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101. Integrated Photonics for NewSpace

Author: Brunetti, G., Saha, N., Campiti, G., di Toma, A., Sasanelli, N., Hassan, F., Armenise, M. N., Ciminelli, C., Angrisani, Leopoldo, Series Editor, Arteaga, Marco, Series Editor, Chakraborty, Samarjit, Series Editor, Chen, Jiming, Series Editor, Chen, Shanben, Series Editor, Chen, Tan Kay, Series Editor, Dillmann, Rüdiger, Series Editor, Duan, Haibin, Series Editor, Ferrari, Gianluigi, Series Editor, Ferre, Manuel, Series Editor, Jabbari, Faryar, Series Editor, Jia, Limin, Series Editor, Kacprzyk, Janusz, Series Editor, Khamis, Alaa, Series Editor, Kroeger, Torsten, Series Editor, Li, Yong, Series Editor, Liang, Qilian, Series Editor, Martín, Ferran, Series Editor, Ming, Tan Cher, Series Editor, Minker, Wolfgang, Series Editor, Misra, Pradeep, Series Editor, Mukhopadhyay, Subhas, Series Editor, Ning, Cun-Zheng, Series Editor, Nishida, Toyoaki, Series Editor, Oneto, Luca, Series Editor, Panigrahi, Bijaya Ketan, Series Editor, Pascucci, Federica, Series Editor, Qin, Yong, Series Editor, Seng, Gan Woon, Series Editor, Speidel, Joachim, Series Editor, Veiga, Germano, Series Editor, Wu, Haitao, Series Editor, Zamboni, Walter, Series Editor, Zhang, Junjie James, Series Editor, Berta, Riccardo, editor, and De Gloria, Alessandro, editor
Published: 2023
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102. Sorting of Live/dead Escherichia Coli by Means of Dielectrophoresis for Rapid Antimicrobial Susceptibility Testing

Author: di Toma, A., Brunetti, G., Sasanelli, N., Armenise, M. N., Ciminelli, C., Angrisani, Leopoldo, Series Editor, Arteaga, Marco, Series Editor, Chakraborty, Samarjit, Series Editor, Chen, Jiming, Series Editor, Chen, Shanben, Series Editor, Chen, Tan Kay, Series Editor, Dillmann, Rüdiger, Series Editor, Duan, Haibin, Series Editor, Ferrari, Gianluigi, Series Editor, Ferre, Manuel, Series Editor, Jabbari, Faryar, Series Editor, Jia, Limin, Series Editor, Kacprzyk, Janusz, Series Editor, Khamis, Alaa, Series Editor, Kroeger, Torsten, Series Editor, Li, Yong, Series Editor, Liang, Qilian, Series Editor, Martín, Ferran, Series Editor, Ming, Tan Cher, Series Editor, Minker, Wolfgang, Series Editor, Misra, Pradeep, Series Editor, Mukhopadhyay, Subhas, Series Editor, Ning, Cun-Zheng, Series Editor, Nishida, Toyoaki, Series Editor, Oneto, Luca, Series Editor, Panigrahi, Bijaya Ketan, Series Editor, Pascucci, Federica, Series Editor, Qin, Yong, Series Editor, Seng, Gan Woon, Series Editor, Speidel, Joachim, Series Editor, Veiga, Germano, Series Editor, Wu, Haitao, Series Editor, Zamboni, Walter, Series Editor, Zhang, Junjie James, Series Editor, Berta, Riccardo, editor, and De Gloria, Alessandro, editor
Published: 2023
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103. Spaceborne LiDAR for Debris Detection and Tracking

Author: Tagliente, M., Campiti, G., Brunetti, G., Armenise, M. N., Ciminelli, C., Angrisani, Leopoldo, Series Editor, Arteaga, Marco, Series Editor, Panigrahi, Bijaya Ketan, Series Editor, Chakraborty, Samarjit, Series Editor, Chen, Jiming, Series Editor, Chen, Shanben, Series Editor, Chen, Tan Kay, Series Editor, Dillmann, Rüdiger, Series Editor, Duan, Haibin, Series Editor, Ferrari, Gianluigi, Series Editor, Ferre, Manuel, Series Editor, Hirche, Sandra, Series Editor, Jabbari, Faryar, Series Editor, Jia, Limin, Series Editor, Kacprzyk, Janusz, Series Editor, Khamis, Alaa, Series Editor, Kroeger, Torsten, Series Editor, Li, Yong, Series Editor, Liang, Qilian, Series Editor, Martín, Ferran, Series Editor, Ming, Tan Cher, Series Editor, Minker, Wolfgang, Series Editor, Misra, Pradeep, Series Editor, Möller, Sebastian, Series Editor, Mukhopadhyay, Subhas, Series Editor, Ning, Cun-Zheng, Series Editor, Nishida, Toyoaki, Series Editor, Oneto, Luca, Series Editor, Pascucci, Federica, Series Editor, Qin, Yong, Series Editor, Seng, Gan Woon, Series Editor, Speidel, Joachim, Series Editor, Veiga, Germano, Series Editor, Wu, Haitao, Series Editor, Zamboni, Walter, Series Editor, Zhang, Junjie James, Series Editor, Cocorullo, Giuseppe, editor, Crupi, Felice, editor, and Limiti, Ernesto, editor
Published: 2023
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104. Understanding the radio relic emission in the galaxy cluster MACS J0717.5+3745: spectral analysis

