [ Be continuously upgradable as computing power increases. [ Be built in a radio-quiet location for uninterrupted observations. [ Use new antenna technology, signal transport, signal processing and computing. [ Have a target construction budget of 1.5 billion for the frequency range from 70 MHz to 10 GHz. As the SKA will be an aperture synthesis instrument, exciting science will be achievable before the full array is complete and initial science results are expected by about The full collecting area at frequencies below about 10 GHz will be operational in 2024.
8 The SKA will consist of an inner core and outer stations arranged in a logspiral pattern and extending to distances of up to km on the right side. A combination of receiving elements, dishes and phased array technology will be exploited to make the SKA versatile, flexible and cost-effective.
9 THE SQUARE KILOMETRE ARRAY 07 THE SKA FOV COMPARED TO ALMA AT λ 3 mm ALMA SKA (LOW FREQ) SKA (HIGH FREQ) PARAMETER FREQUENCY RANGE SENSITIVITY AREA / SYSTEM TEMP SURVEY FIGURE-OF-MERIT FIELD-OF-VIEW ANGULAR RESOLUTION INSTANTANEOUS BANDWIDTH SPECTRAL (FREQUENCY) CHANNELS CALIBRATED POLARISATION PURITY SYNTHESISED IMAGE DYNAMIC RANGE IMAGING PROCESSOR COMPUTATION FINAL PROCESSED DATA OUTPUT Specifications The final design of the SKA will be determined from the outcome of the extensive prototyping and costing exercise that is currently underway. The specifications of the reference design for frequencies up to 10 GHz are listed in the following table. The top level specifications of the SKA at frequencies above 10 GHz have yet to be considered in detail. The extension of the array to these higher frequencies is expected to take place in SPECIFICATION 70 MHz TO 10 GHz M 2 /K (400 µjy IN 1 MINUTE) BETWEEN 70 AND 300 MHz 4x10 7 2x10 10 m 4 K -2 deg 2 DEPENDING ON SENSOR TECHNOLOGY AND FREQUENCY 200 SQUARE DEGREES BETWEEN 70 AND 300 MHz SQUARE DEGREES BETWEEN 0.3 AND 1 GHz 1 SQUARE DEGREE MAXIMUM BETWEEN 1 AND 10GHz <0.1 ARCSECOND BAND CENTRE ± 50% PER BAND PER BASELINE :1 > OPERATIONS/SECOND 10 GB/SECOND MID FREQUENCY APERTURE ARRAYS LOW FREQUENCY APERTURE ARRAYS n Fifty percent of the SKA s total collecting area will be concentrated in the central core region. (Credit: SPDO) 15KM 200KM DIAMETER DISHES 5KM LONG BASELINE STATIONS AT DISTANCES OF AT LEAST 3000KM n The SKA will consist of an inner core and outer stations arranged in a log- spiral pattern and extending to distances of up to km on the right side. A combination of receiving elements, dishes and phased array technology, will be exploited to make the SKA versatile, flexible and cost-effective. (Credit: SPDO)
10 (Credit: T.A. Oosterloo/ASTRON) (M. Bietenholz/York/NRAO) The SKA will observe the very first black holes, stars, and galaxies that shaped the development of the Universe during this important time. The SKA will even be able to detect black holes accreting during the Dark Ages. (Credit: MERLIN) (Credit: W. Reich/MPIfR) (Credit: Kassim/NRL/NRAO)
11 THE SQUARE KILOMETRE ARRAY 09 Transformational Science The SKA will be a highly flexible instrument designed to address a wide range of fundamental questions in astrophysics, fundamental physics, cosmology, particle astrophysics and astrobiology. It will be able to probe previously unexplored parts of the Universe. The diverse spectrum of scientific topics that the SKA can tackle is presented comprehensively in Science with the Square Kilometre Array (Elsevier). From this wealth of possible science a number of key science projects addressing physics beyond our current understanding have been selected: [ Probing the Dark Ages - the first black holes and stars [ Galaxy evolution, cosmology and dark energy [ The origin and evolution of cosmic magnetism [ The cradle of life - searching for life and planets [ Extreme tests of general relativity with pulsars and black holes While these projects address important scientific questions of our time, we cannot foresee the unexpected discoveries that the SKA will make. What is clear is that our understanding of the Universe and its fundamental physics and complexity will be transformed by the SKA. One of the design goals is therefore to maximise the SKA s ability to explore the unknown. n Simulated image showing the neutral hydrogen sky in the early Universe as seen by the SKA, revealing the structure of the cosmos. (Credit: I. Iliev, G. Mellema and collaborators/u. Toronto) j Comparison of current radio observations (far left) and a simulation of SKA observations (left) showing the greatly increased number of faint galaxies expected in observations of the continuum radio sky. (Credit: C. Jackson/ATNF)
