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1. Integrated spatial analysis for human–wildlife coexistence in the American West

Author

Neil Carter, Matthew A Williamson, Sophie Gilbert, Stacy A Lischka, Laura R Prugh, Joshua J Lawler, Alexander L Metcalf, Aerin L Jacob, Bray J Beltrán, Antonio J Castro, Abigail Sage, and Morey Burnham

Subjects
coexistence, spatial integration, conservation planning, wildlife, Environmental technology. Sanitary engineering, TD1-1066, Environmental sciences, GE1-350, Science, Physics, QC1-999
Published
2020
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2. The American West as a social-ecological region: drivers, dynamics and implications for nested social-ecological systems

Author

Kristal Jones, Jesse Abrams, R Travis Belote, Bray J Beltrán, Jodi Brandt, Neil Carter, Antonio J Castro, Brian C Chaffin, Alexander L Metcalf, Gabrielle Roesch-McNally, Kenneth E Wallen, and Matthew A Williamson

Subjects
social-ecological region, social-ecological system, American West, Environmental technology. Sanitary engineering, TD1-1066, Environmental sciences, GE1-350, Science, Physics, QC1-999
Abstract

The American West exists in the popular imagination as a distinct region, and policies and politics often suggest that both the challenges and the opportunities for land management and human well-being across the region are relatively homogeneous. In this paper, we argue that there are key characteristics that define the West as a social-ecological region, and also that there are myriad social-ecological systems (SESs) within the region that require diverse and dynamic approaches to managing change over time. We first conceptualize aridity, topography, and a unique political economy of land as exogenous factors that persist over time and space to define the American West as a contiguous social-ecological region. We then identify a second set of characteristics that show high degrees of variation across SESs within the American West. Finally, we operationalize the relationships between regional characteristics and local dynamics through a set of case studies that exemplify specific types of SESs in the region. The results of these empirical representations of the regional and intra-regional social-ecological dynamics of the contemporary American West highlight the implications for research and management of taking a cross-scale integrated approach to address pressing social-ecological opportunities and challenges in complex adaptive systems.

Published
2019
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3. Population Study of Astrophysical False Positive Detections in the Southern PLATO field

Author

Bray, J. C., Kolb, U., Rowden, P., Farmer, Robert, Boerner, A., and Kozhura, O.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

For the upcoming PLAnetary Transits and Oscillation of stars (PLATO) satellite mission, a large number of target stars are required to yield a statistically significant number of planet transits. Locating the centres of the long duration observational phase (LOP) fields closer to the Galactic plane will increase the target star numbers but also the astrophysical false positives (FPs) from blended eclipsing binary systems. We utilise the Binary Stellar Evolution and Population Synthesis (BiSEPS) code, to create a complete synthetic stellar and planetary population for the proposed southern LOP field (LOPS0), as well as for a representative portion of the northern LOP field (LOPNsub). For LOPS0 we find an overall low FP rate for planets smaller than Neptunes. The FP rate generally shows little variation with Galactic longitude (l), and a modest increase with decreasing Galactic latitude (|b|). The location of the LOPS field centre within the current allowed region is not strongly constrained by FPs. Analysis of LOPNsub suggests a markedly increased number of FPs across the full range of planet radii at low |b| resulting in approximately twice the percent FP rate in the LOPNsub compared to the corresponding southern field segment in the planet radius range -0.2 < log(R/Rsun) <= 0.4. However, only a few percent of fully eclipsing FPs in LOPS0 in this radius range have periods, Comment: 17 pages, 23 figures, 9 tables. Accepted for publication in MNRAS

Published
2022
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5. Exploring compact binary merger host galaxies and environments with $\rm{zELDA}$

Author

Mandhai, S., Lamb, G. P., Tanvir, N. R., Bray, J., Nixon, C. J., Eyles-Ferris, R. A. J., Levan, A. J., and Gompertz, B. P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Compact binaries such as double neutron stars or a neutron star paired with a black-hole, are strong sources of gravitational waves during coalescence and also the likely progenitors of various electromagnetic phenomena, notably short-duration gamma-ray bursts (SGRBs), and kilonovae. In this work, we generate populations of synthetic binaries and place them in galaxies from the large-scale hydrodynamical galaxy evolution simulation EAGLE. With our zELDA code, binaries are seeded in proportion to star formation rate, and we follow their evolution to merger using both the BPASS and COSMIC binary stellar evolution codes. We track their dynamical evolution within their host galaxy potential, to estimate the galactocentric distance at the time of the merger. Finally, we apply observational selection criteria to allow comparison of this model population with the legacy sample of SGRBs. We find a reasonable agreement with the redshift distribution (peaking at $0.526$)., Comment: Accepted for publication in MNRAS, 21 Pages (6 Tables, 14 Figures), 14 Pages Appendix (4 Tables, 16 Figures)

Published
2021
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7. The SKA Particle Array Prototype: The First Particle Detector at the Murchison Radio-astronomy Observatory

Author

Bray, J. D., Williamson, A., Schelfhout, J., James, C. W., Spencer, R. E., Chen, H., Cropper, B. D., Emrich, D., Gould, K. M. L., Haungs, A., Hodder, W., Howland, T., Huege, T., Kenney, D., McPhail, A., Mitchell, S., Niţu, I. C., Roberts, P., Tawn, R., Tickner, J., and Tingay, S. J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report on the design, deployment, and first results from a scintillation detector deployed at the Murchison Radio-astronomy Observatory (MRO). The detector is a prototype for a larger array -- the Square Kilometre Array Particle Array (SKAPA) -- planned to allow the radio-detection of cosmic rays with the Murchison Widefield Array and the low-frequency component of the Square Kilometre Array. The prototype design has been driven by stringent limits on radio emissions at the MRO, and to ensure survivability in a desert environment. Using data taken from Nov.\ 2018 to Feb.\ 2019, we characterize the detector response while accounting for the effects of temperature fluctuations, and calibrate the sensitivity of the prototype detector to through-going muons. This verifies the feasibility of cosmic ray detection at the MRO. We then estimate the required parameters of a planned array of eight such detectors to be used to trigger radio observations by the Murchison Widefield Array., Comment: 17 pages, 14 figures, 3 tables

Published
2020
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8. An updated estimate of the cosmic radio background and implications for ultra-high-energy photon propagation

Author

Niţu, I. C., Bevins, H. T. J., Bray, J. D., and Scaife, A. M. M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present an updated estimate of the cosmic radio background (CRB) and the corresponding attenuation lengths for ultra-high energy photons. This new estimate provides associated uncertainties as a function of frequency derived from observational constraints on key physical parameters. We also present the expected variation in the spectrum of the CRB as a function of these parameters, as well as accounting for the expected variation in spectral index among the population of radio galaxies. The new estimate presented in this work shows better agreement with observational constraints from radio source-count measurements than previous calculations. In the energy regime where we expect cosmogenic photons dominantly attenuated by the CRB, our calculation of the attenuation length differs from previous estimates by a factor of up to 3, depending on energy and the specific model for comparison. These results imply a decrease in the expected number of cosmogenic photons with energies $\sim 10^{19}-10^{20}$ eV.

Published
2020
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9. Low-frequency observations of the Giant Radio Galaxy NGC 6251

Author

Cantwell, T. M., Bray, J. D., Croston, J. H., Scaife, A. M. M., Mulcahy, D. D., Best, P. N., Bruggen, M., Brunetti, G., Callingham, J. R., Clarke, A. O., Hardcastle, M. J., Harwood, J. J., Heald, G., Heesen, V., Iacobelli, M., Jamrozy, M., Morganti, R., Orru, E., O'Sullivan, S. P., Riseley, C. J., Rottgering, H. J. A., Shulevski, A., Sridhar, S. S., Tasse, C., and Van Eck, C. L.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present LOFAR observations at 150 MHz of the borderline FRI/FRII giant radio galaxy NGC 6251. This paper presents the most sensitive and highest-resolution images of NGC 6251 at these frequencies to date, revealing for the first time a low-surface-brightness extension to the northern lobe, and a possible backflow associated with the southern lobe. The integrated spectra of components of NGC 6251 are consistent with previous measurements at higher frequencies, similar to results from other LOFAR studies of nearby radio galaxies. We find the outer structures of NGC 6251 to be either at equipartition or slightly electron dominated, similar to those of FRII sources rather than FRIs; but this conclusion remains tentative because of uncertainties associated with the geometry and the extrapolation of X-ray measurements to determine the external pressure distribution on the scale of the outer lobes. We place lower limits on the ages of the extension of the northern lobe and the backflow of the southern lobe of $t \gtrsim 250$ Myr and $t \gtrsim 210$ Myr respectively. We present the first detection of polarisation at 150 MHz in NGC 6251. Taking advantage of the high Faraday resolution of LOFAR, we place an upper limit on the magnetic field in the group of $B < 0.2 (\Lambda_B / 10 {\rm kpc})^{-0.5} \mu$G for a coherence scale of $\Lambda_B < 60 {\rm kpc}$ and $B < 13 \mu$G for $\Lambda_B = 240$ kpc., Comment: 19 pages, 17 figures; accepted by MNRAS

