The murchison widefield array: Solar science with the low frequency SKA precursor

S. J. Tingay; D. Oberoi; I. Cairns; A. Donea; R. Duffin; W. Arcus; G. Bernardi; Judd Bowman; F. Briggs; J. D. Bunton; R. J. Cappallo; B. E. Corey; A. Deshpande; L. Desouza; D. Emrich; B. M. Gaensler; R. Goeke; L. J. Greenhill; B. J. Hazelton; D. Herne; J. N. Hewitt; M. Johnston-Hollitt; D. L. Kaplan; J. C. Kasper; J. A. Kennewell; B. B. Kincaid; R. Koenig; E. Kratzenberg; C. J. Lonsdale; M. J. Lynch; S. R. McWhirter; D. A. Mitchell; M. F. Morales; E. Morgan; S. M. Ord; J. Pathikulangara; T. Prabu; R. A. Remillard; A. E E Rogers; A. Roshi; J. E. Salah; R. J. Sault; N. Udaya-Shankar; K. S. Srivani; J. Stevens; R. Subrahmanyan; M. Waterson; R. B. Wayth; R. L. Webster; A. R. Whitney; A. Williams; C. L. Williams; J. S B Wyithe

doi:10.1088/1742-6596/440/1/012033

The murchison widefield array: Solar science with the low frequency SKA precursor

S. J. Tingay, D. Oberoi, I. Cairns, A. Donea, R. Duffin, W. Arcus, G. Bernardi, Judd Bowman, F. Briggs, J. D. Bunton, R. J. Cappallo, B. E. Corey, A. Deshpande, L. Desouza, D. Emrich, B. M. Gaensler, R. Goeke, L. J. Greenhill, B. J. Hazelton, D. HerneJ. N. Hewitt, M. Johnston-Hollitt, D. L. Kaplan, J. C. Kasper, J. A. Kennewell, B. B. Kincaid, R. Koenig, E. Kratzenberg, C. J. Lonsdale, M. J. Lynch, S. R. McWhirter, D. A. Mitchell, M. F. Morales, E. Morgan, S. M. Ord, J. Pathikulangara, T. Prabu, R. A. Remillard, A. E E Rogers, A. Roshi, J. E. Salah, R. J. Sault, N. Udaya-Shankar, K. S. Srivani, J. Stevens, R. Subrahmanyan, M. Waterson, R. B. Wayth, R. L. Webster, A. R. Whitney, A. Williams, C. L. Williams, J. S B Wyithe

Earth and Space Exploration, School of (SESE)

Research output: Contribution to journal › Conference article › peer-review

21 Scopus citations

Abstract

The Murchison Widefield Array is a low frequency (80-300 MHz) SKA Precursor, comprising 128 aperture array elements (known as tiles) distributed over an area of 3 km diameter. The MWA is located at the extraordinarily radio quiet Murchison Radioastronomy Observatory in the mid-west of Western Australia, the selected home for the Phase 1 and Phase 2 SKA low frequency arrays. The MWA science goals include: 1) detection of fluctuations in the brightness temperature of the diffuse redshifted 21 cm line of neutral hydrogen from the epoch of reionisation; 2) studies of Galactic and extragalactic processes based on deep, confusion-limited surveys of the full sky visible to the array; 3) time domain astrophysics through exploration of the variable radio sky; and 4) solar imaging and characterisation of the heliosphere and ionosphere via propagation effects on background radio source emission. This paper concentrates on the capabilities of the MWA for solar science and summarises some of the solar science results to date, in advance of the initial operation of the final instrument in 2013.