12 KEY SCIENCE PROJECT: Probing the dark ages the first black holes and stars f What happened after the Big Bang and before the first stars and galaxies formed? Which came first - stars or galaxies? After the Big Bang the Universe expanded and cooled, turning the hot primordial soup of particles into a sea of neutral gas. The process started the period in the evolution of the Universe referred to as the Dark Ages. As the name suggests, there was no light in the Universe during the Dark Ages except for the faint glow remaining from the Big Bang. The small density inhomogeneities left over from the period of fast initial expansion gradually grew under the force of gravity, and eventually formed the first stars and galaxies. The light from these first objects slowly reionised the whole intergalactic medium and ended the Dark Ages. Radio emission in the 21-cm line of neutral hydrogen (HI), as well as molecular lines like those from carbon monoxide (CO) provide the best observational windows through which to detect directly the era when gas in galaxies was first turned into stars. The SKA will be the only telescope able to directly detect this distant epoch, thus providing our best option to look at the first few hundred million years of the evolution of the Universe and the first stars. Moreover, HI 21-cm studies of the neutral intergalactic medium may be the most important window on cosmology since the discovery of the cosmic microwave background. Accreting black holes, such as those forming just after the Dark Ages, may very well be radio signposts of the first structures forming. Not only are these first supermassive black holes important in understanding how galaxies formed, they may also be important in influencing their environment. The SKA will observe the very first black holes, stars and galaxies that shaped the development of the Universe during this important time. The SKA will even be able to detect black holes accreting during the Dark Ages. The SKA will provide detailed pictures and full 3-D maps of the early cosmic web of neutral gas, essential to understand the Universe that we live in today. n The cosmic web of early structures. Galaxies (bright points) form along filaments and sheets in a honey-comb fashion surrounding vast low-density voids (dark regions). (Credit: I. Iliev, G. Mellema)
13 THE SQUARE KILOMETRE ARRAY 11 x HI =0.79 x HI =0.61 x HI =0.42 x HI =0.20 n Simulation snapshot of the complex geometry of reionisation. The galaxies are shown as dark dots, the ionised gas surrounding them is light orange and the neutral gas which the SKA will see is dark green. (Credit: I. Iliev, G. Mellema) j Pockets of neutral gas (black) becoming more ionised (white) with increasing age of the Universe. The cube is 100 Mpc on a side. (Credit: S. Furlanetto) 0 (ARCMIN) V (MHz) j Simulated evolution of the 21-cm emission of neutral hydrogen from the Dark Ages through the epoch of reionisation. Light shows the neutral areas, dark the ionised ones. Horizontally going to the left we look back in time (lower frequency), while the vertical scale shows angle on the sky. The SKA should be able to see this evolution in detail. (Credit: I. Iliev, G. Mellema) n The giant elliptical galaxy, NGC1316 or Fornax A, shown in the radio (orange) superimposed on an optical image. The radio emission consists of two large radio lobes, each about light years across. The giant elliptical galaxy at the centre is cannibalising a smaller galaxy, stripping away material from it that spirals toward a super-massive black hole at the centre of its larger neighbour. (Credit: NRAO, STSci/POSS-II)
14 KEY SCIENCE PROJECT: Galaxy evolution, cosmology and dark energy f What is the mysterious dark energy? How are galaxies born and how do they evolve? DARK ENERGY 73% COLD DARK MATTER 23% NORMAL MATTER 04% n Illustration of the recent finding that the vast majority of the Universe is filled with some unknown dark energy and the yet to be identified cold dark matter. There may also be a significant fraction of hot dark matter. Only a small fraction of the Universe is made up of the normal matter that consists of atoms. The evolution of the Universe and the formation of large scale structure appear to be governed by the strange action of a dark energy. Apart from the observed fact that dark energy has caused a recent acceleration in the expansion of the Universe, its properties are virtually unknown. The structure of the Universe can be determined by observing the cosmic distribution of nature s most fundamental element - hydrogen. Hydrogen is the most abundant element in the Universe and the raw material from which stars form. It is now well established that the rate of star formation in galaxies has evolved dramatically over the last half of the Universe s lifetime. Yet over the same interval, the amount of neutral hydrogen gas appears to have barely changed. Gaining a thorough understanding of galaxy assembly, growth, and evolution remains one of the key challenges for astrophysics. By investigating how galaxies turn gas into stars, the SKA will allow us to understand galaxy formation and evolution. The SKA will track how neutral hydrogen flows into and out of galaxies and will also be able to monitor how gas is exchanged or lost as groups and clusters of galaxies interact with each other. With these data the SKA will measure the geometry of the Universe, and test whether dark energy is a vacuum energy or something more exotic, perhaps providing evidence of genuinely new physics or extra dimensions. Revealing the large-scale structure of the Universe with the SKA will also allow the determination of both the neutrino mass scale and the number of massive neutrinos, connecting astrophysics with particle physics. The SKA and its wide FOV will allow the accurate determination of the rate of evolution in the equation of state of dark energy with cosmic time.
