Science with the Australian Square Kilometre Array Pathfinder

Johnston, S.; Bailes, M.; Bartel, N.; Baugh, C. M.; Bietenholz, M. F.; Blake, Chris; Braun, Róbert; Brown, J. C.; Chatterjee, S.; Darling, J.; Deller, Adam T.; Dodson, Richard; Edwards, Philip; Ekers, R. D.; Ellingsen, S. P.; Feain, Ilana; Gaensler, B. M.; Haverkorn, M.; Hobbs, G.; Hopkins, A. M.; Jackson, C. A.; James, C.; Joncas, G.; Kaspi, V. M.; Kilborn, V. A.; Koribalski, B. S.; Kothes, R.; Landecker, T. L.; Lenc, E.; Lovell, J. E. J.; Macquart, Jean–Pierre; Manchester, R. N.; Matthews, Deanna; McClure-Griffiths, N. M.; Norris, R. P.; Pen, Ue-Li; Phillips, Chris; Power, Chris; Protheroe, R. J.; Sadler, E. M.; Schmidt, B.; Stairs, I. H.; Staveley‐Smith, L.; Stil, J. M.; Taylor, A. R.; Tingay, S. J.; Tzioumis, A. K.; Walker, Mark A.; Wall, J. V.; Wolleben, M.

doi:10.1071/as07033

Cited by 305 publications

(177 citation statements)

References 68 publications

(76 reference statements)

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“…Soon the Australian Square Kilometre Array Pathfinder (ASKAP; Johnston et al 2007) will survey 21 cm emission from H I in the equatorial GAMA fields. In the meantime, 21 cm H I line observations for part of the SAMI sample in the GAMA regions are already available thanks to the Arecibo Legacy Fast ALFA (ALFALFA) survey (Giovanelli et al 2005).…”

Section: Radio 21-cm H Imentioning

confidence: 99%

The SAMI Galaxy Survey: instrument specification and target selection

Bryant

Owers

Robotham

et al. 2015

Monthly Notices of the Royal Astronomical Society

438

394

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Citation for published item:fryntD tFtF nd ywersD wFF nd oothmD eFFqF nd groomD FwF nd hriverD FF nd hrinkwterD wFtF nd vorenteD xFFpF nd gorteseD vF nd ottD xF nd gollessD wF nd heferD eF nd ylorD iFxF nd uonstntopoulosD sFF nd ellenD tFF nd fldryD sF nd frnesD vF nd fuerD eFiF nd flndErwthornD tF nd floomD tFF nd frooksD eFwF nd froughD F nd geilD qF nd gouhD F nd grotonD hF nd hviesD F nd illisD F nd pogrtyD vFwFF nd posterD gF nd qlzerookD uF nd qoodwinD wF nd qreenD eF nd qunwrdhnD wFvF nd rmptonD iF nd roD sFEF nd ropkinsD eFwF nd uewleyD vF nd vwreneD tFF nd veonEvlD FqF nd veslieD F nd wilroyD F nd vewisD qF nd viskeD tF nd v¡ opezE¡ nhezD ¡ eFF nd whjnD F nd wedlingD eFwF nd wetlfeD xF nd weyerD wF nd wouldD tF nd yreshkowD hF nd y9ooleD F nd ryD wF nd ihrdsD FxF nd hnksD F nd hrpD F nd weetD FwF nd homsD eFhF nd oniniD gF nd lherD gFtF @PHISA 9he ews qlxy urvey X instrument spei(tion nd trget seletionF9D wonthly noties of the oyl estronomil oietyFD RRU @QAF ppF PVSUEPVUWF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTThe SAMI Galaxy Survey will observe 3400 galaxies with the Sydney-AAO Multi-object Integral-field spectrograph (SAMI) on the Anglo-Australian Telescope in a 3-yr survey which began in 2013. We present the throughput of the SAMI system, the science basis and specifications for the target selection, the survey observation plan and the combined properties of the selected galaxies. The survey includes four volume-limited galaxy samples based on cuts in a proxy for stellar mass, along with low-stellar-mass dwarf galaxies all selected from the Galaxy And Mass Assembly (GAMA) survey. The GAMA regions were selected because of the vast array of ancillary data available, including ultraviolet through to radio bands. These fields are on the celestial equator at 9, 12 and 14.5 h, and cover a total of 144 deg 2 (in GAMA-I). Higher density environments are also included with the addition of eight clusters. The clusters have spectroscopy from 2-degree Field Galaxy Redshift Survey (2dFGRS) and Sloan Digital Sky Survey (SDSS) and photometry in regions covered by the SDSS and/or VLT Survey Telescope/ATLAS. The aim is to cover a broad range in stellar mass and environment, and therefore the primary survey targets cover redshifts 0.004 < z < 0.095, magnitudes r pet < 19.4, stellar masses 10 7 -10 12 M , and environments from isolated field galaxies through groups to clusters of ∼10 15 M .

