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6 results on '"Corey, B.E"'

1. First limits on the 21 cm power spectrum during the Epoch of X-ray heating

Author

Ewell-Wice, A., Dillon, Joshua, Hewitt, Jacqueline N, Loeb, Abraham, Mesinger, A., Neben, A R, Offringa, A., Tegmark, Max, Barry, N, Beardsley, A. P., Bernardi, G, Briggs, Franklin, Bowman, Judd D, Feng, Lu, Greenhill, Lincoln, Johnston-Hollitt, M, Jacobs, Daniel C., Kaplan, D L, Thyagarajan, Nithyanandan, Oberoi, D, Pindor, B., Prabu, T, Rogers, Alan, Udaya Shankar, N., Srivani, K. S., Whitney, Alan, Williams, Christopher L, Cappallo, R. J, Carroll, P, Corey, B.E, de Oliveira-Costa,, A, Emrich, David, Gaensler, B M, Goeke, R, Hazelton, B, Hurley-Walker, Natasha, Kasper, J.C., Kim, HS, Kratzenberg, Eric, Lenc, E, Line, J, Lonsdale, Colin J, Lynch, Mervyn J, McKinley, B, McWhirter, S.R., Mitchell, D.A., Morales, Miguel F, Morgan, Edward H, Ord, S M, Paul, S, Pober, J. C., Procopio, P., Riding, J, Roshi, A., Sethi, Shiv K, Subrahmanyan, R., Sullivan, I S, Tingay, S.J., Trott, C. M., Waterson, Mark, Wayth, Randall, B., Webster, Rachel L, Williams, A, Wu, Chen, Wyithe, J Stuart B, Ewell-Wice, A., Dillon, Joshua, Hewitt, Jacqueline N, Loeb, Abraham, Mesinger, A., Neben, A R, Offringa, A., Tegmark, Max, Barry, N, Beardsley, A. P., Bernardi, G, Briggs, Franklin, Bowman, Judd D, Feng, Lu, Greenhill, Lincoln, Johnston-Hollitt, M, Jacobs, Daniel C., Kaplan, D L, Thyagarajan, Nithyanandan, Oberoi, D, Pindor, B., Prabu, T, Rogers, Alan, Udaya Shankar, N., Srivani, K. S., Whitney, Alan, Williams, Christopher L, Cappallo, R. J, Carroll, P, Corey, B.E, de Oliveira-Costa,, A, Emrich, David, Gaensler, B M, Goeke, R, Hazelton, B, Hurley-Walker, Natasha, Kasper, J.C., Kim, HS, Kratzenberg, Eric, Lenc, E, Line, J, Lonsdale, Colin J, Lynch, Mervyn J, McKinley, B, McWhirter, S.R., Mitchell, D.A., Morales, Miguel F, Morgan, Edward H, Ord, S M, Paul, S, Pober, J. C., Procopio, P., Riding, J, Roshi, A., Sethi, Shiv K, Subrahmanyan, R., Sullivan, I S, Tingay, S.J., Trott, C. M., Waterson, Mark, Wayth, Randall, B., Webster, Rachel L, Williams, A, Wu, Chen, and Wyithe, J Stuart B

Published
2016

2. On the detection and tracking of space debris using the Murchison Wdefield Array. I. Simulations and test observations demonstrate feasibility