15 THE SQUARE KILOMETRE ARRAY 13 r A simulated SKA observing cone depicting the complex filamentary structure of HI on cosmic scales, which encodes the mysterious physics of the Dark Universe. Each coloured pixel in the cone represents a galaxy emitting neutral hydrogen (HI, rest-frame 21-cm) radiation. (Credit: Danail Obreschkow (Oxford) and the SKADS Sky Simulation team) Wm Wm -2 85MPC = 1 SKA 0 n Combined optical (colours) and radio (contours) image showing the gravitational lens system B where dark matter associated with two galaxies produces multiple images of a background source. (Credit: HST/STScI, MERLIN) 1 A SIMULATED SKA OBSERVING CONE 85MPC Z n Simulation of the filamentary structure of the dark matter today. (Credit: Millennium Gas simulation by F. Pearce/Virgo Consortium)
16 KEY SCIENCE PROJECT: The origin and evolution of cosmic magnetism f Where do we find cosmic magnets and what do they look like? What generates these giant magnetic fields in space? How does magnetism affect the formation of stars and galaxies? r Magnetic fields play important roles in the Universe. This shows magnetic field loops in the Sun s corona in X-ray light. (Credit: TRACE mission/nasa) One of the many remarkable discoveries made by 20th century astronomers was that stars, planets, galaxies, and even diffuse interstellar gas, are all magnetic. Surprisingly, our Universe seems to be free of magnetic charges (monopoles) which would quickly destroy any magnetic field, ensuring that magnetism is long lived. These cosmic magnetic fields play a vital role in controlling how stars and galaxies form, age and evolve. In addition, this naturally occurring magnetism regulates solar activity and space weather, protects the Earth from harmful particles, and is vital for the navigation of birds and other species. However, in spite of the importance and ubiquity of astrophysical magnets, we do not understand what creates them, or how they maintain their strength over billions of years of cosmic time. With the SKA, we can finally open the window to this magnetic Universe. Magnetic fields are illuminated by electrons spiralling around the field lines which emit radio waves, called synchrotron emission. Astronomers will also use the SKA to exploit an effect called Faraday rotation, in which polarised radio light from a background object is subtly changed when it passes through a cloud of gas in which significant magnetism is present. By measuring Faraday rotation in the radio emission from tens of millions of faint, distant, galaxies, the SKA will be able to detect magnetic fields throughout the Universe. The resulting three-dimensional maps of magnetism in the Milky Way, in nearby galaxies and in intergalactic space will reveal what cosmic magnets look like, where they have came from, and what role they have played in the evolving Universe.
