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1. Understanding the HERA Phase i receiver system with simulations and its impact on the detectability of the EoR delay power spectrum

Author: Fagnoni, N, De Lera Acedo, E, Deboer, DR, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carilli, CL, Cheng, C, Dexter, M, Dillon, JS, Ewall-Wice, A, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Josaitis, A, Julius, A, Kern, NS, Kerrigan, J, Kim, H, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, Plante, PL, Lekalake, T, Liu, A, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mena Parra, J, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Neben, AR, Nikolic, B, Parsons, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Smith, C, Syce, A, Thyagarajan, N, Williams, PKG, and Zheng, H
Subjects: instrumentation: interferometers, methods: numerical, techniques: interferometric, telescopes, dark ages, reionization, first stars, astro-ph.IM, dark ages, reionization, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: The detection of the Epoch of Reionization (EoR) delay power spectrum using a 'foreground avoidance method' highly depends on the instrument chromaticity. The systematic effects induced by the radio telescope spread the foreground signal in the delay domain, which contaminates the EoR window theoretically observable. Applied to the Hydrogen Epoch of Reionization Array (HERA), this paper combines detailed electromagnetic and electrical simulations in order to model the chromatic effects of the instrument, and quantify its frequency and time responses. In particular, the effects of the analogue receiver, transmission cables, and mutual coupling are included. These simulations are able to accurately predict the intensity of the reflections occurring in the 150-m cable which links the antenna to the backend. They also show that electromagnetic waves can propagate from one dish to another one through large sections of the array due to mutual coupling. The simulated system time response is attenuated by a factor 104 after a characteristic delay which depends on the size of the array and on the antenna position. Ultimately, the system response is attenuated by a factor 105 after 1400 ns because of the reflections in the cable, which corresponds to characterizable ka-modes above 0.7 $h\,\,\rm {Mpc}^{-1}$ at 150 MHz. Thus, this new study shows that the detection of the EoR signal with HERA Phase I will be more challenging than expected. On the other hand, it improves our understanding of the telescope, which is essential to mitigate the instrument chromaticity.
Published: 2021

2. Detection of cosmic structures using the bispectrum phase. II. First results from application to cosmic reionization using the Hydrogen Epoch of Reionization Array

Author: Thyagarajan, N, Carilli, CL, Nikolic, B, Kent, J, Mesinger, A, Kern, NS, Bernardi, G, Matika, S, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Billings, TS, Bowman, JD, Bradley, RF, Burba, J, Carey, S, Cheng, C, Deboer, DR, Dexter, M, Acedo, EDL, Dillon, JS, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Lekalake, T, Lewis, D, Liu, A, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Molewa, M, Morales, MF, Mosiane, T, Neben, AR, Parsons, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sims, P, Smith, C, Syce, A, Williams, PKG, and Zheng, H
Subjects: astro-ph.CO, astro-ph.IM
Abstract: Characterizing the epoch of reionization (EoR) at z 6 via the redshifted 21 cm line of neutral Hydrogen (H i) is critical to modern astrophysics and cosmology, and thus a key science goal of many current and planned low-frequency radio telescopes. The primary challenge to detecting this signal is the overwhelmingly bright foreground emission at these frequencies, placing stringent requirements on the knowledge of the instruments and inaccuracies in analyses. Results from these experiments have largely been limited not by thermal sensitivity but by systematics, particularly caused by the inability to calibrate the instrument to high accuracy. The interferometric bispectrum phase is immune to antenna-based calibration and errors therein, and presents an independent alternative to detect the EoR H i fluctuations while largely avoiding calibration systematics. Here, we provide a demonstration of this technique on a subset of data from the Hydrogen Epoch of Reionization Array (HERA) to place approximate constraints on the brightness temperature of the intergalactic medium (IGM). From this limited data, at z=7.7 we infer "1σ"upper limits on the IGM brightness temperature to be ≤ 316 "pseudo"mK at κ =0.33 "pseudo"h Mpc-1 (data-limited) and ≤ 1000 "pseudo"mK at κ =0.875 "pseudo"h Mpc-1 (noise-limited). The "pseudo"units denote only an approximate and not an exact correspondence to the actual distance scales and brightness temperatures. By propagating models in parallel to the data analysis, we confirm that the dynamic range required to separate the cosmic H i signal from the foregrounds is similar to that in standard approaches, and the power spectrum of the bispectrum phase is still data-limited (at 106 dynamic range) indicating scope for further improvement in sensitivity as the array build-out continues.
Published: 2020

3. Foreground modelling via Gaussian process regression: An application to HERA data

Author: Ghosh, A, Mertens, F, Bernardi, G, Santos, MG, Kern, NS, Carilli, CL, Grobler, TL, Koopmans, LVE, Jacobs, DC, Liu, A, Parsons, AR, Morales, MF, Aguirre, JE, Dillon, JS, Hazelton, BJ, Smirnov, OM, Gehlot, BK, Matika, S, Alexander, P, Ali, ZS, Beardsley, AP, Benefo, RK, Billings, TS, Bowman, JD, Bradley, RF, Cheng, C, Chichura, PM, Deboer, DR, Acedo, EDL, Ewall-Wice, A, Fadana, G, Fagnoni, N, Fortino, AF, Fritz, R, Furlanetto, SR, Gallardo, S, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Hickish, J, Josaitis, A, Julius, A, Igarashi, AS, Kariseb, M, Kohn, SA, Kolopanis, M, Lekalake, T, Loots, A, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Mathison, N, Matsetela, E, Mesinger, A, Neben, AR, Nikolic, B, Nunhokee, CD, Patra, N, Pieterse, S, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sell, R, Smith, C, Syce, A, Tegmark, M, Thyagarajan, N, Williams, PKG, and Zheng, H
Subjects: instrumentation: interferometers, methods: statistical, dark ages, reionization, first stars, diffuse radiation, large-scale structure of Universe, cosmology: observations, astro-ph.CO, dark ages, reionization, first stars, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: The key challenge in the observation of the redshifted 21-cm signal from cosmic reionization is its separation from the much brighter foreground emission. Such separation relies on the different spectral properties of the two components, although, in real life, the foreground intrinsic spectrum is often corrupted by the instrumental response, inducing systematic effects that can further jeopardize the measurement of the 21-cm signal. In this paper, we use Gaussian Process Regression to model both foreground emission and instrumental systematics in ∼2 h of data from the Hydrogen Epoch of Reionization Array. We find that a simple co-variance model with three components matches the data well, giving a residual power spectrum with white noise properties. These consist of an 'intrinsic' and instrumentally corrupted component with a coherence scale of 20 and 2.4 MHz, respectively (dominating the line-of-sight power spectrum over scales kâ ≤ 0.2 h cMpc-1) and a baseline-dependent periodic signal with a period of ∼1 MHz (dominating over kâ ∼0.4-0.8 h cMpc-1), which should be distinguishable from the 21-cm Epoch of Reionization signal whose typical coherence scale is ∼0.8 MHz.
Published: 2020

4. Redundant-baseline calibration of the hydrogen epoch of reionization array

Author: Dillon, JS, Lee, M, Ali, ZS, Parsons, AR, Orosz, N, Nunhokee, CD, La Plante, P, Beardsley, AP, Kern, NS, Abdurashidova, Z, Aguirre, JE, Alexander, P, Balfour, Y, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Dexter, M, de Lera Acedo, E, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, Lekalake, T, Lewis, D, Liu, A, Ma, YZ, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, S, Neben, AR, Nikolic, B, Pascua, R, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Santos, MG, Sims, P, Smith, C, Syce, A, Tegmark, M, Thyagarajan, N, Williams, PKG, and Zheng, H
Subjects: instrumentation: interferometers, dark ages, reionization, first stars, astro-ph.IM, astro-ph.CO, dark ages, reionization, first stars, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: In 21-cm cosmology, precision calibration is key to the separation of the neutral hydrogen signal from very bright but spectrally smooth astrophysical foregrounds. The Hydrogen Epoch of Reionization Array (HERA), an interferometer specialized for 21-cm cosmology and now under construction in South Africa, was designed to be largely calibrated using the self-consistency of repeated measurements of the same interferometric modes. This technique, known as redundant-baseline calibration resolves most of the internal degrees of freedom in the calibration problem. It assumes, however, on antenna elements with identical primary beams placed precisely on a redundant grid. In this work, we review the detailed implementation of the algorithms enabling redundant-baseline calibration and report results with HERA data.We quantify the effects of real-world non-redundancy and how they compare to the idealized scenario in which redundant measurements differ only in their noise realizations. Finally, we study how non-redundancy can produce spurious temporal structure in our calibration solutions-both in data and in simulations-and present strategies for mitigating that structure.
Published: 2020

5. Optimizing sparse RFI prediction using deep learning

Author: Kerrigan, J, la Plante, P, Kohn, S, Pober, JC, Aguirre, J, Abdurashidova, Z, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Bernardi, G, Bowman, JD, Bradley, RF, Burba, J, Carilli, CL, Cheng, C, DeBoer, DR, Dexter, M, de Lera Acedo, E, Dillon, JS, Estrada, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Glendenning, B, Greig, B, Grobbelaar, J, Gorthi, D, Halday, Z, Hazelton, BJ, Hickish, J, Jacobs, DC, Julius, A, Kern, NS, Kittiwisit, P, Kolopanis, M, Lanman, A, Lekalake, T, Liu, A, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Neben, AR, Parsons, AR, Patra, N, Pieterse, S, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sims, P, Smith, C, Syce, A, Thyagarajan, N, Williams, PKG, and Zheng, H
Subjects: methods: data analysis, techniques: interferometric, astro-ph.IM, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: Radio frequency interference (RFI) is an ever-present limiting factor among radio telescopes even in the most remote observing locations. When looking to retain the maximum amount of sensitivity and reduce contamination for Epoch of Reionization studies, the identification and removal of RFI is especially important. In addition to improved RFI identification, we must also take into account computational efficiency of the RFI-Identification algorithm as radio interferometer arrays such as the Hydrogen Epoch of Reionization Array (HERA) grow larger in number of receivers. To address this, we present a deep fully convolutional neural network (DFCN) that is comprehensive in its use of interferometric data, where both amplitude and phase information are used jointly for identifying RFI. We train the network using simulated HERA visibilities containing mock RFI, yielding a known ‘ground truth’ data set for evaluating the accuracy of various RFI algorithms. Evaluation of the DFCN model is performed on observations from the 67 dish build-out, HERA-67, and achieves a data throughput of 1.6 × 105 HERA time-ordered 1024 channelled visibilities per hour per GPU. We determine that relative to an amplitude only network including visibility phase adds important adjacent time–frequency context which increases discrimination between RFI and non-RFI. The inclusion of phase when predicting achieves a recall of 0.81, precision of 0.58, and F2 score of 0.75 as applied to our HERA-67 observations.
Published: 2019

6. The HERA-19 Commissioning Array: Direction-dependent Effects

Author: Kohn, SA, Aguirre, JE, La Plante, P, Billings, TS, Chichura, PM, Fortino, AF, Igarashi, AS, Benefo, RK, Gallardo, S, Martinot, ZE, Nunhokee, CD, Kern, NS, Bull, P, Liu, A, Alexander, P, Ali, ZS, Beardsley, AP, Bernardi, G, Bowman, JD, Bradley, RF, Carilli, CL, Cheng, C, Deboer, DR, Acedo, EDL, Dillon, JS, Ewall-Wice, A, Fadana, G, Fagnoni, N, Fritz, R, Furlanetto, SR, Glendenning, B, Greig, B, Grobbelaar, J, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kariseb, M, Kolopanis, M, Lekalake, T, Loots, A, Macmahon, D, Malan, L, Malgas, C, Maree, M, Mathison, N, Matsetela, E, Mesinger, A, Morales, MF, Neben, AR, Nikolic, B, Parsons, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sell, R, Smith, C, Syce, A, Tegmark, M, Thyagarajan, N, Williams, PKG, and Zheng, H
Subjects: cosmology: observations, dark ages, reionization, first stars, instrumentation: interferometers, polarization, techniques: interferometric, astro-ph.IM, dark ages, reionization, first stars, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: Foreground power dominates the measurements of interferometers that seek a statistical detection of highly-redshifted H i emission from the Epoch of Reionization (EoR). The chromaticity of the instrument creates a boundary in the Fourier transform of frequency (proportional to k ∥) between spectrally smooth emission, characteristic of the strong synchrotron foreground (the "wedge"), and the spectrally structured emission from H i in the EoR (the "EoR window"). Faraday rotation can inject spectral structure into otherwise smooth polarized foreground emission, which through instrument effects or miscalibration could possibly pollute the EoR window. For instruments pursuing a "foreground avoidance" strategy of simply measuring in the EoR window, and not attempting to model and remove foregrounds, as is the plan for the first stage of the Hydrogen Epoch of Reionization Array (HERA), characterizing the intrinsic instrument polarization response is particularly important. Using data from the HERA 19-element commissioning array, we investigate the polarization response of this new instrument in the power-spectrum domain. We perform a simple image-based calibration based on the unpolarized diffuse emission of the Global Sky Model, and show that it achieves qualitative redundancy between the nominally redundant baselines of the array and reasonable amplitude accuracy. We construct power spectra of all fully polarized coherencies in all pseudo-Stokes parameters, and discuss the achieved isolation of foreground power due to the intrinsic spectral smoothness of the foregrounds, the instrument chromaticity, and the calibration. We compare to simulations based on an unpolarized diffuse sky model and detailed electromagnetic simulations of the dish and feed, confirming that in Stokes I, the calibration does not add significant spectral structure beyond that expected from the interferometer array configuration and the modeled primary beam response. Furthermore, this calibration is stable over the 8 days of observations considered. Excess power is seen in the power spectra of the linear polarization Stokes parameters, which is not easily attributable to leakage via the primary beam, and results from some combination of residual calibration errors and actual polarized emission. Stokes V is found to be highly discrepant from the expectation of zero power, strongly pointing to the need for more accurate polarized calibration.
Published: 2019

7. The hydrogen epoch of reionization array dish III: measuring chromaticity of prototype element with reflectometry

Author: Patra, N, Parsons, AR, DeBoer, DR, Thyagarajan, N, Ewall-Wice, A, Hsyu, G, Leung, TK, Day, CK, de Lera Acedo, E, Aguirre, JE, Alexander, P, Ali, ZS, Beardsley, AP, Bowman, JD, Bradley, RF, Carilli, CL, Cheng, C, Dillon, JS, Fadana, G, Fagnoni, N, Fritz, R, Furlanetto, SR, Glendenning, B, Greig, B, Grobbelaar, J, Hazelton, BJ, Jacobs, DC, Julius, A, Kariseb, MC, Kohn, SA, Lebedeva, A, Lekalake, T, Liu, A, Loots, A, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, Z, Mathison, N, Matsetela, E, Mesinger, A, Morales, MF, Neben, AR, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sell, R, Smith, C, Syce, A, Tegmark, M, Williams, PKG, and Zheng, H
Subjects: Astronomical instrumentation, Methods and techniques-wideband radio interferometry, Delay spectrum technique-EoR power spectrum, cm cosmology, astro-ph.IM, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: Spectral structures due to the instrument response is the current limiting factor for the experiments attempting to detect the redshifted 21 cm signal from the Epoch of Reionization (EoR). Recent advances in the delay spectrum methodology for measuring the redshifted 21 cm EoR power spectrum brought new attention to the impact of an antenna’s frequency response on the viability of making this challenging measurement. The delay spectrum methodology provides a somewhat straightforward relationship between the time-domain response of an instrument that can be directly measured and the power spectrum modes accessible to a 21 cm EoR experiment. In this paper, we derive the explicit relationship between antenna reflection coefficient (S11) measurements made by a Vector Network Analyzer (VNA) and the extent of additional foreground contaminations in delay space. In the light of this mathematical framework, we examine the chromaticity of a prototype antenna element that will constitute the Hydrogen Epoch of Reionization Array (HERA) between 100 and 200 MHz. These reflectometry measurements exhibit additional structures relative to electromagnetic simulations, but we find that even without any further design improvement, such an antenna element will support measuring spatial k modes with line-of-sight components of k∥ > 0.2h Mpc− 1. We also find that when combined with the powerful inverse covariance weighting method used in optimal quadratic estimation of redshifted 21 cm power spectra the HERA prototype elements can successfully measure the power spectrum at spatial modes as low as k∥ > 0.1h Mpc− 1. This work represents a major step toward understanding the HERA antenna element and highlights a straightforward method for characterizing instrument response for future experiments designed to detect the 21 cm EoR power spectrum.
Published: 2018

8. Assessing the provisions for sustainability in economics degree programmes

Author: Leal, W, Dinis, MAP, Morales, MF, Semitiel-García, M, Noguera-Méndez, P, Ruiz de Maya, S, Alarcón-del-Amo, MDC, Esteban-Lloret, N, Pemartín, M, Leal, W, Dinis, MAP, Morales, MF, Semitiel-García, M, Noguera-Méndez, P, Ruiz de Maya, S, Alarcón-del-Amo, MDC, Esteban-Lloret, N, and Pemartín, M
Abstract: Purpose: Higher education institutions (HEIs) offer courses and programmes focusing on sustainability in economics, as courses on sustainable development (SD), which examine the economic, social and environmental dimensions of SD. This paper aims to examine sustainability integration in economics degree programmes. Design/methodology/approach: Through an extensive literature review in Web of Science (WoS) and information search in Google, conducting to 28 relevant case studies, this paper elucidates the emphasis given to sustainability as part of economics degree programmes in HEIs. Findings: The results suggest that, whereas the inclusion of sustainability components in this field is a growing trend, much still needs to be done to ensure that matters related to SD are part of the routine of university students studying economics. Research limitations/implications: It is worth noting that the literature review conducted in WoS was primarily aimed at assisting in the selection of university case studies. The 28 university case studies scrutinised in this study may lack sufficient representation from numerous developing countries. Practical implications: This study highlights challenges in integrating the SD into economics degree programmes, suggesting the need for curriculum adjustments as underscoring operational issues, acting as barriers. The inclusion of sustainability in economics programmes must navigate operational issues stemming from packed timetables and busy schedules, requiring innovative solutions. Social implications: As far as the authors are aware, this study holds substantial importance in its emphasis on implementing sustainability within HEIs’ economics programmes, assisting in pursuing SD. Originality/value: The novelty of this study lies in addressing sustainability with the specific economics focus programmes within the HEIs context.
Published: 2024

9. Mapmaking for precision 21 cm cosmology MAPMAKING for PRECISION 21 CM COSMOLOGY JOSHUA S. DILLON et al.

Author: Dillon, JS, Tegmark, M, Liu, A, Ewall-Wice, A, Hewitt, JN, Morales, MF, Neben, AR, Parsons, AR, and Zheng, H
Subjects: Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract: In order to study the "Cosmic Dawn" and the Epoch of Reionization with 21 cm tomography, we need to statistically separate the cosmological signal from foregrounds known to be orders of magnitude brighter. Over the last few years, we have learned much about the role our telescopes play in creating a putatively foreground-free region called the "EoR window." In this work, we examine how an interferometer's effects can be taken into account in a way that allows for the rigorous estimation of 21 cm power spectra from interferometric maps while mitigating foreground contamination and thus increasing sensitivity. This requires a precise understanding of the statistical relationship between the maps we make and the underlying true sky. While some of these calculations would be computationally infeasible if performed exactly, we explore several well-controlled approximations that make mapmaking and the calculation of map statistics much faster, especially for compact and highly redundant interferometers designed specifically for 21 cm cosmology. We demonstrate the utility of these methods and the parametrized trade-offs between accuracy and speed using one such telescope, the upcoming Hydrogen Epoch of Reionization Array, as a case study.
Published: 2015