Author: Rajpurohit, K., Wittor, D., van Weeren, R. J., Vazza, F., Hoeft, M., Rudnick, L., Locatelli, N., Eilek, J., Forman, W. R., Bonafede, A., Bonnassieux, E., Riseley, C. J., Brienza, M., Brunetti, G., Brüggen, M., Loi, F., Rajpurohit, A. S., Röttgering, H. J. A., Botteon, A., Clarke, T. E., Drabent, A., Domínguez-Fernández, P., Di Gennaro, G., and Gastaldello, F.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Radio relics are diffuse, extended synchrotron sources that originate from shock fronts generated during cluster mergers. The massive merging galaxy cluster MACS J0717.5+3745 hosts one of the more complex relics known to date. We present upgraded Giant Metrewave Radio Telescope band 3 (300-500 MHz) and band 4 (550-850 MHz) observations. These new observations, combined with published VLA and the new LOFAR HBA data, allow us to carry out a detailed, high spatial resolution spectral analysis of the relic over a broad range of frequencies. The integrated spectrum of the relic closely follows a power-law between 144 MHz and 5.5 GHz with a mean spectral slope $\alpha=-1.16\pm0.03$. Despite its complex morphology, the subregions of the relic and the other isolated filaments also follow power-law behaviors, and show similar spectral slopes. Assuming Diffusive Shock Acceleration, we estimate a dominant Mach number of $\sim 3.7$ for the shocks that make up the relic. Comparison with recent numerical simulations suggests that in the case of radio relics, the slopes of the integrated radio spectra are determined by the Mach number of the accelerating shock, with $\alpha$ nearly constant, namely between $-1.13$ and $-1.17$, for Mach numbers $3.5 - 4.0$. The spectral shapes inferred from spatially resolved regions show curvature, we speculate that the relic is inclined along the line-of-sight. The locus of points in the simulated color-color plots changes significantly with the relic viewing angle. We conclude that projection effects and inhomogeneities in the shock Mach number dominate the observed spectral properties of the relic in this complex system. Based on the new observations we raise the possibility that the relic and a narrow-angle-tailed radio galaxy are two different structures projected along the same line-of-sight., Comment: 14 pages, 12 figures
Published: 2020
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105. The Coma cluster at LOFAR frequencies I: insights into particle acceleration mechanisms in the radio bridge

Author: Bonafede, A., Brunetti, G., Vazza, F., Simionescu, A., Giovannini, G., Bonnassieux, E., Shimwell, T. W., Brüggen, M., van Weeren, R. J., Botteon, A., Brienza, M., Cassano, R., Drabent, A., Feretti, L., de Gasperin, F., Gastaldello, F., di Gennaro, G., Rossetti, M., Rottgering, H. J. A., Stuardi, C., and Venturi, T.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Radio synchrotron emission from the bridges of low-density gas connecting galaxy clusters and groups is a challenge for particle acceleration processes. In this work, we analyse the Coma radio bridge using new LOw Frequency ARray (LOFAR) observations at 144 MHz. LOFAR detects the bridge and its substructures with unprecedented sensitivity and resolution. We find that the radio emission peaks on the NGC 4839 group. Towards the halo, in front of the NGC 4839 group, the radio brightness decreases and streams of radio emission connect the NGC 4839 group to the radio relic. Using X-ray observations, we find that thermal and non-thermal plasma are moderately correlated with a sub-linear scaling. We use archival radio data at 326 MHz to constrain the spectral index in the bridge, and quantify the distribution of particles and magnetic field at different frequencies. We find that the spectrum is steeper than $-1.4 \pm 0.2$, and that the emission could be clumpier at 326 MHz than at 144 MHz. Using cosmological simulations and a simplified approach to compute particle acceleration, we derive under which conditions turbulent acceleration of mildly relativistic electrons could generate the radio emission in the bridge. Assuming that the initial energy ratio of the seed electrons is $3 \cdot 10^{-4}$ with respect to the thermal gas, we are able to reproduce the observed luminosity. Our results suggest that the seed electrons released by radiogalaxies in the bridge and the turbulence generated by the motion of gas and galaxies are essential to produce the radio emission., Comment: 16 pages, 8 figures, accepted by the Astrophysical Journal
Published: 2020
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106. The LOFAR Two Meter Sky Survey: Deep Fields, I -- Direction-dependent calibration and imaging

