Kristian Zarb Adami Danny Price M E Jones & the AADC Single vs Dual Band Considerations Instruments:

Slides:

Advertisements

Similar presentations

Arecibo 40th Anniversary Workshop--R. L. Brown The Arecibo Astrometric/Timing Array Robert L. Brown.

Advertisements

NAIC-NRAO School on Single-Dish Radio Astronomy. Arecibo, July 2005

PAPER’s Sweet Sixteen: Imaging the Low Frequency Sky with a Sixteen Element Array Nicole Gugliucci for the PAPER Team* USNC/URSI National Radio Science.

Schediwy: Advantages and Disadvantages of Sparse Aperture Arrays Fermilab: October 2009.

Sparse Array Geometry Mr. Ahmed El-makadema Professor A.K Brown.

1 hour, 6MHz 18’ resolution DNR ~ 5000 Weakest src ~ 10 Jy CygX G Cygnus A Galactic plane PAPER GB32 at 150MHz AIPS reduction W51 G

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.

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,

NEUTRAL HYDROGEN Frank Briggs RSAA and ATNF z = 8 z = 0.

Radio `source’ Goals of telescope: maximize collection of energy (sensitivity or gain) isolate source emission from other sources… (directional gain… dynamic.

Radio Telescopes Large metal dish acts as a mirror for radio waves. Radio receiver at prime focus. Surface accuracy not so important, so easy to make.

The Green Bank Telescope a powerful instrument for enhancing ALMA science Unblocked Aperture Low sidelobes gives high dynamic range Resistance to Interference.

Paul Alexander, Peter Hall Design Issues and Implementation ChallengesAAVP 2010 Design issues and implementation challenges Paul Alexander and Peter Hall.

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,

Sascha D-PAD Sparse Aperture Array.

Performance of station array configurations Sparse vs. Dense, Regular vs Random Jaap D. Bregman AAVP Workshop,Cambridge,

Array Antenna Designs for the SKA-AAlo Eloy de Lera Acedo 1 AAVP 2010, Cambridge, UK. 10/12/10.

Array Design David Woody Owens Valley Radio Observatory presented at NRAO summer school 2002.

LOFAR Antenna Systems Dion Kant, Wim van Cappellen AAVP – 10 December 2010, Cambridge, UK.

Spaceborne Weather Radar

Name1 SKA(DS) System Design Aspects 4 th SKADS Workshop, Lisbon, 2-3 October 2008 SKA(DS) System Design Aspects: building a system Laurens Bakker.

Assessment of RFI measurements for LOFAR Mark Bentum, Albert-Jan Boonstra, Rob Millenaar ASTRON, The Netherlands Telecommunication Engineering, University.

J.M. Wrobel - 25 June 2002 PROPOSALS 1 PROPOSAL WRITING TUTORIAL Outline 30 minutes: Lecture on Generic Issues 60 minutes: Small Groups Write Proposals.

J.M. Wrobel - 19 June 2002 SENSITIVITY 1 SENSITIVITY Outline What is Sensitivity & Why Should You Care? What Are Measures of Antenna Performance? What.

Multiwavelength Continuum Survey of Protostellar Disks in Ophiuchus Left: Submillimeter Array (SMA) aperture synthesis images of 870 μm (350 GHz) continuum.

SKA AA-Low Station Configurations and Trade-off Analysis Nima Razavi-Ghods, Ahmed El-Makadema AAVP 2011, ASTRON, Dwingeloo Dec

Steve Torchinsky SKADS Science Overview Lisbon 2007 Jan 12 SKADS Science Overview.

National Radio Astronomy Observatory May 17, 2006 – Legacy Projects Workshop VLA/VLBA Large Projects Jim Ulvestad Assistant Director, NRAO.

The Square Kilometre Array Department of Astronomy and Atmospheric Sciences, Kyungpook National University 김경묵, 박진태, 방태양, 신지혜, 조창현, 정수진, 현화수 Survey Science.

130 cMpc ~ 1 o z~ = 7.3 Lidz et al ‘Inverse’ views of evolution of large scale structure during reionization Neutral intergalactic medium via HI.

130 cMpc ~ 1 o z = 7.3 Lidz et al ‘Inverse’ views of evolution of large scale structure during reionization Neutral intergalactic medium via HI 21cm.

November 2009, Lunch talk The most compact E configuration for the EVLA. L. Kogan, G. Stanzione, J. Ott, F. Owen National Radio Astronomy Observatory Socorro,

1 100 SKA stations (2020 ) Projets avec SKA. 2 Telescope Project (~2020) for a giant radiotelescope in the centimetre-metre range one square kilometre.

Survey Quality Jim Condon NRAO, Charlottesville. Survey Qualities Leiden 2011 Feb 25 Point-source detection limit S lim Resolution Ω s Brightness sensitivity.

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.

Array Configuration Divya Oberoi MIT Haystack Observatory.

Which dipoles to use to optimize survey speed? –What tapering? –Trade-off between sensitivity, FOV and low side-lobe levels –Station beam stability, pointing.

The KAT/SKA project and Related Research Catherine Cress (UKZN/KAT/UWC)

21 cm Reionization Forecast and Search at GMRT

Judd D. Bowman Hubble Fellow, Caltech Alan E. E. Rogers Haystack Observatory With support from: CSIRO/MRO and Curtin University Thanks to: The organizers.

Development and Commissioning of LOFAR for Astronomy (DCLA) Huub Röttgering Leiden Observatory.

Fundamental limits of radio interferometers: Source parameter estimation Cathryn Trott Randall Wayth Steven Tingay Curtin University International Centre.

