Magnetic fields in the Galaxy via Faraday effect: Future prospects with ASKAP and the SKA
ASKAP in the SKA era -...
Transcript of ASKAP in the SKA era -...
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•CSIRO astronomy and space science (CASS)
Ray Norris, CSIRO Astronomy & Space Science
ASKAP in the SKA era
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Overview
•ASKAP Overview
•ASKAP science in SKA era
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ASKAP =Australian Square Kilometre Array pathfinderA revolutionary new $165m radio telescope in WA
EMUIncreasing human knowledge of the radio sky by a factor of 30
WALLABYMapping half a million
galaxies in HI
CRAFT
COAST
FLASH
GASKAP
VAST
POSSUM
VLBI
DINGO
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Total bandwidth = 2.1THz per antenna
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Current ASKAP status
• All 36 antennas and infrastructure completed,
• Funding in place for 30 PAFs
• Engineering prototype array (“BETA”) currently operating with prototype PAFs on 6 antennas giving 9 beams
• Construction going amazingly well
Planned schedule• 12 MkII PAFS installed by ~Dec 2015
• Early 2016: “shared risk” ASKAP early science
• All PAFs installed by mid-2016
• 2017: Full EMU / WALLABY / other surveys start ??????
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• 29-hour observation with BETA, covering 50 sq deg. RMS =600 μJy (on track for ~10 μJy for EMU!) • ~2000 sources > 10σ• This 6-antenna engineering protoype is already the 2nd-fastest survey
telescope in the world (beaten only by JVLA)• ASKAP-30 will be fastest radio survey telescope in the world
PAFs work (even with only 6 antennas)!
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HI in NGC253with ASKAP-BETA(colours show velocity)
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O z S K A :#r a d i o #a s t r o n o m y #in #t h e #n e x t #d e c a d e #
M i l k y W a y H I
z = 0 . 1 9 2 H I
z = 0 . 8 8 5 O H
z = 0 . 8 8 5 H I
A l l i s o n e t a l . ( i n p r e p . )
A SK A P $E x a m p le :$z"=$2 .5 $q u a sa r$P K S1 8 3 0 Y2 1 1 $700-1500 MHz spectrum of the Einstein Lens quasar
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ASKAP Science38 proposals submitted to ASKAP
2 selected as being highest priority
8 others supported at a lower priority
• EMU all-sky continuum (PI Norris)
• WALLABY all-sky HI(PI Koribalski & Staveley-Smith)
• COAST pulsars etc• CRAFT fast variability• DINGO deep HI• FLASH HI absorption• GASKAP Galactic• POSSUM polarisation• VAST slow variability• VLBI
See talks by Lister Staveley-Smith and Paolo Serra
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Diagram courtesy of Isabella Prandoni
VLA-NVSS75% of skyRms=450μJy, res ~ 45 arcsec~1.8 million galaxies
Uncharted observationalphase space
ASKAP-EMU75% of skyRms=10μJy, res ~ 10 arcsec~70 million galaxiesWould take ~7 years with JVLA
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The EMU Pathfinder:ATLAS=Australia Telescope Large Area Survey7 sq deg to rms=15 μJy
Mao et al. 2010MNRAS.406.2578M
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How does EMU differ from earlier radio surveys?
• Scale – increases the number of known radio sources by a factor of ~30
• About half the sources are star-forming galaxies• 50uJy equiv to R~21.5 for SF galaxy
• Ambition – includes:• Cross-identification with optical/IR catalogues
• Ancillary data (redshifts etc)
• Key science projects as an integral part of the project
• Explicitly includes “discovering the unexpected”
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ASKAP in the SKA era
• SKA-MID has somewhat higher survey speed than ASKAP (but higher spatial resolution)
• Difficult to justify multi-year SKA-MID all-sky survey incrementally better than EMU/WALLABY
• SKA-MID is better suited to doing deeper surveys over a smaller area
• So EMU and WALLABY may remain the premier all-sky surveys in continuum and HI
• ASKAP complements SKA-MID and SKA-LOW
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SKA-era options (with NO upgrades)
After the current science survey projects (EMU, WALLABY, etc) are finished, ASKAP is still the worlds best survey radiotelescope, so what next?
•Continuum: survey the whole sky from 700-1800 MHz to measure spectral shape, rotation measures, etc.
• Approach (but not reach) upper limit of SKA-LOW 350MHz) and MWA (300 MHz)
• Can go deeper than EMU at highest frequency
•HI: integrate longer to go deeper
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SKA-era options (with upgrades)• Intimate relationship between ASKAP & SKA?
• Upgrade PAFs to double the sensitivity
• Extend baselines to increase continuum resolution:
• Beat down confusion limit
• Better optical ID’s
• Resolved images of millions of SF galaxies and AGN (and tell the difference!)
• Extend frequency range to meet the 350 MHz of SKA-LOW?
• Wide-field VLBI to Parkes and ATCA?
ATCA strategy workshop on 1 June
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Conclusion• SKA rebaselining means that ASKAP’s role will be even more significant in the SKA era
• E.g. all-sky radio continuum cosmology
• Even with no upgrades, ASKAP will be a valuable complement to SKA-LOW and SKA-MID
• With upgrades, it effectively becomes a rebaselined SKA-SURVEY
• Possible (RPN, not CSIRO!) timeline:
• 2016-2019?: ASKAP completes current SSPs
• 2020? on: upgraded ASKAP becomes part of SKA
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Western Australia
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Redshift distribution of EMU sources
Based on SKADS (Wilman et al; 2006, 2008)
<z>=1.1 for SF/SB<z>=1.9 for AGN
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EMU Key Science Projects
Project Leader
EMU Value-Added Catalogue Nick Seymour
Characterising the Radio Sky Ian Heywood
EMU Cosmology David Parkinson
Cosmic Web Shea Brown
Clusters of Galaxies Melanie JohnstonHollitt & Chiara Ferrari
Cosmic star formation history Andrew Hopkins
Radio-loud AGN Anna Kapinska
Radio AGN in the EoR Jose Afonso
Radio-quiet AGN Isabella Prandoni
Local Universe Josh Marvil
The Galactic Plane Roland Kothes
SCORPIO: Radio Stars Grazia Umana
WTF: Mining Data for the Unexpected
Ray NorrisSee http://askap.pbworks.com/KeyProjects for details