Author: Tasse, C., Shimwell, T., Hardcastle, M. J., O'Sullivan, S. P., van Weeren, R., Best, P. N., Bester, L., Hugo, B., Smirnov, O., Sabater, J., Calistro-Rivera, G., de Gasperin, F., Morabito, L. K., Röttgering, H., Williams, W. L., Bonato, M., Bondi, M., Botteon, A., Brüggen, M., Brunetti, G., Chyży, K. T., Garrett, M. A., Gürkan, G., Jarvis, M. J., Kondapally, R., Mandal, S., Prandoni, I., Repetti, A., Retana-Montenegro, E., Schwarz, D. J., Shulevski, A., and Wiaux, Y.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Low Frequency Array (LOFAR) is an ideal instrument to conduct deep extragalactic surveys. It has a large field of view and is sensitive to large scale and compact emission. It is, however, very challenging to synthesize thermal noise limited maps at full resolution, mainly because of the complexity of the low-frequency sky and the direction dependent effects (phased array beams and ionosphere). In this first paper of a series we present a new calibration and imaging pipeline that aims at producing high fidelity, high dynamic range images with LOFAR High Band Antenna data, while being computationally efficient and robust against the absorption of unmodeled radio emission. We apply this calibration and imaging strategy to synthesize deep images of the Bootes and LH fields at 150 MHz, totaling $\sim80$ and $\sim100$ hours of integration respectively and reaching unprecedented noise levels at these low frequencies of $\lesssim30$ and $\lesssim23$ $\mu$Jy/beam in the inner $\sim3$ deg$^2$. This approach is also being used to reduce the LoTSS-wide data for the second data release., Comment: This paper is part of the 1st data release of the LoTSS Deep Fields. Electronic data catalogues will be made available on journal publication
Published: 2020
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107. Diffuse Radio Emission from Galaxy Clusters in the LOFAR Two-metre Sky Survey Deep Fields

Author: Osinga, E., van Weeren, R. J., Boxelaar, J., Brunetti, G., Botteon, A., Brüggen, M., Shimwell, T. W., Bonafede, A., Best, P. N., Bonato, M., Cassano, R., Gastaldello, F., di Gennaro, G., Hardcastle, M. J., Mandal, S., Rossetti, M., Röttgering, H. J. A., and Sabater, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Low-frequency radio observations are revealing an increasing number of diffuse synchrotron sources from galaxy clusters, dominantly in the form of radio halos or radio relics. The existence of this diffuse synchrotron emission indicates the presence of relativistic particles and magnetic fields. It is still an open question what mechanisms exactly are responsible for the population of relativistic electrons driving this synchrotron emission. The LOFAR Two-metre Sky Survey Deep Fields offer a unique view of this problem. Reaching noise levels below 30 $\mu$Jy/beam, these are the deepest images made at the low frequency of 144 MHz. This paper presents a search for diffuse emission in galaxy clusters in the first data release of the LOFAR Deep Fields. We detect a new high-redshift radio halo with a flux density of $8.9 \pm 1.0$ mJy and corresponding luminosity of $P_{144\mathrm{MHz}}=(3.6 \pm 0.6)\times10^{25}$ W Hz$^{-1}$ in an X-ray detected cluster at $z=0.77$ with a mass estimate of $M_{500} = 3.3_{-1.7}^{+1.1} \times 10^{14} M_\odot.$ Deep upper limits are placed on clusters with non-detections. We compare the results to the correlation between halo luminosity and cluster mass derived for radio halos found in the literature. This study is one of few to find diffuse emission in low mass ($M_{500} < 5\times10^{14} M_\odot$) systems and shows that deep low-frequency observations of galaxy clusters are fundamental for opening up a new part of parameter space in the study of non-thermal phenomena in galaxy clusters., Comment: This paper is part of the 1st data release of the LoTSS Deep Fields. Re-submitted paper (reply to referee)
Published: 2020
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108. LOFAR Detection of a Low-Power Radio Halo in the Galaxy Cluster Abell 990