Anadian ydrogen ntensity apping xperiment CHIMECHIME CHIMECHIME WiggleZ Dark Ages Stars 13.7Gy CMB Big Bang Reionization 1100 z∞ SDSS 7Gy CHIME.

ASKAP Capabilities John Reynolds on behalf of the SEIC and ASKAP team.

Molecular Clouds in in the LMC at High Resolution: The Importance of Short ALMA Baselines T. Wong 1,2,4, J. B. Whiteoak 1, M. Hunt 2, J. Ott 1, Y.-N. Chin.

S.A. Torchinsky SKADS Workshop 10 October 2007 Simulations: The Loop from Science to Engineering and back S.A. Torchinsky SKADS Project Scientist.

Mário Santos1 EoR / 21cm simulations 4 th SKADS Workshop, Lisbon, 2-3 October 2008 Epoch of Reionization / 21cm simulations Mário Santos CENTRA - IST.

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.

Ariadne’s Thread Kristian Zarb Adami. Simulator Aims ۞ Provide the system architect a tool to visualise trade-offs in designs ۞ Provide the scientist.

Observing Strategies at cm wavelengths Making good decisions Jessica Chapman Synthesis Workshop May 2003.

A Modular K-Band Focal Plane Array for the Green Bank Telescope Matt Morgan National Radio Astronomy Observatory 9/28/2007.

The Mission  Explore the Dark Ages through the neutral hydrogen distribution  Constrain the populations of the first stars and first black holes.  Measure.

The Allen Telescope Array Douglas Bock Radio Astronomy Laboratory University of California, Berkeley Socorro, August 23, 2001.

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.

Future Radio Interferometers Jim Ulvestad National Radio Astronomy Observatory.

C.Carilli, AUI Board October 2006 ISAC-run three year process: Quantified ‘experiments’ for future large area cm telescopes 50 chapters, 90 authors, 25%

Rosie Bolton 2 nd SKADS Workshop October 2007 SKADS System Design and Costing: Update and next steps Rosie Bolton University of Cambridge.

Big Bang f(HI) ~ 0 f(HI) ~ 1 f(HI) ~ History of Baryons (mostly hydrogen) Redshift Recombination Reionization z = 1000 (0.4Myr) z = 0 (13.6Gyr) z.

Why do we need interferometry? Measuring the gas distribution and rotation in disk galaxies: radio observations with interferometer arrays and aperture.

SKA1-LOW CONFIGURATION CONSULTATION WS P. Dewdney

EoR/Cosmic Dawn SWG Feedback on SKA1-Low Array Configuration Cath Trott Brad Greig, Leon Koopmans, Andrei Mesinger, Garrelt Mellema, Jonathan Pritchard.

WVU Astronomy / Engineering and The Green Bank Observatory Richard Prestage Scientist, NRAO.

On the Doorstep of Reionization Judd D. Bowman (Caltech) March 11, 2009 DIY 21 cm cosmology.

Upcoming Instruments to Probe Reionization… Frank Briggs ANU.

Atacama Large Millimeter/submillimeter Array Karl G. Jansky Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array ngVLA: Reconfigurability.

Nithyanandan Thyagarajan1, Aaron R. Parsons2,

Phased Array Feeds Wim van Cappellen

Goals of telescope: Radio `source’

Presentation transcript:

Kristian Zarb Adami Danny Price M E Jones & the AADC Single vs Dual Band Considerations Instruments:

The new shopping list

DRM Current Requirements Frequency (MHz) Sky Coverage (deg 2 ) Survey speed (m 2 K -1 ) Relevant FoM EoR Extended EoR - 21-cm forest , Extended? HI Absorption , m 4 K -2 deg 2 Point source Pulsar surveys ,000500Pulsar Continuum deep-field Point source Intensity mapping Extended

Important to...  Distinguish between Point Source Sensitivity:  And Brightness Sensitivity:

Comparing  Point Source Sensitivity Survey Speed  with Temperature Sensitivity Survey Speed  Increasing the collecting area A e while keeping f constant will increase the PFoM, but will not increase the BFoM.  Increasing the filling factor f while keeping the collecting area A e constant will increase the BFoM, but not the PFoM (so long as the source remains resolved).

A 3x3 gridded array with spacing d. In the regime where the collecting areas of individual antennas do not overlap, the overall collecting area is the sum of all individual collecting areas.

T sys vs frequency

Comparison of brightness sensitivity between single (dashed) and dual (continuous) band implementations for SKA-low. An antenna gain of 9dBi has been used.

Ratio of brightness sensitivity survey speed between the dual and single band implementations. At 200MHz, the single implementation is sparse while the dual band is fully filled; at about 320MHz, the dual band becomes sparse also, and the ratio becomes constant. An antenna gain of 9dBi has been used.

Epoch of Re-ionisation

However...  The Science Case between MHz seems rather weak except for (Wyithe and Loeb): “ Our novel result implies that future radio experiments should be tuned to a characteristic angular scale of ∼ 0.5 ◦ and have a minimum frequency bandwidth of ∼ 8 MHz for an optimal detection of 21cm flux fluctuations near the end of reionization.”

Next Steps...  Progress the Single vs Dual Considerations Document with realisitc OSKAR-2 dynamic range simulations  Feedback into the DRM process requirements for Brightness Sensitivity and Brightness Sensitivity Survey metrics  Discuss in detail the 50MHz requirements and produce an engineering response to the Cosmic Dawn/EOR Paper  Discuss in detail the MHz science requirements and the requirements for Intensity Mapping Experiments at these frequencies

Fitness Functions Correlation with Ideal Baseline Histogram (user defined)

Typical Chromosomes (golden ratio elements in stations)

Typical Chromosomes (random elements in stations)

Antenna Design