10. Improved Constraints on the 21 cm EoR Power Spectrum and the X-Ray Heating of the IGM with HERA Phase I Observations

Author: Abdurashidova, THCZ, Adams, T, Aguirre, JE, Alexander, P, Ali, ZS, Baartman, R, Balfour, Y, Barkana, R, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Breitman, D, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, Choudhuri, S, DeBoer, DR, De Lera Acedo, E, Dexter, M, Dillon, JS, Ely, J, Ewall-Wice, A, Fagnoni, N, Fialkov, A, Fritz, R, Furlanetto, Gale-Sides, K, Garsden, H, Glendenning, B, Gorce, A, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Heimersheim, S, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kern, NS, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Lewis, D, Liu, A, Loots, A, Ma, YZ, MacMahon, DHE, Malan, L, Malgas, K, Malgas, C, Maree, M, Marero, B, Martinot, ZE, McBride, L, Mesinger, A, Mirocha, J, Molewa, M, Morales, MF, Mosiane, T, Muñoz, JB, Murray, SG, Nagpal, V, Neben, AR, Nikolic, B, Nunhokee, CD, Nuwegeld, H, Parsons, AR, Pascua, R, Patra, N, Pieterse, S, Qin, Y, Razavi-Ghods, N, Robnett, J, Rosie, K, Santos, MG, Sims, P, Singh, S, Smith, C, Swarts, H, Tan, J, Thyagarajan, N, Wilensky, MJ, Williams, PKG, Van Wyngaarden, P, Zheng, H, Aguirre, JE [0000-0002-4810-666X], Barkana, R [0000-0002-1557-693X], Beardsley, AP [0000-0001-9428-8233], Bernardi, G [0000-0002-0916-7443], Bowman, JD [0000-0002-8475-2036], Bradley, RF [0000-0003-1172-8331], Breitman, D [0000-0002-2349-3341], Bull, P [0000-0001-5668-3101], Carilli, CL [0000-0001-6647-3861], Choudhuri, S [0000-0002-2338-935X], DeBoer, DR [0000-0003-3197-2294], de Lera Acedo, E [0000-0001-8530-6989], Dillon, JS [0000-0003-3336-9958], Ewall-Wice, A [0000-0002-0086-7363], Fagnoni, N [0000-0001-5300-3166], Fialkov, A [0000-0002-1369-633X], Furlanetto, SR [0000-0002-0658-1243], Gorce, A [0000-0002-1712-737X], Gorthi, D [0000-0002-0829-167X], Greig, B [0000-0002-4085-2094], Hazelton, BJ [0000-0001-7532-645X], Heimersheim, S [0000-0001-9631-4212], Hewitt, JN [0000-0002-4117-570X], Jacobs, DC [0000-0002-0917-2269], Kern, NS [0000-0002-8211-1892], Kerrigan, J [0000-0002-1876-272X], Kittiwisit, P [0000-0003-0953-313X], Kohn, SA [0000-0001-6744-5328], Kolopanis, M [0000-0002-2950-2974], Lanman, A [0000-0003-2116-3573], La Plante, P [0000-0002-4693-0102], Liu, A [0000-0001-6876-0928], Ma, YZ [0000-0001-8108-0986], Mesinger, A [0000-0003-3374-1772], Mirocha, J [0000-0002-8802-5581], Morales, MF [0000-0001-7694-4030], Muñoz, JB [0000-0002-8984-0465], Murray, SG [0000-0003-3059-3823], Nagpal, V [0000-0001-5909-4433], Neben, AR [0000-0001-7776-7240], Nikolic, B [0000-0001-7168-2705], Nunhokee, CD [0000-0002-5445-6586], Parsons, AR [0000-0002-5400-8097], Pascua, R [0000-0003-0073-5528], Patra, N [0000-0002-9457-1941], Qin, Y [0000-0002-4314-1810], Razavi-Ghods, N [0000-0003-2930-5396], Rosie, K [0000-0003-3611-8804], Santos, MG [0000-0003-3892-3073], Sims, P [0000-0002-2871-0413], Singh, S [0000-0001-7755-902X], Tan, J [0000-0001-6161-7037], Thyagarajan, N [0000-0003-1602-7868], Wilensky, MJ [0000-0001-7716-9312], Williams, PKG [0000-0003-3734-3587], Zheng, H [0000-0001-8267-3425], and Apollo - University of Cambridge Repository
Subjects: Space and Planetary Science, 5101 Astronomical Sciences, Astronomy and Astrophysics, 51 Physical Sciences
Abstract: We report the most sensitive upper limits to date on the 21 cm epoch of reionization power spectrum using 94 nights of observing with Phase I of the Hydrogen Epoch of Reionization Array (HERA). Using similar analysis techniques as in previously reported limits, we find at 95% confidence that Δ2(k = 0.34 h Mpc−1) ≤ 457 mK2 at z = 7.9 and that Δ2(k = 0.36 h Mpc−1) ≤ 3496 mK2 at z = 10.4, an improvement by a factor of 2.1 and 2.6, respectively. These limits are mostly consistent with thermal noise over a wide range of k after our data quality cuts, despite performing a relatively conservative analysis designed to minimize signal loss. Our results are validated with both statistical tests on the data and end-to-end pipeline simulations. We also report updated constraints on the astrophysics of reionization and the cosmic dawn. Using multiple independent modeling and inference techniques previously employed by HERA Collaboration, we find that the intergalactic medium must have been heated above the adiabatic cooling limit at least as early as z = 10.4, ruling out a broad set of so-called “cold reionization” scenarios. If this heating is due to high-mass X-ray binaries during the cosmic dawn, as is generally believed, our result’s 99% credible interval excludes the local relationship between soft X-ray luminosity and star formation and thus requires heating driven by evolved low-metallicity stars.
Published: 2023

11. Characterization of inpaint residuals in interferometric measurements of the epoch of reionization

Author: Pagano, M, Liu, J, Liu, A, Kern, NS, Ewall-Wice, A, Bull, P, Pascua, R, Ravanbakhsh, S, Abdurashidova, Z, Adams, T, Aguirre, JE, Alexander, P, Ali, ZS, Baartman, R, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Acedo, EDL, Dexter, M, Dillon, JS, Eksteen, N, Ely, J, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kariseb, M, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Loots, A, MacMahon, DHE, Malan, L, Malgas, C, Malgas, K, Marero, B, Martinot, ZE, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Neben, AR, Nikolic, B, Nuwegeld, H, Parsons, AR, Patra, N, Pieterse, S, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Smith, C, Swarts, H, Thyagarajan, N, van Wyngaarden, P, Williams, PKG, Zheng, H, Pagano, M, Liu, J, Liu, A, Kern, NS, Ewall-Wice, A, Bull, P, Pascua, R, Ravanbakhsh, S, Abdurashidova, Z, Adams, T, Aguirre, JE, Alexander, P, Ali, ZS, Baartman, R, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Acedo, EDL, Dexter, M, Dillon, JS, Eksteen, N, Ely, J, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kariseb, M, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Loots, A, MacMahon, DHE, Malan, L, Malgas, C, Malgas, K, Marero, B, Martinot, ZE, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Neben, AR, Nikolic, B, Nuwegeld, H, Parsons, AR, Patra, N, Pieterse, S, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Smith, C, Swarts, H, Thyagarajan, N, van Wyngaarden, P, Williams, PKG, and Zheng, H
Abstract: To mitigate the effects of Radio Frequency Interference (RFI) on the data analysis pipelines of 21 cm interferometric instruments, numerous inpaint techniques have been developed. In this paper, we examine the qualitative and quantitative errors introduced into the visibilities and power spectrum due to inpainting. We perform our analysis on simulated data as well as real data from the Hydrogen Epoch of Reionization Array (HERA) Phase 1 upper limits. We also introduce a convolutional neural network that is capable of inpainting RFI corrupted data. We train our network on simulated data and show that our network is capable of inpainting real data without requiring to be retrained. We find that techniques that incorporate high wavenumbers in delay space in their modelling are best suited for inpainting over narrowband RFI. We show that with our fiducial parameters discrete prolate spheroidal sequences (dpss) and clean provide the best performance for intermittent RFI while Gaussian progress regression (gpr) and least squares spectral analysis (lssa) provide the best performance for larger RFI gaps. However, we caution that these qualitative conclusions are sensitive to the chosen hyperparameters of each inpainting technique. We show that all inpainting techniques reliably reproduce foreground dominated modes in the power spectrum. Since the inpainting techniques should not be capable of reproducing noise realizations, we find that the largest errors occur in the noise dominated delay modes. We show that as the noise level of the data comes down, clean and dpss are most capable of reproducing the fine frequency structure in the visibilities.
Published: 2023

12. Bayesian jackknife tests with a small number of subsets: application to HERA 21 cm power spectrum upper limits

Author: Wilensky, MJ, Kennedy, F, Bull, P, Dillon, JS, Abdurashidova, Z, Adams, T, Aguirre, JE, Alexander, P, Ali, ZS, Baartman, R, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, de Lera Acedo, E, Dexter, M, Eksteen, N, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kariseb, M, Kern, NS, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Liu, A, Loots, A, MacMahon, DHE, Malan, L, Malgas, C, Malgas, K, Marero, B, Martinot, ZE, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, SG, Neben, AR, Nikolic, B, Nuwegeld, H, Parsons, AR, Patra, N, Pieterse, S, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Swarts, H, Thyagarajan, N, van Wyngaarden, P, Williams, PKG, Zheng, H, Wilensky, MJ, Kennedy, F, Bull, P, Dillon, JS, Abdurashidova, Z, Adams, T, Aguirre, JE, Alexander, P, Ali, ZS, Baartman, R, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, de Lera Acedo, E, Dexter, M, Eksteen, N, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kariseb, M, Kern, NS, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Liu, A, Loots, A, MacMahon, DHE, Malan, L, Malgas, C, Malgas, K, Marero, B, Martinot, ZE, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, SG, Neben, AR, Nikolic, B, Nuwegeld, H, Parsons, AR, Patra, N, Pieterse, S, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Swarts, H, Thyagarajan, N, van Wyngaarden, P, Williams, PKG, and Zheng, H
Abstract: We present a Bayesian jackknife test for assessing the probability that a data set contains biased subsets, and, if so, which of the subsets are likely to be biased. The test can be used to assess the presence and likely source of statistical tension between different measurements of the same quantities in an automated manner. Under certain broadly applicable assumptions, the test is analytically tractable. We also provide an open-source code, chiborg, that performs both analytic and numerical computations of the test on general Gaussian-distributed data. After exploring the information theoretical aspects of the test and its performance with an array of simulations, we apply it to data from the Hydrogen Epoch of Reionization Array (HERA) to assess whether different sub-seasons of observing can justifiably be combined to produce a deeper 21 cm power spectrum upper limit. We find that, with a handful of exceptions, the HERA data in question are statistically consistent and this decision is justified. We conclude by pointing out the wide applicability of this test, including to CMB experiments and the H0 tension.
Published: 2023

13. First results of a study of TeV emission from GRBs in Milagrito

Author: McEnery, JE, Atkins, R, Benbow, W, Berley, D, Chen, ML, Coyne, DG, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, McConnell, M, McCullough, JF, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Shen, B, Shoup, A, Sinnis, C, Smith, AJ, Sullivan, GW, Tumer, T, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: Milagrito, a detector sensitive to gamma-rays at TeV energies, monitored thenorthern sky during the period February 1997 through May 1998. With a largefield of view and high duty cycle, this instrument was used to perform a searchfor TeV counterparts to gamma-ray bursts. Within the Milagrito field of view 54gamma-ray bursts at keV energies were observed by the Burst And TransientSatellite Experiment (BATSE) aboard the Compton Gamma-Ray Observatory. Thispaper describes the results of a preliminary analysis to search for TeVemission correlated with BATSE detected bursts. Milagrito detected an excess ofevents coincident both spatially and temporally with GRB 970417a, with chanceprobability $2.8 \times 10^{-5}$ within the BATSE error radius. No othersignificant correlations were detected. Since 54 bursts were examined thechance probability of observing an excess with this significance in any ofthese bursts is $1.5 \times 10^{-3}$. The statistical aspects and physicalimplications of this result are discussed.
Published: 2000

14. First results of a study of TeV emission from GRBs in Milagrito

Author: Miller, RS, Atkins, R, Benbow, W, Berley, D, Chen, ML, Coyne, DG, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, McConnell, M, McCullough, JF, McEnery, JE, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Shen, B, Shoup, A, Sinnis, C, Smith, AJ, Sullivan, GW, Tumer, T, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: Milagrito, a detector sensitive to gamma-rays at TeV energies, monitored thenorthern sky during the period February 1997 through May 1998. With a largefield of view and high duty cycle, this instrument was used to perform a searchfor TeV counterparts to gamma-ray bursts. Within the Milagrito field of view 54gamma-ray bursts at keV energies were observed by the Burst And TransientSatellite Experiment (BATSE) aboard the Compton Gamma-Ray Observatory. Thispaper describes the results of a preliminary analysis to search for TeVemission correlated with BATSE detected bursts. Milagrito detected an excess ofevents coincident both spatially and temporally with GRB 970417a, with chanceprobability $2.8 \times 10^{-5}$ within the BATSE error radius. No othersignificant correlations were detected. Since 54 bursts were examined thechance probability of observing an excess with this significance in any ofthese bursts is $1.5 \times 10^{-3}$. The statistical aspects and physicalimplications of this result are discussed.
Published: 2000

15. Instrumented Water Tanks can Improve Air Shower Detector Sensitivity

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: Previous works have shown that water Cherenkov detectors have superiorsensitivity to those of scintillation counters as applied to detectingextensive air showers (EAS). This is in large part due to their much highersensitivity to EAS photons which are more than five times more numerous thanEAS electrons. Large area water Cherenkov detectors can be constructedrelatively cheaply and operated reliably. A sparse detector array has beendesigned which uses these types of detectors to substantially increase the areaover which the Milagro Gamma Ray Observatory collects EAS information.Improvements to the Milagro detector's performance characteristics andsensitivity derived from this array and preliminary results from a prototypearray currently installed near the Milagro detector will be presented.
Published: 1999

16. Calibration of the Milagro Cosmic Ray Telescope

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: The Milagro detector is an air shower array which uses the water Cherenkovtechnique and is capable of continuously monitoring the sky at energies near 1TeV. The detector consists of 20000 metric tons of pure water instrumented with723 photo-multiplier tubes (PMTs). The PMTs are arranged in a two-layerstructure on a lattice of 3 m spacing covering 5000 $m^2$ area. The directionof the shower is determined from the relative timing of the PMT signals,necessitating a common time reference and amplitude slewing corrections toimprove the time resolution. The calibration system to provide these consistsof a pulsed laser driving 30 diffusing light sources deployed in the pond toallow cross-calibration of the PMTs. The system is capable of calibrating timesand the pulse-heights from the PMTs using the time-over-threshold technique.The absolute energy scale is provided using single muons passing through thedetector. The description of the calibration system of the Milagro detector andits prototype Milagrito will be presented.
Published: 1999

17. Status of the Milagro Gamma Ray Observatory

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: The Milagro Gamma Ray Observatory is the world's first large-area waterCherenkov detector capable of continuously monitoring the sky at TeV energies.Located in northern New Mexico, Milagro will perform an all sky survey of theNorthern Hemisphere at energies between ~250 GeV and 50 TeV. With a high dutycycle, large detector area (~5000 square meters), and a wide field-of-view (~1sr), Milagro is uniquely capable of searching for transient and DC sources ofhigh-energy gamma-ray emission. Milagro has been operating since February,1999. The current status of the Milagro Observatory and initial results will bediscussed.
Published: 1999

18. Study of the Shadows of the Moon and the Sun with VHE Cosmic Rays

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: Milagrito, a prototype for the Milagro detector, operated for 15 months in1997-8 and collected 8.9 billion events. It was the first extensive air shower(EAS) array sensitive to showers intiated by primaries with energy below 1 TeV.The shadows of the sun and moon observed with cosmic rays can be used to studysystematic pointing shifts and measure the angular resolution of EAS arrays.Below a few TeV, the paths of cosmic rays coming toward the earth are bent bythe helio- and geo-magnetic fields. This is expected to distort and displacethe shadows of the sun and the moon. The moon shadow, offset from the nominal(undeflected) position, has been observed with high statistical significance inMilagrito. This can be used to establish energy calibrations, as well as tosearch for the anti-matter content of the VHE cosmic ray flux. The shadow ofthe sun has also been observed with high significance.
Published: 1999

19. Search for Short Duration Bursts of TeV Gamma Rays with the Milagrito Telescope

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: The Milagrito water Cherenkov telescope operated for over a year. The mostprobable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400Hz. We have developed an efficient technique for searching the entire sky forshort duration bursts of TeV photons. Such bursts may result from "traditional"gamma-ray bursts that were not in the field-of-view of any other instruments,the evaporation of primordial black holes, or some as yet undiscoveredphenomenon. We have begun to search the Milagrito data set for bursts ofduration 10 seconds. Here we will present the technique and the expectedresults. Final results will be presented at the conference.
Published: 1999

20. Detection of 6 November 1997 Ground Level Event by Milagrito

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: Solar Energetic Particles from the 6 November 1997 solar flare/CME(coronalmass ejection) with energies exceeding 10 GeV have been detected by Milagrito,a prototype of the Milagro Gamma Ray Observatory. While particle accelerationbeyond 1 GeV at the Sun is well established, few data exist for protons or ionsbeyond 10 GeV. The Milagro observatory, a ground based water Cherenkov detectordesigned for observing very high energy gamma ray sources, can also be used tostudy the Sun. Milagrito, which operated for approximately one year in 1997/98,was sensitive to solar proton and neutron fluxes above ~5- 10 GeV. Milagritooperated in a scaler mode, which was primarily sensitive to muons, low energyphotons, and electrons, and the detector operated in a mode sensitive toshowers and high zenith angle muons. In its scaler mode, Milagrito registered arate increase coincident with the 6 November 1997 ground level event observedby Climax and other neutron monitors. A preliminary analysis suggests thepresence of >10 GeV particles.
Published: 1999

21. Milagrito Detection of TeV Emission from Mrk 501

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: The Milagro water Cherenkov detector near Los Alamos, New Mexico, has beenoperated as a sky monitor at energies of a few TeV between February 1997 andApril 1998. Serving as a test run for the full Milagro detector, Milagrito hastaken data during the strong and long-lasting 1997 flare of Mrk 501. We presentresults from the analysis of Mrk 501 and compare the excess and backgroundrates with expectations from the detector simulations.
Published: 1999

22. Search for a TeV Component of GRBs using the Milagrito Detector

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: Observing gamma ray bursts (GRBs) in the TeV energy range can be extremelyvaluable in providing insight to GRB radiation mechanisms and in constrainingsource distances. The Milagrito detector was an air shower array which used thewater Cherenkov technique to search for TeV sources. Data from this detectorwas analyzed to look for a TeV component of GRBs coincident with low energy-rays detected by the BATSE instrument on the Compton Gamma Ray Observatory. Asample of 54 BATSE GRBs which were in the field of view of the Milagritodetector during its lifetime (February 1997 to May 1998) was used.
Published: 1999

23. An All-Sky Search for Steady VHE Gamma-Ray Sources

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Subjects: astro-ph
Abstract: The Milagrito water Cherenkov detector in the Jemez Mountains near LosAlamos, New Mexico took data from February 1997 to April 1998. Milagrito servedas a prototype for the larger Milagro detector, which has just begunoperations. Milagrito was the first large-aperture gamma-ray detector withsensitivity to gamma rays below 1 TeV. We report here on a search for steadyemission from point sources over most of the northern sky using data fromMilagrito.
Published: 1999