17 THE SQUARE KILOMETRE ARRAY 15 j Two possible sources for the intergalactic magnetic field are the jets in Active Galactic Nuclei (AGNs) and Pulsar Nebulae. These images show the well studied examples of the AGN and surrounding radio galaxy 3C153 (top) and the Crab supernova remnant (bottom) which harbours a radio pulsar. (Credit: NRAO) n The SKA will investigate cosmic magnetism by observing Faraday rotation of polarised radio waves. j Optical image of the spiral galaxy M51 with the magnetic field determined from radio observations superimposed. (Credit: Hubble Heritage/NASA/ STSci, R. BECK/MPIfR)
18 KEY SCIENCE PROJECT: The cradle of life - searching for life and planets f Are we alone in the Universe? Do Earth-like planets orbit other stars? Could the complex molecules in star forming regions be the starting point for life? n Concept of an extrasolar planet. (Credit: NASA) The first of these questions is one of the most fundamental problems that has been contemplated by humanity across the ages. The 21st century may see this question answered definitively, with the SKA playing a key role. The first decade of the 21st century has seen an explosion in the number of planets known outside the solar system. None of these are known to harbour life. Yet, the possibility of finding life-supporting planets has moved from mere speculation to being a goal of astronomers. Observations with the SKA will contribute to a wide range of astrobiological goals, from understanding how planets form, to searching for more planets and to the understanding of the planets detected. The gas from which stars form is known to contain surprisingly complex organic molecules. Today, molecules containing as many as 13 atoms are known. Do even more complex molecules exist? Might some of these complex molecules include the building blocks of life? With its exquisite sensitivity, the SKA will be able to probe for even more rare and exotic species of molecules. Most of the planets in the Milky Way Galaxy may orbit stars that are small and cool, known as M dwarves. The SKA s superb angular resolution will also enable it to monitor the motions of these stars, looking for any tell-tale wobbles due to orbiting planets. The Earth s radio wave radiation is generated by humans, by our TV transmitters, radars, and other transmissions. Detection of artificial transmissions from a planet around another star would be the most compelling evidence for life elsewhere and a profound moment for all of humanity. While searches for extraterrestrial transmission have been conducted before, the SKA sensitivity will allow for the first time signals to be detected from nearby stars that are no stronger than those generated by our own 21st century TVs and radars.
19 THE SQUARE KILOMETRE ARRAY 17 jr The cycle of life. Interstellar gas and molecules form stars, planetary disks and finally planets, before a dying star redistributes the ingredients back into space. During this cycle complex organic molecules are formed. (Credit: B. Saxton/NRAO)
20 KEY SCIENCE PROJECT: Extreme tests of general relativity with pulsars and black holes f Was Einstein right or will general relativity eventually fail? What are the properties of black holes? Are there still ripples in space-time from the early Universe? n Pulsar orbiting a black hole. Einstein s theory of general relativity has passed all tests with flying colours, so far. But, it may still not be the last word in our understanding of nature s most fundamental force - gravity. Scientists around the world are struggling to find a theory of quantum gravity which would combine gravitation with the bizarre world of quantum physics. We can confront Einstein s predictions and those of other theories of gravity experimentally by exploiting the Universe s best clocks - pulsars. The SKA will discover tens of thousands of them, some of which will orbit stellar-sized and supermassive black holes. These systems can be used to put Einstein s theories to the most extreme test ever, in particular general relativity s description of black holes. Most theories of gravity also predict ripples in space-time which propagate through the Universe as gravitational waves. While pulsars provide the only evidence for the existence of gravitational waves so far, they do not only produce them but observations of pulsars can also lead to the detection of gravitational waves. Using pulsars, the SKA will act as a huge gravitational wave detector, discovering and studying spacetime ripples left over from the early Universe from exotic phenomena like cosmic strings or merging super-massive black holes. The SKA will be sensitive to nano-hz frequencies which are much lower than those probed by ground-based detectors such as the Laser Interferometer Gravitational-wave Observatory (LIGO) or spacebased detectors like the Laser Interferometer Space Antenna (LISA).
