ASKAP HI AllSky Survey WALLABY

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ASKAP HI All-Sky Survey(WALLABY)

• Bärbel Koribalski
• (CSIRO ATNF)

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WALLABYB. Koribalski (ATNF) L. Staveley-Smith
(UWA)
ASKAP driver precursor to SKA HI surveys !
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WALLABY parameters

• Survey time one year (longer?)
• Sky coverage 1 (1.5) hemispheres
• -90o to 0o (30o) DEC, max. 50o DEC
• FOV 5.5 x 5.5 degr2 footprint
  (i.e. 400x ATCA primary beam)
• Velocity coverage -2,000 to 60,000 km/s
• BW 300 MHz divided into 16,384 channels
  
• Resolution 30, 4 km/s ( 10 postage stamps)
• Integration time 12 (8) hours per pointing
• Line sensitivity 1.3 (1.5) mJy/b. per channel
• 330 TB total storage for Stokes-I cubes

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Discussion

• Survey area vs. sensitivity
• one hemisphere, 12h per pointing, one year
• 1.5 hemispheres, 8h per pointing, one year
• 1.5 hemispheres, 12h per pointing, 1.5 years
• HI Science drivers Synergies
• Large-scale structure, BAO, HI mass functions
• Evolution of galaxies - need to integrate long
  enough to detect massive HI galaxies at survey
  edge (z 0.26, D 800 Mpc )
• 8h integration time ? MHI 5? limit
• 5 x 106 M? (D 10 Mpc)
• 5 x 108 M? (D 100 Mpc)
• 3 x 1010 M? (D 800 Mpc)

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WALLABY Science

• Study the Evolution of galaxies (out to z 0.2)
• detect 500,000 HI-rich galaxies (x20)
• use HI stacking for many more galaxies
• measure SFRs for all detected galaxies
• ASKAP Survey Outputs
• line emission from 1.13 to 1.43 GHz (HI, OH,
  recomb. Lines, )
• radio continuum polarisation
• ? Commensal surveys
• WALLABY, EMU-wide, ARMPIT-wide, HI/OH-absorption,
  OHmega/kilo-masers, Galactic Magellanic HI,

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• (1o x 1o)

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Koribalski Lopez-Sanchez (2009)
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HIZOA J0836-43 Vhel 10689 km/s D 148 Mpc w20
610 km/s w50 566 km/s MHI 7.5 x 1010
M? Mdyn 1.4 x 1012 M? SFR 35 M? per
year Donley, Koribalski, Staveley-Smith et al.
2006
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HIZOA J0836-43 Vhel 10689 km/s D 148
Mpc w20 610 km/s w50 566 km/s MHI 7.5 x
1010 M? Mdyn 1.4 x 1012 M? SFR 35 M? per
year
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NGC 612 PKS 0131-36 z 0.0297 vhel 8900 km/s
Emonts et al. 2008
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Key Science Areas

• A census of the local galaxy population
• Local Group, Local Volume, dwarf galaxies
• Structure Evolution of Galaxies
• HI mass function as a function of local density,
  galaxy morphology and redshift
• gas mass as a function of environment star
  formation
• The Cosmic web
• large-scale power spectrum, peculiar velocity
  field, local density field, HI filaments,
  clustering properties, etc.

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e.g., HI in galaxies at z 0.05
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Tools Simulations

• 3D source finder
• the majority of sources is unresolved
• extended sources (e.g., galaxies, filaments,
  clouds, etc.)
• very extended sources (e.g., inter-connected
  galaxy groups, HVCs, streams, )
• (semi)-automatic fitting of source properties
• Optical/infrared identification
• etc.

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The Local Volume HI Survey (LVHIS) B. Koribalski,
A. Lopez-Sanchez, E. Kirby, E. van Eymeren, L.
Staveley-Smith, E. de Blok, J. Ott, N. Bonne,
Jerjen
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The HIPASS experience 15 resolution 13
mJy/beam 18 km/s
HIPASS data
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VLA HI data 20 x 20 degr2 3116 pointings ?370
hours 16 resolution 3.4 1019 cm-2
by Aeree Chung et al.
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HI filament near M99
M 99
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45 kpc