24. Direct Optimal Mapping for 21cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array

Author: Xu, Z, Hewitt, JN, Chen, KF, Kim, H, Dillon, JS, Kern, NS, Morales, MF, Hazelton, BJ, Byrne, R, Fagnoni, N, Acedo, EDL, Abdurashidova, Z, Adams, T, Aguirre, JE, Alexander, P, Ali, ZS, Baartman, R, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Dexter, M, Eksteen, N, Ely, J, Ewall-Wice, A, Fritz, R, Furlanetto, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hickish, J, Jacobs, DC, Julius, A, Kariseb, M, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, Plante, PL, Liu, A, Loots, A, Ma, YZ, Edward MacMahon, DH, Malan, L, Malgas, C, Malgas, K, Marero, B, Martinot, ZE, Mesinger, A, Molewa, M, Mosiane, T, Murray, SG, Neben, AR, Nikolic, B, Nuwegeld, H, Parsons, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Smith, C, Swarts, H, Thyagarajan, N, Wyngaarden, PVV, Williams, PKG, Zheng, H, Xu, Z [0000-0001-5112-2567], Hewitt, JN [0000-0002-4117-570X], Chen, KF [0000-0002-3839-0230], Dillon, JS [0000-0003-3336-9958], Kern, NS [0000-0002-8211-1892], Morales, MF [0000-0001-7694-4030], Hazelton, BJ [0000-0001-7532-645X], Byrne, R [0000-0003-4980-2736], Aguirre, JE [0000-0002-4810-666X], Beardsley, AP [0000-0001-9428-8233], Bernardi, G [0000-0002-0916-7443], Bowman, JD [0000-0002-8475-2036], Bradley, RF [0000-0003-1172-8331], Bull, P [0000-0001-5668-3101], Carilli, CL [0000-0001-6647-3861], DeBoer, DR [0000-0003-3197-2294], Ewall-Wice, A [0000-0002-0086-7363], Furlanetto, SR [0000-0002-0658-1243], Gorthi, D [0000-0002-0829-167X], Greig, B [0000-0002-4085-2094], Jacobs, DC [0000-0002-0917-2269], Kerrigan, J [0000-0002-1876-272X], Kittiwisit, P [0000-0003-0953-313X], Kohn, SA [0000-0001-6744-5328], Kolopanis, M [0000-0002-2950-2974], Lanman, A [0000-0003-2116-3573], Plante, PL [0000-0002-4693-0102], Liu, A [0000-0001-6876-0928], Ma, YZ [0000-0001-8108-0986], Mesinger, A [0000-0003-3374-1772], Murray, SG [0000-0003-3059-3823], Neben, AR [0000-0001-7776-7240], Parsons, AR [0000-0002-5400-8097], Patra, N [0000-0002-9457-1941], Pober, JC [0000-0002-3492-0433], Sims, P [0000-0002-2871-0413], Thyagarajan, N [0000-0003-1602-7868], Williams, PKG [0000-0003-3734-3587], Apollo - University of Cambridge Repository, Xu, Zhilei, Hewitt, Jacqueline N., Chen, Kai-Feng, Kim, Honggeun, Dillon, Joshua S., Kern, Nicholas S., Morales, Miguel F., Hazelton, Bryna J., Byrne, Ruby, Fagnoni, Nicola, de Lera Acedo, Eloy, Abdurashidova, Zara, Adams, Tyrone, Aguirre, James E., Alexander, Paul, Ali, Zaki S., Baartman, Rushelle, Balfour, Yanga, Beardsley, Adam P., Bernardi, Gianni, Billings, Tashalee S., Bowman, Judd D., Bradley, Richard F., Bull, Philip, Burba, Jacob, Carey, Steven, Carilli, Chris L., Cheng, Carina, Deboer, David R., Dexter, Matt, Eksteen, Nico, Ely, John, Ewall-Wice, Aaron, Fritz, Randall, Furlanetto, Steven R., Gale-Sides, Kingsley, Glendenning, Brian, Gorthi, Deepthi, Greig, Bradley, Grobbelaar, Jasper, Halday, Ziyaad, Hickish, Jack, Jacobs, Daniel C., Julius, Austin, Kariseb, Maccalvin, Kerrigan, Joshua, Kittiwisit, Piyanat, Kohn, Saul A., Kolopanis, Matthew, Lanman, Adam, La Plante, Paul, Liu, Adrian, Loots, Anita, Ma, Yin-Zhe, Harold Edward MacMahon, David, Malan, Lourence, Malgas, Cresshim, Malgas, Keith, Marero, Bradley, Martinot, Zachary E., Mesinger, ANDREI ALBERT, Molewa, Mathakane, Mosiane, Tshegofalang, Murray, Steven G., Neben, Abraham R., Nikolic, Bojan, Nuwegeld, Han, Parsons, Aaron R., Patra, Nipanjana, Pieterse, Samantha, Pober, Jonathan C., Razavi-Ghods, Nima, Robnett, Jame, Rosie, Kathryn, Sims, Peter, Smith, Craig, Swarts, Hilton, Thyagarajan, Nithyanandan, Van Van Wyngaarden, Pieter, Williams, Peter K. G., and Zheng, Haoxuan
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), model, maps, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic radio-emission, 5109 Space Sciences, power spectrum, calibration, 10 mhz, Settore FIS/05 - Astronomia e Astrofisica, 5101 Astronomical Sciences, Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), upper limit, 51 Physical Sciences, 5107 Particle and High Energy Physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Motivated by the desire for wide-field images with well-defined statistical properties for 21cm cosmology, we implement an optimal mapping pipeline that computes a maximum likelihood estimator for the sky using the interferometric measurement equation. We demonstrate this direct optimal mapping with data from the Hydrogen Epoch of Reionization (HERA) Phase I observations. After validating the pipeline with simulated data, we develop a maximum likelihood figure-of-merit for comparing four sky models at 166MHz with a bandwidth of 100kHz. The HERA data agree with the GLEAM catalogs to, 16 pages, 10 figures, 2 tables, published on ApJ
Published: 2022

25. Automated Detection of Antenna Malfunctions in Large-N Interferometers: A case study With the Hydrogen Epoch of Reionization Array

Author: Storer, D, Dillon, JS, Jacobs, DC, Morales, MF, Hazelton, BJ, Ewall-Wice, A, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Acedo, EL, Dexter, M, Dynes, S, Ely, J, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hewitt, JN, Hickish, J, Huang, T, Josaitis, A, Julius, A, Kariseb, M, Kern, NS, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Liu, A, Loots, A, MacMahon, D, Malan, L, Malgas, C, Martinot, ZE, Mesinger, A, Molewa, M, Mosiane, T, Murray, SG, Neben, AR, Nikolic, B, Nunhokee, CD, Parsons, AR, Pascua, R, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Riley, D, Robnett, J, Rosie, K, Santos, MG, Sims, P, Singh, S, Smith, C, Tan, J, Thyagarajan, N, Williams, PKG, Zheng, H, Storer, D, Dillon, JS, Jacobs, DC, Morales, MF, Hazelton, BJ, Ewall-Wice, A, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Acedo, EL, Dexter, M, Dynes, S, Ely, J, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hewitt, JN, Hickish, J, Huang, T, Josaitis, A, Julius, A, Kariseb, M, Kern, NS, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Liu, A, Loots, A, MacMahon, D, Malan, L, Malgas, C, Martinot, ZE, Mesinger, A, Molewa, M, Mosiane, T, Murray, SG, Neben, AR, Nikolic, B, Nunhokee, CD, Parsons, AR, Pascua, R, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Riley, D, Robnett, J, Rosie, K, Santos, MG, Sims, P, Singh, S, Smith, C, Tan, J, Thyagarajan, N, Williams, PKG, and Zheng, H
Abstract: We present a framework for identifying and flagging malfunctioning antennas in large radio interferometers. We outline two distinct categories of metrics designed to detect outliers along known failure modes of large arrays: cross‐correlation metrics, based on all antenna pairs, and auto‐correlation metrics, based solely on individual antennas. We define and motivate the statistical framework for all metrics used, and present tailored visualizations that aid us in clearly identifying new and existing systematics. We implement these techniques using data from 105 antennas in the Hydrogen Epoch of Reionization Array (HERA) as a case study. Finally, we provide a detailed algorithm for implementing these metrics as flagging tools on real data sets.
Published: 2022

26. A map of diffuse radio emission at 182 MHz to enhance epoch of reionization observations in the Southern hemisphere

Author: Byrne, R, Morales, MF, Hazelton, B, Sullivan, I, Barry, N, Lynch, C, Line, JLB, Jacobs, DC, Byrne, R, Morales, MF, Hazelton, B, Sullivan, I, Barry, N, Lynch, C, Line, JLB, and Jacobs, DC
Abstract: We present a broad-band map of polarized diffuse emission at 167–198 MHz developed from data from the Murchison Widefield Array (MWA). The map is designed to improve visibility simulation and precision calibration for 21 cm Epoch of Reionization (EoR) experiments. It covers a large swath – 11 000 sq. deg. – of the Southern hemisphere sky in all four Stokes parameters and captures emission on angular scales of 1–9°. The band-averaged diffuse structure is pre-dominantly unpolarized but has significant linearly polarized structure near RA = 0 h. We evaluate the accuracy of the map by combining it with the GLEAM catalogue and simulating an observation from the MWA, demonstrating that the accuracy of the short baselines (6.1–50 wavelengths) now approaches the accuracy of the longer baselines typically used for EoR calibration. We discuss how to use the map for visibility simulation for a variety of interferometric arrays. The map has potential to improve calibration accuracy for experiments such as the Hydrogen Epoch of Reionization Array and the forthcoming Square Kilometre Array as well as the MWA.
Published: 2022

27. Multi-frequency angular power spectrum of the 21 cm signal from the Epoch of Reionisation using the Murchison Widefield Array

Author: Trott, CM, Mondal, R, Mellema, G, Murray, SG, Greig, B, Line, JLB, Barry, N, Morales, MF, Trott, CM, Mondal, R, Mellema, G, Murray, SG, Greig, B, Line, JLB, Barry, N, and Morales, MF
Abstract: Context. The Multi-frequency Angular Power Spectrum (MAPS) is an alternative to spherically averaged power spectra, and computes local fluctuations in the angular power spectrum without need for line-of-sight spectral transform. Aims. We aimed to test different approaches to MAPS and treatment of the foreground contamination, and compare with the spherically averaged power spectrum, and the single-frequency angular power spectrum. Methods. We applied the MAPS to 110 h of data in z = 6.2-7.5 obtained for the Murchison Widefield Array Epoch of Reionisation experiment to compute the statistical power of 21 cm brightness temperature fluctuations. In the presence of bright foregrounds, a filter was applied to remove large-scale modes prior to MAPS application, significantly reducing MAPS power due to systematics. Results. The MAPS showed a contrast of 102-103 to a simulated 21 cm cosmological signal for spectral separations of 0-4 MHz after application of the filter, reflecting results for the spherically averaged power spectrum. The single-frequency angular power spectrum was also computed. At z = 7.5 and l = 200, we found an angular power of 53 mK2, exceeding a simulated cosmological signal power by a factor of one thousand. Residual spectral structure, inherent to the calibrated data, and not spectral leakage from large-scale modes, was the dominant source of systematic power bias. The single-frequency angular power spectrum yielded slightly poorer results compared with the spherically averaged power spectrum, having applied a spectral filter to reduce foregrounds. Exploration of other filters may improve this result, along with consideration of wider bandwidths.
Published: 2022