Author

Tingay, Steven, Kaplan, D.L., McKinley, B., Briggs, F., Wayth, Randall, Hurley-Walker, N., Kennewell, J., Smith, C., Zhang, K., Arcus, W., Bhat, Ramesh, Emrich D., Herne, D., Kudryavtseva, N., Lynch, M., Ord, S.M., Waterson, M., Barnes, D.G., Bell, M., Gaensler, B.M., Lenc, E., Bernardi, G., Greenhill, L.J., Kasper, J.C., Bowman, J.D., Jacobs, D., Bunton, J.D., Desouza, L., Koenig, R., Pathikulangara, J., Stevens, J., Cappallo, R.J., Corey, B.E., Kincaid, B.B., Kratzenberg, E., Lonsdale, C.J., McWhirter, S.R., Rogers, A.E.E., Salah, J.E., Whitney, A.R., Deshpande, A., Prabu, T., Udaya Shankar, N., Srivani, K.S., Subrahmanyan, R., Ewall-Wice, A., Feng, L., Goeke, R., Morgan, E., Remillard, R.A., Williams, C.L., Hazelton, B.J., Morales, M.F., Johnston-Hollitt, M., Mitchell, D.A., Procopio, P., Riding, J., Webster, R.L., Wyithe, J.S.B., Oberoi, D., Roshi, A., Sault, R.J., Williams, A., Tingay, Steven, Kaplan, D.L., McKinley, B., Briggs, F., Wayth, Randall, Hurley-Walker, N., Kennewell, J., Smith, C., Zhang, K., Arcus, W., Bhat, Ramesh, Emrich D., Herne, D., Kudryavtseva, N., Lynch, M., Ord, S.M., Waterson, M., Barnes, D.G., Bell, M., Gaensler, B.M., Lenc, E., Bernardi, G., Greenhill, L.J., Kasper, J.C., Bowman, J.D., Jacobs, D., Bunton, J.D., Desouza, L., Koenig, R., Pathikulangara, J., Stevens, J., Cappallo, R.J., Corey, B.E., Kincaid, B.B., Kratzenberg, E., Lonsdale, C.J., McWhirter, S.R., Rogers, A.E.E., Salah, J.E., Whitney, A.R., Deshpande, A., Prabu, T., Udaya Shankar, N., Srivani, K.S., Subrahmanyan, R., Ewall-Wice, A., Feng, L., Goeke, R., Morgan, E., Remillard, R.A., Williams, C.L., Hazelton, B.J., Morales, M.F., Johnston-Hollitt, M., Mitchell, D.A., Procopio, P., Riding, J., Webster, R.L., Wyithe, J.S.B., Oberoi, D., Roshi, A., Sault, R.J., and Williams, A.

Abstract

The Murchison Widefield Array (MWA) is a new low-frequency interferometric radio telescope, operating in the benign radio frequency environment of remote Western Australia. The MWA is the low-frequency precursor to the Square Kilometre Array (SKA) and is the first of three SKA precursors to be operational, supporting a varied science mission ranging from the attempted detection of the Epoch of Reionization to the monitoring of solar flares and space weather. In this paper we explore the possibility that the MWA can be used for the purposes of Space Situational Awareness (SSA). In particular we propose that the MWA can be used as an element of a passive radar facility operating in the frequency range 87.5-108 MHz (the commercial FM broadcast band). In this scenario the MWA can be considered the receiving element in a bi-static radar configuration, with FM broadcast stations serving as non-cooperative transmitters. The FM broadcasts propagate into space, are reflected off debris in Earth orbit, and are received at the MWA. The imaging capabilities of the MWA can be used to simultaneously detect multiple pieces of space debris, image their positions on the sky as a function of time, and provide tracking data that can be used to determine orbital parameters. Such a capability would be a valuable addition to Australian and global SSA assets, in terms of southern and eastern hemispheric coverage. We provide a feasibility assessment of this proposal, based on simple calculations and electromagnetic simulations, that shows that the detection of sub-meter size debris should be possible (debris radius of >0.5 m to ∼1000 km altitude). We also present a proof-of-concept set of observations that demonstrate the feasibility of the proposal, based on the detection and tracking of the International Space Station via reflected FM broadcast signals originating in southwest Western Australia. These observations broadly validate our calculations and simulations. We discuss some signifi

Published
2013

3. A New Layout Optimization Technique for Interferometric Arrays, Applied to the Murchison Widefield Array

Author

Beardsley, A.P., Hazelton, B.J., Morales, M.F., Capallo, R.J., Goeke, R., Emrich, D., Lonsdale, C.J., Arcus, W., Barnes, D., Bernardi, G., Bowman, J.D., Bunton, J.D., Corey, B.E., Deshpande, A., DeSouza, L., Gaensler, B.M., Greenhill, L.J., Herne, D., Hewitt, J.N., Kaplan, D.L., Kasper, J.C., Kincaid, B.B., Koenig, R., Kratzenberg, E., Lynch, M.J., McWhirter, S.R., Mitchell, D.A., Morgan, E., Oberoi, D., Ord, S.M., Pathikulangara, J., Prabu, T., Remillard, R.A., Rogers, A.E.E., Roshi, A., Salah, J.E., Sault, R.J., Udaya Shankar, N., Srivani, K.S., Stevens, J., Subrahmanyan, R., Tingay, Steven, Wayth, Randall, Waterson, M., Webster, R.L., Whitney, A.R., Williams, A., Wyithe, J.S.B., Beardsley, A.P., Hazelton, B.J., Morales, M.F., Capallo, R.J., Goeke, R., Emrich, D., Lonsdale, C.J., Arcus, W., Barnes, D., Bernardi, G., Bowman, J.D., Bunton, J.D., Corey, B.E., Deshpande, A., DeSouza, L., Gaensler, B.M., Greenhill, L.J., Herne, D., Hewitt, J.N., Kaplan, D.L., Kasper, J.C., Kincaid, B.B., Koenig, R., Kratzenberg, E., Lynch, M.J., McWhirter, S.R., Mitchell, D.A., Morgan, E., Oberoi, D., Ord, S.M., Pathikulangara, J., Prabu, T., Remillard, R.A., Rogers, A.E.E., Roshi, A., Salah, J.E., Sault, R.J., Udaya Shankar, N., Srivani, K.S., Stevens, J., Subrahmanyan, R., Tingay, Steven, Wayth, Randall, Waterson, M., Webster, R.L., Whitney, A.R., Williams, A., and Wyithe, J.S.B.