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Section: Radio 21-cm H Imentioning

confidence: 99%

The SAMI Galaxy Survey: instrument specification and target selection

Bryant

Owers

Robotham

et al. 2015

Monthly Notices of the Royal Astronomical Society

438

394

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“…In the ASKAP, three station configurations are available, a very compact configuration with maximum baseline of 400 m, a medium compact configuration with maximum baseline of 2 km, and an extended configuration with maximum baseline of 8 km [15].…”

Section: Brief Review Of Other Next-generation Telescopesmentioning

confidence: 99%

“…Next-generation radio telescopes, such as Square Kilometre Array Pathfinder (ASKAP) [15], Murchinson Widefield Array (MWA) [16], Meerkat [17], Square kilometre Array (SKA) [18,19], and Low-Frequency Array (LOFAR) [20], are expected to achieve a wider dynamic range and higher angular resolution than current instruments.…”

Section: Introductionmentioning

confidence: 99%

A Multi-Feature Visibility Processing Algorithm for Radio Interferometric Imaging on Next-Generation Telescopes

Chiou¹,

Kiang²,

Mittra³

2014

PIER C

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Abstract-The visibility distribution, which is related to the configuration of stations, can be categorized into different features, each having different levels of data number density. A computationally efficient multi-feature image reconstruction algorithm, well adapted for next-generation telescopes, is proposed based on this observation, which is more flexible to handle massive amount of visibility data expected in the future. In reconstructing the M87 image with the visibility data simulated on the Low-Frequency Array (LOFAR), this algorithm turns out to be a few hundreds to one thousand times faster and is more resilient to noises than the conventional algorithms.

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“…The GALFACTS polarized continuum survey (PI: A. R. Taylor) will map the entire sky visible from Arecibo in a 300 MHz frequency band centered on 1.4 GHz by 2012, whereas the STAPS survey (PI: M. Haverkorn) will cover 500 MHz around the same frequency in the Southern sky. Radio polarimetric observations are also planned with the Australian SKA Pathfinder (Johnston et al, 2007), which should be fully operational by 2013. Finally, the Galactic Magneto-Ionic Medium Survey (GMIMS, PI: M. Wolleben), a major project consisting of six independent radio polarimetric surveys, is collecting highresolution (~ 30') all-sky polarization data in a near-continuous frequency band ranging from 300 MHz to 1.8 GHz.…”

Section: Radio Surveys In the Next Decadementioning

confidence: 99%

Foreground Science Knowledge and Prospects

Brown¹,

Dobler²,

Dotson³

et al. 2009

AIP Conference Proceedings

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Detecting "B-mode" (i.e., divergence free) polarization in the Cosmic Microwave Background (CMB) would open a new window on the very early Universe. However, the polarized microwave sky is dominated by polarized Galactic dust and synchrotron emissions, which may hinder our ability to test inflationary predictions. In this paper, we report on our knowledge of these "Galactic foregrounds," as well as on how a CMB satellite mission aiming at detecting a primordial B-mode signal ("CMBPol") will contribute to improving it. We review the observational and analysis techniques used to constrain the structure of the Galactic magnetic field, whose presence is responsible for the polarization of Galactic emissions. Although our current understanding of the magnetized interstellar medium is somewhat limited, dramatic improvements in our knowledge of its properties are expected by the time CMBPol flies. Thanks to high resolution and high sensitivity instruments observing the whole sky at frequencies between 30 GHz and 850 GHz, CMBPol will not only improve this picture by observing the synchrotron emission from our galaxy, but also help constrain dust models. Polarized emission from interstellar dust indeed dominates over any other signal in CMBPol's highest frequency channels. Observations at these wavelengths, combined with groundbased studies of starlight polarization, will therefore enable us to improve our understanding of dust properties and of the mechanism(s) responsible for the alignment of dust grains with the Galactic magnetic field. CMBPol will also shed new light on observations that are presently not well understood. Morphological studies of anomalous dust and synchrotron emissions will indeed constrain their natures and properties, while searching for fluctuations in the emission from heliospheric dust will test our understanding of the circumheliospheric interstellar medium. Finally, acquiring more information on the properties of extra-Galactic sources will be necessary in order to maximize the cosmological constraints extracted from CMBPol's observations of CMB lensing.

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Science with the Australian Square Kilometre Array Pathfinder

Cited by 305 publications

References 68 publications

The SAMI Galaxy Survey: instrument specification and target selection

The SAMI Galaxy Survey: instrument specification and target selection

A Multi-Feature Visibility Processing Algorithm for Radio Interferometric Imaging on Next-Generation Telescopes

Foreground Science Knowledge and Prospects

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