28. Design, construction and operation of the ProtoDUNE-SP Liquid Argon TPC

Author: Collaboration, DUNE, Abud, AA, Abi, B, Acciarri, R, Acero, MA, Adames, MR, Adamov, G, Adams, D, Adinolfi, M, Aduszkiewicz, A, Aguilar, J, Ahmad, Z, Ahmed, J, Ali-Mohammadzadeh, B, Alion, T, Allison, K, Monsalve, SA, Alrashed, M, Alt, C, Alton, A, Amedo, P, Anderson, J, Andreopoulos, C, Andreotti, M, Andrews, MP, Andrianala, F, Andringa, S, Anfimov, N, Ankowski, A, Antoniassi, M, Antonova, M, Antoshkin, A, Antusch, S, Aranda-Fernandez, A, Ariga, A, Arnold, LO, Arroyave, MA, Asaadi, J, Asquith, L, Aurisano, A, Aushev, V, Autiero, D, Ayala-Torres, M, Azfar, F, Back, A, Back, H, Back, JJ, Backhouse, C, Baesso, P, Bagaturia, I, Bagby, L, Balashov, N, Balasubramanian, S, Baldi, P, Baller, B, Bambah, B, Barao, F, Barenboim, G, Barker, GJ, Barkhouse, W, Barnes, C, Barr, G, Monarca, JB, Barros, A, Barros, N, Barrow, JL, Basharina-Freshville, A, Bashyal, A, Basque, V, Belchior, E, Battat, JBR, Battisti, F, Bay, F, Alba, JLB, Beacom, JF, Bechetoille, E, Behera, B, Bellantoni, L, Bellettini, G, Bellini, V, Beltramello, O, Belver, D, Benekos, N, Montiel, CB, Neves, FB, Berger, J, Berkman, S, Bernardini, P, Berner, RM, Berns, H, Bertolucci, S, Betancourt, M, Rodríguez, AB, Bevan, A, Bezerra, TJC, Bhattacharjee, M, Bhuller, S, Bhuyan, B, Biagi, S, Bian, J, Biassoni, M, Biery, K, Bilki, B, Bishai, M, Bitadze, A, Blake, A, Blaszczyk, FDM, Blazey, GC, Blucher, E, Boissevain, J, Bolognesi, S, Bolton, T, Bomben, L, Bonesini, M, Bongrand, M, Bonini, F, Booth, A, Booth, C, Boran, F, Bordoni, S, Borkum, A, Boschi, T, Bostan, N, Bour, P, Bourgeois, C, Boyd, SB, Boyden, D, Bracinik, J, Braga, D, Brailsford, D, Branca, A, Brandt, A, Bremer, J, Brew, C, Brianne, E, Brice, SJ, Brizzolari, C, Bromberg, C, Brooijmans, G, Brooke, J, Bross, A, Brunetti, G, Brunetti, M, Buchanan, N, Budd, H, Butorov, I, Cagnoli, I, Caiulo, D, Calabrese, R, Calafiura, P, Calcutt, J, Calin, M, Calvez, S, Calvo, E, Caminata, A, Campanelli, M, Cankocak, K, Caratelli, D, Carini, G, Carlus, B, Carneiro, MF, Carniti, P, Terrazas, IC, Carranza, H, Carroll, T, Casta, JF, Castillo, A, Castromonte, C, Catano-Mur, E, Cattadori, C, Cavalier, F, Cavanna, F, Centro, S, Cerati, G, Cervelli, A, Villanueva, AC, Chalifour, M, Chappell, A, Chardonnet, E, Charitonidis, N, Chatterjee, A, Chattopadhyay, S, Chen, H, Chen, K, Chen, M, Chen, Y, Chen, Z, Cheon, Y, Cherdack, D, Chi, C, Childress, S, Chiriacescu, A, Chisnall, G, Cho, K, Choate, S, Chokheli, D, Chong, PS, Choubey, S, Christensen, A, Christian, D, Christodoulou, G, Chukanov, A, Chung, M, Church, E, Cicero, V, Clarke, P, Coan, TE, Cocco, AG, Coelho, JAB, Conley, E, Conley, R, Conrad, JM, Convery, M, Copello, S, Corwin, L, Valentim, R, Cremaldi, L, Cremonesi, L, Crespo-Anadon, JI, Crisler, M, Cristaldo, E, Cross, R, Cudd, A, Cuesta, C, Cui, Y, Cussans, D, Dabrowski, M, Dalager, O, Motta, HD, Peres, LDS, David, C, David, Q, Davies, GS, Davini, S, Dawson, J, De, K, Almeida, RMD, Debbins, P, Bonis, ID, Decowski, MP, Gouvea, AD, Holanda, PCD, Astiz, ILDI, Deisting, A, Jong, PD, Delbart, A, Delepine, D, Delgado, M, Dell'Acqua, A, Lurgio, PD, Neto, JRTDM, DeMuth, DM, Dennis, S, Densham, C, Deptuch, GW, Roeck, AD, Romeri, VD, Souza, GD, Devi, R, Dharmapalan, R, Dias, M, Diaz, F, Diaz, JS, Domizio, SD, Giulio, LD, Ding, P, Noto, LD, Distefano, C, Diurba, R, Diwan, M, Djurcic, Z, Doering, D, Dolan, S, Dolek, F, Dolinski, MJ, Domine, L, Douglas, D, Douillet, D, Drake, G, Drielsma, F, Duarte, L, Duchesneau, D, Duffy, K, Dunne, P, Durkin, T, Duyang, H, Dvornikov, O, Dwyer, DA, Dyshkant, AS, Eads, M, Earle, A, Edmunds, D, Eisch, J, Emberger, L, Emery, S, Ereditato, A, Erjavec, T, Escobar, CO, Eurin, G, Evans, JJ, Ewart, E, Ezeribe, AC, Fahey, K, Falcone, A, Faní, M, Farnese, C, Farzan, Y, Fedoseev, D, Felix, J, Feng, Y, Fernandez-Martinez, E, Menendez, PF, Morales, MF, Ferraro, F, Fields, L, Filip, P, Filthaut, F, Fiorentini, A, Fiorini, M, Fitzpatrick, RS, Flanagan, W, Fleming, B, Flight, R, Forero, DV, Fowler, J, Fox, W, Franc, J, Francis, K, Franco, D, Freeman, J, Freestone, J, Fried, J, Friedland, A, Robayo, FF, Fuess, S, Furic, I, Furmanski, AP, Gabrielli, A, Gago, A, Gallagher, H, Gallas, A, Gallego-Ros, A, Gallice, N, Galymov, V, Gamberini, E, Gamble, T, Ganacim, F, Gandhi, R, Gandrajula, R, Gao, F, Gao, S, B, ACG, Garcia-Gamez, D, García-Peris, MA, Gardiner, S, Gastler, D, Gauvreau, J, Ge, G, Gelli, B, Gendotti, A, Gent, S, Ghorbani-Moghaddam, Z, Giammaria, P, Giammaria, T, Gibin, D, Gil-Botella, I, Gilligan, S, Girerd, C, Giri, AK, Gnani, D, Gogota, O, Gold, M, Gollapinni, S, Gollwitzer, K, Gomes, RA, Bermeo, LVG, Fajardo, LSG, Gonnella, F, Gonzalez-Cuevas, JA, Diaz, DG, Gonzalez-Lopez, M, Goodman, MC, Goodwin, O, Goswami, S, Gotti, C, Goudzovski, E, Grace, C, Graham, M, Gran, R, Granados, E, Granger, P, Grant, A, Grant, C, Gratieri, D, Green, P, Greenler, L, Greer, J, Grenard, J, Griffith, WC, Groh, M, Grudzinski, J, Grzelak, K, Gu, W, Guardincerri, E, Guarino, V, Guarise, M, Guenette, R, Guerard, E, Guerzoni, M, Guglielmi, A, Guo, B, Guthikonda, KK, Gutierrez, R, Guzowski, P, Guzzo, MM, Gwon, S, Ha, C, Habig, A, Hadavand, H, Haenni, R, Hahn, A, Haiston, J, Hamacher-Baumann, P, Hamernik, T, Hamilton, P, Han, J, Harris, DA, Hartnell, J, Harton, J, Hasegawa, T, Hasnip, C, Hatcher, R, Hatfield, KW, Hatzikoutelis, A, Hayes, C, Hayrapetyan, K, Hays, J, Hazen, E, He, M, Heavey, A, Heeger, KM, Heise, J, Hennessy, K, Henry, S, Morquecho, MAH, Herner, K, Hertel, L, Hewes, J, Higuera, A, Hill, T, Hillier, SJ, Himmel, A, Hirsch, LR, Ho, J, Hoff, J, Holin, A, Hoppe, E, Horton-Smith, GA, Hostert, M, Hourlier, A, Howard, B, Howell, R, Hristova, I, Hronek, MS, Huang, J, Hugon, J, Iles, G, Ilic, N, Iliescu, AM, Illingworth, R, Ingratta, G, Ioannisian, A, Isenhower, L, Itay, R, Izmaylov, A, Jackson, CM, Jain, V, James, E, Jang, W, Jargowsky, B, Jediny, F, Jena, D, Jeong, YS, Jesus-Valls, C, Ji, X, Jiang, L, Jimenez, S, Jipa, A, Johnson, R, Johnston, N, Jones, B, Jones, SB, Judah, M, Jung, CK, Junk, T, Jwa, Y, Kabirnezhad, M, Kaboth, A, Kadenko, I, Kalra, D, Kakorin, I, Kalitkina, A, Kamiya, F, Kaneshige, N, Karagiorgi, G, Karaman, G, Karcher, A, Karolak, M, Karyotakis, Y, Kasai, S, Kasetti, SP, Kashur, L, Kazaryan, N, Kearns, E, Keener, P, Kelly, KJ, Kemp, E, Kemularia, O, Ketchum, W, Kettell, SH, Khabibullin, M, Khotjantsev, A, Khvedelidze, A, Kim, D, King, B, Kirby, B, Kirby, M, Klein, J, Koehler, K, Koerner, LW, Kohn, S, Koller, PP, Kolupaeva, L, Korablev, D, Kordosky, M, Kosc, T, Kose, U, Kostelecky, VA, Kothekar, K, Krennrich, F, Kreslo, I, Kropp, W, Kudenko, Y, Kudryavtsev, VA, Kulagin, S, Kumar, J, Kumar, P, Kunze, P, Kuruppu, C, Kus, V, Kutter, T, Kvasnicka, J, Kwak, D, Lambert, A, Land, BJ, Lande, K, Lane, CE, Lang, K, Langford, T, Langstaff, M, Larkin, J, Lasorak, P, Last, D, Lastoria, C, Laundrie, A, Laurenti, G, Lawrence, A, Lazanu, I, LaZur, R, Lazzaroni, M, Le, T, Leardini, S, Learned, J, LeBrun, P, LeCompte, T, Lee, C, Lee, SY, Miotto, GL, Lehnert, R, Oliveira, MALD, Leitner, M, Lepin, LM, Li, L, Li, SW, Li, T, Li, Y, Liao, H, Lin, CS, Lin, Q, Lin, S, Ling, J, Lister, A, Littlejohn, BR, Liu, J, Lockwitz, S, Loew, T, Lokajicek, M, Lomidze, I, Long, K, Loo, K, Lord, T, LoSecco, JM, Louis, WC, Lu, X-G, Luk, KB, Luo, X, Luppi, E, Lurkin, N, Lux, T, Luzio, VP, MacFarlane, D, Machado, AA, Machado, P, Macias, CT, Macier, JR, Maddalena, A, Madera, A, Madigan, P, Magill, S, Mahn, K, Maio, A, Major, A, Maloney, JA, Mandrioli, G, Mandujano, RC, Maneira, J, Manenti, L, Manly, S, Mann, A, Manolopoulos, K, Plata, MM, Manyam, VN, Manzanillas, L, Marchan, M, Marchionni, A, Marciano, W, Marfatia, D, Mariani, C, Maricic, J, Marie, R, Marinho, F, Marino, AD, Marsden, D, Marshak, M, Marshall, CM, Marshall, J, Marteau, J, Martin-Albo, J, Martinez, N, Caicedo, DAM, Martynenko, S, Mascagna, V, Mason, K, Mastbaum, A, Masud, M, Matichard, F, Matsuno, S, Matthews, J, Mauger, C, Mauri, N, Mavrokoridis, K, Mawby, I, Mazza, R, Mazzacane, A, Mazzucato, E, McAskill, T, McCluskey, E, McConkey, N, McFarland, KS, McGrew, C, McNab, A, Mefodiev, A, Mehta, P, Melas, P, Mena, O, Menary, S, Mendez, H, Mendez, P, M, DP, Menegolli, A, Meng, G, Messier, MD, Metcalf, W, Mettler, T, Mewes, M, Meyer, H, Miao, T, Michna, G, Miedema, T, Mikola, V, Milincic, R, Miller, G, Miller, W, Mills, J, Milne, C, Mineev, O, Miranda, OG, Miryala, S, Mishra, CS, Mishra, SR, Mislivec, A, Mladenov, D, Mocioiu, I, Moffat, K, Moggi, N, Mohanta, R, Mohayai, TA, Mokhov, N, Molina, J, Bueno, LM, Montagna, E, Montanari, A, Montanari, C, Montanari, D, Zetina, LMM, Moon, J, Moon, SH, Mooney, M, Moor, AF, Moreno, D, Morris, C, Mossey, C, Motuk, E, Moura, CA, Mousseau, J, Mouster, G, Mu, W, Mualem, L, Mueller, J, Muether, M, Mufson, S, Muheim, F, Muir, A, Mulhearn, M, Munford, D, Muramatsu, H, Murphy, S, Musser, J, Nachtman, J, Nagu, S, Nalbandyan, M, Nandakumar, R, Naples, D, Narita, S, Nath, A, Navas-Nicolás, D, Navrer-Agasson, A, Nayak, N, Nebot-Guinot, M, Negishi, K, Nelson, JK, Nesbit, J, Nessi, M, Newbold, D, Newcomer, M, Newhart, D, Newton, H, Nichol, R, Nicolas-Arnaldos, F, Niner, E, Nishimura, K, Norman, A, Norrick, A, Northrop, R, Novella, P, Nowak, JA, Oberling, M, Ochoa-Ricoux, JP, Campo, AOD, Olivier, A, Olshevskiy, A, Onel, Y, Onishchuk, Y, Ott, J, Pagani, L, Pakvasa, S, Palacio, G, Palamara, O, Palestini, S, Paley, JM, Pallavicini, M, Palomares, C, Palomino-Gallo, JL, Vazquez, WP, Pantic, E, Paolone, V, Papadimitriou, V, Papaleo, R, Papanestis, A, Paramesvaran, S, Parke, S, Parozzi, E, Parsa, Z, Parvu, M, Pascoli, S, Pasqualini, L, Pasternak, J, Pater, J, Patrick, C, Patrizii, L, Patterson, RB, Patton, SJ, Patzak, T, Paudel, A, Paulos, B, Paulucci, L, Pavlovic, Z, Pawloski, G, Payne, D, Pec, V, Peeters, SJM, Pennacchio, E, Penzo, A, Peres, OLG, Perry, J, Pershey, D, Pessina, G, Petrillo, G, Petta, C, Petti, R, Piastra, F, Pickering, L, Pietropaolo, F, Plunkett, R, Poling, R, Pons, X, Poonthottathil, N, Poppi, F, Pordes, S, Porter, J, Potekhin, M, Potenza, R, Potukuchi, BVKS, Pozimski, J, Pozzato, M, Prakash, S, Prakash, T, Prest, M, Prince, S, Psihas, F, Pugnere, D, Qian, X, Bazetto, MCQ, Raaf, JL, Radeka, V, Rademacker, J, Radics, B, Rafique, A, Raguzin, E, Rai, M, Rajaoalisoa, M, Rakhno, I, Rakotonandrasana, A, Rakotondravohitra, L, Ramachers, YA, Rameika, R, Delgado, MAR, Ramson, B, Rappoldi, A, Raselli, G, Ratoff, P, Raut, S, Razakamiandra, RF, Rea, E, Real, JS, Rebel, B, Reggiani-Guzzo, M, Rehak, T, Reichenbacher, J, Reitzner, SD, Sfar, HR, Renshaw, A, Rescia, S, Resnati, F, Reynolds, A, Ribas, M, Riboldi, S, Riccio, C, Riccobene, G, Rice, LCJ, Ricol, J, Rigamonti, A, Rigaut, Y, Rivera, D, Robert, A, Rochester, L, Roda, M, Rodrigues, P, Alonso, MJR, Bonilla, ER, Rondon, JR, Villa, LAR, Rosauro-Alcaraz, S, Rosenberg, M, Rosier, P, Roskovec, B, Rossella, M, Rossi, M, Rout, J, Roy, P, Roy, S, Rubbia, A, Rubbia, C, Rubio, FC, Russell, B, Ruterbories, D, Rybnikov, A, Saa-Hernandez, A, Saakyan, R, Sacerdoti, S, Safford, T, Sahu, N, Sala, P, Samios, N, Samoylov, O, Sanchez, MC, Sandberg, V, Sanders, DA, Sankey, D, Santana, S, Santos-Maldonado, M, Saoulidou, N, Sapienza, P, Sarasty, C, Sarcevic, I, Savage, G, Savinov, V, Scaramelli, A, Scarff, A, Scarpelli, A, Schaffer, T, Schellman, H, Schifano, S, Schlabach, P, Schmitz, D, Scholberg, K, Schukraft, A, Segreto, E, Selyunin, A, Senise, CR, Sensenig, J, Seoane, M, Seong, I, Sergi, A, Sgalaberna, D, Shaevitz, MH, Shafaq, S, Shamma, M, Sharankova, R, Sharma, HR, Sharma, R, Kumar, R, Shaw, T, Shepherd-Themistocleous, C, Sheshukov, A, Shin, S, Shoemaker, I, Shooltz, D, Shrock, R, Siegel, H, Simard, L, Simon, F, Simos, N, Sinclair, J, Sinev, G, Singh, J, Singh, L, Singh, V, Sipos, R, Sippach, FW, Sirri, G, Sitraka, A, Siyeon, K, Skarpaas, K, Smith, A, Smith, E, Smith, P, Smolik, J, Smy, M, Snider, EL, Snopok, P, Snowden-Ifft, D, Nunes, MS, Sobel, H, Soderberg, M, Sokolov, S, Salinas, CJS, Soldner-Remböld, S, Soleti, SR, Solomey, N, Solovov, V, Sondheim, WE, Sorel, M, Sotnikov, A, Soto-Oton, J, Sousa, A, Soustruznik, K, Spagliardi, F, Spanu, M, Spitz, J, Spooner, NJC, Spurgeon, K, Staley, R, Stancari, M, Stanco, L, Stanley, R, Stein, R, Steiner, HM, Lisboa, AFS, Stewart, J, Stillwell, B, Stock, J, Stocker, F, Stokes, T, Strait, M, Strauss, T, Striganov, S, Stuart, A, Suarez, JG, Sullivan, H, Summers, D, Surdo, A, Susic, V, Suter, L, Sutera, CM, Svoboda, R, Szczerbinska, B, Szelc, AM, Tanaka, HA, Oregui, BT, Tapper, A, Tariq, S, Tatar, E, Tayloe, R, Teklu, AM, Tenti, M, Terao, K, Ternes, CA, Terranova, F, Testera, G, Thakore, T, Thea, A, Thompson, JL, Thorn, C, Timm, SC, Tishchenko, V, Todd, J, Tomassetti, L, Tonazzo, A, Torbunov, D, Torti, M, Tortola, M, Tortorici, F, Tosi, N, Totani, D, Toups, M, Touramanis, C, Travaglini, R, Trevor, J, Trilov, S, Trzaska, WH, Tsai, Y, Tsai, YT, Tsamalaidze, Z, Tsang, KV, Tsverava, N, Tufanli, S, Tull, C, Tyley, E, Tzanov, M, Uboldi, L, Uchida, MA, Urheim, J, Usher, T, Uzunyan, S, Vagins, MR, Vahle, P, Valdiviesso, GA, Valencia, E, Pia, V, Vallari, Z, Vallazza, E, Valle, JWF, Vallecorsa, S, Berg, RV, Water, RGVD, Varanini, F, Vargas, D, Varner, G, Vasel, J, Vasina, S, Vasseur, G, Vaughan, N, Vaziri, K, Ventura, S, Verdugo, A, Vergani, S, Vermeulen, MA, Verzocchi, M, Vicenzi, M, Souza, HVD, Vignoli, C, Vilela, C, Viren, B, Vrba, T, Wachala, T, Waldron, AV, Wallbank, M, Wallis, C, Wang, H, Wang, J, Wang, L, Wang, MHLS, Wang, Y, Warburton, K, Warner, D, Wascko, MO, Waters, D, Watson, A, Weatherly, P, Weber, A, Weber, M, Wei, H, Weinstein, A, Wenman, D, Wetstein, M, White, A, Whitehead, LH, Whittington, D, Wilking, MJ, Wilkinson, C, Williams, Z, Wilson, F, Wilson, RJ, Wisniewski, W, Wolcott, J, Wongjirad, T, Wood, A, Wood, K, Worcester, E, Worcester, M, Wret, C, Wu, W, Xiao, Y, Xie, F, Yandel, E, Yang, G, Yang, K, Yang, S, Yang, T, Yankelevich, A, Yershov, N, Yonehara, K, Young, T, Yu, B, Yu, H, Yu, J, Yuan, W, Zaki, R, Zalesak, J, Zambelli, L, Zamorano, B, Zani, A, Zazueta, L, Zeller, GP, Zennamo, J, Zeug, K, Zhang, C, Zhao, M, Zhivun, E, Zhu, G, Zilberman, P, Zimmerman, ED, Zito, M, Zucchelli, S, Zuklin, J, Zutshi, V, Zwaska, R, XENON (IHEF, IoP, FNWI), Other Research IHEF (IoP, FNWI), ATLAS (IHEF, IoP, FNWI), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), DUNE, UAM. Departamento de Física Teórica, A. Abed Abud, B. Abi, R. Acciarri, M.A. Acero, M.R. Adame, G. Adamov, D. Adam, M. Adinolfi, A. Aduszkiewicz, J. Aguilar, Z. Ahmad, J. Ahmed, B. Ali-Mohammadzadeh, T. Alion, K. Allison, S. Alonso Monsalve, M. Alrashed, C. Alt, A. Alton, P. Amedo, J. Anderson, C. Andreopoulo, M. Andreotti, M.P. Andrew, F. Andrianala, S. Andringa, N. Anfimov, A. Ankowski, M. Antoniassi, M. Antonova, A. Antoshkin, S. Antusch, A. Aranda-Fernandez, A. Ariga, L.O. Arnold, M.A. Arroyave, J. Asaadi, L. Asquith, A. Aurisano, V. Aushev, D. Autiero, M. Ayala-Torre, F. Azfar, A. Back, H. Back, J.J. Back, C. Backhouse, P. Baesso, I. Bagaturia, L. Bagby, N. Balashov, S. Balasubramanian, P. Baldi, B. Baller, B. Bambah, F. Barao, G. Barenboim, G.J. Barker, W. Barkhouse, C. Barne, G. Barr, J. Barranco Monarca, A. Barro, N. Barro, J.L. Barrow, A. Basharina-Freshville, A. Bashyal, V. Basque, E. Belchior, J.B.R. Battat, F. Battisti, F. Bay, J.L. Bazo Alba, J.F. Beacom, E. Bechetoille, B. Behera, L. Bellantoni, G. Bellettini, V. Bellini, O. Beltramello, D. Belver, N. Beneko, C. Benitez Montiel, F. Bento Neve, J. Berger, S. Berkman, P. Bernardini, R.M. Berner, H. Bern, S. Bertolucci, M. Betancourt, A. Betancur Rodr??guez, A. Bevan, T.J.C. Bezerra, M. Bhattacharjee, S. Bhuller, B. Bhuyan, S. Biagi, J. Bian, M. Biassoni, K. Biery, B. Bilki, M. Bishai, A. Bitadze, A. Blake, F.D.M. Blaszczyk, G.C. Blazey, E. Blucher, J. Boissevain, S. Bolognesi, T. Bolton, L. Bomben, M. Bonesini, M. Bongrand, F. Bonini, A. Booth, C. Booth, F. Boran, S. Bordoni, A. Borkum, T. Boschi, N. Bostan, P. Bour, C. Bourgeoi, S.B. Boyd, D. Boyden, J. Bracinik, D. Braga, D. Brailsford, A. Branca, A. Brandt, J. Bremer, C. Brew, E. Brianne, S.J. Brice, C. Brizzolari, C. Bromberg, G. Brooijman, J. Brooke, A. Bro, G. Brunetti, M. Brunetti, N. Buchanan, H. Budd, I. Butorov, I. Cagnoli, D. Caiulo, R. Calabrese, P. Calafiura, J. Calcutt, M. Calin, S. Calvez, E. Calvo, A. Caminata, M. Campanelli, K. Cankocak, D. Caratelli, G. Carini, B. Carlu, M.F. Carneiro, P. Carniti, I. Caro Terraza, H. Carranza, T. Carroll, J.F. Casta, A. Castillo, C. Castromonte, E. Catano-Mur, C. Cattadori, F. Cavalier, F. Cavanna, S. Centro, G. Cerati, A. Cervelli, A. Cervera Villanueva, M. Chalifour, A. Chappell, E. Chardonnet, N. Charitonidi, A. Chatterjee, S. Chattopadhyay, H. Chen, K. Chen, M. Chen, Y. Chen, Z. Chen, Y. Cheon, D. Cherdack, C. Chi, S. Childre, A. Chiriacescu, G. Chisnall, K. Cho, S. Choate, D. Chokheli, P.S. Chong, S. Choubey, A. Christensen, D. Christian, G. Christodoulou, A. Chukanov, M. Chung, E. Church, V. Cicero, P. Clarke, T.E. Coan, A.G. Cocco, J.A.B. Coelho, E. Conley, R. Conley, J.M. Conrad, M. Convery, S. Copello, L. Corwin, R. Valentim, L. Cremaldi, L. Cremonesi, J.I. Crespo-Anad??n, M. Crisler, E. Cristaldo, R. Cro, A. Cudd, C. Cuesta, Y. Cui, D. Cussan, M. Dabrowski, O. Dalager, H. da Motta, L. Da Silva Pere, C. David, Q. David, G.S. Davie, S. Davini, J. Dawson, K. De, R.M. De Almeida, P. Debbin, I. De Boni, M.P. Decowski, A. de Gouv??a, P.C. De Holanda, I.L. De Icaza Astiz, A. Deisting, P. De Jong, A. Delbart, D. Delepine, M. Delgado, A. Dell'Acqua, P. De Lurgio, J.R.T. de Mello Neto, D.M. DeMuth, S. Denni, C. Densham, G.W. Deptuch, A. De Roeck, V. De Romeri, G. De Souza, R. Devi, R. Dharmapalan, M. Dia, F. Diaz, J.S. D??az, S. Di Domizio, L. Di Giulio, P. Ding, L. Di Noto, C. Distefano, R. Diurba, M. Diwan, Z. Djurcic, D. Doering, S. Dolan, F. Dolek, M.J. Dolinski, L. Domine, D. Dougla, D. Douillet, G. Drake, F. Drielsma, L. Duarte, D. Duchesneau, K. Duffy, P. Dunne, T. Durkin, H. Duyang, O. Dvornikov, D.A. Dwyer, A.S. Dyshkant, M. Ead, A. Earle, D. Edmund, J. Eisch, L. Emberger, S. Emery, A. Ereditato, T. Erjavec, C.O. Escobar, G. Eurin, J.J. Evan, E. Ewart, A.C. Ezeribe, K. Fahey, A. Falcone, M. Fani', C. Farnese, Y. Farzan, D. Fedoseev, J. Felix, Y. Feng, E. Fernandez-Martinez, P. Fernandez Menendez, M. Fernandez Morale, F. Ferraro, L. Field, P. Filip, F. Filthaut, A. Fiorentini, M. Fiorini, R.S. Fitzpatrick, W. Flanagan, B. Fleming, R. Flight, D.V. Forero, J. Fowler, W. Fox, J. Franc, K. Franci, D. Franco, J. Freeman, J. Freestone, J. Fried, A. Friedland, F. Fuentes Robayo, S. Fue, I. Furic, A.P. Furmanski, A. Gabrielli, A. Gago, H. Gallagher, A. Galla, A. Gallego-Ro, N. Gallice, V. Galymov, E. Gamberini, T. Gamble, F. Ganacim, R. Gandhi, R. Gandrajula, F. Gao, S. Gao, A.C. Garcia B., D. Garcia-Gamez, M.??. Garc??a-Peri, S. Gardiner, D. Gastler, J. Gauvreau, G. Ge, B. Gelli, A. Gendotti, S. Gent, Z. Ghorbani-Moghaddam, P. Giammaria, T. Giammaria, D. Gibin, I. Gil-Botella, S. Gilligan, C. Girerd, A.K. Giri, D. Gnani, O. Gogota, M. Gold, S. Gollapinni, K. Gollwitzer, R.A. Gome, L.V. Gomez Bermeo, L.S. Gomez Fajardo, F. Gonnella, J.A. Gonzalez-Cueva, D. Gonzalez Diaz, M. Gonzalez-Lopez, M.C. Goodman, O. Goodwin, S. Goswami, C. Gotti, E. Goudzovski, C. Grace, M. Graham, R. Gran, E. Granado, P. Granger, A. Grant, C. Grant, D. Gratieri, P. Green, L. Greenler, J. Greer, J. Grenard, W.C. Griffith, M. Groh, J. Grudzinski, K. Grzelak, W. Gu, E. Guardincerri, V. Guarino, M. Guarise, R. Guenette, E. Guerard, M. Guerzoni, A. Guglielmi, B. Guo, K.K. Guthikonda, R. Gutierrez, P. Guzowski, M.M. Guzzo, S. Gwon, C. Ha, A. Habig, H. Hadavand, R. Haenni, A. Hahn, J. Haiston, P. Hamacher-Baumann, T. Hamernik, P. Hamilton, J. Han, D.A. Harri, J. Hartnell, J. Harton, T. Hasegawa, C. Hasnip, R. Hatcher, K.W. Hatfield, A. Hatzikouteli, C. Haye, K. Hayrapetyan, J. Hay, E. Hazen, M. He, A. Heavey, K.M. Heeger, J. Heise, K. Hennessy, S. Henry, M.A. Hernandez Morquecho, K. Herner, L. Hertel, J. Hewe, A. Higuera, T. Hill, S.J. Hillier, A. Himmel, L.R. Hirsch, J. Ho, J. Hoff, A. Holin, E. Hoppe, G.A. Horton-Smith, M. Hostert, A. Hourlier, B. Howard, R. Howell, I. Hristova, M.S. Hronek, J. Huang, J. Hugon, G. Ile, N. Ilic, A.M. Iliescu, R. Illingworth, G. Ingratta, A. Ioannisian, L. Isenhower, R. Itay, A. Izmaylov, C.M. Jackson, V. Jain, E. Jame, W. Jang, B. Jargowsky, F. Jediny, D. Jena, Y.S. Jeong, C. Jes??s-Vall, X. Ji, L. Jiang, S. Jim??nez, A. Jipa, R. Johnson, N. Johnston, B. Jone, S.B. Jone, M. Judah, C.K. Jung, T. Junk, Y. Jwa, M. Kabirnezhad, A. Kaboth, I. Kadenko, D. Kalra, I. Kakorin, A. Kalitkina, F. Kamiya, N. Kaneshige, G. Karagiorgi, G. Karaman, A. Karcher, M. Karolak, Y. Karyotaki, S. Kasai, S.P. Kasetti, L. Kashur, N. Kazaryan, E. Kearn, P. Keener, K.J. Kelly, E. Kemp, O. Kemularia, W. Ketchum, S.H. Kettell, M. Khabibullin, A. Khotjantsev, A. Khvedelidze, D. Kim, B. King, B. Kirby, M. Kirby, J. Klein, K. Koehler, L.W. Koerner, S. Kohn, P.P. Koller, L. Kolupaeva, D. Korablev, M. Kordosky, T. Kosc, U. Kose, V.A. Kosteleck??, K. Kothekar, F. Krennrich, I. Kreslo, W. Kropp, Y. Kudenko, V.A. Kudryavtsev, S. Kulagin, J. Kumar, P. Kumar, P. Kunze, C. Kuruppu, V. Ku, T. Kutter, J. Kvasnicka, D. Kwak, A. Lambert, B.J. Land, K. Lande, C.E. Lane, K. Lang, T. Langford, M. Langstaff, J. Larkin, P. Lasorak, D. Last, C. Lastoria, A. Laundrie, G. Laurenti, A. Lawrence, I. Lazanu, R. LaZur, M. Lazzaroni, T. Le, S. Leardini, J. Learned, P. LeBrun, T. LeCompte, C. Lee, S.Y. Lee, G. Lehmann Miotto, R. Lehnert, M.A. Leigui de Oliveira, M. Leitner, L.M. Lepin, L. Li, S.W. Li, T. Li, Y. Li, H. Liao, C.S. Lin, Q. Lin, S. Lin, J. Ling, A. Lister, B.R. Littlejohn, J. Liu, S. Lockwitz, T. Loew, M. Lokajicek, I. Lomidze, K. Long, K. Loo, T. Lord, J.M. LoSecco, W.C. Loui, X.-G. Lu, K.B. Luk, X. Luo, E. Luppi, N. Lurkin, T. Lux, V.P. Luzio, D. MacFarlane, A.A. Machado, P. Machado, C.T. Macia, J.R. Macier, A. Maddalena, A. Madera, P. Madigan, S. Magill, K. Mahn, A. Maio, A. Major, J.A. Maloney, G. Mandrioli, R.C. Mandujano, J. Maneira, L. Manenti, S. Manly, A. Mann, K. Manolopoulo, M. Manrique Plata, V.N. Manyam, L. Manzanilla, M. Marchan, A. Marchionni, W. Marciano, D. Marfatia, C. Mariani, J. Maricic, R. Marie, F. Marinho, A.D. Marino, D. Marsden, M. Marshak, C.M. Marshall, J. Marshall, J. 