Prototype SKA Technologies at Molonglo: 1. Overview and Science Goals A.J. Green 1, J.D. Bunton 2, D. Campbell-Wilson 1, L.E. Cram 1, R.G. Davison 1, R.W.

Slides:



Advertisements
Similar presentations
SKAMP Square Kilometre Array Molonglo Prototype. Supporting Institutions  University of Sydney  Argus Technologies  ATNF  ICT Centre.
Advertisements

Molonglo SKA Prototyping and MNRF
29 Jan 2003 ANITA Workshop - SKAMP & VO Considerations - G. "Ñima" Warr 1 The SKAMP Project & Virtual Observatory Considerations.
Arecibo 40th Anniversary Workshop--R. L. Brown The Arecibo Astrometric/Timing Array Robert L. Brown.
MeerKAT Large Survey Projects SAAO Board, Roy Booth (SA SKA Project)
Cosmology using 21 cm emission Jeff Peterson, CMU Talk 1…Update on early ionization telescopes (LOFAR, PAST, GMRT) Talk 2…Proposed Redshift survey.
HI Stacking: Past, Present and Future HI Pathfinder Workshop Perth, February 2-4, 2011 Philip Lah.
Comparison of SKA Survey Speeds John D. Bunton, CSIRO TIP Figures of Merit SKA survey bandwidth can be large e.g. HI for redshifts up to 4. Thus it is.
Probing the field of Radio Astronomy with the SKA and the Hartebeesthoek Radio Observatory: An Engineer’s perspective Sunelle Otto Hartebeesthoek Radio.
HI in galaxies at intermediate redshifts Jayaram N Chengalur NCRA/TIFR Philip Lah (ANU) Frank Briggs (ANU) Matthew Colless (AAO) Roberto De Propris (CTIO)
HI from z ~ 0 – 1 with FAST D.J. Pisano West Virginia University NRAO.
SKAMP - the Molonglo SKA Demonstrator M.J. Kesteven CSIRO ATNF, T. J. Adams, D. Campbell-Wilson, A.J. Green E.M. Sadler University of Sydney, J.D. Bunton,
The SKA Molonglo Prototype (SKAMP) Project Molonglo 40th Anniversary, November 2005.
2 Jul 2002 ASA-SKAMP 1 The Square Kilometre Array Molonglo Prototype (SKAMP) Molonglo AUSTRALIA Brisbane Darwin Perth Canberra Hobart Adelaide Melbourne.
SKAMP - the Molonglo SKA Demonstrator M.J. Kesteven CSIRO ATNF, T. J. Adams, D. Campbell-Wilson, A.J. Green E.M. Sadler University of Sydney, J.D. Bunton,
Fundamentals of Radio Astronomy Lyle Hoffman, Lafayette College ALFALFA Undergraduate Workshop Union College, 2005 July 06.
Prototype SKA Technologies at Molonglo: 1. Overview and Science Goals A.J. Green 1, J.D. Bunton 2, D. Campbell-Wilson 1, L.E. Cram 1, R.G. Davison 1, R.W.
Transient Science with the Allen Telescope Array Geoff Bower Berkeley.
The Future of the Past Harvard University Astronomy 218 Concluding Lecture, May 4, 2000.
Prototype SKA Technologies at Molonglo: 2. Antenna and Front End G.B. Warr 1,2, J.D. Bunton 3, D. Campbell-Wilson 1, R.G. Davison 1, R.W. Hunstead 1, D.A.
Sascha D-PAD Sparse Aperture Array.
Prototype SKA Technologies at Molonglo: 3. Beamformer and Correlator J.D. Bunton Telecommunications and Industrial Physics, CSIRO. Australia. Correlator.
Cylindrical Reflector SKA Update
The SKA Molonglo Prototype (SKAMP) Project SKA Meeting - April 2006 Anne Green.
Project status and specifications Douglas Bock Project Manager 1.
Telescopes of the future: SKA and SKA demonstrators Elaine Sadler, University of Sydney Aperture synthesis techniques have now been in use for over 40.
Panorama of the Universe: Daily all-sky surveys with the SKA John D. Bunton, CSIRO TIP, Ronald D. Ekers, CSIRO ATNF and Elaine M. Sadler, University of.
July 2001SKA Technologies at Molonglo1 Prototype SKA technologies at Molonglo – 1. Overview & Science Goals Joint project between the University of Sydney,
3 Oct 2001 Adelaide SKA Symposium-Prototyping SKA Technologies at Molonglo 1 Prototyping SKA Technologies at Molonglo Molonglo AUSTRALIA Brisbane Darwin.
What’s Going on in Canada?