Published
2020
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10. What impact does pre-sojourn preparation have on host-culture adjustment for sojourning students? : a case-study of a SINO-UK Joint Programme

Author

Richards-Bray, J. E., Li, Daguo, and Floyd, Alan

Abstract

It is widely known that sojourning students experience a major, stressful life event (Savicki & Adams, 2007) as they adjust to the host-culture, which can deleteriously affect their experience and academic achievement. Therefore, this longitudinal study evaluates the impact of internationalisation at home preparation on the adjustment of one cohort of sojourning Chinese students to the host-social and academic cultures of a UK university. Undertaken primarily in a post-1992 UK university, it uses a mixed methods explanatory sequential design (Creswell, Plano Clark, Gutmann, & Hanson, 2003), conducted in two connected phases, a quantitative followed by a qualitative stage, with the emphasis being on the qualitative phase. An initial pre-sojourn questionnaire gathered background data, demographic information and assisted sampling. Following arrival in the UK, and involving 7 participants, qualitative data were collected through diaries, semi-structured interviews at three points during the year, and other artefacts such as photographs and videos. Within the context of internationalisation of education, specifically transnational education and internationalisation at home, the data were analysed against the conceptual framework of cultural background including intercultural competence, cultural adjustment and autonomy, linked with agency and transformative learning theory. The findings demonstrate that the students adjusted well, having been successfully prepared by the internationalisation at home preparation, the summer camp and sojourning as a group. Individual factors such as personality, motivation for sojourning and parental influence were also important. These results may assist policymakers and practitioners in the field to facilitate a smoother University transition for their students, in particular through the development of deep transnational partnerships.

Published
2020
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12. Applications of antenna-level buffering

Author

Nelles, A., Bray, J. D., and James, C. W.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The purpose of this document is to discuss applications of the antenna-level buffering capability being implemented in SKA-LOW. In addition to their scientific motivation -- to detect and study cosmic rays interacting in the atmosphere -- these buffers provide access to low-level data for engineering and development work. Experience has shown that antenna-level buffered data can assist with antenna calibration, localising RFI, and diagnosing fundamental hardware problems. In this document, we describe several of these applications, with close reference to experience with LOFAR, ACTA, Parkes, and the OVRO-LWA.

Published
2019

14. An upper limit on the strength of the extragalactic magnetic field from ultra-high-energy cosmic-ray anisotropy

Author

Bray, J. D. and Scaife, A. M. M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

If ultra-high-energy cosmic rays originate from extragalactic sources, the offsets of their arrival directions from these sources imply an upper limit on the strength of the extragalactic magnetic field. The Pierre Auger Collaboration has recently reported that anisotropy in the arrival directions of cosmic rays is correlated with several types of extragalactic objects. If these cosmic rays originate from these objects, they imply a limit on the extragalactic magnetic field strength of B < 0.7-2.2 x 10^-9 (lambda_B / 1 Mpc)^-1/2 G for coherence lengths lambda_B < 100 Mpc and B < 0.7-2.2 x 10^-10 G at larger scales. This is comparable to existing upper limits at lambda_B = 1 Mpc, and improves on them by a factor 4-12 at larger scales. The principal source of uncertainty in our results is the unknown cosmic-ray composition., Comment: 9 pages, 3 figures, accepted by ApJ

Published
2018
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15. Neutron Star Kicks II: Revision and further testing of the conservation of momentum 'kick' model

Author

Bray, J. C. and Eldridge, J. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

In Bray and Eldridge (2017), we proposed a simple neutron star kick formula, v kick = alpha (M ejecta / M remnant) + beta to explain the observed 2D velocities of young single neutron stars. Using this kick we found that there is no statistically significant preference for a kick orientation nor for any of the three initial mass function (IMF) slopes tested, and that populations including binary stars reproduced the kick distribution better than single star only populations. However, recent analysis by Janka (2017), prompted us to revisit our basic assumptions and our new analysis has led to revised best-fit kick values of alpha=100 km per second and beta = -170 km per second. The reduction of beta to a negative value is due to using the 2D observed kick velocity distribution rather than the modelled 3D velocity distribution for neutron stars (NS). To further test the validity of the new kick, we have created synthetic populations of runaway star and double neutron star (DNS) binaries at solar metallicity (Z=0.02) using our best-fit kick. We find our new kick values create runaway star velocities and DNS period distributions in agreement with the comparable observational distributions with only the DNS eccentricities in tension with the observations. From our DNS and BH-BH datasets we estimate a predicted DNS merger rate at solar metallicity of 3,864 (+1,570/-2,371) per cubic Gpc per yr and a BH-BH merger rate of 5 (+40/-1) per cubic Gpc per yr., Comment: Accepted for publication in MNRAS

Published
2018
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17. Binary Population and Spectral Synthesis Version 2.1: construction, observational verification and new results

Author

Eldridge, J. J., Stanway, E. R., Xiao, L., McClelland, L. A. S., Taylor, G., Ng, M., Greis, S. M. L., and Bray, J. C.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The Binary Population and Spectral Synthesis (BPASS) suite of binary stellar evolution models and synthetic stellar populations provides a framework for the physically motivated analysis of both the integrated light from distant stellar populations and the detailed properties of those nearby. We present a new version 2.1 data release of these models, detailing the methodology by which BPASS incorporates binary mass transfer and its effect on stellar evolution pathways, as well as the construction of simple stellar populations. We demonstrate key tests of the latest BPASS model suite demonstrating its ability to reproduce the colours and derived properties of resolved stellar populations, including well- constrained eclipsing binaries. We consider observational constraints on the ratio of massive star types and the distribution of stellar remnant masses. We describe the identification of supernova progenitors in our models, and demonstrate a good agreement to the properties of observed progenitors. We also test our models against photometric and spectroscopic observations of unresolved stellar populations, both in the local and distant Universe, finding that binary models provide a self-consistent explanation for observed galaxy properties across a broad redshift range. Finally, we carefully describe the limitations of our models, and areas where we expect to see significant improvement in future versions., Comment: 69 pages, 45 figures. Accepted for publication in PASA. Accompanied by a full, documented data release at http://bpass.auckland.ac.nz and http://warwick.ac.uk/bpass

Published
2017
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18. LOFAR MSSS: Discovery of a 2.56 Mpc giant radio galaxy associated with a disturbed galaxy group

Author

Clarke, A. O., Heald, G., Jarrett, T., Bray, J. D., Hardcastle, M. J., Cantwell, T. M., Scaife, A. M. M., Brienza, M., Bonafede, A., Breton, R. P., Broderick, J. W., Carbone, D., Croston, J. H., Farnes, J. S., Harwood, J. J., Heesen, V., Horneffer, A., van der Horst, A. J., Iacobelli, M., Jurusik, W., Kokotanekov, G., McKean, J. P., Morabito, L. K., Mulcahy, D. D., Nikiel-Wroczynski, B. S., Orru, E., Paladino, R., Pandey-Pommier, M., Pietka, M., Pizzo, R., Pratley, L., Riseley, C. J., Rottgering, H. J. A., Rowlinson, A., Sabater, J., Sendlinger, K., Shulevski, A., Sridhar, S. S., Stewart, A. J., Tasse, C., van Velzen, S., van Weeren, R. J., and Wise, M. W.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report on the discovery in the LOFAR Multifrequency Snapshot Sky Survey (MSSS) of a giant radio galaxy (GRG) with a projected size of $2.56 \pm 0.07$ Mpc projected on the sky. It is associated with the galaxy triplet UGC 9555, within which one is identified as a broad-line galaxy in the Sloan Digital Sky Survey (SDSS) at a redshift of $0.05453 \pm 1 \times 10^{-5} $, and with a velocity dispersion of $215.86 \pm 6.34$ km/s. From archival radio observations we see that this galaxy hosts a compact flat-spectrum radio source, and we conclude that it is the active galactic nucleus (AGN) responsible for generating the radio lobes. The radio luminosity distribution of the jets, and the broad-line classification of the host AGN, indicate this GRG is orientated well out of the plane of the sky, making its physical size one of the largest known for any GRG. Analysis of the infrared data suggests that the host is a lenticular type galaxy with a large stellar mass ($\log~\mathrm{M}/\mathrm{M}_\odot = 11.56 \pm 0.12$), and a moderate star formation rate ($1.2 \pm 0.3~\mathrm{M}_\odot/\mathrm{year}$). Spatially smoothing the SDSS images shows the system around UGC 9555 to be significantly disturbed, with a prominent extension to the south-east. Overall, the evidence suggests this host galaxy has undergone one or more recent moderate merger events and is also experiencing tidal interactions with surrounding galaxies, which have caused the star formation and provided the supply of gas to trigger and fuel the Mpc-scale radio lobes., Comment: Compressed for arXiv, see journal for full resolution images

Published
2017
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19. The EXPLAIN (Hyperpolarised Xenon Magnetic Resonance Pulmonary Imaging in Patients With Long-COVID) Study: The Primary Outcome