Abstract

Antenna layout is an important design consideration for radio interferometers because it determines the quality of the snapshot point spread function (PSF, or array beam). This is particularly true for experiments targeting the 21-cm Epoch of Reionization signal as the quality of the foreground subtraction depends directly on the spatial dynamic range and thus the smoothness of the baseline distribution. Nearly all sites have constraints on where antennas can be placed even at the remote Australian location of the Murchison Widefield Array (MWA) there are rock outcrops, flood zones, heritages areas, emergency runways and trees. These exclusion areas can introduce spatial structure into the baseline distribution that enhances the PSF sidelobes and reduces the angular dynamic range. In this paper we present a new method of constrained antenna placement that reduces the spatial structure in the baseline distribution. This method not only outperforms random placement algorithms that avoid exclusion zones, but surprisingly outperforms random placement algorithms without constraints to provide what we believe are the smoothest constrained baseline distributions developed to date. We use our new algorithm to determine antenna placements for the originally planned MWA, and present the antenna locations, baseline distribution and snapshot PSF for this array choice.

Published
2012

4. Interferometric Imaging with the 32 Element Murchison Wide-Field Array

Author

Ord, S., Mitchell, D., Wayth, Randall, Greenhill, L., Bernadi, G., Gleadow, A., Edgar, R.G., Clarke, M.A., Allen, G., Arcus, Wayne, Benkevitch, L., Bowman, J.D., Briggs, F.H., Bunton, J.D., Burns, S., Cappallo, R.J., Coles, W.A., Corey, B.E., DeSouza, L., Doeleman, S.S., Derome, M., Deshpande, A., Emrich, D., Goeke, M.R., Gopalakrishna, M.R., Herne, David, Hewitt, J.N., Kamini, P.A., Kaplan, D.L., Kasper, J.C., Kincaid, B.B., Kocz, J., Kowald, E., Kratzenberg, E., Kumar, D., Lonsdale, C., Lynch, Mervyn, McWhirter, S., Madhavi, S., Matejek, M., Morales, M., Morgan, E., Oberoi, D., Pathikulangara, J., Prabu, T., Rogers, A., Roshi, A., Salah, J., Schinkel, A., Udaya, S.N., Srivani, K., Stevens, J., Tingay, Steven, Vaccarella, A., Waterson, Mark, Ord, S., Mitchell, D., Wayth, Randall, Greenhill, L., Bernadi, G., Gleadow, A., Edgar, R.G., Clarke, M.A., Allen, G., Arcus, Wayne, Benkevitch, L., Bowman, J.D., Briggs, F.H., Bunton, J.D., Burns, S., Cappallo, R.J., Coles, W.A., Corey, B.E., DeSouza, L., Doeleman, S.S., Derome, M., Deshpande, A., Emrich, D., Goeke, M.R., Gopalakrishna, M.R., Herne, David, Hewitt, J.N., Kamini, P.A., Kaplan, D.L., Kasper, J.C., Kincaid, B.B., Kocz, J., Kowald, E., Kratzenberg, E., Kumar, D., Lonsdale, C., Lynch, Mervyn, McWhirter, S., Madhavi, S., Matejek, M., Morales, M., Morgan, E., Oberoi, D., Pathikulangara, J., Prabu, T., Rogers, A., Roshi, A., Salah, J., Schinkel, A., Udaya, S.N., Srivani, K., Stevens, J., Tingay, Steven, Vaccarella, A., and Waterson, Mark

Abstract

The Murchison Wide-Field Array (MWA) is a low-frequency radio telescope, currently under construction, intended to search for the spectral signature of the epoch of reionization (EOR) and to probe the structure of the solar corona. Sited in western Australia, the full MWA will comprise 8192 dipoles grouped into 512 tiles and will be capable of imaging the sky south of 40° declination, from 80 MHz to 300 MHz with an instantaneous field of view that is tens of degrees wide and a resolution of a few arcminutes. A 32 station prototype of the MWA has been recently commissioned and a set of observations has been taken that exercise the whole acquisition and processing pipeline. We present Stokes I, Q, and U images from two ~4 hr integrations of a field 20° wide centered on Pictoris A. These images demonstrate the capacity and stability of a real-time calibration and imaging technique employing the weighted addition of warped snapshots to counter extreme wide-field imaging distortions.