High-Frequency GPS sources from the AT20G survey Paul Hancock - University of Sydney Australia Ron Ekers (ATNF, PI), Sarah Burke(Swinburne), Mark Calabretta.
The SKA Molonglo Prototype (SKAMP) Project MNRF Symposium Report, June 2005.
Multiwavelength Continuum Survey of Protostellar Disks in Ophiuchus Left: Submillimeter Array (SMA) aperture synthesis images of 870 μm (350 GHz) continuum.
HI absorption-line science: exciting opportunities with ASKAP- 12 Elaine Sadler University of Sydney / CAASTRO on behalf of the ASKAP FLASH team 5 August.
“First Light” From New Probes of the Dark Ages and Reionization Judd D. Bowman (Caltech) Hubble Fellows Symposium 2008.
Solar observation modes: Commissioning and operational C. Vocks and G. Mann 1. Spectrometer and imaging modes 2. Commissioning proposals 3. Operational.
LBA Calibrator Survey Chris Phillips eVLBI Project Scientist 23 July 2009.
Wideband Imaging and Measurements ASTRONOMY AND SPACE SCIENCE Jamie Stevens | ATCA Senior Systems Scientist / ATCA Lead Scientist 2 October 2014.
10 January 2006AAS EVLA Town Hall Meeting1 The EVLA: A North American Partnership The EVLA Project on the Web
ATLASGAL ATLASGAL APEX Telescope Large Area Survey of the Galaxy F. Schuller, K. Menten, P. Schilke, et al. Max Planck Institut für Radioastronomie.
Molecular Gas and Dust in SMGs in COSMOS Left panel is the COSMOS field with overlays of single-dish mm surveys. Right panel is a 0.3 sq degree map at.
The Murchison Wide Field Array Murchison, ~300 km from Geraldton.
Mileura Widefield Array – Low Frequency Demonstrator MHz * Currently in “Early Deployment” phase Goal: HI at redshift 6 to 17.
Australian Astronomy MNRF Development of Monolithic Microwave Integrated Circuits (MMIC) ATCA Broadband Backend (CABB)
Arecibo Frontiers – 12 Sep Beyond the Frontiers: The Road From Arecibo to The Radio Synoptic Survey Telescope (RSST) Steven T. Myers National Radio.
S.A. Torchinsky SKADS Workshop 10 October 2007 Simulations: The Loop from Science to Engineering and back S.A. Torchinsky SKADS Project Scientist.
Imaging Molecular Gas in a Nearby Starburst Galaxy NGC 3256, a nearby luminous infrared galaxy, as imaged by the SMA. (Left) Integrated CO(2-1) intensity.
LOFAR LOw Frequency Array => most distant, high redshift Universe !? Consortium of international partners… Dutch ASTRON USA Haystack Observatory (MIT)
Centre of Excellence for All-sky Astrophysics MWA Project: Centre of Excellence for All-sky Astrophysics Centre of Excellence for All-sky.
Murchison Widefield Array (MWA) : Design and Status Divya Oberoi, Lenoid Benkevitch MIT Haystack Observatory doberoi, On behalf.
Manchester April The Structure of Radio Sources The Molonglo Papers The Structure of Radio Sources The Molonglo Papers Resolving the Sky with radio.
Observing Strategies at cm wavelengths Making good decisions Jessica Chapman Synthesis Workshop May 2003.
ALMA and the Call for Early Science The Atacama Large (Sub)Millimeter Array (ALMA) is now under construction on the Chajnantor plain of the Chilean Andes.
ALMA Science Examples Min S. Yun (UMass/ANASAC). ALMA Science Requirements  High Fidelity Imaging  Precise Imaging at 0.1” Resolution  Routine Sub-mJy.
The Allen Telescope Array Douglas Bock Radio Astronomy Laboratory University of California, Berkeley Socorro, August 23, 2001.
Review of developments in Australasia and mainland Asia Steven Tingay Swinburne University of Technology Next Generation correlator meeting, JIVE 27 -
Bright & Dark Galaxies from the HIPASS Radio Survey Marianne T. Doyle *1, Michael J. Drinkwater 1, David J. Rohde 1, Mike Read 2, Baerbel S Koribalski.
Foreground Contamination and the EoR Window Nithyanandan Thyagarajan N. Udaya Shankar Ravi Subrahmanyan (Raman Research Institute, Bangalore)
Observed and Simulated Foregrounds for Reionization Studies with the Murchison Widefield Array Nithyanandan Thyagarajan, Daniel Jacobs, Judd Bowman + MWA.
17 Dec 2004 E.M. Sadler 1 University of Sydney Facilities Sydney University Stellar Interferometer (SUSI) Molonglo Radio Telescope (MOST/SKAMP) Used for.