Author

Ng, K.L., primary, Saunders, L.C., additional, Collier, G., additional, Grist, J., additional, Strickland, S., additional, Gustafsson, L., additional, Smith, L.J., additional, Hughes, P.J.C., additional, Kainth, N., additional, Evans, R.I., additional, Laws, A., additional, Renju Thomas, S., additional, Rodgers, J.L., additional, Jones, S.A., additional, Newman, T.L., additional, Plowright, M.L., additional, Dryhurst-Pearce, L., additional, Jacob, K., additional, McIntyre, A., additional, Capener, D., additional, Bray, J., additional, Durrant, M., additional, Yeung, K., additional, Walters, H., additional, Matthews, V., additional, Watson, L., additional, Elbehairy, A., additional, Vuddamalay, G., additional, Abu Eid, G., additional, Viktorie, M.S., additional, Cox, M., additional, Harris, V., additional, Lachut, M., additional, Mulvey, N., additional, Hickes, W., additional, Rahman, N., additional, Horsley, A., additional, Davies, H.E., additional, Thompson, R.A.A., additional, Wild, J.M., additional, Gleeson, F.V., additional, and Fraser, E., additional

Published
2024
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20. Prospects for detecting ultra-high-energy particles with FAST

Author

James, C. W., Bray, J. D., and Ekers, R. D.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The origin of the highest-energy particles in nature, the ultra-high-energy (UHE) cosmic rays, is still unknown. In order to resolve this mystery, very large detectors are required to probe the low flux of these particles - or to detect the as-yet unobserved flux of UHE neutrinos predicted from their interactions. The `lunar Askaryan technique' is a method to do both. When energetic particles interact in a dense medium, the Askaryan effect produces intense coherent pulses of radiation in the MHz--GHz range. By using radio telescopes to observe the Moon and look for nanosecond pulses, the entire visible lunar surface ($20$ million km$^2$) can be used as an UHE particle detector. A large effective area over a broad bandwidth is the primary telescope requirement for lunar observations, which makes large single-aperture instruments such as the Five-Hundred-Meter Aperture Spherical Radio Telescope (FAST) well-suited to the technique. In this contribution, we describe the lunar Askaryan technique and its unique observational requirements. Estimates of the sensitivity of FAST to both the UHE cosmic ray and neutrino flux are given, and we describe the methods by which lunar observations with FAST, particularly if equipped with a broadband phased-array feed, could detect the flux of UHE cosmic rays., Comment: 15 pages, 10 figures. To be published in a special issue on FAST in RAA

Published
2016

21. Minimal prospects for radio detection of extensive air showers in the atmosphere of Jupiter

Author

Bray, J. D. and Nelles, A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

One possible approach for detecting ultra-high-energy cosmic rays and neutrinos is to search for radio emission from extensive air showers created when they interact in the atmosphere of Jupiter, effectively utilizing Jupiter as a particle detector. We investigate the potential of this approach. For searches with current or planned radio telescopes we find that the effective area for detection of cosmic rays is substantial (~3*10^7 km^2), but the acceptance angle is so small that the typical geometric aperture (~10^3 km^2 sr) is less than that of existing terrestrial detectors, and cosmic rays also cannot be detected below an extremely high threshold energy (~10^23 eV). The geometric aperture for neutrinos is slightly larger, and greater sensitivity can be achieved with a radio detector on a Jupiter-orbiting satellite, but in neither case is this sufficient to constitute a practical detection technique. Exploitation of the large surface area of Jupiter for detecting ultra-high-energy particles remains a long-term prospect that will require a different technique, such as orbital fluorescence detection., Comment: 15 pages, 15 figures, 2 tables, accepted for publication in ApJ

Published
2016
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22. Neutron Star Kicks and their Relationship to Supernovae Ejecta Mass

Author

Bray, J. C. and Eldridge, J. J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We propose a simple model to explain the velocity of young neutron stars. We attempt to confirm a relationship between the amount of mass ejected in the formation of the neutron star and the `kick' velocity imparted to the compact remnant resulting from the process. We assume the velocity is given by $v_{\rm kick}=\alpha\,(M_{\rm ejecta} / M_{\rm remnant}) + \beta\,$. To test this simple relationship we use the BPASS (Binary Population and Spectral Synthesis) code to create stellar population models from both single and binary star evolutionary pathways. We then use our Remnant Ejecta and Progenitor Explosion Relationship (REAPER) code to apply different $\alpha$ and $\beta$ values and three different `kick' orientations then record the resulting velocity probability distributions. We find that while a single star population provides a poor fit to the observational data, the binary population provides an excellent fit. Values of $\alpha=70\, {\rm km\,s^{-1}}$ and $\beta=110\,{\rm km\,s^{-1}}$ reproduce the \cite{RN165} observed 2-dimensional velocities and $\alpha=70\, {\rm km\,s^{-1}}$ and $\beta=120\,{\rm km\,s^{-1}}$ reproduce their inferred 3-dimensional velocity distribution for nearby single neutron stars with ages less than 3 Myrs. After testing isotropic, spin-axis aligned and orthogonal to spin-axis `kick' orientations, we find no statistical preference for a `kick' orientation. While ejecta mass cannot be the only factor that determines the velocity of supernovae compact remnants, we suggest it is a significant contributor and that the ejecta based `kick' should replace the Maxwell-Boltzmann velocity distribution currently used in many population synthesis codes., Comment: 15 pages, 9 figures, 2 tables. Accepted for publication in MNRAS. Neutron Star Kicks and their Relationship to Supernovae Ejecta Mass J. C. Bray; J. J. Eldridge Monthly Notices of the Royal Astronomical Society 2016

Published
2016
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25. The lunar Askaryan technique: a technical roadmap

Author

Bray, J. D., Alvarez-Muniz, J., Buitink, S., Dagkesamanskii, R. D., Ekers, R. D., Falcke, H., Gayley, K. G., Huege, T., James, C. W., Mevius, M., Mutel, R. L., Protheroe, R. J., Scholten, O., Spencer, R. E., and ter Veen, S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The lunar Askaryan technique, which involves searching for Askaryan radio pulses from particle cascades in the outer layers of the Moon, is a method for using the lunar surface as an extremely large detector of ultra-high-energy particles. The high time resolution required to detect these pulses, which have a duration of around a nanosecond, puts this technique in a regime quite different from other forms of radio astronomy, with a unique set of associated technical challenges which have been addressed in a series of experiments by various groups. Implementing the methods and techniques developed by these groups for detecting lunar Askaryan pulses will be important for a future experiment with the Square Kilometre Array (SKA), which is expected to have sufficient sensitivity to allow the first positive detection using this technique. Key issues include correction for ionospheric dispersion, beamforming, efficient triggering, and the exclusion of spurious events from radio-frequency interference. We review the progress in each of these areas, and consider the further progress expected for future application with the SKA., Comment: Proceedings of the 34th International Cosmic Ray Conference (ICRC 2015), The Hague, The Netherlands