Published
2010

5. The Murchison Widefield Array

Author

RFI2010, Mitchell, Daniel A., Greenhill, Lincoln J., Ord, Stephen M., Bernardi, Gianni, Wayth, Randall B., Edgar, Richard G., Clarke, Michael A., Dale, Kevin, Pfister, Hanspeter, Gleadow, Stewart J., Arcus, Wayne, Briggs, F.H., Benkevitch, L., Bowman, J.D., Bunton, J.D., Burns, S., Cappallo, R.J., Corey, B.E., de Oliveira-Costa, A., Desouza, L., Doeleman, S.S., Derome, M.F., Emrich, David, Glossop, Mark, Goeke, R., Gopala Krishna, M.R., Hazelton, B., Herne, David, Hewitt, J.N., Kamini, P.A., Kaplan, D.L., Kasper, J.C., Kincaid, B.B., Kocz, J., Kowald, E., Kratzenberg, E., Kumar, D., Lonsdale, C.J., Lynch, M.J., Madhavi, S., Matejek, M., McWhirter, S.R., Morales, M.F., Morgan, E., Oberoi, D., Pathikulangara, J., Prabu, T., Rogers, A., Salah, J.E., Sault, R.J., Udaya Shankar, N., Srivani, K.S., Stevens, J., Tingay, Steven, Vaccarella, A., Waterson, Mark, Webster, R.L., Whitney, A.R., Williams, A., Williams, C., RFI2010, Mitchell, Daniel A., Greenhill, Lincoln J., Ord, Stephen M., Bernardi, Gianni, Wayth, Randall B., Edgar, Richard G., Clarke, Michael A., Dale, Kevin, Pfister, Hanspeter, Gleadow, Stewart J., Arcus, Wayne, Briggs, F.H., Benkevitch, L., Bowman, J.D., Bunton, J.D., Burns, S., Cappallo, R.J., Corey, B.E., de Oliveira-Costa, A., Desouza, L., Doeleman, S.S., Derome, M.F., Emrich, David, Glossop, Mark, Goeke, R., Gopala Krishna, M.R., Hazelton, B., Herne, David, Hewitt, J.N., Kamini, P.A., Kaplan, D.L., Kasper, J.C., Kincaid, B.B., Kocz, J., Kowald, E., Kratzenberg, E., Kumar, D., Lonsdale, C.J., Lynch, M.J., Madhavi, S., Matejek, M., McWhirter, S.R., Morales, M.F., Morgan, E., Oberoi, D., Pathikulangara, J., Prabu, T., Rogers, A., Salah, J.E., Sault, R.J., Udaya Shankar, N., Srivani, K.S., Stevens, J., Tingay, Steven, Vaccarella, A., Waterson, Mark, Webster, R.L., Whitney, A.R., Williams, A., and Williams, C.

Published
2010

6. The Compact Radio Source 2021+614 : Simultaneous 2.3 and 8.3 GHz Mark III VLBI Observations

Author

Bartel, N., Shapiro, I.I., Corey, B.E., Marcaide, J.M., Rogers, A.E.E., Whitney, A.R., Cappallo, R.J., Kühr, H., Graham, D., Bååth, L.B., Bartel, N., Shapiro, I.I., Corey, B.E., Marcaide, J.M., Rogers, A.E.E., Whitney, A.R., Cappallo, R.J., Kühr, H., Graham, D., and Bååth, L.B.

Abstract

Second-epoch VLBI observations of the flat-spectrum radio source 2021+614 made simultaneously at 2.3 and 8.3 GHz with the Mark III system are reported. The maps derived from these observations reveal a complex, frequency-dependent radio structure on the milliarcsecond scale. The object has four nearly collinear components oriented at a position angle of about 35 degrees and embedded in an extended region. Two of these are optically thin, one has a flat spectrum, and the other appears to be synchrotron self-absorbed in the frequency range 2.3-8.3 GHz. No significant structural variation is found at either frequency between epochs separated by about three years. The formal estimate of the transverse velocity between two components, one with a flat and the other with an inverted spectrum, is v/c = 0.7 + or - 2.3. Remarkable similarities between 2021+614 and the unusual source 0316+413 are discussed.

Published
1984

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