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H., Khabibullin, M., Khotjantsev, A., Khvedelidze, A., Kim, D., King, B., Kirby, B., Kirby, M., Klein, J., Koehler, K., Koerner, L. W., Kohn, S., Koller, P. P., Kolupaeva, L., Korablev, D., Kordosky, M., Kosc, T., Kose, U., Kostelecky, V. A., Kothekar, K., Krennrich, F., Kreslo, I., Kropp, W., Kudenko, Y., Kudryavtsev, V. A., Kulagin, S., Kumar, J., Kumar, P., Kunze, P., Kuruppu, C., Kus, V., Kutter, T., Kvasnicka, J., Kwak, D., Lambert, A., Land, B. J., Lande, K., Lane, C. E., Lang, K., Langford, T., Langstaff, M., Larkin, J., Lasorak, P., Last, D., Lastoria, C., Laundrie, A., Laurenti, G., Lawrence, A., Lazanu, I., Lazur, R., Lazzaroni, M., Le, T., Leardini, S., Learned, J., Lebrun, P., Lecompte, T., Lee, C., Lee, S. Y., Miotto, G. L., Lehnert, R., de Oliveira, M. A. L., Leitner, M., Lepin, L. M., Li, L., Li, S. W., Li, T., Li, Y., Liao, H., Lin, C. S., Lin, Q., Lin, S., Ling, J., Lister, A., Littlejohn, B. R., Liu, J., Lockwitz, S., Loew, T., Lokajicek, M., Lomidze, I., Long, K., Loo, K., Lord, T., Losecco, J. M., Louis, W. C., Lu, X. -G., Luk, K. B., Luo, X., Luppi, E., Lurkin, N., Lux, T., Luzio, V. P., Macfarlane, D., Machado, A. A., Machado, P., Macias, C. T., Macier, J. R., Maddalena, A., Madera, A., Madigan, P., Magill, S., Mahn, K., Maio, A., Major, A., Maloney, J. A., Mandrioli, G., Mandujano, R. C., Maneira, J., Manenti, L., Manly, S., Mann, A., Manolopoulos, K., Plata, M. M., Manyam, V. N., Manzanillas, L., Marchan, M., Marchionni, A., Marciano, W., Marfatia, D., Mariani, C., Maricic, J., Marie, R., Marinho, F., Marino, A. D., Marsden, D., Marshak, M., Marshall, C. M., Marshall, J., Marteau, J., Martin-Albo, J., Martinez, N., Caicedo, D. A. M., Martynenko, S., Mascagna, V., Mason, K., Mastbaum, A., Masud, M., Matichard, F., Matsuno, S., Matthews, J., Mauger, C., Mauri, N., Mavrokoridis, K., Mawby, I., Mazza, R., Mazzacane, A., Mazzucato, E., Mcaskill, T., Mccluskey, E., Mcconkey, N., Mcfarland, K. S., Mcgrew, C., Mcnab, A., Mefodiev, A., Mehta, P., Melas, P., Mena, O., Menary, S., Mendez, H., Mendez, P., Menegolli, A., Meng, G., Messier, M. D., Metcalf, W., Mettler, T., Mewes, M., Meyer, H., Miao, T., Michna, G., Miedema, T., Mikola, V., Milincic, R., Miller, G., Miller, W., Mills, J., Milne, C., Mineev, O., Miranda, O. G., Miryala, S., Mishra, C. S., Mishra, S. R., Mislivec, A., Mladenov, D., Mocioiu, I., Moffat, K., Moggi, N., Mohanta, R., Mohayai, T. A., Mokhov, N., Molina, J., Bueno, L. M., Montagna, E., Montanari, A., Montanari, C., Montanari, D., Zetina, L. M. M., Moon, J., Moon, S. H., Mooney, M., Moor, A. F., Moreno, D., Morris, C., Mossey, C., Motuk, E., Moura, C. A., Mousseau, J., Mouster, G., Mu, W., Mualem, L., Mueller, J., Muether, M., Mufson, S., Muheim, F., Muir, A., Mulhearn, M., Munford, D., Muramatsu, H., Murphy, S., Musser, J., Nachtman, J., Nagu, S., Nalbandyan, M., Nandakumar, R., Naples, D., Narita, S., Nath, A., Navas-Nicolas, D., Navrer-Agasson, A., Nayak, N., Nebot-Guinot, M., Negishi, K., Nelson, J. K., Nesbit, J., Nessi, M., Newbold, D., Newcomer, M., Newhart, D., Newton, H., Nichol, R., Nicolas-Arnaldos, F., Niner, E., Nishimura, K., Norman, A., Norrick, A., Northrop, R., Novella, P., Nowak, J. A., Oberling, M., Ochoa-Ricoux, J. P., Del Campo, A. O., Olivier, A., Olshevskiy, A., Onel, Y., Onishchuk, Y., Ott, J., Pagani, L., Pakvasa, S., Palacio, G., Palamara, O., Palestini, S., Paley, J. M., Pallavicini, M., Palomares, C., Palomino-Gallo, J. L., Vazquez, W. P., Pantic, E., Paolone, V., Papadimitriou, V., Papaleo, R., Papanestis, A., Paramesvaran, S., Parke, S., Parozzi, E., Parsa, Z., Parvu, M., Pascoli, S., Pasqualini, L., Pasternak, J., Pater, J., Patrick, C., Patrizii, L., Patterson, R. B., Patton, S. J., Patzak, T., Paudel, A., Paulos, B., Paulucci, L., Pavlovic, Z., Pawloski, G., Payne, D., Pec, V., Peeters, S. J. M., Pennacchio, E., Penzo, A., Peres, O. L. G., Perry, J., Pershey, D., Pessina, G., Petrillo, G., Petta, C., Petti, R., Piastra, F., Pickering, L., Pietropaolo, F., Plunkett, R., Poling, R., Pons, X., Poonthottathil, N., Poppi, F., Pordes, S., Porter, J., Potekhin, M., Potenza, R., Potukuchi, B. V. K. S., Pozimski, J., Pozzato, M., Prakash, S., Prakash, T., Prest, M., Prince, S., Psihas, F., Pugnere, D., Qian, X., Bazetto, M. C. Q., Raaf, J. L., Radeka, V., Rademacker, J., Radics, B., Rafique, A., Raguzin, E., Rai, M., Rajaoalisoa, M., Rakhno, I., Rakotonandrasana, A., Rakotondravohitra, L., Ramachers, Y. A., Rameika, R., Delgado, M. A. R., Ramson, B., Rappoldi, A., Raselli, G., Ratoff, P., Raut, S., Razakamiandra, R. F., Rea, E., Real, J. S., Rebel, B., Reggiani-Guzzo, M., Rehak, T., Reichenbacher, J., Reitzner, S. D., Sfar, H. R., Renshaw, A., Rescia, S., Resnati, F., Reynolds, A., Ribas, M., Riboldi, S., Riccio, C., Riccobene, G., Rice, L. C. J., Ricol, J., Rigamonti, A., Rigaut, Y., Rivera, D., Robert, A., Rochester, L., Roda, M., Rodrigues, P., Alonso, M. J. R., Bonilla, E. R., Rondon, J. R., Villa, L. A. R., Rosauro-Alcaraz, S., Rosenberg, M., Rosier, P., Roskovec, B., Rossella, M., Rossi, M., Rout, J., Roy, P., Roy, S., Rubbia, A., Rubbia, C., Rubio, F. C., Russell, B., Ruterbories, D., Rybnikov, A., Saa-Hernandez, A., Saakyan, R., Sacerdoti, S., Safford, T., Sahu, N., Sala, P., Samios, N., Samoylov, O., Sanchez, M. C., Sandberg, V., Sanders, D. A., Sankey, D., Santana, S., Santos-Maldonado, M., Saoulidou, N., Sapienza, P., Sarasty, C., Sarcevic, I., Savage, G., Savinov, V., Scaramelli, A., Scarff, A., Scarpelli, A., Schaffer, T., Schellman, H., Schifano, S., Schlabach, P., Schmitz, D., Scholberg, K., Schukraft, A., Segreto, E., Selyunin, A., Senise, C. R., Sensenig, J., Seoane, M., Seong, I., Sergi, A., Sgalaberna, D., Shaevitz, M. H., Shafaq, S., Shamma, M., Sharankova, R., Sharma, H. R., Sharma, R., Kumar, R., Shaw, T., Shepherd-Themistocleous, C., Sheshukov, A., Shin, S., Shoemaker, I., Shooltz, D., Shrock, R., Siegel, H., Simard, L., Simon, F., Simos, N., Sinclair, J., Sinev, G., Singh, J., Singh, L., Singh, V., Sipos, R., Sippach, F. W., Sirri, G., Sitraka, A., Siyeon, K., Skarpaas, K., Smith, A., Smith, E., Smith, P., Smolik, J., Smy, M., Snider, E. L., Snopok, P., Snowden-Ifft, D., Nunes, M. S., Sobel, H., Soderberg, M., Sokolov, S., Salinas, C. J. S., Soldner-Rembold, S., Soleti, S. R., Solomey, N., Solovov, V., Sondheim, W. E., Sorel, M., Sotnikov, A., Soto-Oton, J., Sousa, A., Soustruznik, K., Spagliardi, F., Spanu, M., Spitz, J., Spooner, N. J. C., Spurgeon, K., Staley, R., Stancari, M., Stanco, L., Stanley, R., Stein, R., Steiner, H. M., Lisboa, A. F. S., Stewart, J., Stillwell, B., Stock, J., Stocker, F., Stokes, T., Strait, M., Strauss, T., Striganov, S., Stuart, A., Suarez, J. G., Sullivan, H., Summers, D., Surdo, A., Susic, V., Suter, L., Sutera, C. M., Svoboda, R., Szczerbinska, B., Szelc, A. M., Tanaka, H. A., Oregui, B. T., Tapper, A., Tariq, S., Tatar, E., Tayloe, R., Teklu, A. M., Tenti, M., Terao, K., Ternes, C. A., Terranova, F., Testera, G., Thakore, T., Thea, A., Thompson, J. L., Thorn, C., Timm, S. C., Tishchenko, V., Todd, J., Tomassetti, L., Tonazzo, A., Torbunov, D., Torti, M., Tortola, M., Tortorici, F., Tosi, N., Totani, D., Toups, M., Touramanis, C., Travaglini, R., Trevor, J., Trilov, S., Trzaska, W. H., Tsai, Y., Tsai, Y. -T., Tsamalaidze, Z., Tsang, K. V., Tsverava, N., Tufanli, S., Tull, C., Tyley, E., Tzanov, M., Uboldi, L., Uchida, M. A., Urheim, J., Usher, T., Uzunyan, S., Vagins, M. R., Vahle, P., Valdiviesso, G. A., Valencia, E., Pia, V., Vallari, Z., Vallazza, E., Valle, J. W. F., Vallecorsa, S., van Berg, R., van de Water, R. G., Varanini, F., Vargas, D., Varner, G., Vasel, J., Vasina, S., Vasseur, G., Vaughan, N., Vaziri, K., Ventura, S., Verdugo, A., Vergani, S., Vermeulen, M. A., Verzocchi, M., Vicenzi, M., de Souza, H. V., Vignoli, C., Vilela, C., Viren, B., Vrba, T., Wachala, T., Waldron, A. V., Wallbank, M., Wallis, C., Wang, H., Wang, J., Wang, L., Wang, M. H. L. S., Wang, Y., Warburton, K., Warner, D., Wascko, M. O., Waters, D., Watson, A., Weatherly, P., Weber, A., Weber, M., Wei, H., Weinstein, A., Wenman, D., Wetstein, M., White, A., Whitehead, L. H., Whittington, D., Wilking, M. J., Wilkinson, C., Williams, Z., Wilson, F., Wilson, R. J., Wisniewski, W., Wolcott, J., Wongjirad, T., Wood, A., Wood, K., Worcester, E., Worcester, M., Wret, C., Wu, W., Xiao, Y., Xie, F., Yandel, E., Yang, G., Yang, K., Yang, S., Yang, T., Yankelevich, A., Yershov, N., Yonehara, K., Young, T., Yu, B., Yu, H., Yu, J., Yuan, W., Zaki, R., Zalesak, J., Zambelli, L., Zamorano, B., Zani, A., Zazueta, L., Zeller, G. P., Zennamo, J., Zeug, K., Zhang, C., Zhao, M., Zhivun, E., Zhu, G., Zilberman, P., Zimmerman, E. D., Zito, M., Zucchelli, S., Zuklin, J., Zutshi, V., Zwaska, R., Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), UK Research and Innovation, Abud, A, Abi, B, Acciarri, R, Acero, M, Adames, M, Adamov, G, Adams, D, Adinolfi, M, Aduszkiewicz, A, Aguilar, J, Ahmad, Z, Ahmed, J, Ali-Mohammadzadeh, B, Alion, T, Allison, K, Monsalve, S, Alrashed, M, Alt, C, Alton, A, Amedo, P, Anderson, J, Andreopoulos, C, Andreotti, M, Andrews, M, Andrianala, F, Andringa, S, Anfimov, N, Ankowski, A, Antoniassi, M, Antonova, M, Antoshkin, A, Antusch, S, Aranda-Fernandez, A, Ariga, A, Arnold, L, Arroyave, M, Asaadi, J, Asquith, L, Aurisano, A, Aushev, V, Autiero, D, Ayala-Torres, M, Azfar, F, Back, A, Back, H, Back, J, Backhouse, C, Baesso, P, Bagaturia, I, Bagby, L, Balashov, N, Balasubramanian, S, Baldi, P, Baller, B, Bambah, B, Barao, F, Barenboim, G, Barker, G, Barkhouse, W, Barnes, C, Barr, G, Monarca, J, Barros, A, Barros, N, Barrow, J, Basharina-Freshville, A, Bashyal, A, Basque, V, Belchior, E, Battat, J, Battisti, F, Bay, F, Alba, J, Beacom, J, Bechetoille, E, Behera, B, Bellantoni, L, Bellettini, G, Bellini, V, Beltramello, O, Belver, D, Benekos, N, Montiel, C, Neves, F, Berger, J, Berkman, S, Bernardini, P, Berner, R, Berns, H, Bertolucci, S, Betancourt, M, Rodriguez, A, Bevan, A, Bezerra, T, Bhattacharjee, M, Bhuller, S, Bhuyan, B, Biagi, S, Bian, J, Biassoni, M, Biery, K, Bilki, B, Bishai, M, Bitadze, A, Blake, A, Blaszczyk, F, Blazey, G, Blucher, E, Boissevain, J, Bolognesi, S, Bolton, T, Bomben, L, Bonesini, M, Bongrand, M, Bonini, F, Booth, A, Booth, C, Boran, F, Bordoni, S, Borkum, A, Boschi, T, Bostan, N, Bour, P, Bourgeois, C, Boyd, S, Boyden, D, Bracinik, J, Braga, D, Brailsford, D, Branca, A, Brandt, A, Bremer, J, Brew, C, Brianne, E, Brice, S, Brizzolari, C, Bromberg, C, Brooijmans, G, Brooke, J, Bross, A, Brunetti, G, Brunetti, M, Buchanan, N, Budd, H, Butorov, I, Cagnoli, I, Caiulo, D, Calabrese, R, Calafiura, P, Calcutt, J, Calin, M, Calvez, S, Calvo, E, Caminata, A, Campanelli, M, Cankocak, K, Caratelli, D, Carini, G, Carlus, B, Carneiro, M, Carniti, P, Terrazas, I, Carranza, H, Carroll, T, Casta, J, Castillo, A, Castromonte, C, Catano-Mur, E, Cattadori, C, Cavalier, F, Cavanna, F, Centro, S, Cerati, G, Cervelli, A, Villanueva, A, Chalifour, M, Chappell, A, Chardonnet, E, Charitonidis, N, Chatterjee, A, Chattopadhyay, S, Chen, H, Chen, K, Chen, M, Chen, Y, Chen, Z, Cheon, Y, Cherdack, D, Chi, C, Childress, S, Chiriacescu, A, Chisnall, G, Cho, K, Choate, S, Chokheli, D, Chong, P, Choubey, S, Christensen, A, Christian, D, Christodoulou, G, Chukanov, A, Chung, M, Church, E, Cicero, V, Clarke, P, Coan, T, Cocco, A, Coelho, J, Conley, E, Conley, R, Conrad, J, Convery, M, Copello, S, Corwin, L, Valentim, R, Cremaldi, L, Cremonesi, L, Crespo-Anadon, J, Crisler, M, Cristaldo, E, Cross, R, Cudd, A, Cuesta, C, Cui, Y, Cussans, D, Dabrowski, M, Dalager, O, da Motta, H, da Silva Peres, L, David, C, David, Q, Davies, G, Davini, S, Dawson, J, De, K, de Almeida, R, Debbins, P, de Bonis, I, Decowski, M, de Gouvea, A, de Holanda, P, de Icaza Astiz, I, Deisting, A, de Jong, P, Delbart, A, Delepine, D, Delgado, M, Dell'Acqua, A, de Lurgio, P, de Mello Neto, J, Demuth, D, Dennis, S, Densham, C, Deptuch, G, de Roeck, A, de Romeri, V, de Souza, G, Devi, R, Dharmapalan, R, Dias, M, Diaz, F, Diaz, J, Di Domizio, S, Di Giulio, L, Ding, P, Di Noto, L, Distefano, C, Diurba, R, Diwan, M, Djurcic, Z, Doering, D, Dolan, S, Dolek, F, Dolinski, M, Domine, L, Douglas, D, Douillet, D, Drake, G, Drielsma, F, Duarte, L, Duchesneau, D, Duffy, K, Dunne, P, Durkin, T, Duyang, H, Dvornikov, O, Dwyer, D, Dyshkant, A, Eads, M, Earle, A, Edmunds, D, Eisch, J, Emberger, L, Emery, S, Ereditato, A, Erjavec, T, Escobar, C, Eurin, G, Evans, J, Ewart, E, Ezeribe, A, Fahey, K, Falcone, A, Fani, M, Farnese, C, Farzan, Y, Fedoseev, D, Felix, J, Feng, Y, Fernandez-Martinez, E, Menendez, P, Morales, M, Ferraro, F, Fields, L, Filip, P, Filthaut, F, Fiorentini, A, Fiorini, M, Fitzpatrick, R, Flanagan, W, Fleming, B, Flight, R, Forero, D, Fowler, J, Fox, W, Franc, J, Francis, K, Franco, D, Freeman, J, Freestone, J, Fried, J, Friedland, A, Robayo, F, Fuess, S, Furic, I, Furmanski, A, Gabrielli, A, Gago, A, Gallagher, H, Gallas, A, Gallego-Ros, A, Gallice, N, Galymov, V, Gamberini, E, Gamble, T, Ganacim, F, Gandhi, R, Gandrajula, R, Gao, F, Gao, S, Garcia, A, Garcia-Gamez, D, Garcia-Peris, M, Gardiner, S, Gastler, D, Gauvreau, J, Ge, G, Gelli, B, Gendotti, A, Gent, S, Ghorbani-Moghaddam, Z, Giammaria, P, Giammaria, T, Gibin, D, Gil-Botella, I, Gilligan, S, Girerd, C, Giri, A, Gnani, D, Gogota, O, Gold, M, Gollapinni, S, Gollwitzer, K, Gomes, R, Bermeo, L, Fajardo, L, Gonnella, F, Gonzalez-Cuevas, J, Diaz, D, Gonzalez-Lopez, M, Goodman, M, Goodwin, O, Goswami, S, Gotti, C, Goudzovski, E, Grace, C, Graham, M, Gran, R, Granados, E, Granger, P, Grant, A, Grant, C, Gratieri, D, Green, P, Greenler, L, Greer, J, Grenard, J, Griffith, W, Groh, M, Grudzinski, J, Grzelak, K, Gu, W, Guardincerri, E, Guarino, V, Guarise, M, Guenette, R, Guerard, E, Guerzoni, M, Guglielmi, A, Guo, B, Guthikonda, K, Gutierrez, R, Guzowski, P, Guzzo, M, Gwon, S, Ha, C, Habig, A, Hadavand, H, Haenni, R, Hahn, A, Haiston, J, Hamacher-Baumann, P, Hamernik, T, Hamilton, P, Han, J, Harris, D, Hartnell, J, Harton, J, Hasegawa, T, Hasnip, C, Hatcher, R, Hatfield, K, Hatzikoutelis, A, Hayes, C, Hayrapetyan, K, Hays, J, Hazen, E, He, M, Heavey, A, Heeger, K, Heise, J, Hennessy, K, Henry, S, Morquecho, M, Herner, K, Hertel, L, Hewes, J, Higuera, A, Hill, T, Hillier, S, Himmel, A, Hirsch, L, Ho, J, Hoff, J, Holin, A, Hoppe, E, Horton-Smith, G, Hostert, M, Hourlier, A, Howard, B, Howell, R, Hristova, I, Hronek, M, Huang, J, Hugon, J, Iles, G, Ilic, N, Iliescu, A, Illingworth, R, Ingratta, G, Ioannisian, A, Isenhower, L, Itay, R, Izmaylov, A, Jackson, C, Jain, V, James, E, Jang, W, Jargowsky, B, Jediny, F, Jena, D, Jeong, Y, Jesus-Valls, C, Ji, X, Jiang, L, Jimenez, S, Jipa, A, Johnson, R, Johnston, N, Jones, B, Jones, S, Judah, M, Jung, C, Junk, T, Jwa, Y, Kabirnezhad, M, Kaboth, A, Kadenko, I, Kalra, D, Kakorin, I, Kalitkina, A, Kamiya, F, Kaneshige, N, Karagiorgi, G, Karaman, G, Karcher, A, Karolak, M, Karyotakis, Y, Kasai, S, Kasetti, S, Kashur, L, Kazaryan, N, Kearns, E, Keener, P, Kelly, K, Kemp, E, Kemularia, O, Ketchum, W, Kettell, S, Khabibullin, M, Khotjantsev, A, Khvedelidze, A, Kim, D, King, B, Kirby, B, Kirby, M, Klein, J, Koehler, K, Koerner, L, Kohn, S, Koller, P, Kolupaeva, L, Korablev, D, Kordosky, M, Kosc, T, Kose, U, Kostelecky, V, Kothekar, K, Krennrich, F, Kreslo, I, Kropp, W, Kudenko, Y, Kudryavtsev, V, Kulagin, S, Kumar, J, Kumar, P, Kunze, P, Kuruppu, C, Kus, V, Kutter, T, Kvasnicka, J, Kwak, D, Lambert, A, Land, B, Lande, K, Lane, C, Lang, K, Langford, T, Langstaff, M, Larkin, J, Lasorak, P, Last, D, Lastoria, C, Laundrie, A, Laurenti, G, Lawrence, A, Lazanu, I, Lazur, R, Lazzaroni, M, Le, T, Leardini, S, Learned, J, Lebrun, P, Lecompte, T, Lee, C, Lee, S, Miotto, G, Lehnert, R, de Oliveira, M, Leitner, M, Lepin, L, Li, L, Li, S, Li, T, Li, Y, Liao, H, Lin, C, Lin, Q, Lin, S, Ling, J, Lister, A, Littlejohn, B, Liu, J, Lockwitz, S, Loew, T, Lokajicek, M, Lomidze, I, Long, K, Loo, K, Lord, T, Losecco, J, Louis, W, Lu, X, Luk, K, Luo, X, Luppi, E, Lurkin, N, Lux, T, Luzio, V, Macfarlane, D, Machado, A, Machado, P, Macias, C, Macier, J, Maddalena, A, Madera, A, Madigan, P, Magill, S, Mahn, K, Maio, A, Major, A, Maloney, J, Mandrioli, G, Mandujano, R, Maneira, J, Manenti, L, Manly, S, Mann, A, Manolopoulos, K, Plata, M, Manyam, V, Manzanillas, L, Marchan, M, Marchionni, A, Marciano, W, Marfatia, D, Mariani, C, Maricic, J, Marie, R, Marinho, F, Marino, A, Marsden, D, Marshak, M, Marshall, C, Marshall, J, Marteau, J, Martin-Albo, J, Martinez, N, Caicedo, D, Martynenko, S, Mascagna, V, Mason, K, Mastbaum, A, Masud, M, Matichard, F, Matsuno, S, Matthews, J, Mauger, C, Mauri, N, Mavrokoridis, K, Mawby, I, Mazza, R, Mazzacane, A, Mazzucato, E, Mcaskill, T, Mccluskey, E, Mcconkey, N, Mcfarland, K, Mcgrew, C, Mcnab, A, Mefodiev, A, Mehta, P, Melas, P, Mena, O, Menary, S, Mendez, H, Mendez, P, Menegolli, A, Meng, G, Messier, M, Metcalf, W, Mettler, T, Mewes, M, Meyer, H, Miao, T, Michna, G, Miedema, T, Mikola, V, Milincic, R, Miller, G, Miller, W, Mills, J, Milne, C, Mineev, O, Miranda, O, Miryala, S, Mishra, C, Mishra, S, Mislivec, A, Mladenov, D, Mocioiu, I, Moffat, K, Moggi, N, Mohanta, R, Mohayai, T, Mokhov, N, Molina, J, Bueno, L, Montagna, E, Montanari, A, Montanari, C, Montanari, D, Zetina, L, Moon, J, Moon, S, Mooney, M, Moor, A, Moreno, D, Morris, C, Mossey, C, Motuk, E, Moura, C, Mousseau, J, Mouster, G, Mu, W, Mualem, L, Mueller, J, Muether, M, Mufson, S, Muheim, F, Muir, A, Mulhearn, M, Munford, D, Muramatsu, H, Murphy, S, Musser, J, Nachtman, J, Nagu, S, Nalbandyan, M, Nandakumar, R, Naples, D, Narita, S, Nath, A, Navas-Nicolas, D, Navrer-Agasson, A, Nayak, N, Nebot-Guinot, M, Negishi, K, Nelson, J, Nesbit, J, Nessi, M, Newbold, D, Newcomer, M, Newhart, D, Newton, H, Nichol, R, Nicolas-Arnaldos, F, Niner, E, Nishimura, K, Norman, A, Norrick, A, Northrop, R, Novella, P, Nowak, J, Oberling, M, Ochoa-Ricoux, J, Del Campo, A, Olivier, A, Olshevskiy, A, Onel, Y, Onishchuk, Y, Ott, J, Pagani, L, Pakvasa, S, Palacio, G, Palamara, O, Palestini, S, Paley, J, Pallavicini, M, Palomares, C, Palomino-Gallo, J, Vazquez, W, Pantic, E, Paolone, V, Papadimitriou, V, Papaleo, R, Papanestis, A, Paramesvaran, S, Parke, S, Parozzi, E, Parsa, Z, Parvu, M, Pascoli, S, Pasqualini, L, Pasternak, J, Pater, J, Patrick, C, Patrizii, L, Patterson, R, Patton, S, Patzak, T, Paudel, A, Paulos, B, Paulucci, L, Pavlovic, Z, Pawloski, G, Payne, D, Pec, V, Peeters, S, Pennacchio, E, Penzo, A, Peres, O, Perry, J, Pershey, D, Pessina, G, Petrillo, G, Petta, C, Petti, R, Piastra, F, Pickering, L, Pietropaolo, F, Plunkett, R, Poling, R, Pons, X, Poonthottathil, N, Poppi, F, Pordes, S, Porter, J, Potekhin, M, Potenza, R, Potukuchi, B, Pozimski, J, Pozzato, M, Prakash, S, Prakash, T, Prest, M, Prince, S, Psihas, F, Pugnere, D, Qian, X, Bazetto, M, Raaf, J, Radeka, V, Rademacker, J, Radics, B, Rafique, A, Raguzin, E, Rai, M, Rajaoalisoa, M, Rakhno, I, Rakotonandrasana, A, Rakotondravohitra, L, Ramachers, Y, Rameika, R, Ramson, B, Rappoldi, A, Raselli, G, Ratoff, P, Raut, S, Razakamiandra, R, Rea, E, Real, J, Rebel, B, Reggiani-Guzzo, M, Rehak, T, Reichenbacher, J, Reitzner, S, Sfar, H, Renshaw, A, Rescia, S, Resnati, F, Reynolds, A, Ribas, M, Riboldi, S, Riccio, C, Riccobene, G, Rice, L, Ricol, J, Rigamonti, A, Rigaut, Y, Rivera, D, Robert, A, Rochester, L, Roda, M, Rodrigues, P, Alonso, M, Bonilla, E, Rondon, J, Villa, L, Rosauro-Alcaraz, S, Rosenberg, M, Rosier, P, Roskovec, B, Rossella, M, Rossi, M, Rout, J, Roy, P, Roy, S, Rubbia, A, Rubbia, C, Rubio, F, Russell, B, Ruterbories, D, Rybnikov, A, Saa-Hernandez, A, Saakyan, R, Sacerdoti, S, Safford, T, Sahu, N, Sala, P, Samios, N, Samoylov, O, Sanchez, M, Sandberg, V, Sanders, D, Sankey, D, Santana, S, Santos-Maldonado, M, Saoulidou, N, Sapienza, P, Sarasty, C, Sarcevic, I, Savage, G, Savinov, V, Scaramelli, A, Scarff, A, Scarpelli, A, Schaffer, T, Schellman, H, Schifano, S, Schlabach, P, Schmitz, D, Scholberg, K, Schukraft, A, Segreto, E, Selyunin, A, Senise, C, Sensenig, J, Seoane, M, Seong, I, Sergi, A, Sgalaberna, D, Shaevitz, M, Shafaq, S, Shamma, M, Sharankova, R, Sharma, H, Sharma, R, Kumar, R, Shaw, T, Shepherd-Themistocleous, C, Sheshukov, A, Shin, S, Shoemaker, I, Shooltz, D, Shrock, R, Siegel, H, Simard, L, Simon, F, Simos, N, Sinclair, J, Sinev, G, Singh, J, Singh, L, Singh, V, Sipos, R, Sippach, F, Sirri, G, Sitraka, A, Siyeon, K, Skarpaas, K, Smith, A, Smith, E, Smith, P, Smolik, J, Smy, M, Snider, E, Snopok, P, Snowden-Ifft, D, Nunes, M, Sobel, H, Soderberg, M, Sokolov, S, Salinas, C, Soldner-Rembold, S, Soleti, S, Solomey, N, Solovov, V, Sondheim, W, Sorel, M, Sotnikov, A, Soto-Oton, J, Sousa, A, Soustruznik, K, Spagliardi, F, Spanu, M, Spitz, J, Spooner, N, Spurgeon, K, Staley, R, Stancari, M, Stanco, L, Stanley, R, Stein, R, Steiner, H, Lisboa, A, Stewart, J, Stillwell, B, Stock, J, Stocker, F, Stokes, T, Strait, M, Strauss, T, Striganov, S, Stuart, A, Suarez, J, Sullivan, H, Summers, D, Surdo, A, Susic, V, Suter, L, Sutera, C, Svoboda, R, Szczerbinska, B, Szelc, A, Tanaka, H, Oregui, B, Tapper, A, Tariq, S, Tatar, E, Tayloe, R, Teklu, A, Tenti, M, Terao, K, Ternes, C, Terranova, F, Testera, G, Thakore, T, Thea, A, Thompson, J, Thorn, C, Timm, S, Tishchenko, V, Todd, J, Tomassetti, L, Tonazzo, A, Torbunov, D, Torti, M, Tortola, M, Tortorici, F, Tosi, N, Totani, D, Toups, M, Touramanis, C, Travaglini, R, Trevor, J, Trilov, S, Trzaska, W, Tsai, Y, Tsamalaidze, Z, Tsang, K, Tsverava, N, Tufanli, S, Tull, C, Tyley, E, Tzanov, M, Uboldi, L, Uchida, M, Urheim, J, Usher, T, Uzunyan, S, Vagins, M, Vahle, P, Valdiviesso, G, Valencia, E, Pia, V, Vallari, Z, Vallazza, E, Valle, J, Vallecorsa, S, van Berg, R, van de Water, R, Varanini, F, Vargas, D, Varner, G, Vasel, J, Vasina, S, Vasseur, G, Vaughan, N, Vaziri, K, Ventura, S, Verdugo, A, Vergani, S, Vermeulen, M, Verzocchi, M, Vicenzi, M, de Souza, H, Vignoli, C, Vilela, C, Viren, B, Vrba, T, Wachala, T, Waldron, A, Wallbank, M, Wallis, C, Wang, H, Wang, J, Wang, L, Wang, M, Wang, Y, Warburton, K, Warner, D, Wascko, M, Waters, D, Watson, A, Weatherly, P, Weber, A, Weber, M, Wei, H, Weinstein, A, Wenman, D, Wetstein, M, White, A, Whitehead, L, Whittington, D, Wilking, M, Wilkinson, C, Williams, Z, Wilson, F, Wilson, R, Wisniewski, W, Wolcott, J, Wongjirad, T, Wood, A, Wood, K, Worcester, E, Worcester, M, Wret, C, Wu, W, Xiao, Y, Xie, F, Yandel, E, Yang, G, Yang, K, Yang, S, Yang, T, Yankelevich, A, Yershov, N, Yonehara, K, Young, T, Yu, B, Yu, H, Yu, J, Yuan, W, Zaki, R, Zalesak, J, Zambelli, L, Zamorano, B, Zani, A, Zazueta, L, Zeller, G, Zennamo, J, Zeug, K, Zhang, C, Zhao, M, Zhivun, E, Zhu, G, Zilberman, P, Zimmerman, E, Zito, M, Zucchelli, S, Zuklin, J, Zutshi, V, and Zwaska, R
Subjects: Technology, Physics - Instrumentation and Detectors, gas and liquid scintillators), Noble liquid detectors (scintillation, ionization, double-phase), 7. Clean energy, 01 natural sciences, 09 Engineering, High Energy Physics - Experiment, Visible and IR Photons (Solid-State) (PIN Diodes, APDs, Si-PMTs, G-APDs, CCDs, EBCCDs, EMCCDs, CMOS imagers, etc.), High Energy Physics - Experiment (hep-ex), Noble liquid detectors (scintillation, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], APDs, Detectors and Experimental Techniques, physics.ins-det, Instrumentation, Instruments & Instrumentation, Photon detectors for UV, QC, Mathematical Physics, 02 Physical Sciences, Scintillation and light emission processes (solid, EBCCDs, scintillation and light emission processes (solid, gas and liquid scintillators), irradiation, Photon detectors for UV, visible and IR photons (solid-state) (PIN diodes, APDs, Si-PMTs, G-APDs, CCDs, EBCCDs, EMCCDs, CMOS imagers, etc), Si-PMTs, Instrumentation and Detectors (physics.ins-det), Scintillators, scintillation and light emission processes (solid, gas and liquid scintillators), double-phase), Nuclear & Particles Physics, LIGHT, Scintillation and light emission processes (solid, gas, liquid scintillators), Scintillators, Time projection Chambers (TPC), Visible and IR photons (solid-state) (PIN diodes, APDs, Si-PMTs, G-APDs, CCDs, EBCCDs, EMCCDs, CMOS imagers, etc), G-APDs, Particle Physics - Experiment, performance, CERN Lab, FOS: Physical sciences, fabrication, Visible and IR photons (solid-state) (PIN diodes, gas, 0103 physical sciences, ionization, liquid scintillators), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], High Energy Physics, 010306 general physics, CMOS imagers, Noble Liquid Detectors (Scintillation, Ionization, Double-Phase), activity report, detector: design, etc), Science & Technology, DUNE, hep-ex, 010308 nuclear & particles physics, visible and IR photons (solid-state) (PIN diodes, APDs, Si-PMTs, G-APDs, CCDs, EBCCDs, EMCCDs, CMOS imagers, etc), Física, CCDs, Scintillator, time projection chamber: liquid argon, Scintillation and Light Emission Processes (Solid, Gas and Liquid Scintillators), Noble liquid detectors (scintillation, ionization, double-phase), Photon detectors for UV, Scintillation and light emission processes (solid, gas, liquid scintillators), Scintillators, Time projection Chambers (TPC), Visible and IR photons (solid-state) (PIN diodes, APDs, Si-PMTs, G-APDs, CCDs, EBCCDs, EMCCDs, CMOS imagers, etc), EMCCDs, Experimental High Energy Physics
Abstract: The ProtoDUNE-SP detector was constructed and operated on the CERN Neutrino Platform. We gratefully acknowledge the support of the CERN management, and the CERN EP, BE, TE, EN and IT Departments for NP04/ProtoDUNE-SP. This document was prepared by the DUNE collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, HEP User Facility. Fermilab is managed by Fermi Research Alliance, LLC (FRA), acting under Contract No. DE-AC02-07CH11359. This work was supported by CNPq, FAPERJ, FAPEG and FAPESP, Brazil; CFI, IPP and NSERC, Canada; CERN; MŠMT, Czech Republic; ERDF, H2020-EU and MSCA, European Union; CNRS/IN2P3 and CEA, France; INFN, Italy; FCT, Portugal; NRF, South Korea; CAM, Fundación “La Caixa”, Junta de Andalucía-FEDER, and MICINN, Spain; SERI and SNSF, Switzerland; TÜBİTAK, Turkey; The Royal Society and UKRI/STFC, United Kingdom; DOE and NSF, United States of America. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231., The ProtoDUNE-SP detector is a single-phase liquid argon time projection chamber (LArTPC) that was constructed and operated in the CERN North Area at the end of the H4 beamline. This detector is a prototype for the first far detector module of the Deep Underground Neutrino Experiment (DUNE), which will be constructed at the Sandford Underground Research Facility (SURF) in Lead, South Dakota, U.S.A. The ProtoDUNE-SP detector incorporates full-size components as designed for DUNE and has an active volume of 7 × 6 × 7.2 m3. The H4 beam delivers incident particles with well-measured momenta and high-purity particle identification. ProtoDUNE-SP's successful operation between 2018 and 2020 demonstrates the effectiveness of the single-phase far detector design. This paper describes the design, construction, assembly and operation of the detector components., Fermi Research Alliance, LLC DE-AC02-07CH11359, H2020-EU, National Science Foundation, U.S. Department of Energy DE-AC02-05CH11231, Office of Science, Fermilab, H2020 Marie Skłodowska-Curie Actions, CERN, UK Research and Innovation, Natural Sciences and Engineering Research Council of Canada, Science and Technology Facilities Council, Royal Society, European Commission, Singapore Eye Research Institute, Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, Fundação de Amparo à Pesquisa do Estado de São Paulo, Fundação para a Ciência e a Tecnologia, Conselho Nacional de Desenvolvimento Científico e Tecnológico, National Research Foundation of Korea, Instituto Nazionale di Fisica Nucleare, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Centre National de la Recherche Scientifique, Ministerio de Ciencia e Innovación, Fundação de Amparo à Pesquisa do Estado de Goiás, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, European Regional Development Fund, Junta de Andalucía, Institut National de Physique Nucléaire et de Physique des Particules
Published: 2022