Published
2015

26. The LOFAR Multifrequency Snapshot Sky Survey (MSSS) I. Survey description and first results

Author

Heald, G. H., Pizzo, R. F., Orrú, E., Breton, R. P., Carbone, D., Ferrari, C., Hardcastle, M. J., Jurusik, W., Macario, G., Mulcahy, D., Rafferty, D., Asgekar, A., Brentjens, M., Fallows, R. A., Frieswijk, W., Toribio, M. C., Adebahr, B., Arts, M., Bell, M. R., Bonafede, A., Bray, J., Broderick, J., Cantwell, T., Carroll, P., Cendes, Y., Clarke, A. O., Croston, J., Daiboo, S., de Gasperin, F., Gregson, J., Harwood, J., Hassall, T., Heesen, V., Horneffer, A., van der Horst, A. J., Iacobelli, M., Jelić, V., Jones, D., Kant, D., Kokotanekov, G., Martin, P., McKean, J. P., Morabito, L. K., Nikiel-Wroczyński, B., Offringa, A., Pandey, V. N., Pandey-Pommier, M., Pietka, M., Pratley, L., Riseley, C., Rowlinson, A., Sabater, J., Scaife, A. M. M., Scheers, L. H. A., Sendlinger, K., Shulevski, A., Sipior, M., Sobey, C., Stewart, A. J., Stroe, A., Swinbank, J., Tasse, C., Trüstedt, J., Varenius, E., van Velzen, S., Vilchez, N., van Weeren, R. J., Wijnholds, S., Williams, W. L., de Bruyn, A. G., Nijboer, R., Wise, M., Alexov, A., Anderson, J., Avruch, I. M., Beck, R., Bell, M. E., van Bemmel, I., Bentum, M. J., Bernardi, G., Best, P., Breitling, F., Brouw, W. N., Brüggen, M., Butcher, H. R., Ciardi, B., Conway, J. E., de Geus, E., de Jong, A., de Vos, M., Deller, A., Dettmar, R. J., Duscha, S., Eislöffel, J., Engels, D., Falcke, H., Fender, R., Garrett, M. A., Grießmeier, J., Gunst, A. W., Hamaker, J. P., Hessels, J. W. T., Hoeft, M., Hörandel, J., Holties, H. A., Intema, H., Jackson, N. J., Jütte, E., Karastergiou, A., Klijn, W. F. A., Kondratiev, V. I., Koopmans, L. V. E., Kuniyoshi, M., Kuper, G., Law, C., van Leeuwen, J., Loose, M., Maat, P., Markoff, S., McFadden, R., McKay-Bukowski, D., Mevius, M., Miller-Jones, J. C. A., Morganti, R., Munk, H., Nelles, A., Noordam, J. E., Norden, M. J., Paas, H., Polatidis, A. G., Reich, W., Renting, A., Röttgering, H., Schoenmakers, A., Schwarz, D., Sluman, J., Smirnov, O., Stappers, B. W., Steinmetz, M., Tagger, M., Tang, Y., ter Veen, S., Thoudam, S., Vermeulen, R., Vocks, C., Vogt, C., Wijers, R. A. M. J., Wucknitz, O., Yatawatta, S., and Zarka, P.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present the Multifrequency Snapshot Sky Survey (MSSS), the first northern-sky LOFAR imaging survey. In this introductory paper, we first describe in detail the motivation and design of the survey. Compared to previous radio surveys, MSSS is exceptional due to its intrinsic multifrequency nature providing information about the spectral properties of the detected sources over more than two octaves (from 30 to 160 MHz). The broadband frequency coverage, together with the fast survey speed generated by LOFAR's multibeaming capabilities, make MSSS the first survey of the sort anticipated to be carried out with the forthcoming Square Kilometre Array (SKA). Two of the sixteen frequency bands included in the survey were chosen to exactly overlap the frequency coverage of large-area Very Large Array (VLA) and Giant Metrewave Radio Telescope (GMRT) surveys at 74 MHz and 151 MHz respectively. The survey performance is illustrated within the "MSSS Verification Field" (MVF), a region of 100 square degrees centered at J2000 (RA,Dec)=(15h,69deg). The MSSS results from the MVF are compared with previous radio survey catalogs. We assess the flux and astrometric uncertainties in the catalog, as well as the completeness and reliability considering our source finding strategy. We determine the 90% completeness levels within the MVF to be 100 mJy at 135 MHz with 108" resolution, and 550 mJy at 50 MHz with 166" resolution. Images and catalogs for the full survey, expected to contain 150,000-200,000 sources, will be released to a public web server. We outline the plans for the ongoing production of the final survey products, and the ultimate public release of images and source catalogs., Comment: 23 pages, 19 figures. Accepted for publication in Astronomy & Astrophysics. MSSS Verification Field images and catalog data may be downloaded from http://vo.astron.nl

Published
2015
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27. High-precision measurements of extensive air showers with the SKA

Author

Huege, T., Bray, J. D., Buitink, S., Dallier, R., Ekers, R. D., Falcke, H., Haungs, A., James, C. W., Martin, L., Revenu, B., Scholten, O., Schröder, F. G., and Zilles, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract

As of 2023, the Square Kilometre Array will constitute the world's largest radio telescope, offering unprecedented capabilities for a diverse science programme in radio astronomy. At the same time, the SKA will be ideally suited to detect extensive air showers initiated by cosmic rays in the Earth's atmosphere via their radio emission. With its very dense and uniform antenna spacing in a fiducial area of one km$^2$ and its large bandwidth of 50-350 MHz, the low-frequency part of the SKA will provide very precise measurements of individual cosmic ray air showers. These precision measurements will allow detailed studies of the mass composition of cosmic rays in the energy region of transition from a Galactic to an extragalactic origin. Also, the SKA will facilitate three-dimensional "tomography" of the electromagnetic cascades of air showers, allowing the study of particle interactions at energies beyond the reach of the LHC. Finally, studies of possible connections between air showers and lightning initiation can be taken to a new level with the SKA. We discuss the science potential of air shower detection with the SKA and report on the technical requirements and project status., Comment: Proceedings of the 34th ICRC, The Hague, The Netherlands, PoS(ICRC2015)309

Published
2015

28. A limit on the ultra-high-energy neutrino flux from lunar observations with the Parkes radio telescope

Author

Bray, J. D., Ekers, R. D., Roberts, P., Reynolds, J. E., James, C. W., Phillips, C. J., Protheroe, R. J., McFadden, R. A., and Aartsen, M. G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report a limit on the ultra-high-energy neutrino flux based on a non-detection of radio pulses from neutrino-initiated particle cascades in the Moon, in observations with the Parkes radio telescope undertaken as part of the LUNASKA project. Due to the improved sensitivity of these observations, which had an effective duration of 127 hours and a frequency range of 1.2-1.5 GHz, this limit extends to lower neutrino energies than those from previous lunar radio experiments, with a detection threshold below 10^20 eV. The calculation of our limit allows for the possibility of lunar-origin pulses being misidentified as local radio interference, and includes the effect of small-scale lunar surface roughness. The targeting strategy of the observations also allows us to place a directional limit on the neutrino flux from the nearby radio galaxy Centaurus A., Comment: Accepted by Physical Review D; 11 pages, 8 figures, 1 table

Published
2015
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29. A lunar radio experiment with the Parkes radio telescope for the LUNASKA project

Author

Bray, J. D., Ekers, R. D., Roberts, P., Reynolds, J. E., James, C. W., Phillips, C. J., Protheroe, R. J., McFadden, R. A., and Aartsen, M. G.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We describe an experiment using the Parkes radio telescope in the 1.2-1.5 GHz frequency range as part of the LUNASKA project, to search for nanosecond-scale pulses from particle cascades in the Moon, which may be triggered by ultra-high-energy astroparticles. Through the combination of a highly sensitive multi-beam radio receiver, a purpose-built backend and sophisticated signal-processing techniques, we achieve sensitivity to radio pulses with a threshold electric field strength of 0.0053 $\mu$V/m/MHz, lower than previous experiments by a factor of three. We observe no pulses in excess of this threshold in observations with an effective duration of 127 hours. The techniques we employ, including compensating for the phase, dispersion and spectrum of the expected pulse, are relevant for future lunar radio experiments., Comment: Accepted by Astroparticle Physics; 23 pages, 17 figures, 3 tables

Published
2014
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30. Can the masses of isolated planetary-mass gravitational lenses be measured by terrestrial parallax?

Author

Freeman, M., Philpott, L. C., Abe, F., Albrow, M. D., Bennett, D. P., Bond, I. A., Botzler, C. S., Bray, J. C., Cherrie, J. M., Christie, G. W., Dionnet, Z., Gould, A., Han, C., Heyrovsky, D., McCormick, J. M., Moorhouse, D. M., Muraki, Y., Natusch, T., Rattenbury, N. J., Skowron, J., Sumi, T., Suzuki, D., Tan, T. -G., Tristram, P. J., and Yock, P. C. M.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Recently Sumi et al. (2011) reported evidence for a large population of planetary-mass objects (PMOs) that are either unbound or orbit host stars in orbits > 10 AU. Their result was deduced from the statistical distribution of durations of gravitational microlensing events observed by the MOA collaboration during 2006 and 2007. Here we study the feasibility of measuring the mass of an individual PMO through microlensing by examining a particular event, MOA-2011-BLG-274. This event was unusual as the duration was short, the magnification high, the source-size effect large and the angular Einstein radius small. Also, it was intensively monitored from widely separated locations under clear skies at low air masses. Choi et al. (2012) concluded that the lens of the event may have been a PMO but they did not attempt a measurement of its mass. We report here a re-analysis of the event using re-reduced data. We confirm the results of Choi et al. and attempt a measurement of the mass and distance of the lens using the terrestrial parallax effect. Evidence for terrestrial parallax is found at a 3 sigma level of confidence. The best fit to the data yields the mass and distance of the lens as 0.80 +/- 0.30 M_J and 0.80 +/- 0.25 kpc respectively. We exclude a host star to the lens out to a separation ~ 40 AU. Drawing on our analysis of MOA-2011-BLG-274 we propose observational strategies for future microlensing surveys to yield sharper results on PMOs including those down to super-Earth mass., Comment: 44 pages, 12 figures, to appear in ApJ

Published
2014
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31. First indirect drive inertial confinement fusion campaign at Laser Megajoule

Author

Liberatore, S., primary, Gauthier, P., additional, Willien, J. L., additional, Masson-Laborde, P. E., additional, Philippe, F., additional, Poujade, O., additional, Alozy, E., additional, Botrel, R., additional, Boutoux, G., additional, Bray, J., additional, Caillaud, T., additional, Chicanne, C., additional, Chollet, C., additional, Debayle, A., additional, Depierreux, S., additional, Duchastenier, W., additional, Ferri, M., additional, Henry, O., additional, Hoch, P., additional, Laffite, S., additional, Landoas, O., additional, Le-Deroff, L., additional, Lefebvre, E., additional, Legay, G., additional, Marmajou, I., additional, Meyer, C., additional, Molina, K., additional, Morice, O., additional, Peche, E., additional, Prunet, P., additional, Riquier, R., additional, Rosch, R., additional, Tassin, V., additional, Vaisseau, X., additional, and Villette, B., additional