Author: Hoang, N. D., Shimwell, T. W., Osinga, E., Bonafede, A., Brüggen, M., Botteon, A., Brunetti, G., Cassano, R., Cuciti, V., Drabent, A., Jones, C., Röttgering, H. J. A., and van Weeren, R. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Radio halos are extended ($\sim{\rm Mpc}$), steep-spectrum sources found in the central region of dynamically disturbed clusters of galaxies. Only a handful of radio halos have been reported to reside in galaxy clusters with a mass $M_{500}\lesssim5\times10^{14}\,M_\odot$. In this paper we present a LOFAR 144 MHz detection of a radio halo in the galaxy cluster Abell 990 with a mass of $M_{500}=(4.9\pm0.3)\times10^{14}\,M_\odot$. The halo has a projected size of $\sim$700$\,{\rm kpc}$ and a flux density of $20.2\pm2.2\,{\rm mJy}$ or a radio power of $1.2\pm0.1\times10^{24}\,{\rm W\,Hz}^{-1}$ at the cluster redshift ($z=0.144$) which makes it one of the two halos with the lowest radio power detected to date. Our analysis of the emission from the cluster with Chandra archival data using dynamical indicators shows that the cluster is not undergoing a major merger but is a slightly disturbed system with a mean temperature of $5\,{\rm keV}$. The low X-ray luminosity of $L_{X}=(3.66\pm0.08)\times10^{44}\,{\rm ergs\,s}^{-1}$ in the 0.1--2.4 keV band implies that the cluster is one of the least luminous systems known to host a radio halo. Our detection of the radio halo in Abell 990 opens the possibility of detecting many more halos in poorly-explored less-massive clusters with low-frequency telescopes such as LOFAR, MWA (Phase II) and uGMRT.
Published: 2020
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109. LOFAR observations of galaxy clusters in HETDEX

Author: van Weeren, R. J., Shimwell, T. W., Botteon, A., Brunetti, G., Brüggen, M., Boxelaar, J. M., Cassano, R., Di Gennaro, G., Andrade-Santos, F., Bonnassieux, E., Bonafede, A., Cuciti, V., Dallacasa, D., de Gasperin, F., Gastaldello, F., Hardcastle, M. J., Hoeft, M., Kraft, R . P., Mandal, S., Rossetti, M., Röttgering, H. J. A., Tasse, C., and Wilber, A. G.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Diffuse cluster radio sources, in the form of radio halos and relics, reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). These cosmic rays are thought to be (re-)accelerated through ICM turbulence and shock waves generated by cluster merger events. Here we characterize the presence of diffuse radio emission in known galaxy clusters in the HETDEX Spring Field, covering 424 deg$^2$. For this, we developed a method to extract individual targets from LOFAR observations processed with the LoTSS DDF-pipeline. This procedure enables improved calibration and joint imaging and deconvolution of multiple pointings of selected targets. The calibration strategy can also be used for LOFAR Low-Band Antenna (LBA) and international-baseline observations. The fraction of Planck PSZ2 clusters with any diffuse radio emission apparently associated with the ICM is $73\pm17\%$. We detect a total of 10 radio halos and 12 candidate halos in the HETDEX Spring Field. Five clusters host radio relics. The fraction of radio halos in Planck PSZ2 clusters is $31\pm11\%$, and $62\pm15\%$ when including the candidate radio halos. Based on these numbers, we expect that there will be at least $183 \pm 65$ radio halos found in the LoTSS survey in PSZ2 clusters, in agreement with predictions. The integrated flux densities for the radio halos were computed by fitting exponential models to the radio images. From these flux densities, we determine the cluster mass (M$_{500}$) and Compton Y parameter (Y$_{500}$) 150 MHz radio power (P$_{\rm{150 MHz}}$) scaling relations for Planck PSZ2-detected radio halos. We find that the slopes of these relations are steeper than those determined from the 1.4 GHz radio powers. However, considering the uncertainties this is not a statistically significant result., Comment: submitted, 35 pages and 45 figures
Published: 2020
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110. Abell 1430: A merging cluster with exceptional diffuse radio emission