Original language	English (US)
Article number	012033
Journal	Journal of Physics: Conference Series
Volume	440
Issue number	1
DOIs	https://doi.org/10.1088/1742-6596/440/1/012033
State	Published - 2013
Event	Eclipse on the Coral Sea: Cycle 24 Ascending - Palm Cove, QLD, Australia Duration: Nov 12 2012 → Nov 16 2012

ASJC Scopus subject areas

General Physics and Astronomy

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10.1088/1742-6596/440/1/012033

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Tingay, S. J., Oberoi, D., Cairns, I., Donea, A., Duffin, R., Arcus, W., Bernardi, G., Bowman, J., Briggs, F., Bunton, J. D., Cappallo, R. J., Corey, B. E., Deshpande, A., Desouza, L., Emrich, D., Gaensler, B. M., Goeke, R., Greenhill, L. J., Hazelton, B. J., ... Wyithe, J. S. B. (2013). The murchison widefield array: Solar science with the low frequency SKA precursor. Journal of Physics: Conference Series, 440(1), Article 012033. https://doi.org/10.1088/1742-6596/440/1/012033

Tingay, SJ, Oberoi, D, Cairns, I, Donea, A, Duffin, R, Arcus, W, Bernardi, G, Bowman, J, Briggs, F, Bunton, JD, Cappallo, RJ, Corey, BE, Deshpande, A, Desouza, L, Emrich, D, Gaensler, BM, Goeke, R, Greenhill, LJ, Hazelton, BJ, Herne, D, Hewitt, JN, Johnston-Hollitt, M, Kaplan, DL, Kasper, JC, Kennewell, JA, Kincaid, BB, Koenig, R, Kratzenberg, E, Lonsdale, CJ, Lynch, MJ, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Ord, SM, Pathikulangara, J, Prabu, T, Remillard, RA, Rogers, AEE, Roshi, A, Salah, JE, Sault, RJ, Udaya-Shankar, N, Srivani, KS, Stevens, J, Subrahmanyan, R, Waterson, M, Wayth, RB, Webster, RL, Whitney, AR, Williams, A, Williams, CL & Wyithe, JSB 2013, 'The murchison widefield array: Solar science with the low frequency SKA precursor', Journal of Physics: Conference Series, vol. 440, no. 1, 012033. https://doi.org/10.1088/1742-6596/440/1/012033

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title = "The murchison widefield array: Solar science with the low frequency SKA precursor",

abstract = "The Murchison Widefield Array is a low frequency (80-300 MHz) SKA Precursor, comprising 128 aperture array elements (known as tiles) distributed over an area of 3 km diameter. The MWA is located at the extraordinarily radio quiet Murchison Radioastronomy Observatory in the mid-west of Western Australia, the selected home for the Phase 1 and Phase 2 SKA low frequency arrays. The MWA science goals include: 1) detection of fluctuations in the brightness temperature of the diffuse redshifted 21 cm line of neutral hydrogen from the epoch of reionisation; 2) studies of Galactic and extragalactic processes based on deep, confusion-limited surveys of the full sky visible to the array; 3) time domain astrophysics through exploration of the variable radio sky; and 4) solar imaging and characterisation of the heliosphere and ionosphere via propagation effects on background radio source emission. This paper concentrates on the capabilities of the MWA for solar science and summarises some of the solar science results to date, in advance of the initial operation of the final instrument in 2013.",

author = "Tingay, {S. J.} and D. Oberoi and I. Cairns and A. Donea and R. Duffin and W. Arcus and G. Bernardi and Judd Bowman and F. Briggs and Bunton, {J. D.} and Cappallo, {R. J.} and Corey, {B. E.} and A. Deshpande and L. Desouza and D. Emrich and Gaensler, {B. M.} and R. Goeke and Greenhill, {L. J.} and Hazelton, {B. J.} and D. Herne and Hewitt, {J. N.} and M. Johnston-Hollitt and Kaplan, {D. L.} and Kasper, {J. C.} and Kennewell, {J. A.} and Kincaid, {B. B.} and R. Koenig and E. Kratzenberg and Lonsdale, {C. J.} and Lynch, {M. J.} and McWhirter, {S. R.} and Mitchell, {D. A.} and Morales, {M. F.} and E. Morgan and Ord, {S. M.} and J. Pathikulangara and T. Prabu and Remillard, {R. A.} and Rogers, {A. E E} and A. Roshi and Salah, {J. E.} and Sault, {R. J.} and N. Udaya-Shankar and Srivani, {K. S.} and J. Stevens and R. Subrahmanyan and M. Waterson and Wayth, {R. B.} and Webster, {R. L.} and Whitney, {A. R.} and A. Williams and Williams, {C. L.} and Wyithe, {J. S B}",

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doi = "10.1088/1742-6596/440/1/012033",

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AU - Tingay, S. J.