Published
2023
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32. P177 129Xe MRI phenotyping and longitudinal change in patients with asthma and/or COPD and normal pulmonary function tests

Author

Marshall, H, primary, Smith, LJ, additional, Biancardi, A, additional, Collier, GJ, additional, Chan, HF, additional, Capener, D, additional, Bray, J, additional, Jakymelen, D, additional, Saunders, L, additional, Astley, J, additional, Tahir, BA, additional, Munro, R, additional, Rodgers, O, additional, Ball, J, additional, Hughes, PJC, additional, Rajaram, S, additional, Swift, AJ, additional, Stewart, NJ, additional, Norquay, G, additional, Brook, ML, additional, Armstrong, L, additional, Hardaker, L, additional, Hughes, R, additional, and Wild, JM, additional

Published
2023
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34. P176 Bronchodilator response discordance in patients with asthma and/or COPD assessed by 129Xe-MRI and spirometry

Author

Smith, LJ, primary, Marshall, H, additional, Biancardi, A, additional, Collier, GJ, additional, Chan, HF, additional, Capener, D, additional, Bray, J, additional, Jakymelen, D, additional, Saunders, L, additional, Astley, J, additional, Tahir, BA, additional, Munro, R, additional, Rodgers, O, additional, Ball, J, additional, Hughes, PJC, additional, Rajaram, S, additional, Swift, AJ, additional, Stewart, NJ, additional, Norquay, G, additional, Brook, ML, additional, Armstrong, L, additional, Hardaker, L, additional, Hughes, R, additional, and Wild, JM, additional

Published
2023
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36. Comparison of algorithms for determination of rotation measure and Faraday structure I. 1100 - 1400 MHz

Author

Sun, X. H., Rudnick, L., Akahori, Takuya, Anderson, C. S., Bell, M. R., Bray, J. D., Farnes, J. S., Ideguchi, S., Kumazaki, K., O'Brien, T., O'Sullivan, S. P., Scaife, A. M. M., Stepanov, R., Stil, J., Takahashi, K., van Weeren, R. J., and Wolleben, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(abridged) We run a Faraday structure determination data challenge to benchmark the currently available algorithms including Faraday synthesis (previously called RM synthesis in the literature), wavelet, compressive sampling and $QU$-fitting. The frequency set is similar to POSSUM/GALFACTS with a 300 MHz bandwidth from 1.1 to 1.4 GHz. We define three figures of merit motivated by the underlying science: a) an average RM weighted by polarized intensity, RMwtd, b) the separation $\Delta\phi$ of two Faraday components and c) the reduced chi-squared. Based on the current test data of signal to noise ratio of about 32, we find that: (1) When only one Faraday thin component is present, most methods perform as expected, with occasional failures where two components are incorrectly found; (2) For two Faraday thin components, QU-fitting routines perform the best, with errors close to the theoretical ones for RMwtd, but with significantly higher errors for $\Delta\phi$. All other methods including standard Faraday synthesis frequently identify only one component when $\Delta\phi$ is below or near the width of the Faraday point spread function; (3) No methods, as currently implemented, work well for Faraday thick components due to the narrow bandwidth; (4) There exist combinations of two Faraday components which produce a large range of acceptable fits and hence large uncertainties in the derived single RMs; in these cases, different RMs lead to the same Q, U behavior, so no method can recover a unique input model., Comment: 15 pages, 8 figures, 5 tables, accepted by AJ. Some figures have been degraded, for a full resolution version, see http://physics.usyd.edu.au/~xhsun/datachallengeI.pdf

Published
2014
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37. Lunar detection of ultra-high-energy cosmic rays and neutrinos with the Square Kilometre Array

Author

Bray, J. D., Alvarez-Muñiz, J., Buitink, S., Dagkesamanskii, R. D., Ekers, R. D., Falcke, H., Gayley, K. G., Huege, T., James, C. W., Mevius, M., Mutel, R. L., Protheroe, R. J., Scholten, O., Spencer, R. E., and ter Veen, S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The origin of the most energetic particles in nature, the ultra-high-energy (UHE) cosmic rays, is still a mystery. Only the most energetic of these have sufficiently small angular deflections to be used for directional studies, and their flux is so low that even the 3,000 km^2 Pierre Auger detector registers only about 30 cosmic rays per year of these energies. A method to provide an even larger aperture is to use the lunar Askaryan technique, in which ground-based radio telescopes search for the nanosecond radio flashes produced when a cosmic ray interacts with the Moon's surface. The technique is also sensitive to UHE neutrinos, which may be produced in the decays of topological defects from the early universe. Observations with existing radio telescopes have shown that this technique is technically feasible, and established the required procedure: the radio signal should be searched for pulses in real time, compensating for ionospheric dispersion and filtering out local radio interference, and candidate events stored for later analysis. For the Square Kilometre Array (SKA), this requires the formation of multiple tied-array beams, with high time resolution, covering the Moon, with either SKA1-LOW or SKA1-MID. With its large collecting area and broad bandwidth, the SKA will be able to detect the known flux of UHE cosmic rays using the visible lunar surface - millions of square km - as the detector, providing sufficient detections of these extremely rare particles to address the mystery of their origin., Comment: Contribution to the conference on "Advancing Astrophysics with the Square Kilometre Array" for the SKA science book; revised, accepted version

Published
2014

38. Precision measurements of cosmic ray air showers with the SKA

Author

Huege, T., Bray, J. D., Buitink, S., Dallier, R., Ekers, R. D., Falcke, H., James, C. W., Martin, L., Revenu, B., Scholten, O., and Schröder, F. G.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Supplemented with suitable buffering techniques, the low-frequency part of the SKA can be used as an ultra-precise detector for cosmic-ray air showers at very high energies. This would enable a wealth of scientific applications: the physics of the transition from Galactic to extragalactic cosmic rays could be probed with very high precision mass measurements, hadronic interactions could be studied up to energies well beyond the reach of man-made particle accelerators, air shower tomography could be performed with very high spatial resolution exploiting the large instantaneous bandwidth and very uniform instantaneous $u$-$v$ coverage of SKA1-LOW, and the physics of thunderstorms and possible connections between cosmic rays and lightning initiation could be studied in unprecedented levels of detail. In this article, we describe the potential of the SKA as an air shower radio detector from the perspective of existing radio detection efforts and discuss the associated technical requirements., Comment: Contribution to the conference "Advancing Astrophysics with the Square Kilometre Array", June 8-13, 2014, Giardini Naxos, Italy; Proceedings of Science, PoS(AASKA14)148; final accepted version (minor changes wrt. v1)

Published
2014

40. Safety and efficacy of intraperitoneal drain placement after emergency colorectal surgery: An international, prospective cohort study