Galactic Legacy Projects Naomi McClure-Griffiths Australia Telescope National Facility, CSIRO NRAO Legacy Projects Meeting, 17 May 2006.
1 ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) Netherlands Institute for Radio Astronomy Astronomy at ASTRON George Heald.
Multi-beaming & Wide Field Surveys
Early Continuum Science with ASKAP
Phased Array Feeds Wim van Cappellen
MPIfR Results from the A. Chippendale ATUC, 14 Nov 2016
Pulsar Timing with ASKAP Simon Johnston ATNF, CSIRO
Some Illustrative Use Cases
Survey Science with the SKA Molonglo Pathfinder
SKAMP Square Kilometre Array Molonglo Prototype
Presentation transcript:

Prototype SKA Technologies at Molonglo: 1. Overview and Science Goals A.J. Green 1, J.D. Bunton 2, D. Campbell-Wilson 1, L.E. Cram 1, R.G. Davison 1, R.W. Hunstead 1, D.A. Mitchell 1,3, A.J. Parfitt 2, E.M. Sadler 1, G.B. Warr 1,3 1 School of Physics, University of Sydney, 2 Telecommunications and Industrial Physics, CSIRO, 3 Australia Telescope National Facility, CSIRO. Australia. Abstract The Molonglo radio telescope in south-east Australia is an east- west array of two colinear cylindrical paraboloids with a total length of 1.6 km. Its collecting area is the largest of any radio telescope in the Southern Hemisphere. We propose to equip the telescope with new feeds, low-noise amplifiers, digital filterbank and FX correlator as an SKA demonstrator with continuous frequency coverage in multibeam mode from MHz. This will allow us to develop and test several new technologies as well as providing a sensitive astronomical instrument for exploring the distant universe. Funding for this project is currently being sought from the Australian Government's Major National Research Facilities (MNRF) program. SKA Technologies Our goals in this project are to develop and test technologies relevant to the SKA, and to apply them to a range of science projects. The ‘signal path’ diagram shows how these technologies fit together - more details of the individual components are given in two companion posters. Important features of the telescope include: Multibeaming Wide instantaneous field of view Digital Beamforming FX Correlators Frequency and Pointing Agility Wideband linefeeds and LNAs Cylindrical Antenna Prototype – in particular addressing Polarisation purity Beam variability/stability Inter-antenna patch coupling Adaptive Null steering and Adaptive Noise cancellation Target Specifications The science goals listed below take advantage of several unique features of the Molonglo telescope - its large collecting area, wide field of view and fully-sampled uv coverage (i.e. excellent sensitivity to diffuse and extended radio sources with complex structure). The new system will give continuous spectral coverage over the range MHz, re-opening the low- frequency radio spectrum in the southern hemisphere. Low-frequency radio spectrometry ( MHz) Selection of objects via their radio spectral shape, e.g. candidate high-redshift (z>3) galaxies with ultra-steep radio spectra (de Breuck et al. 2000), which allow us to study the formation of galaxies and massive black holes. Redshifted HI ( MHz) HI in absorption against bright continuum sources over a wide redshift range (z=0 to 3). HI in emission - evolution of the HI mass function from z=0 to 0.5. Will be able to detect a bright spiral galaxy (2.5 x solar masses of HI,  V=200 km/s) at z=0.1 in 12 hours (see figure opposite). Low-frequency Galactic recombination lines Recombination lines of carbon and hydrogen can be used to probe the partially-ionized ISM and constrain the physical conditions (Anantharamaiah & Kantharia 1999). Gamma Ray Bursters Electronic beam steering gives 5% chance of monitoring instantaneously on alert. Concurrent Pulsars and Source Flux Monitoring 18 to 400 square deg 2 accessible around main beam. Real time dedispersion. Pulsar and SETI Searches (optional 64 fanbeam system) Fast high sensitivity search. Molonglo Continuum Confusion (10 beams/source) at  =  60° Bock et al 1999 SUMSS 843 MHz Rengelink et al 1997 WENSS 325 MHz Wall MHz beam size: 43” x 43” csc|  | beam size: 112” x 112” csc|  | beam size: 26” x 26” csc|  | The analog delay line beamformer reduces the meridian distance range (dark blue). The imaging beam (light blue) is formed in the middle of this range. The independent fanbeam (yellow) can be placed anywhere within this range. Optionally, 64 fanbeams can be formed within the imaging beam. References K.R. Anantharamaiah and N.G. Kantharia (1999). In “New Perspectives on the ISM”, ASP 168, 197 D. G. Barnes et. al. (2001) MNRAS D. C.