29. Effects of model incompleteness on the drift-scan calibration of radio telescopes

Author: Gehlot, BK, Jacobs, DC, Bowman, JD, Mahesh, N, Murray, SG, Kolopanis, M, Beardsley, AP, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Bernardi, G, Billings, TS, Bradley, RF, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Dexter, M, Acedo, EDL, Dillon, JS, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Julius, A, Kern, NS, Kerrigan, J, Kittiwisit, P, Kohn, SA, Lanman, A, La Plante, P, Lekalake, T, Lewis, D, Liu, A, Ma, Y-Z, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Monsalve, RA, Morales, MF, Mosiane, T, Neben, AR, Nikolic, B, Parsons, AR, Pascua, R, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Santos, MG, Sims, P, Smith, C, Syce, A, Tegmark, M, Thyagarajan, N, Williams, PKG, Zheng, H, Gehlot, BK, Jacobs, DC, Bowman, JD, Mahesh, N, Murray, SG, Kolopanis, M, Beardsley, AP, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Bernardi, G, Billings, TS, Bradley, RF, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Dexter, M, Acedo, EDL, Dillon, JS, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Julius, A, Kern, NS, Kerrigan, J, Kittiwisit, P, Kohn, SA, Lanman, A, La Plante, P, Lekalake, T, Lewis, D, Liu, A, Ma, Y-Z, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Monsalve, RA, Morales, MF, Mosiane, T, Neben, AR, Nikolic, B, Parsons, AR, Pascua, R, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Santos, MG, Sims, P, Smith, C, Syce, A, Tegmark, M, Thyagarajan, N, Williams, PKG, and Zheng, H
Abstract: Precision calibration poses challenges to experiments probing the redshifted 21-cm signal of neutral hydrogen from the Cosmic Dawn and Epoch of Reionization (z ∼ 30–6). In both interferometric and global signal experiments, systematic calibration is the leading source of error. Though many aspects of calibration have been studied, the overlap between the two types of instruments has received less attention. We investigate the sky based calibration of total power measurements with a HERA dish and an EDGES-style antenna to understand the role of autocorrelations in the calibration of an interferometer and the role of sky in calibrating a total power instrument. Using simulations we study various scenarios such as time variable gain, incomplete sky calibration model, and primary beam model. We find that temporal gain drifts, sky model incompleteness, and beam inaccuracies cause biases in the receiver gain amplitude and the receiver temperature estimates. In some cases, these biases mix spectral structure between beam and sky resulting in spectrally variable gain errors. Applying the calibration method to the HERA and EDGES data, we find good agreement with calibration via the more standard methods. Although instrumental gains are consistent with beam and sky errors similar in scale to those simulated, the receiver temperatures show significant deviations from expected values. While we show that it is possible to partially mitigate biases due to model inaccuracies by incorporating a time-dependent gain model in calibration, the resulting errors on calibration products are larger and more correlated. Completely addressing these biases will require more accurate sky and primary beam models.
Published: 2021