Author

Sgro, A, Blanco-Colino, R, Ahmed, W, Brindl, N, Gujjuri, R, Lapolla, P, Mills, E, Perez-Ajates, S, Soares, A, Varghese, C, Xu, W, Mclean, K, Chapman, S, Espin-Basany, E, Glasbey, J, Mihaljevic, A, Nepogodiev, D, Pata, F, Pellino, G, Pockney, P, Dudi-Venkata, N, Egoroff, N, Ludbrook, I, Raubenheimer, K, Richards, T, Delibegovic, S, Salibasic, M, Amjad, T, Dorr-Harim, C, Gedeon, N, Gsenger, J, Tachezy, M, Bini, S, Gallo, G, Gori, A, Picciariello, A, Podda, M, Riboni, C, Machatschek, M, Nguyen, A, Jakubauskas, M, Kryzauskas, M, Poskus, T, Kuiper, S, Wang, J, Wells, C, Bissett, I, Augestad, K, Steinholt, I, Vieira, B, Juloski, J, Anabitarte Bautista, O, Kasmy El Kasmy, Y, Martin-Borregon, P, Ossola Revilla, M, Van Straten, S, Aktas, M, Baki, B, Akhbari, M, Baker, D, Bhatia, S, Brown, S, Cambridge, W, Kamarajah, S, Khaw, R, Kouli, O, Murray, V, Trout, I, Yasin, I, Wong, J, Reyhani, H, Wong, K, Pancharatnam, R, Chia, W, Walmsley, A, Hassane, A, Saeed, D, Wang, B, Walters, B, Nowinka, Z, Alsaif, A, Mirza, M, Foster, K, Luu, J, Kakodkar, P, Hughes, J, Yogarajah, T, Antypas, A, Rahman, A, Bradbury, M, Mclarnon, M, Nagi, S, Riad, A, Erotocritou, M, Kyriacou, H, Kaminskaite, V, Alfadhel, S, Fatimah Hussain, Q, Handa, A, Massy-Westropp, C, Custovic, S, Dimov, R, Mughal, H, Slavchev, M, Ivanov, T, Gouvas, N, Hegazi, A, Kocian, P, Kjaer, M, Mark-Christensen, A, Papakonstantinou, D, Machairas, N, Triantafyllou, T, Garoufalia, Z, Korkolis, D, Castaldi, A, Giaccari, S, Spolverato, G, Pagano, G, Milone, M, Turri, G, Colombo, F, Cucinotta, E, Poillucci, G, Perra, T, Tutino, R, Belia, F, Coletta, D, Belli, A, Rega, D, Cianci, P, Pirozzolo, G, Di Lena, M, Perrone, F, Giani, A, Lovisetto, F, Grassia, M, Pipitone Federico, N, Ferrara, F, Biancafarina, A, Tamini, N, Sinibaldi, G, Tuminello, F, Galleano, R, Sasia, D, Bragaglia, L, de Manzoni Garberini, A, Pesce, A, Cassaro, F, Venturelli, P, Canu, G, Esposito, G, Campanelli, M, Cardia, R, Ricciardiello, M, Sagnotta, A, Canonico, G, De Marco, G, Cappiello, A, Pinotti, E, Carlei, F, Lisi, G, Bagaglini, G, Farrugia, M, Meima - van Praag, E, Monteiro, C, Pereira, M, Botelho, P, Quigley, A, O'Neill, A, Gaule, L, Crone, L, Arnold, A, Grama, F, Beuca, A, Tulina, I, Litvin, A, Panyko, A, Ossola, M, Trujillo Diaz, J, Marin Santos, J, Alonso Batanero, E, Gortazar de las Casas, S, Soldevila Verdeguer, C, Colas-Ruiz, E, Talal El-Abur, I, Garcia Dominguez, M, Delorme, M, Sauvain, M, Ozmen, B, Ozkan, B, Calikoglu, F, Kural, S, Zafer, F, Kaya, Y, Yalcinkaya, A, Kargici, K, Tepe, M, Tatar, O, Kabadayi, E, Yildirim, A, Hurmuzlu, D, Korkmaz, K, Sharma, P, Troller, R, Hagan, N, Mooney, J, Light, A, Tansey, M, Bhojwani, D, Mcging, R, Mallon, A, Fadel, M, Spilsbury, C, James, R, O'Brien, S, Isaac, A, Balasubramanya, S, Sadik, H, Gala, T, Chen, J, Turner, B, Goh, E, Hassan, K, Karam, M, Mason, P, Tzoumas, N, Noton, T, Seehra, J, Ahmed, N, Motiwale, R, Tanna, V, Argyriou, A, Bylapudi, S, Grace, N, Latif, S, Hounat, A, Kiam, J, Zaidi, M, Elsamani, K, Hughes, C, Suresh, A, Sinan, L, El-Dalil, D, Khoo, E, Salim, E, Stark, D, Minhas, N, Fowler, G, Rees, E, Giudiceandrea, I, Bardon, A, Jayawardena, P, Dieseru, N, Murphy, A, Yates, C, Ziolkowska, K, Rafie, A, Khoda, F, Okocha, M, Ashdown, T, Vitish-Sharma, P, Gilliland, J, Toh, S, Jones, K, Devine, A, Berry, A, Mcdonnell, S, Olivier, J, Richardson, G, Lim, H, Slim, N, Elsayeh, K, Sammour, T, Sarpanov, A, Belev, N, Dimitrov, D, Dusek, T, Ntomi, V, Sotiropoulos, G, Theodorou, D, Nikiteas, N, Balalis, D, Antropoli, C, Altomare, D, Luglio, G, De Palma, G, Pedrazzani, C, Simonelli, L, Brozzetti, S, Porcu, A, Massani, M, Grazi, G, Izzo, F, Delrio, P, Restini, E, Chetta, G, Lantone, G, Ferrari, G, Lucchi, A, De Prizio, M, Caristo, G, Borghi, F, Petrucciani, N, Huscher, C, Cocorullo, G, Tonini, V, Medas, F, Sica, G, Cillara, N, Anastasi, A, Bianco, F, Giuliani, A, Carlini, M, Selvaggi, F, Sammarco, G, Ozolins, A, Malasonoks, A, Andrejevic, P, Tanis, P, van de Ven, A, Gerhards, M, Ribeiro da Silva, B, Silva, A, Lima, M, Kavanagh, D, Mccawley, N, Bintintan, V, Karamarkovic, A, Sanz Ortega, G, De Andres-Asenjo, B, Nevado Garcia, C, Garcia Florez, L, Segura-Sampedro, J, Blas Laina, J, Ponchietti, L, Buchwald, P, Gialamas, E, Ozben, V, Rencuzogullari, A, Gecim, I, Altinel, Y, Isik, O, Yoldas, T, Isik, A, Leventoglu, S, Erturk, M, Guner, A, Guler, S, Attaallah, W, Ugur, M, Ozbalci, G, Marzook, H, Eardley, N, Smolarek, S, Morgan, R, Roxburgh, C, Lala, A, Salama, Y, Singh, B, Khanna, A, Evans, M, Shaikh, I, Maradi Thippeswamy, K, Appleton, B, Moug, S, Smith, I, Smart, N, Shah, P, Williams, G, Khera, G, Goede, A, Varcada, M, Parmar, C, Duff, S, Hargest, R, Marriott, P, Speake, D, Ben Sassi, A, Furfaro, B, Daudu, D, Golijanin, N, Yek, W, Capasso, G, Mansour, L, Niu, N, Seow, W, Hamidovic, A, Kulovic, E, Letic, E, Aljic, A, Helez, M, Banji-Kelan, A, Dimitrova, N, Kavradjieva, P, Ivanov, V, Jukaku, A, Hadzhiev, D, Gabarski, A, Karamanliev, M, Vladova, P, Iliev, S, Yotsov, T, Epsilonupsilonsigmataualphathetaiotaomicronupsilon, E, Vetsa, K, Stavrinidou, O, Papatheodorou, P, Liassides, T, Georgiou, T, Al Nassrallah, M, Altaf, R, Negametzyanov, M, Zagibova, D, Foltys, F, Stefanova, H, Paspala, A, Bompetsi, G, Sidiropoulos, T, Stamopoulos, P, Triantafyllou, A, Theodoropoulos, C, Kimpizi, A, Palyvou, T, Charalabopoulos, A, Syllaios, A, Schizas, D, Liatsou, E, Baili, E, Vagios, I, Tomara, N, Davakis, S, Palumbo, A, Foroni, F, Dibra, R, Papagni, V, Urbani, A, Rossin, E, Nezi, G, Romano, P, Amendola, A, Esposito, E, Manigrasso, M, Anoldo, P, Vertaldi, S, Gecchele, G, Sabrina, Z, Guerci, C, Cammarata, F, Lamperti, G, Zaffaroni, G, Benuzzi, L, Ferrario, L, Cigognini, M, Mazzeo, C, Badessi, G, Pintabona, G, Fassari, A, Mingoli, A, Cirillo, B, D'Alterio, C, Brachini, G, Tancredi, M, Zambon, M, Aulicino, M, Sapienza, P, Liberatore, P, Scanu, A, Feo, C, Iacomino, A, Pelizzo, P, Rossi, S, Vigna, S, Grossi, U, Grillo, V, Agnes, A, Schena, C, Marincola, G, Oddi, A, Perotti, B, Mario, V, Perri, P, Zazza, S, Aversano, A, Scala, D, Di Lauro, K, Leongito, M, Piccirillo, M, Patrone, R, Capuzzolo, S, Vignotto, C, Bao, Q, Giuseppe, C, Angarano, E, Marino, F, Pezzolla, F, Gigante, G, Magistro, C, Crippa, J, Maspero, M, Carnevali, P, Trapani, R, Zonta, S, Agostinelli, L, Vittori, L, Romeo, L, Doria, E, Farnesi, F, Danna, R, Andolfi, E, Pellicano', G, Angelini, M, Scricciolo, M, Zanframundo, C, Ciulli, C, Ripamonti, L, Cigagna, L, Oldani, M, Larcinese, A, Rossi, D, Picone, E, Crescentini, G, Marano, A, Migliore, M, Giuffrida, M, Palagi, S, Testa, V, Borrello, A, Lucarini, A, Garofalo, E, Canali, G, Orlandi, P, Nervegna, F, Marchegiani, F, Damoli, I, Licata, A, Trovato, C, Alicata, F, Sardo, F, Milazzo, M, Randisi, B, Dominici, D, Sartarelli, L, Zanni, M, Pisanu, A, Soddu, C, Delogu, D, Erdas, E, Campus, F, Cappellacci, F, Casti, F, Marcialis, J, Atzeni, J, Sensi, B, Franceschilli, M, Bellato, V, Cannavera, A, Putzu, G, di Mola, F, Picardi, B, Solinas, L, Loponte, M, Rossi del Monte, S, Di Martino, C, Linari, C, Spagni, G, Capezzuoli, L, Tirloni, L, Nelli, T, Caridi, A, Elter, C, Camassa, M, D'Amico, S, Bargellini, T, Incollingo, P, Montuori, M, Maffione, F, Romano, L, Valiyeva, S, Spoletini, D, Menegon Tasselli, F, Sciaudone, G, Selvaggi, L, Menna, M, De Paola, G, Fulginiti, S, Truskovs, A, Weiss, C, Saknitis, G, Rauscher, J, Larnovskis, J, Jeyarajan-Davidsson, M, Nitisa, D, Gille, N, Reiser, S, Roshan, M, Leseman, C, van Dalen, A, Top, C, Detering, R, Matos, C, Silva, C, Pinto, D, Mendes, J, Couto, J, Leite, M, Velez, C, Damasio Cotovio, M, Cinza, A, Pedroso de Lima, R, Boyle, E, Yang, H, Banerjee, I, Rahmat, S, Afzal, Z, Reid, C, Dumitrascu, F, Croyle, J, Gressmann, K, Cullen, N, Graham, A, Nasehi, A, Montano King, C, Martin, B, Stokell, C, Sanderson, N, Farnan, R, Jassim, S, Chan, B, Chua Vi Long, K, Kaka, N, Pandey, S, Neo, W, Chitul, A, Bezede, C, Cincilei, D, David, A, Blaga, M, Blaga, S, Fagarasan, V, Khetagurova, M, Rodimov, S, 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S., Szal A., Khan A., O'Sullivan C., Baker E., Joseph-Gubral J., Hadley E., Trivedi R., Igwelaezoh E., Barton H., Allison W., Hurst W., Alam F., Parkes I., Jamshaid M., Azizan N., Burgher T., Afzal A., Eltilib I., Zahid M., Sadiq O., Lloyd A., Ho R., Brazukas A., Li C. H., Kamdar M., Mohamed Nazeer M. N., Mighiu A., Kim D., Wilkins L., Kuo L., Rafe T., Maduka D., Cheema H., Farag K., Abdellatif M., Nzewi R., Kruczynska A., Grasselli H., Yousuff M., Bassi R., Mann A. K., Chopra J., Shaikh M., D Sa S., Tsimplis V., Ghanchi A., Skene E., Asim K., Zaheer M., Chan S., Dalton H., Gibbons K., Adderley O., Chukwujindu I., Jayasuriya I., Sivanu K., Borumand M., Chick G., Bridges I., Tomlin J., McKenna J., Nandra N., Grieco C., Quek F. F., Mercer R., Brankin-Frisby T., Sattar A., Aslam A., Edelsten E., Shafi S., Kouli T., Ford V., Gurung F., Fernandes M., Deader N., Ponniah R., Jamieson S., Davies A., Taubwurcel J., Aung M. T., Desai R., Begum S., Jamadar T., Kangatharan A., Rzeszowski B., Ho C., Yap S. H. K., Prendergast M., Sethi R., Duku A., Lowe C., Bray J., Ghobrial M., Nichita V., Wagstaff A., Rengasamy E., Abu Hassan F., Mahmood H., Savill N., Shah S., Almeida T., Edwards A., Catchpole B., Halford Z., Carmichael A., Alsusa H., Boyd M., Williams J., Feyi-Waboso J., Patel M., Zeidan Z., Bailey E., Bapty J., Brazkiewicz M., Tremlett A., Pringle H., Mankal S., Chung W., Parry-Jones E., Anderson K., Mcforrester A., Stanley A., Hoather A., Wise H., Laid I., Scriven J., Braniste A., Wilson A., Le Blevec L., Pakunwanich N., Evans N., Chong H. L., White C., Hunter J., Haque M., Vanalia P., Murdoch S., Choudhary T., McCann A., Harun A., Shah H., Hunt S., Shafiq Y., Bickley-Morris E., Emms L., Dare M., Akula Y., Deliyannis E., Mayes F., Ellacott M., Zagorac Z., Farren A., Manning C., Hughed C., Stewart E. G., Lim K. H., Chohan N., Thaker A., Thompson B., Ahari D., Burdekin E., Okwu U., Akintunde A., Lhaf F., Douthwaite J., Govindan R., Leelamanthep S., Gull E., Wright F., Dundas L., Mackdermott N., Burchi-Khairy T., Campbell I., Walsh J., Yeo J. Y., Meehan S., Banerjee D., Fu M., Kawka M., Ali T., Hussain Z., Thomas C., Ahmad H., Moroney J., Yick C., Risquet R., Ntuiabane D., Shimato M., Khan M., Ilangovan S., Vaselli N. M., Smithers R., Uhanowita Marage R., Valnarov-Boulter A., Kayran J., Banerjee M., Parekh-Hill N., Hooper A., Bowen J., Jagdish R., Mcquoid C., Khan N., O Hare R., Jeffery S., Zahid A., Elsworth C., Walter L., Dhillon S., Rao S., Anthony A., Ashaye A., Phillips N., Faderani R., Pengelly S., Choi S., Kwak S. Y., Lau Y. H. L., Bagheri K., Ong D. Y. C., Kerr E., Falconer K., Clancy N., Douglas S., Zhang Y., Greenfield F., Mutanga I., McAlinden J., Willis L., Adefolaju A., Agarwal H., Barter R., Harris G., Spencer G., Lee M. W., V Vadiveloo T., Herbert G., Patel R., Shah M., El Falaha S., Wong C., Soare C., Akram J., Bozhkova L., Ma Y., Vo U. G., Tan H. W. N., Leto L., Kamal M. A., Hadzhieva E., Krastev P., Tonchev P., Kokkinos G., Pozotou I., Sabbagh D., Votava J., St F., Koliakos N., Tsaparas P., Zografos G., Mantas D., Tsourouflis G., Fradelos E., Trigiante G., Labellarte G., Resta G., Capelli G., D'Amore A., Verlingieri V., Campagnaro T., Maffioli A., Viscosi F., De Lucia C., Meneghini S., Fancellu A., Colella M., Biondi A., De Peppo V., Pace U., Albino V., Gattulli D., Piangerelli A., Kalivaci D., Sisto G., Mazzola M., Caneparo A., Lunghi E. G., Nespoli L. C., Angrisani M., Langone A., Gelarda E., Virgilio E., Angelini E., Fornasier C., Asero S., Filippone E., Frongia F., Calo P. G., Panaccio P., Ipponi P., Gili S., Braccio B., Tiesi V., Stolcers K., Kokaine L., Novikovs V., Capel L., Bastiaenen V., Heijmans H., Henriques S., Gan S. Z., Ramanayake H., Nolan M., Temperley H., Ciofic E., Pop B. A., Kurtenkov M., Jovanovic M., Vician M., Egea Arias P., Beltran de Heredia J., Labalde Martinez M., De Santiago Alvarez I., Alvarez-Gallego M., Rodriguez Artigas J. M., Dwidar O., Korkmaz H. K., Eray I. C., Meric S., Aydin R., Cetin B., Karaca B. E., Kuyumcu O. F., Yuksel E., Uprak T. K., Karabulut K., Kavukcu E., Mansor A., Hackett R., Zammit-Maempel M., Sabaratnam R., Maan A., Ferarrio I., Dixon L., Halai H., Sethi S., Nelson L., Grassam-rowe A., Krishnan E., Deeny D., McKeever M., George Pandeth A., Dhavala P., Sreenivasan S., Sundaram Venkatesan G., Zhu L., Atiyah Z., Gregory J., Morey T., Seymour Z., Holdsworth L., Abdelmahmoud S., Bourhill J., Bisheet G., Shaw J., Kulkarni K., Kumarakulasingam P., Pillay S., Al-Habsi R., Kungwengwe G., Richards J., Davoudi K., Ibrahim B., Tailor B., Zayed M., Chen F., Bailey S., Sheefat S., Nawaz G., Pawar R., Marsh S., Sam Z. H., Roy Bentley S., Simpson C., Hughes J., Lim Y., Ooi R., Toh W. H., Mannion P., Lovett A., Kincius A., Hussein S., Kirby E., Beckett R. G., Salmon J., Glynn T., Choo S. Y., Lyons S., Browne D., Ravindran W., Ahmad S., Zhu X., McNulty J., McCarthy L., Ng J., Karmally Z., McTeir K., Hanna M., Tan E., Namdeo S., Schembri R., and Pusey E.