-J. Bock, M. I. Large and E. M. Sadler (1999). AJ C. de Breuck, W. van Breugel, H. Rottgering and G. Miley (2000). A & AS 143, 303 R. B. Rengelink, Y. Tang, A. G. de Bruyn, G. K. Miley, M. N. Bremer, H. J. A. Röttgering and M. A. R. Bremer (1997). Astron. Astrophys. Suppl. Ser J. V. Wall (1994). Aust. J. Phys Further Information The Molonglo Telescope has been operated by the University of Sydney since Major achievements include the Molonglo Reference Catalogue (MRC; 408 MHz) and a sensitive all-sky imaging survey, the Sydney University Molonglo Sky Survey (SUMSS; 843 MHz) which will be completed in Observing Modes The telescope will have several modes of operation - making it possible, for example, to carry out deep spectral-line observations with integration times of hours or days, while simultaneously monitoring the continuum emission of other sources well outside the main beam. Wide Field Imaging Full integration over 12 hours or multiple snapshots. Spectral Line Observations FX mode 2048 channels, each kHz ( km/s). FXF mode 1 or 2 channels with 768 complex lags. Independent Fanbeam Observations An independent fanbeam can be formed within ±6° (1420 MHz) or ±27° (300 MHz) of the imaging beam. This could be used for pulsar timing or flux monitoring. Optional digital beamformer with 64 fanbeams Pulsar and SETI search observing. Interleaved Observing The electronic beamforming enables rapid changes (< 1 s) in observing frequency and meridian distance. The frequency agility allows for spectral index determination using interleaved frequencies. The meridian angle agility makes 10,000 deg 2 of sky accessible during routine 12h observations allowing for, for example, source monitoring or calibration. The scientific and technological goals of this project focus on radio spectrometry of mJy-level continuum sources and wide- field spectral-line observations, which are unaffected by confusion in the Molonglo beam. We note however, that images from the high-frequency end of the bandpass (where the angular resolution is highest) will help deconfuse lower- frequency images, so that the effective continuum confusion limit should be well below 0.1 mJy (a full 12 hr synthesis observation will reach a 5 sigma detection limit of ~0.17 mJy in a 30 MHz continuum band near 1400 MHz). The nearby radio galaxy Fornax A at 843 MHz, showing the excellent image quality made possible by the continuous uv coverage of the Molonglo telescope. Parameter1420 MHz300 MHz Frequency Coverage300–1420 MHz Bandwidth (BW)250 MHz Resolution (  < -30°)26" x 26" csc|  |123" x 123" csc|  | Imaging field of view 1.5° x 1.5° csc|  |7.7° x 7.7° csc|  | UV coverageFully sampled T sys < 50K< 150K System noise (1  ) 12 hr: 8 min: 11  Jy/beam 100  Jy/beam 33  Jy/beam 300  Jy/beam PolarisationDual Linear CorrelatorI and Q (Full Stokes at 125 MHz BW) Frequency resolution120–1 kHz (FXF mode: 240 Hz) Independent fanbeam1.3’ x 1.5°6.2’ x 7.7° Indep. fanbeam offset±6°±6°±27° Sky accessible in < 1 s180 deg deg 2 Signal Path Cylindrical Parabolic Collectors (Two collinear 778 m x 12 m) MHz Feed and LNA (7,400 feeds, 14,800 LNAs) Delay line beamforming (Over 9 feeds) Analog to Digital Converter (1,600 8 bit 250 MHz BW ADCs) Digital delay beamforming (80 10 m x 10 m patches) Digital filterbank (160) (Two 250 MHz/patch) FX Correlator (3,160 baselines, 2,048 channels) Signal processing & storage (imaging, spectrometer, searching...) See Prototype SKA Technologies at Molonglo: 2. Antenna and Front End See Prototype SKA Technologies at Molonglo: 3. Beamformer and Correlator Independent fanbeam (1 within 9 feed field of view) Digital Beamformer (64 fanbeams within imaging beam) Molonglo AUSTRALIA Brisbane Darwin Perth Canberra Hobart Adelaide Melbourne Sydney + Antenna Pattern Single feed beam Delay line beam Independent fanbeam Imaging beam Photo D. Bock The red line shows the HI mass limit (for H 0 = 50 km/s/Mpc, q 0 = 0.5) reached by the HI Parkes All-Sky Survey (HIPASS; Barnes et al. 2001) for a galaxy with velocity width  V = 200 km/s in a 500 s observation. Molonglo will be able to reach similar mass limits over the redshift range z=0.03 to 0.26 with integration times of ~120 hours per 1.7 deg 2 field, allowing a direct measure of the evolution of the HI mass function over this redshift range. Science Goals (10 x 12 hr) Molonglo (12 hr) HIPASS (8 min) log 10 M lim (HI) (M  ) Sensitivity of the Molonglo telescope for high-redshift HI observations.