30. A Real Time Processing system for big data in astronomy: Applications to HERA

Author: La Plante, P, Williams, PKG, Kolopanis, M, Dillon, JS, Beardsley, AP, Kern, NS, Wilensky, M, Ali, ZS, Abdurashidova, Z, Aguirre, JE, Alexander, P, Balfour, Y, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Dexter, M, Acedo, EDL, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kerrigan, J, Kittiwisit, P, Kohn, SA, Lanman, A, Lekalake, T, Lewis, D, Liu, A, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, S, Neben, AR, Nikolic, B, Parsons, AR, Pascua, R, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Santos, MG, Sims, P, Smith, C, Syce, A, Thyagarajan, N, Zheng, H, La Plante, P, Williams, PKG, Kolopanis, M, Dillon, JS, Beardsley, AP, Kern, NS, Wilensky, M, Ali, ZS, Abdurashidova, Z, Aguirre, JE, Alexander, P, Balfour, Y, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carey, S, Carilli, CL, Cheng, C, DeBoer, DR, Dexter, M, Acedo, EDL, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kerrigan, J, Kittiwisit, P, Kohn, SA, Lanman, A, Lekalake, T, Lewis, D, Liu, A, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, S, Neben, AR, Nikolic, B, Parsons, AR, Pascua, R, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Santos, MG, Sims, P, Smith, C, Syce, A, Thyagarajan, N, and Zheng, H
Published: 2021

31. Understanding the HERA Phase i receiver system with simulations and its impact on the detectability of the EoR delay power spectrum

Author: Fagnoni, N, De Lera Acedo, E, Deboer, DR, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Bernardi, G, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carilli, CL, Cheng, C, Dexter, M, Dillon, JS, Ewall-Wice, A, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Josaitis, A, Julius, A, Kern, NS, Kerrigan, J, Kim, H, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, Plante, PL, Lekalake, T, Liu, A, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mena Parra, J, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Neben, AR, Nikolic, B, Parsons, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Smith, C, Syce, A, Thyagarajan, N, Williams, PKG, Zheng, H, De Lera Acedo, Eloy [0000-0001-8530-6989], Alexander, Paul [0000-0002-0292-9513], Nikolic, Bojan [0000-0001-7168-2705], Razavi-Ghods, Nima [0000-0003-2930-5396], and Apollo - University of Cambridge Repository
Subjects: interferometers [instrumentation], first stars, Astrophysics::Instrumentation and Methods for Astrophysics, numerical [methods], telescopes, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, interferometric [techniques], methods: numerical, dark ages, reionization, techniques: interferometric, reionization, dark ages, instrumentation: interferometers, Astronomical and Space Sciences, astro-ph.IM
Abstract: The detection of the Epoch of Reionization (EoR) delay power spectrum using a "foreground avoidance method" highly depends on the instrument chromaticity. The systematic effects induced by the radio-telescope spread the foreground signal in the delay domain, which contaminates the EoR window theoretically observable. Applied to the Hydrogen Epoch of Reionization Array (HERA), this paper combines detailed electromagnetic and electrical simulations in order to model the chromatic effects of the instrument, and quantify its frequency and time responses. In particular, the effects of the analogue receiver, transmission cables, and mutual coupling are included. These simulations are able to accurately predict the intensity of the reflections occurring in the 150-m cable which links the antenna to the back-end. They also show that electromagnetic waves can propagate from one dish to another one through large sections of the array due to mutual coupling. The simulated system time response is attenuated by a factor $10^{4}$ after a characteristic delay which depends on the size of the array and on the antenna position. Ultimately, the system response is attenuated by a factor $10^{5}$ after 1400 ns because of the reflections in the cable, which corresponds to characterizable ${k_\parallel}$-modes above 0.7 $h\;\rm{Mpc}^{-1}$ at 150 MHz. Thus, this new study shows that the detection of the EoR signal with HERA Phase I will be more challenging than expected. On the other hand, it improves our understanding of the telescope, which is essential to mitigate the instrument chromaticity.
Published: 2020
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32. Imaging and Modeling Data from the Hydrogen Epoch of Reionization Array

Author: Carilli, CL, Thyagarajan, N, Kent, J, Nikolic, B, Gale-Sides, K, Kern, NS, Bernardi, G, Mesinger, A, Matika, S, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Cheng, C, Deboer, DR, Dexter, M, Acedo, EDL, Dillon, JS, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Josaitis, A, Julius, A, Kerrigan, J, Kim, H, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, Plante, PL, Lekalake, T, Liu, A, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Molewa, M, Morales, MF, Mosiane, T, Neben, AR, Parra, JM, Parsons, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Syce, A, Williams, PKG, Zheng, H, Carilli, CL, Thyagarajan, N, Kent, J, Nikolic, B, Gale-Sides, K, Kern, NS, Bernardi, G, Mesinger, A, Matika, S, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Cheng, C, Deboer, DR, Dexter, M, Acedo, EDL, Dillon, JS, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Josaitis, A, Julius, A, Kerrigan, J, Kim, H, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, Plante, PL, Lekalake, T, Liu, A, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Molewa, M, Morales, MF, Mosiane, T, Neben, AR, Parra, JM, Parsons, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Robnett, J, Rosie, K, Sims, P, Syce, A, Williams, PKG, and Zheng, H
Abstract: We analyze data from the Hydrogen Epoch of Reionization Array (HERA). This is the third in a series of papers on the closure phase delay spectrum technique designed to detect the H i 21 cm emission from cosmic reionization. We present the details of the data and models employed in the power spectral analysis and discuss limitations to the process. We compare images and visibility spectra made with HERA data to parallel quantities generated from sky models based on the Galactic and Extra-Galactic All-Sky MWA (GLEAM) survey, incorporating the HERA telescope model. We find reasonable agreement between images made from HERA data with those generated from the models, down to the confusion level. For the visibility spectra, there is broad agreement between model and data across the full band of ∼80 MHz. However, models with only GLEAM sources do not reproduce a roughly sinusoidal spectral structure at the tens of percent level seen in the observed visibility spectra on scales of ∼10 MHz on 29 m baselines. We find that this structure is likely due to diffuse Galactic emission, predominantly the Galactic plane, filling the far sidelobes of the antenna primary beam. We show that our current knowledge of the frequency dependence of the diffuse sky radio emission, and the primary beam at large zenith angles, is inadequate to provide an accurate reproduction of the diffuse structure in the models. We discuss some implications arising due to this missing structure in the models, in terms of calibration, and in the search for the H i 21 cm signal, as well as possible mitigation techniques.
Published: 2020

33. Mitigating Internal Instrument Coupling for 21 cm Cosmology. II. A Method Demonstration with the Hydrogen Epoch of Reionization Array

Author: Kern, NS, Parsons, AR, Dillon, JS, Lanman, AE, Liu, A, Bull, P, Ewall-Wice, A, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Bernardi, G, Bowman, JD, Bradley, RF, Burba, J, Carilli, CL, Cheng, C, Deboer, DR, Dexter, M, De Lera Acedo, E, Fagnoni, N, Fritz, R, Furlanetto, SR, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, La Plante, P, Lekalake, T, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, SG, Neben, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sims, P, Smith, C, Syce, A, Thyagarajan, N, Williams, PKG, Zheng, H, Kern, NS, Parsons, AR, Dillon, JS, Lanman, AE, Liu, A, Bull, P, Ewall-Wice, A, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Bernardi, G, Bowman, JD, Bradley, RF, Burba, J, Carilli, CL, Cheng, C, Deboer, DR, Dexter, M, De Lera Acedo, E, Fagnoni, N, Fritz, R, Furlanetto, SR, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, La Plante, P, Lekalake, T, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, SG, Neben, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sims, P, Smith, C, Syce, A, Thyagarajan, N, Williams, PKG, and Zheng, H
Abstract: We present a study of internal reflection and cross-coupling systematics in Phase I of the Hydrogen Epoch of Reionization Array (HERA). In a companion paper, we outlined the mathematical formalism for such systematics and presented algorithms for modeling and removing them from the data. In this work, we apply these techniques to data from HERA's first observing season as a method demonstration. The data show evidence for systematics that, without removal, would hinder a detection of the 21 cm power spectrum for the targeted Epoch of Reionization (EoR) line-of-sight modes in the range 0.2 h Mpc < $" SRC="apjab5e8aieqn1.gif"/ < 0.5 h Mpc . In particular, we find evidence for nonnegligible amounts of spectral structure in the raw autocorrelations that overlaps with the EoR window and is suggestive of complex instrumental effects. Through systematic modeling on a single night of data, we find we can recover these modes in the power spectrum down to the integrated noise floor, achieving a dynamic range in the EoR window of 10 in power (mK units) with respect to the bright galactic foreground signal. Future work with deeper integrations will help determine whether these systematics can continue to be mitigated down to EoR levels. For future observing seasons, HERA will have upgraded analog and digital hardware to better control these systematics in the field. -1 -1 -1 -1 6 2
Published: 2020

34. Absolute Calibration Strategies for the Hydrogen Epoch of Reionization Array and Their Impact on the 21 cm Power Spectrum

Author: Kern, NS, Dillon, JS, Parsons, AR, Carilli, CL, Bernardi, G, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carey, S, Cheng, C, Deboer, DR, Dexter, M, De Lera Acedo, E, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Lekalake, T, Liu, A, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, SG, Neben, AR, Nikolic, B, Nunhokee, CD, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sims, P, Smith, C, Syce, A, Thyagarajan, N, Williams, PKG, Zheng, H, Kern, NS, Dillon, JS, Parsons, AR, Carilli, CL, Bernardi, G, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Billings, TS, Bowman, JD, Bradley, RF, Bull, P, Burba, J, Carey, S, Cheng, C, Deboer, DR, Dexter, M, De Lera Acedo, E, Ely, J, Ewall-Wice, A, Fagnoni, N, Fritz, R, Furlanetto, SR, Gale-Sides, K, Glendenning, B, Gorthi, D, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kerrigan, J, Kittiwisit, P, Kohn, SA, Kolopanis, M, Lanman, A, La Plante, P, Lekalake, T, Liu, A, Macmahon, D, Malan, L, Malgas, C, Maree, M, Martinot, ZE, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Mosiane, T, Murray, SG, Neben, AR, Nikolic, B, Nunhokee, CD, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sims, P, Smith, C, Syce, A, Thyagarajan, N, Williams, PKG, and Zheng, H
Abstract: We discuss absolute calibration strategies for Phase I of the Hydrogen Epoch of Reionization Array (HERA), which aims to measure the cosmological 21 cm signal from the Epoch of Reionization. HERA is a drift-scan array with a 10° wide field of view, meaning bright, well-characterized point-source transits are scarce. This, combined with HERA's redundant sampling of the uv plane and the modest angular resolution of the Phase I instrument, make traditional sky-based and self-calibration techniques difficult to implement with high dynamic range. Nonetheless, in this work, we demonstrate calibration for HERA using point-source catalogs and electromagnetic simulations of its primary beam. We show that unmodeled diffuse flux and instrumental contaminants can corrupt the gain solutions and present a gain-smoothing approach for mitigating their impact on the 21 cm power spectrum. We also demonstrate a hybrid sky and redundant calibration scheme and compare it to pure sky-based calibration, showing only a marginal improvement to the gain solutions at intermediate delay scales. Our work suggests that the HERA Phase I system can be well calibrated for a foreground avoidance power spectrum estimator by applying direction-independent gains with a small set of degrees of freedom across the frequency and time axes.
Published: 2020

35. H <scp>I</scp>21-cm Cosmology and the Bispectrum: Closure Diagnostics in Massively Redundant Interferometric Arrays

Author: Carilli, CL, Nikolic, B, Thyagarajan, N, Gale-Sides, K, Abdurashidova, Z, Aguirre, JE, Alexander, P, Ali, ZS, Balfour, Y, Beardsley, AP, Bernardi, G, Bowman, JD, Bradley, RF, Burba, J, Cheng, C, DeBoer, DR, Dexter, M, Acedo, EDL, Dillon, JS, Ewall-Wice, A, Fadana, G, Fagnoni, N, Fritz, R, Furlanetto, SR, Ghosh, A, Glendenning, B, Greig, B, Grobbelaar, J, Halday, Z, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kariseb, M, Kohn, SA, Kolopanis, M, Lekalake, T, Liu, A, Loots, A, MacMahon, D, Malan, L, Malgas, C, Maree, M, Martinot, Z, Matsetela, E, Mesinger, A, Molewa, M, Morales, MF, Neben, AR, Parsons, AR, Patra, N, Pieterse, S, Plante, PL, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sell, R, Sims, P, Smith, C, Syce, A, Williams, PKG, and Zheng, H
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Phase (waves), Closure (topology), FOS: Physical sciences, Condensed Matter Physics, 01 natural sciences, Computational physics, Interferometry, 0103 physical sciences, Closure phase, Redundancy (engineering), General Earth and Planetary Sciences, Electrical and Electronic Engineering, Allan variance, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Reionization, Bispectrum, astro-ph.IM
Abstract: New massively redundant low frequency arrays allow for a novel investigation of closure relations in interferometry. We employ commissioning data from the Hydrogen Epoch of Reionization Array to investigate closure quantities in this densely packed grid array of 14m antennas operating at 100 MHz to 200 MHz. We investigate techniques that utilize closure phase spectra for redundant triads to estimate departures from redundancy for redundant baseline visibilities. We find a median absolute deviation from redundancy in closure phase across the observed frequency range of about 4.5deg. This value translates into a non-redundancy per visibility phase of about 2.6deg, using prototype electronics. The median absolute deviations from redundancy decrease with longer baselines. We show that closure phase spectra can be used to identify ill-behaved antennas in the array, independent of calibration. We investigate the temporal behavior of closure spectra. The Allan variance increases after a one minute stride time, due to passage of the sky through the primary beam of the transit telescope. However, the closure spectra repeat to well within the noise per measurement at corresponding local sidereal times (LST) from day to day. In future papers in this series we will develop the technique of using closure phase spectra in the search for the HI 21cm signal from cosmic reionization., 32 pages. 11 figures. Accepted to Radio Science
Published: 2018

36. The Murchison Widefield Array Transients Survey (MWATS). A search for low-frequency variability in a bright Southern hemisphere sample

Author: Bell, ME, Murphy, T, Hancock, PJ, Callingham, JR, Johnston, S, Kaplan, DL, Hunstead, RW, Sadler, EM, Croft, S, White, SV, Hurley-Walker, N, Chhetri, R, Morgan, JS, Edwards, PG, Rowlinson, A, Offringa, AR, Bernardi, G, Bowman, JD, Briggs, F, Cappallo, RJ, Deshpande, AA, Gaensler, BM, Greenhill, LJ, Hazelton, BJ, Johnston-Hollitt, M, Lonsdale, CJ, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Oberoi, D, Ord, SM, Prabu, T, Shankar, NU, Srivani, KS, Subrahmanyan, R, Tingay, SJ, Wayth, RB, Webster, RL, Williams, A, Williams, CL, Bell, ME, Murphy, T, Hancock, PJ, Callingham, JR, Johnston, S, Kaplan, DL, Hunstead, RW, Sadler, EM, Croft, S, White, SV, Hurley-Walker, N, Chhetri, R, Morgan, JS, Edwards, PG, Rowlinson, A, Offringa, AR, Bernardi, G, Bowman, JD, Briggs, F, Cappallo, RJ, Deshpande, AA, Gaensler, BM, Greenhill, LJ, Hazelton, BJ, Johnston-Hollitt, M, Lonsdale, CJ, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Oberoi, D, Ord, SM, Prabu, T, Shankar, NU, Srivani, KS, Subrahmanyan, R, Tingay, SJ, Wayth, RB, Webster, RL, Williams, A, and Williams, CL
Published: 2019

37. Polarized Foreground Power Spectra from the HERA-19 Commissioning Array

Author: Kohn, S, Chichura, PM, Igarashi, AS, Fortino, AF, Aguirre, JE, Benefo, RK, Billings, TS, Gallardo, S, Plante, PL, Martinot, ZE, Nunhokee, CD, Alexander, P, Ali, ZS, Beardsley, AP, Bernardi, G, Bowman, JD, Bradley, RF, Carilli, CL, Cheng, C, DeBoer, DR, Acedo, EDL, Dillon, JS, Ewall-Wice, A, Fadana, G, Fagnoni, N, Fritz, R, Furlanetto, SR, Glendenning, B, Greig, B, Grobbelaar, J, Hazelton, BJ, Hewitt, JN, Hickish, J, Jacobs, DC, Julius, A, Kariseb, M, Kern, NS, Kolopanis, M, Lekalake, T, Liu, A, Loots, A, MacMahon, D, Malan, L, Malgas, C, Maree, M, Mathison, N, Matsetela, E, Mesinger, A, Morales, MF, Neben, AR, Nikolic, B, Parsons, AR, Patra, N, Pieterse, S, Pober, JC, Razavi-Ghods, N, Ringuette, J, Robnett, J, Rosie, K, Sell, R, Smith, C, Syce, A, Tegmark, M, Thyagarajan, N, Williams, PKG, and Zheng, H
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, astro-ph.IM
Abstract: Foreground power dominates the measurements of interferometers that seek a statistical detection of highly-redshifted HI emission from the Epoch of Reionization (EoR). The inherent spectral smoothness of synchrotron radiation, the dominant foreground emission mechanism, and the chromaticity of the instrument allows these experiments to delineate a boundary between spectrally smooth and structured emission in Fourier space (the "wedge" or "pitchfork", and the "EoR Window", respectively). Faraday rotation can inject spectral structure into otherwise smooth polarized foreground emission, which through instrument effects or miscalibration could possibly pollute the EoR Window. Using data from the Hydrogen Epoch of Reionization Array (HERA) 19-element commissioning array, we investigate the polarization response of this new instrument in the power spectrum domain. We confirm the expected structure of foreground emission in Fourier space predicted by Thyagarajan et al. (2015a, 2016) for a HERA-type dish, and detect polarized power within the pitchfork. Using simulations of the polarized response of HERA feeds, we find that almost all of the power in Stokes Q, U and V can be attributed to instrumental leakage effects. Power consistent with noise in the EoR window suggests a negligible amount of spectrally-structured polarized power, to the noise-levels attained. This lends confidence to deep integrations with HERA in the future, but with a lower noise floor these future studies will also have to investigate their polarized response.
Published: 2018