AU - Oberoi, D.

AU - Cairns, I.

AU - Donea, A.

AU - Duffin, R.

AU - Arcus, W.

AU - Bernardi, G.

AU - Bowman, Judd

AU - Briggs, F.

AU - Bunton, J. D.

AU - Cappallo, R. J.

AU - Corey, B. E.

AU - Deshpande, A.

AU - Desouza, L.

AU - Emrich, D.

AU - Gaensler, B. M.

AU - Goeke, R.

AU - Greenhill, L. J.

AU - Hazelton, B. J.

AU - Herne, D.

AU - Hewitt, J. N.

AU - Johnston-Hollitt, M.

AU - Kaplan, D. L.

AU - Kasper, J. C.

AU - Kennewell, J. A.

AU - Kincaid, B. B.

AU - Koenig, R.

AU - Kratzenberg, E.

AU - Lonsdale, C. J.

AU - Lynch, M. J.

AU - McWhirter, S. R.

AU - Mitchell, D. A.

AU - Morales, M. F.

AU - Morgan, E.

AU - Ord, S. M.

AU - Pathikulangara, J.

AU - Prabu, T.

AU - Remillard, R. A.

AU - Rogers, A. E E

AU - Roshi, A.

AU - Salah, J. E.

AU - Sault, R. J.

AU - Udaya-Shankar, N.

AU - Srivani, K. S.

AU - Stevens, J.

AU - Subrahmanyan, R.

AU - Waterson, M.

AU - Wayth, R. B.

AU - Webster, R. L.

AU - Whitney, A. R.

AU - Williams, A.

AU - Williams, C. L.

AU - Wyithe, J. S B

PY - 2013

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N2 - The Murchison Widefield Array is a low frequency (80-300 MHz) SKA Precursor, comprising 128 aperture array elements (known as tiles) distributed over an area of 3 km diameter. The MWA is located at the extraordinarily radio quiet Murchison Radioastronomy Observatory in the mid-west of Western Australia, the selected home for the Phase 1 and Phase 2 SKA low frequency arrays. The MWA science goals include: 1) detection of fluctuations in the brightness temperature of the diffuse redshifted 21 cm line of neutral hydrogen from the epoch of reionisation; 2) studies of Galactic and extragalactic processes based on deep, confusion-limited surveys of the full sky visible to the array; 3) time domain astrophysics through exploration of the variable radio sky; and 4) solar imaging and characterisation of the heliosphere and ionosphere via propagation effects on background radio source emission. This paper concentrates on the capabilities of the MWA for solar science and summarises some of the solar science results to date, in advance of the initial operation of the final instrument in 2013.

AB - The Murchison Widefield Array is a low frequency (80-300 MHz) SKA Precursor, comprising 128 aperture array elements (known as tiles) distributed over an area of 3 km diameter. The MWA is located at the extraordinarily radio quiet Murchison Radioastronomy Observatory in the mid-west of Western Australia, the selected home for the Phase 1 and Phase 2 SKA low frequency arrays. The MWA science goals include: 1) detection of fluctuations in the brightness temperature of the diffuse redshifted 21 cm line of neutral hydrogen from the epoch of reionisation; 2) studies of Galactic and extragalactic processes based on deep, confusion-limited surveys of the full sky visible to the array; 3) time domain astrophysics through exploration of the variable radio sky; and 4) solar imaging and characterisation of the heliosphere and ionosphere via propagation effects on background radio source emission. This paper concentrates on the capabilities of the MWA for solar science and summarises some of the solar science results to date, in advance of the initial operation of the final instrument in 2013.

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DO - 10.1088/1742-6596/440/1/012033

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JO - Journal of Physics: Conference Series

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Y2 - 12 November 2012 through 16 November 2012

ER -

The murchison widefield array: Solar science with the low frequency SKA precursor

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