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Unlocking the Cosmic Frontier: ASKAP's Revolutionary Radio Telescope Survey

The ASKAP (Australian Square Kilometre Array Pathfinder) radio telescope will transform our understanding of the universe. With an impressive 30 µJy/beam RMS sensitivity during 12-hour integrations, ASKAP aims to double the known radio sources and shed light on the evolution of radio-loud Active Galactic Nuclei (AGN). Key goals include significantly increasing sub-mJy source counts and constraining star formation at z~0.5. ASKAP's wide frequency coverage from 700-1800 MHz and advanced capabilities will also enable profound discoveries in cosmology and galactic astronomy.

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Unlocking the Cosmic Frontier: ASKAP's Revolutionary Radio Telescope Survey

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  1. Early Continuum Science with ASKAP CSIRO Astronomy & space Science Ray Norris, Nick Seymour (CASS) , Andrew Hopkins (AAO)

  2. ASKAP12+ will be one of the most powerful survey radio telescopes in the world 30uJy/beam rms in a 12hour integration Confusion noise ~<20uJy/beam

  3. Stripe 82/SPT Blurb B2

  4. ASKAP12+ Stripe 82/SPT Blurb B2

  5. Main Science Goals • Double the total number of radio sources known • Constrain evolution of radio-loud AGN population

  6. Main Science Goals • Double the total number of radio sources known • Constrain evolution of radio-loud AGN population Mao et al. 2012

  7. Main Science Goals • Double the total number of radio sources known • Constrain evolution of radio-loud AGN population • Increase the total number of sub-mJy radio sources by two orders of magnitude • Constrain star formation to z~0.5

  8. Main Science Goals • Double the total number of radio sources known • Constrain evolution of radio-loud AGN population • Increase the total number of sub-mJy radio sources by an order of magnitude • Constrain star formation to z~0.5

  9. Main Science Goals • Double the total number of radio sources known • Constrain evolution of radio-loud AGN population • Increase the total number of sub-mJy radio sources by an order of magnitude • Constrain star formation to z~0.5

  10. Compliment full EMU • Cover full 700-1800MHz frequency range • Switch between 3 bands every 20mins • Obtain spectral index and spectral curvature information

  11. Compliment full EMU • Cover full 700-1800MHz frequency range • Switch between 3 bands every 20mins • Obtain spectral index and spectral curvature information • Characterise faint population • Obtain unique samples of rare sources: USS, GPS • Allow spectral index and curvature to be compared to full EMU determined over narrower range • Obtain polarisation and RM measurements which are very important in diagnosis of faint populations

  12. Additional EMU Science • Cosmology • Galactic Astronomy • Local Galaxies • Serendipitous discoveries Additional ASKAP Science • The polarised sky • HI absorption • Transients • Legacy value to astronomical community

  13. Discussion points • Can the correlator be adapted to 384MHz (or =>366MHz) ? • Angular resolution is key: confusion and cross-identification • Can the full bandwidth be imaged simultaneously? • Which areas of sky would be prioritised? • Deep survey expected by combining regular observations of standard field (as part of science verification).

  14. Presentation title | Presenter name | Page 14

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