38. Low Altitude Solar Magnetic Reconnection, Type III Solar Radio Bursts, and X-ray Emissions

Author: Cairns, IH, Lobzin, VV, Donea, A, Tingay, SJ, McCauley, PI, Oberoi, D, Duffin, RT, Reiner, MJ, Hurley-Walker, N, Kudryavtseva, NA, Melrose, DB, Harding, JC, Bernardi, G, Bowman, JD, Cappallo, RJ, Corey, BE, Deshpande, A, Emrich, D, Goeke, R, Hazelton, BJ, Johnston-Hollitt, M, Kaplan, DL, Kasper, JC, Kratzenberg, E, Lonsdale, CJ, Lynch, MJ, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Ord, SM, Prabu, T, Roshi, A, Shankar, NU, Srivani, KS, Subrahmanyan, R, Wayth, RB, Waterson, M, Webster, RL, Whitney, AR, Williams, A, Williams, CL, Cairns, IH, Lobzin, VV, Donea, A, Tingay, SJ, McCauley, PI, Oberoi, D, Duffin, RT, Reiner, MJ, Hurley-Walker, N, Kudryavtseva, NA, Melrose, DB, Harding, JC, Bernardi, G, Bowman, JD, Cappallo, RJ, Corey, BE, Deshpande, A, Emrich, D, Goeke, R, Hazelton, BJ, Johnston-Hollitt, M, Kaplan, DL, Kasper, JC, Kratzenberg, E, Lonsdale, CJ, Lynch, MJ, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Ord, SM, Prabu, T, Roshi, A, Shankar, NU, Srivani, KS, Subrahmanyan, R, Wayth, RB, Waterson, M, Webster, RL, Whitney, AR, Williams, A, and Williams, CL
Abstract: Type III solar radio bursts are the Sun's most intense and frequent nonthermal radio emissions. They involve two critical problems in astrophysics, plasma physics, and space physics: how collective processes produce nonthermal radiation and how magnetic reconnection occurs and changes magnetic energy into kinetic energy. Here magnetic reconnection events are identified definitively in Solar Dynamics Observatory UV-EUV data, with strong upward and downward pairs of jets, current sheets, and cusp-like geometries on top of time-varying magnetic loops, and strong outflows along pairs of open magnetic field lines. Type III bursts imaged by the Murchison Widefield Array and detected by the Learmonth radiospectrograph and STEREO B spacecraft are demonstrated to be in very good temporal and spatial coincidence with specific reconnection events and with bursts of X-rays detected by the RHESSI spacecraft. The reconnection sites are low, near heights of 5-10 Mm. These images and event timings provide the long-desired direct evidence that semi-relativistic electrons energized in magnetic reconnection regions produce type III radio bursts. Not all the observed reconnection events produce X-ray events or coronal or interplanetary type III bursts; thus different special conditions exist for electrons leaving reconnection regions to produce observable radio, EUV, UV, and X-ray bursts.
Published: 2018

39. An All-Sky Search for Steady VHE Gamma-Ray Sources

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Abstract: The Milagrito water Cherenkov detector in the Jemez Mountains near Los Alamos, New Mexico took data from February 1997 to April 1998. Milagrito served as a prototype for the larger Milagro detector, which has just begun operations. Milagrito was the first large-aperture gamma-ray detector with sensitivity to gamma rays below 1 TeV. We report here on a search for steady emission from point sources over most of the northern sky using data from Milagrito.
Published: 2017

40. Study of the Shadows of the Moon and the Sun with VHE Cosmic Rays

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Abstract: Milagrito, a prototype for the Milagro detector, operated for 15 months in 1997-8 and collected 8.9 billion events. It was the first extensive air shower (EAS) array sensitive to showers intiated by primaries with energy below 1 TeV. The shadows of the sun and moon observed with cosmic rays can be used to study systematic pointing shifts and measure the angular resolution of EAS arrays. Below a few TeV, the paths of cosmic rays coming toward the earth are bent by the helio- and geo-magnetic fields. This is expected to distort and displace the shadows of the sun and the moon. The moon shadow, offset from the nominal (undeflected) position, has been observed with high statistical significance in Milagrito. This can be used to establish energy calibrations, as well as to search for the anti-matter content of the VHE cosmic ray flux. The shadow of the sun has also been observed with high significance.
Published: 2017

41. Search for Short Duration Bursts of TeV Gamma Rays with the Milagrito Telescope

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Abstract: The Milagrito water Cherenkov telescope operated for over a year. The most probable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400 Hz. We have developed an efficient technique for searching the entire sky for short duration bursts of TeV photons. Such bursts may result from "traditional" gamma-ray bursts that were not in the field-of-view of any other instruments, the evaporation of primordial black holes, or some as yet undiscovered phenomenon. We have begun to search the Milagrito data set for bursts of duration 10 seconds. Here we will present the technique and the expected results. Final results will be presented at the conference.
Published: 2017

42. Instrumented Water Tanks can Improve Air Shower Detector Sensitivity

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Abstract: Previous works have shown that water Cherenkov detectors have superior sensitivity to those of scintillation counters as applied to detecting extensive air showers (EAS). This is in large part due to their much higher sensitivity to EAS photons which are more than five times more numerous than EAS electrons. Large area water Cherenkov detectors can be constructed relatively cheaply and operated reliably. A sparse detector array has been designed which uses these types of detectors to substantially increase the area over which the Milagro Gamma Ray Observatory collects EAS information. Improvements to the Milagro detector's performance characteristics and sensitivity derived from this array and preliminary results from a prototype array currently installed near the Milagro detector will be presented.
Published: 2017

43. Search for a TeV Component of GRBs using the Milagrito Detector

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Abstract: Observing gamma ray bursts (GRBs) in the TeV energy range can be extremely valuable in providing insight to GRB radiation mechanisms and in constraining source distances. The Milagrito detector was an air shower array which used the water Cherenkov technique to search for TeV sources. Data from this detector was analyzed to look for a TeV component of GRBs coincident with low energy -rays detected by the BATSE instrument on the Compton Gamma Ray Observatory. A sample of 54 BATSE GRBs which were in the field of view of the Milagrito detector during its lifetime (February 1997 to May 1998) was used.
Published: 2017

44. Milagrito Detection of TeV Emission from Mrk 501

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Abstract: The Milagro water Cherenkov detector near Los Alamos, New Mexico, has been operated as a sky monitor at energies of a few TeV between February 1997 and April 1998. Serving as a test run for the full Milagro detector, Milagrito has taken data during the strong and long-lasting 1997 flare of Mrk 501. We present results from the analysis of Mrk 501 and compare the excess and background rates with expectations from the detector simulations.
Published: 2017

45. Calibration of the Milagro Cosmic Ray Telescope

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Abstract: The Milagro detector is an air shower array which uses the water Cherenkov technique and is capable of continuously monitoring the sky at energies near 1 TeV. The detector consists of 20000 metric tons of pure water instrumented with 723 photo-multiplier tubes (PMTs). The PMTs are arranged in a two-layer structure on a lattice of 3 m spacing covering 5000 $m^2$ area. The direction of the shower is determined from the relative timing of the PMT signals, necessitating a common time reference and amplitude slewing corrections to improve the time resolution. The calibration system to provide these consists of a pulsed laser driving 30 diffusing light sources deployed in the pond to allow cross-calibration of the PMTs. The system is capable of calibrating times and the pulse-heights from the PMTs using the time-over-threshold technique. The absolute energy scale is provided using single muons passing through the detector. The description of the calibration system of the Milagro detector and its prototype Milagrito will be presented.
Published: 2017

46. Status of the Milagro Gamma Ray Observatory

Author: Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB
Abstract: The Milagro Gamma Ray Observatory is the world's first large-area water Cherenkov detector capable of continuously monitoring the sky at TeV energies. Located in northern New Mexico, Milagro will perform an all sky survey of the Northern Hemisphere at energies between ~250 GeV and 50 TeV. With a high duty cycle, large detector area (~5000 square meters), and a wide field-of-view (~1 sr), Milagro is uniquely capable of searching for transient and DC sources of high-energy gamma-ray emission. Milagro has been operating since February, 1999. The current status of the Milagro Observatory and initial results will be discussed.
Published: 2017

47. Spectral Energy Distribution and Radio Halo of NGC 253 at Low Radio Frequencies

Author: Kapińska, AD, Staveley-Smith, L, Crocker, R, Meurer, GR, Bhandari, S, Hurley-Walker, N, Offringa, AR, Hanish, DJ, Seymour, N, Ekers, RD, Bell, ME, Callingham, JR, Dwarakanath, KS, For, BQ, Gaensler, BM, Hancock, PJ, Hindson, L, Johnston-Hollitt, M, Lenc, E, McKinley, B, Morgan, J, Procopio, P, Wayth, RB, Wu, C, Zheng, Q, Barry, N, Beardsley, AP, Bowman, JD, Briggs, F, Carroll, P, Dillon, JS, Ewall-Wice, A, Feng, L, Greenhill, LJ, Hazelton, BJ, Hewitt, JN, Jacobs, DJ, Kim, HS, Kittiwisit, P, Line, J, Loeb, A, Mitchell, DA, Morales, MF, Neben, AR, Paul, S, Pindor, B, Pober, JC, Riding, J, Sethi, SK, Shankar, NU, Subrahmanyan, R, Sullivan, IS, Tegmark, M, Thyagarajan, N, Tingay, SJ, Trott, CM, Webster, RL, Wyithe, SB, Cappallo, RJ, Deshpande, AA, Kaplan, DL, Lonsdale, CJ, McWhirter, SR, Morgan, E, Oberoi, D, Ord, SM, Prabu, T, Srivani, KS, Williams, A, Williams, CL, Kapińska, AD, Staveley-Smith, L, Crocker, R, Meurer, GR, Bhandari, S, Hurley-Walker, N, Offringa, AR, Hanish, DJ, Seymour, N, Ekers, RD, Bell, ME, Callingham, JR, Dwarakanath, KS, For, BQ, Gaensler, BM, Hancock, PJ, Hindson, L, Johnston-Hollitt, M, Lenc, E, McKinley, B, Morgan, J, Procopio, P, Wayth, RB, Wu, C, Zheng, Q, Barry, N, Beardsley, AP, Bowman, JD, Briggs, F, Carroll, P, Dillon, JS, Ewall-Wice, A, Feng, L, Greenhill, LJ, Hazelton, BJ, Hewitt, JN, Jacobs, DJ, Kim, HS, Kittiwisit, P, Line, J, Loeb, A, Mitchell, DA, Morales, MF, Neben, AR, Paul, S, Pindor, B, Pober, JC, Riding, J, Sethi, SK, Shankar, NU, Subrahmanyan, R, Sullivan, IS, Tegmark, M, Thyagarajan, N, Tingay, SJ, Trott, CM, Webster, RL, Wyithe, SB, Cappallo, RJ, Deshpande, AA, Kaplan, DL, Lonsdale, CJ, McWhirter, SR, Morgan, E, Oberoi, D, Ord, SM, Prabu, T, Srivani, KS, Williams, A, and Williams, CL
Abstract: © 2017. The American Astronomical Society. All rights reserved. We present new radio continuum observations of NGC 253 from the Murchison Widefield Array at frequencies between 76 and 227 MHz. We model the broadband radio spectral energy distribution for the total flux density of NGC 253 between 76 MHz and 11 GHz. The spectrum is best described as a sum of a central starburst and extended emission. The central component, corresponding to the inner 500 pc of the starburst region of the galaxy, is best modeled as an internally free-free absorbed synchrotron plasma, with a turnover frequency around 230 MHz. The extended emission component of the spectrum of NGC 253 is best described as a synchrotron emission flattening at low radio frequencies. We find that 34% of the extended emission (outside the central starburst region) at 1 GHz becomes partially absorbed at low radio frequencies. Most of this flattening occurs in the western region of the southeast halo, and may be indicative of synchrotron self-absorption of shock-reaccelerated electrons or an intrinsic low-energy cutoff of the electron distribution. Furthermore, we detect the large-scale synchrotron radio halo of NGC 253 in our radio images. At 154-231 MHz the halo displays the well known X-shaped/horn-like structure, and extends out to ∼8 kpc in the z-direction (from the major axis).
Published: 2017

48. A large-scale, low-frequency murchison widefield array survey of galactic H II regions between 260 < l < 340

Author: Hindson, L, Johnston-Hollitt, M, Hurley-Walker, N, Callingham, JR, Su, H, Morgan, J, Bell, M, Bernardi, G, Bowman, JD, Briggs, F, Cappallo, RJ, Deshpande, AA, Dwarakanath, KS, For, BQ, Gaensler, BM, Greenhill, LJ, Hancock, P, Hazelton, BJ, Kapinska, AD, Kaplan, DL, Lenc, E, Lonsdale, CJ, Mckinley, B, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Oberoi, D, Offringa, A, Ord, SM, Procopio, P, Prabu, T, Udaya Shankar, N, Srivani, KS, Staveley-Smith, L, Subrahmanyan, R, Tingay, SJ, Wayth, RB, Webster, RL, Williams, A, Williams, CL, Wu, C, and Zheng, Q
Subjects: Astronomy & Astrophysics
Abstract: © Astronomical Society of Australia 2016. We have compiled a catalogue of H ii regions detected with the Murchison Widefield Array between 72 and 231 MHz. The multiple frequency bands provided by the Murchison Widefield Array allow us identify the characteristic spectrum generated by the thermal Bremsstrahlung process in H ii regions. We detect 306 H ii regions between 260◦ < l < 340◦ and report on the positions, sizes, peak, integrated flux density, and spectral indices of these H ii regions. By identifying the point at which H ii regions transition from the optically thin to thick regime, we derive the physical properties including the electron density, ionised gas mass, and ionising photon flux, towards 61 H ii regions. This catalogue of H ii regions represents the most extensive and uniform low frequency survey of H ii regions in the Galaxy to date.
Published: 2016

49. THE SPECTRAL VARIABILITY OF THE GHZ-PEAKED SPECTRUM RADIO SOURCE PKS 1718-649 AND A COMPARISON OF ABSORPTION MODELS

Author: Tingay, SJ, Macquart, J-P, Collier, JD, Rees, G, Callingham, JR, Stevens, J, Carretti, E, Wayth, RB, Wong, GF, Trott, CM, McKinley, B, Bernardi, G, Bowman, JD, Briggs, F, Cappallo, RJ, Corey, BE, Deshpande, AA, Emrich, D, Gaensler, BM, Goeke, R, Greenhill, LJ, Hazelton, BJ, Johnston-Hollitt, M, Kaplan, DL, Kasper, JC, Kratzenberg, E, Lonsdale, CJ, Lynch, MJ, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Oberoi, D, Ord, SM, Prabu, T, Rogers, AEE, Roshi, A, Shankar, NU, Srivani, KS, Subrahmanyan, R, Waterson, M, Webster, RL, Whitney, AR, Williams, A, Williams, CL, Tingay, SJ, Macquart, J-P, Collier, JD, Rees, G, Callingham, JR, Stevens, J, Carretti, E, Wayth, RB, Wong, GF, Trott, CM, McKinley, B, Bernardi, G, Bowman, JD, Briggs, F, Cappallo, RJ, Corey, BE, Deshpande, AA, Emrich, D, Gaensler, BM, Goeke, R, Greenhill, LJ, Hazelton, BJ, Johnston-Hollitt, M, Kaplan, DL, Kasper, JC, Kratzenberg, E, Lonsdale, CJ, Lynch, MJ, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Oberoi, D, Ord, SM, Prabu, T, Rogers, AEE, Roshi, A, Shankar, NU, Srivani, KS, Subrahmanyan, R, Waterson, M, Webster, RL, Whitney, AR, Williams, A, and Williams, CL
Abstract: Using the new wideband capabilities of the Australia Telescope Compact Array (ATCA), we obtain spectra for PKS 1718-649, a well-known gigahertz-peaked spectrum radio source. The observations, between approximately 1 and 10 GHz over three epochs spanning approximately 21 months, reveal variability both above the spectral peak at ~3 GHz and below the peak. The combination of the low and high frequency variability cannot be easily explained using a single absorption mechanism, such as free-free absorption or synchrotron self-absorption. We find that the PKS 1718-649 spectrum and its variability are best explained by variations in the free-free optical depth on our line-of-sight to the radio source at low frequencies (below the spectral peak) and the adiabatic expansion of the radio source itself at high frequencies (above the spectral peak). The optical depth variations are found to be plausible when X-ray continuum absorption variability seen in samples of Active Galactic Nuclei is considered. We find that the cause of the peaked spectrum in PKS 1718-649 is most likely due to free-free absorption. In agreement with previous studies, we find that the spectrum at each epoch of observation is best fit by a free-free absorption model characterised by a power-law distribution of free-free absorbing clouds. This agreement is extended to frequencies below the 1 GHz lower limit of the ATCA by considering new observations with Parkes at 725 MHz and 199 MHz observations with the newly operational Murchison Widefield Array. These lower frequency observations argue against families of absorption models (both free-free and synchrotron self-absorption) that are based on simple homogenous structures.
Published: 2015

50. Ionospheric Modelling using GPS to Calibrate the MWA. I: Comparison of First Order Ionospheric Effects between GPS Models and MWA Observations

Author: Arora, BS, Morgan, J, Ord, SM, Tingay, SJ, Hurley-Walker, N, Bell, M, Bernardi, G, Bhat, NDR, Briggs, F, Callingham, JR, Deshpande, AA, Dwarakanath, KS, Ewall-Wice, A, Feng, L, For, B-Q, Hancock, P, Hazelton, BJ, Hindson, L, Jacobs, D, Johnston-Hollitt, M, Kapinska, AD, Kudryavtseva, N, Lenc, E, McKinley, B, Mitchell, D, Oberoi, D, Offringa, AR, Pindor, B, Procopio, P, Riding, J, Staveley-Smith, L, Wayth, RB, Wu, C, Zheng, Q, Bowman, JD, Cappallo, RJ, Corey, BE, Emrich, D, Goeke, R, Greenhill, LJ, Kaplan, DL, Kasper, JC, Kratzenberg, E, Lonsdale, CJ, Lynch, MJ, McWhirter, SR, Morales, MF, Morgan, E, Prabu, T, Rogers, AEE, Roshi, A, Shankar, NU, Srivani, KS, Subrahmanyan, R, Waterson, M, Webster, RL, Whitney, AR, Williams, A, Williams, CL, Arora, BS, Morgan, J, Ord, SM, Tingay, SJ, Hurley-Walker, N, Bell, M, Bernardi, G, Bhat, NDR, Briggs, F, Callingham, JR, Deshpande, AA, Dwarakanath, KS, Ewall-Wice, A, Feng, L, For, B-Q, Hancock, P, Hazelton, BJ, Hindson, L, Jacobs, D, Johnston-Hollitt, M, Kapinska, AD, Kudryavtseva, N, Lenc, E, McKinley, B, Mitchell, D, Oberoi, D, Offringa, AR, Pindor, B, Procopio, P, Riding, J, Staveley-Smith, L, Wayth, RB, Wu, C, Zheng, Q, Bowman, JD, Cappallo, RJ, Corey, BE, Emrich, D, Goeke, R, Greenhill, LJ, Kaplan, DL, Kasper, JC, Kratzenberg, E, Lonsdale, CJ, Lynch, MJ, McWhirter, SR, Morales, MF, Morgan, E, Prabu, T, Rogers, AEE, Roshi, A, Shankar, NU, Srivani, KS, Subrahmanyan, R, Waterson, M, Webster, RL, Whitney, AR, Williams, A, and Williams, CL
Abstract: We compare first-order (refractive) ionospheric effects seen by the MWA with the ionosphere as inferred from GPS data. The first-order ionosphere manifests itself as a bulk position shift of the observed sources across an MWA field of view. These effects can be computed from global ionosphere maps provided by GPS analysis centres, namely the CODE. However, for precision radio astronomy applications, data from local GPS networks needs to be incorporated into ionospheric modelling. For GPS observations, the ionospheric parameters are biased by GPS receiver instrument delays, among other effects, also known as receiver DCBs. The receiver DCBs need to be estimated for any non-CODE GPS station used for ionosphere modelling. In this work, single GPS station-based ionospheric modelling is performed at a time resolution of 10 min. Also the receiver DCBs are estimated for selected Geoscience Australia GPS receivers, located at Murchison Radio Observatory, Yarragadee, Mount Magnet and Wiluna. The ionospheric gradients estimated from GPS are compared with that inferred from MWA. The ionospheric gradients at all the GPS stations show a correlation with the gradients observed with the MWA. The ionosphere estimates obtained using GPS measurements show promise in terms of providing calibration information for the MWA.
Published: 2015

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