21 THE SQUARE KILOMETRE ARRAY 19 r The best test so far of Einstein s theory in strong gravitational fields is provided by the only known double pulsar system, where two pulsars orbit each other in 145 min. (Credit: M. Kramer) r Pulsars discovered and monitored with the SKA will act like a cosmic gravitational wave detector, allowing the study of ripples in the fabric of spacetime that propagate at ultra-low frequencies. (Credit: D. Champion, M. Kramer) n Pulsars orbiting black holes will test Einstein s description of these enigmatic objects to the extreme. (Credit: M. Kramer)
22 FLEXIBLE DESIGN: Exploration of the unknown f Can we predict everything in the Universe on the basis of what we know now? What else will we discover when exploring the cosmic frontier? Radio astronomy was responsible for many of the fundamental discoveries in physics and astrophysics in the last century. The list is long and includes: [ The cosmic microwave background [ Quasars [ Pulsars [ Gravitational lenses [ Masers [ Gravitational waves [ Interstellar molecules [ The first extrasolar planets [ Galactic magnetic fields [ Dark matter and many more. Many of the discoveries happened unexpectedly, so we should be prepared for the possibility. However, the scientific challenges outlined in previous pages are today s most exciting problems - will they still be the outstanding problems that will confront astronomers and humankind in the period 2020 to 2050 and beyond, when the SKA will be in its most productive years? If history is any example, the excitement of the SKA may not arise out of current questions, but from new questions that will be raised by the new types of observations that the SKA will permit. The SKA is a tool for as-yet-unborn users, and so the SKA will be a versatile, multi purpose instrument whose flexibility allows us to expect the unexpected. The unique sensitivity, the possibility of multiple independent beams on the sky, and the extremely large field-of-view make the SKA a discovery machine. We cannot predict what we will find, but we know it will surprise us. n Cosmic explosions of unknown type may be detectable as radio signals with the SKA. (Credit: NASA) j Image of the cosmic microwave background radiation (CMB) anisotropy. (Credit: WMAP/NASA))
23 THE SQUARE KILOMETRE ARRAY 21 SKA Engineering f The SKA - a technological and engineering challenge n Complete integrated-circuit receivers based on CMOS technology. (Credit: (left) S. Jackson/CSIRO & Macquarie Univ., (right) University of Calgary) PEAK SPEED (FLOPS) DOUBLING TIME = 1.5YR YEAR INTRODUCED n According to Moore s law, computer power doubles every 18 months. By the time of completion of the SKA, computers should be 100 times more powerful than today. (Credit: M. Kramer) SKA 09 BLUE GENE/P 08 LOFAR 07 BLUE GENE/L 06 PARAGON 05 CRAY-2 04 CYPER CDC IBM UNIVAC The SKA demands new approaches to designing radio telescopes. The path to the SKA involves mass producing low-cost antennas and using programmable signal processing engines, or even general-purpose computers, within the instrument s signal path. Pushing the instrument in the direction of a software telescope allows designers to take advantage of Moore s law for digital hardware - processing power doubles every 18 months. Even with the expertise of a multi-national collaboration, the scale of the SKA makes it challenging to translate the SKA concept into the world s foremost radio astronomical facility. New technology, and progress in fundamental engineering science are both required. These breakthroughs can only happen with the collaboration of industrial partners offering expertise in fields such as information and communication technology, high performance computing and mass production manufacturing techniques. Areas of particular relevance include: [ Low-cost collecting area [ Low-noise, highly integrated, receivers [ Phased array antenna technology [ Wideband optical fibre signal transport systems [ Fast, high resolution, analogue-to-digital converters [ High-performance computing engines [ Data storage and innovative retrieval technologies. In order to achieve both high brightness sensitivity and high resolution images of the radio sky, the elements of the SKA will be distributed in an inner array and in groups of receiving elements located further away from the core. The signals will be transported from the stations back to a central processing engine where the data are manipulated to form images and time series, and to combat the effects of harmful radio frequency interference (RFI) signals. r Receiving elements used in phased-array technology. (Credit: NRC/DRAO)
24 To meet the requirements for the wide frequency range, and to enable multiple fields-of-view at low frequencies, at least three antenna concepts will need to be implemented.
25 THE SQUARE KILOMETRE ARRAY 23 SKA Engineering f Antenna Engineering - Overcoming the cost barrier The key feature of the SKA - its enormous collecting area - can only be realised by moving away from traditional telescope designs and by constructing efficient, broadband, low-cost antennas capable of multiple beam operation. This goes hand-in-hand with the development of low-cost, low-noise radio frequency amplifiers and highly-integrated receivers. Several innovative approaches are being investigated to find an optimum enabling technology solution for the key science projects. To meet the requirements for the wide frequency range, and to enable multiple fields-of-view at low frequencies, at least three antenna concepts will need to be implemented. n Some of the antenna concepts under investigation for the SKA. Far right: sparse aperture array dipoles. Middle right: dense aperture array tiles. Above: high frequency dishes. (Credit: Xilostudios)
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Enter your answers on the form provided. Be sure to write your name and student ID number on the first blank at the bottom of the form. Please mark the version (B) in the Key ID space at the top of the
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Resolution Astronomers need to be able to look at objects in the sky with high precision. Resolution, or resolving power, is a measure of how well an eye, or a telescope, can do this. It is measured by
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First Discoveries The Sloan Digital Sky Survey began operating on June 8, 1998. Since that time, SDSS scientists have been hard at work analyzing data and drawing conclusions. This page describes seven
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