Abstract

Aim: Intraperitoneal drains are often placed during emergency colorectal surgery. However, there is a lack of evidence supporting their use. This study aimed to describe the efficacy and safety of intraperitoneal drain placement after emergency colorectal surgery. Method: COMPlicAted intra-abdominal collectionS after colorectal Surgery (COMPASS) is a prospective, international, cohort study into which consecutive adult patients undergoing emergency colorectal surgery were enrolled (from 3 February 2020 to 8 March 2020). The primary outcome was the rate of intraperitoneal drain placement. Secondary outcomes included rate and time-to-diagnosis of postoperative intraperitoneal collections, rate of surgical site infections (SSIs), time to discharge and 30-day major postoperative complications (Clavien–Dindo III–V). Multivariable logistic and Cox proportional hazards regressions were used to estimate the independent association of the outcomes with drain placement. Results: Some 725 patients (median age 68.0 years; 349 [48.1%] women) from 22 countries were included. The drain insertion rate was 53.7% (389 patients). Following multivariable adjustment, drains were not significantly associated with reduced rates (odds ratio [OR] = 1.56, 95% CI: 0.48–5.02, p = 0.457) or earlier detection (hazard ratio [HR] = 1.07, 95% CI: 0.61–1.90, p = 0.805) of collections. Drains were not significantly associated with worse major postoperative complications (OR = 1.26, 95% CI: 0.67–2.36, p = 0.478), delayed hospital discharge (HR = 1.11, 95% CI: 0.91–1.36, p = 0.303) or increased risk of SSIs (OR = 1.61, 95% CI: 0.87–2.99, p = 0.128). Conclusion: This is the first study investigating placement of intraperitoneal drains following emergency colorectal surgery. The safety and clinical benefit of drains remain uncertain. Equipoise exists for randomized trials to define the safety and efficacy of drains in emergency colorectal surgery.

