wallaby-survey...•wallaby (hi) and emu (continuum) are the two key survey science projects 16 17...
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Lister Staveley-Smithwallaby-survey.org
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Outline• HI surveys – science goals• Wallaby• Cosmic flows• Northern counterparts• TAIPAN synergies
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Wallaby goals• Local Group/Volume
• Understanding Galaxies
• Cosmology
• Legacy
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Environmental suppression
No transition (gas-bearing) galaxies within 300 kpc of Milky Way:
• stripping or ionization?
(Westmeier et al. 2015; Spekkens et al. 2014)
gas-richgas poor
DISTANCE FROM MILKY WAY
GAS
RICH
NES
S
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ASKAP Wallaby• Local Group/Volume
• Understanding Galaxies
• Cosmology
• Legacy
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Gas accretion onto galaxiesNGC 891: Oosterloo, Fraternali & Sancisi (2007)
EBHIS: Kerp et al. (2016)
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Galaxy evolution
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Driver et al. (2018)
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ASKAP Wallaby• Local Group/Volume
• Understanding Galaxies
• Cosmology
• Legacy
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Redshift-space distortionsHI optical
Beutler9
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ASKAP Wallaby• Local Group/Volume
• Understanding Galaxies
• Cosmology
• Legacy
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Comparison with other legacy surveys
Area 3 π 2.8 π 0.7 π Redshift 0 - 0.26 0 - 0.04 0 - 0.06rms20 km/s 0.7 mJy/beam 13 mJy/beam 1.5 mJy/beamRes 30 arcsec, 4 km/s 15 arcmin, 18 km/s 3.5 arcmin, 5 km/sNdet 500,000 5,000 30,000
Wallaby = Widefield ASKAP L-band Legacy All-sky Blind surveY
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ASKAP HI surveys
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Dens
ity o
f Spe
ctra
(N/d
eg2 )
Area (deg2)
2 Orders of Magnitude Improvement
Existing SurveyLimit
Meyer
SKA pathfinder HI surveys:
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Spherical cap tiling (Robotham)
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Sensitivity images (Robotham)
Raw tile pattern – max/min=2.3 4-pt dither – max/min=1.2
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Australian SKA Pathfinder (ASKAP)• Radio interferometer – 36 ×12-m dishes
• CSIRO Phased Array Feed (PAF) technology: 36 beams
• Frequency range 700 to 1800 MHz
• Instantaneous bandwidth 300 MHz
• Maximum baseline 6 km
• SKA precursor on a radio-quiet site
• Wallaby (HI) and EMU (continuum) are the two key survey science projects
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Murchison Shire
Netherlands
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Boolardy Station
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Population density (people/km2)
0.0001
0.0100
1.0000
100.0000
Netherlands
Australia WA
Greenland
Murchison
Antarctica
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A radio-quiet siteSydney:Population 5M
Narrabri (ATCA):Population 6,000
Murchison, WAPopulation 160
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Wallaby timeline• Sept 2014: commissioning science with BETA (6 antennas)
• Oct 2016: early science commences (12 antennas, 48 MHz)
• Oct 2017: early science concludes (16 antennas, 240 MHz, 650 hrs)
• Dec 2018: Full ASKAP functionality (36 antennas)
• Mar 2019: pilot survey commences (400 hrs)
• Late 2020: Pawsey supercomputer upgrade
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First ASKAP BETA+Wallabyscience paper (Serra et al. 2015)
IC 1459 group24
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Wallaby timeline• Sept 2014: commissioning science with BETA (6 antennas)
• Oct 2016: early science commences (12 antennas, 48 MHz)
• Oct 2017: early science concludes (16 antennas, 240 MHz, 650 hrs)
• Dec 2018: Full ASKAP functionality (36 antennas)
• Mar 2019: pilot survey commences (400 hrs)
• Late 2020: Pawsey supercomputer upgrade
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Early Science (ES) focus: environment
Preprocessing inand outsidegroups
Wallaby SWG3 pre-processing workshop –Swinburne March 8-10 (Kilborn and Wong)
19 groups
Kilborn+09
When did galaxies lose their gas?
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WALLABY ES fields
Westmeier27 |
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Early Science progress
ES data is virtually identical to the Wallaby main survey data in resolution and sensitivity28 |
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ES1 coverageES1NGC 7232 field and beam patternon coloured DSS
IC 5201
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NGC 7162/A in the NGC 7232 group
Reynolds et al. (submitted)
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IC 5201 in the NGC 7232 group
NGC 7232 group
Kleiner et al. (to be submitted)31 |
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Tidal dwarf galaxies
BETA HI clouds
ASKAP-12 HI clouds
Lee-Waddell et al. (submitted)
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ES3 coverageES3Dorado field and beam patternon coloured DSS
6 deg
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DoradoNGC 1566 galaxy group
Agali, Rhee et al (to be submitted)
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Taipan/WALLABY synergies
Da Cunha et al. (2017): Taipan white paper – Predictions based on GALFORM model of Lagos et al. (2012) using Mill I and II
Overlap dynamic range at intermediate stellar masses:→ high mass galaxies are gas poor→ low mass galaxies too faint for optical survey
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Taipan/WALLABY synergies
Overlap region:→ blue cloud and green valley→ high HI masses
Da Cunha et al. (2017): Taipan white paper – Predictions based on GALFORM model of Lagos et al. (2012) using Mill I and II
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Summary• Wallaby science has started (4+2 ES fields - same
area, resolution and sensitivity as ASKAP-36)• Initial science focus: pre-processing in group
environment• Wallaby is zero-redshift, all-sky ‘anchor’ for high-z
studies – most O/IR synergy with TAIPAN, SkyMapper, VISTA, VST, LSST
• Expected completion 2020/21
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