Published
2023

42. LUNASKA neutrino search with the Parkes and ATCA telescopes

Author

Bray, J. D., Ekers, R. D., Protheroe, R. J., James, C. W., Phillips, C. J., Roberts, P., Brown, A., Reynolds, J. E., McFadden, R. A., and Aartsen, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Moon is used as a target volume for ultra-high energy neutrino searches with terrestrial radio telescopes. The LUNASKA project has conducted observations with the Parkes and ATCA telescopes; and, most recently, with both of them in combination. We present an analysis of the data obtained from these searches, including validation and calibration results for the Parkes-ATCA experiment, as well as a summary of prospects for future observations., Comment: 13 pages, 7 figures, Proceedings of the ARENA 2012 workshop (Erlangen, Germany)

Published
2013
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44. Noise statistics in a fast digital radio receiver: the Bedlam backend for the Parkes Radio Telescope

Author

Bray, J. D., Ekers, R. D., and Roberts, P.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The digital record of the voltage in a radio telescope receiver, after frequency conversion and sampling at a finite rate, is not a perfect representation of the original analog signal. To detect and characterise a transient event with a duration comparable to the inverse bandwidth it is necessary to compensate for these effects, which modifies the statistics of the signal, making it difficult to determine the significance of a potential detection. We present an analysis of these modified statistics and demonstrate them with experimental results from Bedlam, a new digital backend for the Parkes radio telescope., Comment: 21 pages, 8 figures, accepted for publication in Experimental Astronomy

Published
2012
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45. Observations and modelling of pulsed radio emission from CU Virginis

Author

Lo, K. K., Bray, J. D., Hobbs, G., Murphy, T., Gaensler, B. M., Melrose, D., Ravi, V., Manchester, R. M., and Keith, M. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present 13 cm and 20 cm radio observations of the magnetic chemically peculiar star CU Virginis taken with the Australia Telescope Compact Array. We detect two circularly polarised radio pulses every rotation period which confirm previous detections. In the first pulse, the lower frequency emission arrives before the higher frequency emission and the ordering reverses in the second pulse. In order to explain the frequency dependence of the time between the two pulses, we construct a geometric model of the magnetosphere of CU Virginis, and consider various emission angles relative to the magnetic field lines. A simple electron cyclotron maser emission model, in which the emission is perpendicular to the magnetic field lines, is not consistent with our data. A model in which the emission is refracted through cold plasma in the magnetosphere is shown to have the correct pulse arrival time frequency dependence., Comment: Accepted by MNRAS

Published
2012
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46. LUNASKA simultaneous neutrino searches with multiple telescopes

Author

Bray, J. D., Ekers, R. D., James, C. W., Roberts, P., Brown, A., Phillips, C. J., Protheroe, R. J., Reynolds, J. E., McFadden, R. A., and Aartsen, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The most sensitive method for detecting neutrinos at the very highest energies is the lunar Cherenkov technique, which employs the Moon as a target volume, using conventional radio telescopes to monitor it for nanosecond-scale pulses of Cherenkov radiation from particle cascades in its regolith. Multiple-antenna radio telescopes are difficult to effectively combine into a single detector for this purpose, while single antennas are more susceptible to false events from radio interference, which must be reliably excluded for a credible detection to be made. We describe our progress in excluding such interference in our observations with the single-antenna Parkes radio telescope, and our most recent experiment (taking place the week before the ICRC) using it in conjunction with the Australia Telescope Compact Array, exploiting the advantages of both types of telescope., Comment: 4 pages, 4 figures, in Proceedings of the 32nd International Cosmic Ray Conference (Beijing 2011)

Published
2011
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47. Status and Strategies of Current LUNASKA Lunar Cherenkov Observations with the Parkes Radio Telescope

Author

Bray, J. D., Ekers, R. D., Roberts, P., Reynolds, J. E., James, C. W., Phillips, C. J., McFadden, R. A., Protheroe, R. J., Aartsen, M., and Alvarez-Muñiz, J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

LUNASKA (Lunar UHE Neutrino Astrophysics with the Square Kilometre Array) is an ongoing project conducting lunar Cherenkov observations in order to develop techniques for detecting neutrinos with the next generation of radio telescopes. Our current observing campaign is with the 64-metre Parkes radio telescope, using a multibeam receiver with 300 MHz of bandwidth from 1.2-1.5 GHz. Here we provide an overview of the various factors that must be considered in the signal processing for such an experiment. We also briefly describe the flux limits which we expect to set with our current observations, including a directional limit for Centaurus A., Comment: 4 pages, 5 figures, Proceedings of ARENA 2010, Nantes, France

Published
2010
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48. Observations of radio pulses from CU Virginis

Author

Ravi, V., Hobbs, G., Wickramasinghe, D., Champion, D. J., Keith, M., Manchester, R. N., Norris, R. P., Bray, J. D., Ferrario, L., and Melrose, D.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The magnetic chemically peculiar star CU Virginis is a unique astrophysical laboratory for stellar magnetospheres and coherent emission processes. It is the only known main sequence star to emit a radio pulse every rotation period. Here we report on new observations of the CU Virginis pulse profile in the 13 and 20\,cm radio bands. The profile is known to be characterised by two peaks of 100$\%$ circularly polarised emission that are thought to arise in an electron-cyclotron maser mechanism. We find that the trailing peak is stable at both 13 and 20\,cm, whereas the leading peak is intermittent at 13\,cm. Our measured pulse arrival times confirm the discrepancy previously reported between the putative stellar rotation rates measured with optical data and with radio observations. We suggest that this period discrepancy might be caused by an unknown companion or by instabilities in the emission region. Regular long-term pulse timing and simultaneous multi-wavelength observations are essential to clarify the behaviour of this emerging class of transient radio source., Comment: Accepted by MNRAS Letters; 5 pages, 2 figures, 3 tables

Published
2010
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49. LUNASKA experiments using the Australia Telescope Compact Array to search for ultra-high energy neutrinos and develop technology for the lunar Cherenkov technique

Author

James, C. W., Ekers, R. D., Alvarez-Muñiz, J., Bray, J. D., McFadden, R. A., Phillips, C. J., Protheroe, R. J., and Roberts, P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We describe the design, performance, sensitivity and results of our recent experiments using the Australia Telescope Compact Array (ATCA) for lunar Cherenkov observations with a very wide (600 MHz) bandwidth and nanosecond timing, including a limit on an isotropic neutrino flux. We also make a first estimate of the effects of small-scale surface roughness on the effective experimental aperture, finding that contrary to expectations, such roughness will act to increase the detectability of near-surface events over the neutrino energy-range at which our experiment is most sensitive (though distortions to the time-domain pulse profile may make identification more difficult). The aim of our "Lunar UHE Neutrino Astrophysics using the Square Kilometer Array" (LUNASKA) project is to develop the lunar Cherenkov technique of using terrestrial radio telescope arrays for ultra-high energy (UHE) cosmic ray (CR) and neutrino detection, and in particular to prepare for using the Square Kilometer Array (SKA) and its path-finders such as the Australian SKA Pathfinder (ASKAP) and the Low Frequency Array (LOFAR) for lunar Cherenkov experiments., Comment: 27 pages, 18 figures, 4 tables.

Published
2009
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50. Results of LUNASKA lunar Cherenkov observations at the ATCA

Author

James, C. W., Ekers, R. D., Philips, C. J., Protheroe, R. J., Roberts, P., Robinson, R. A., Alvarez-Muñiz, J., and Bray, J. D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The lunar Cherenkov technique is a method to use radio-telescopes to detect ultra-high energy cosmic rays (CR) and neutrinos ($\nu$). By observing the short-duration ($\sim$few nanosecond) pulses of coherent Cherenkov radiation emitted from particle cascades via the Askaryan Effect in the Moon's outer layers (nominally the regolith), the primary particles initiating the cascades may be identified. Our collaboration (LUNASKA) aims to develop the technique to be used with the next generation of giant radio-arrays. Here, we present the results of our two preliminary UHE particle searches using this technique with three antennas at the Australia Telescope Compact Array (ATCA) during February and May 2008., Comment: Presented at the 31st International Cosmic Ray Conference, Lodz, Poland, 2009

Published
2009

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