Author: Hoeft, M., Dumba, C., Drabent, A., Rajpurohit, K., Rossetti, M., Nuza, S. E., van Weeren, R. J., Meusinger, H., Botteon, A., Brunetti, G., Shimwell, T. W., Cassano, R., Brüggen, M., Röttgering, H. J. A., Gastaldello, F., Lovisari, L., Yepes, G., Andrade-Santos, F., and Eckert, D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Diffuse radio emission has been found in many galaxy clusters, predominantly in massive systems which are in the state of merging. The radio emission can usually be classified as relic or halo emission, which are believed to be related to merger shocks or volume-filling turbulence, respectively. Recent observations have revealed radio bridges for some pairs of very closeby galaxy clusters. The mechanisms that may allow to explain the high specific density of relativistic electrons, necessary to explain the radio luminosity of these bridge regions, are poorly explored. We analyse the galaxy cluster Abell 1430 with LoTSS data in detail and complement it with recent JVLA L-band observations, XMM-Newton, Chandra, and SDSS data. Moreover, we compare our results to clusters extracted from the "The Three Hundred Project" cosmological simulation. We find that Abell 1430 consists of two components, namely A1430-A and A1430-B. We speculate that the two components undergo an off-axis merger. The more massive component shows diffuse radio emission which can be classified as radio halo showing a low radio power given the mass of the cluster. Most interestingly, there is extended diffuse radio emission, dubbed as the `Pillow', which is apparently related to A1430-B and thus related to low density intracluster or intergalactic medium. To date, a only few examples for emission originating from such regions are known. These discoveries are crucial to constrain possible acceleration mechanisms, which may allow to explain the presence of relativistic electrons in these regions. Our results indicate a spectral index of $\alpha_{144\,\text{MHz}}^{1.5\,\text{GHz}}=-1.4\pm0.5$ for the Pillow. If future observations confirm a slope as flat as the central value of -1.4 or even flatter, this would pose a severe challenge for the electron acceleration scenarios., Comment: 14 pages, 12 figures, accepted for publication in A&A
Published: 2020
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111. Study of scintillation light collection, production and propagation in a 4 tonne dual-phase LArTPC

Author: Aimard, B., Aizawa, L., Alt, C., Asaadi, J., Auger, M., Aushev, V., Autiero, D., Balaceanu, A., Balik, G., Balleyguier, L., Bechetoille, E., Belver, D., Blebea-Apostu, A. M., Bolognesi, S., Bordoni, S., Bourgeois, N., Bourguille, B., Bremer, J., Brown, G., Brunetti, G., Brunetti, L., Caiulo, D., Calin, M., Calvo, E., Campanelli, M., Cankocak, K., Cantini, C., Carlus, B., Cautisanu, B. M., Chalifour, M., Chappuis, A., Charitonidis, N., Chatterjee, A., Chiriacescuf, A., Chiu, P., Conforti, S., Cotte, P., Crivelli, P., Cuesta, C., Dawson, J., De Bonis, I., De La Taille, C., Delbart, A., Di Luise, S., Doizon, F., Drancourt, C., Duchesneau, D., Dulucq, F., Duval, F., Emery, S., Ereditato, A., Falcone, A., Fusshoeller, K., Gallego-Ros, A., Galymov, V., Geffroy, N., Gendotti, A., Gherghel-Lascu, A., Gil-Botella, I., Girerd, C., Gomoiu, M. C., Gorodetzky, P., Hamada, E., Hanni, R., Hasegawa, T., Holin, A., Horikawa, S., Ikeno, M., Jiménez, S., Jipa, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasami, K., Kishishita, T., Konari, H., Kreslo, I., Kryn, D., Kunzé, P., Kurokawa, M., Kuromori, Y., Lastoria, C., Lazanu, I., Lehmann-Miotto, G., Leyton, M., Lira, N., Loo, K., Lorca, D., Lutz, P., Lux, T., Maalampi, J., Maire, G., Maki, M., Manenti, L., Margineanu, R. M., Marteau, J., Martin-Chassard, G., Mathez, H., Mazzucato, E., Misitano, G., Mladenov, D., Bueno, L. Molina, Mosu, T. S., Mu, W., Murphy, S., Nakayoshi, K., Narita, S., Navas-Nicolás, D., Negishi, K., Nessi, M., Niculescu-Oglinzanu, M., Noto, F., Noury, A., Onishchuk, Y., Palomares, C., Parvu, M., Patzak, T., Penichot, Y., Pennacchio, E., Periale, L., Pessard, H., Pietropaolo, F., Pugnere, D., Radics, B., Redondo, D., Regenfus, C., Remoto, A., Resnati, F., Ristea, O., Rubbia, A., Saftoiu, A., Sakashita, K., Sanchez, F., Santos, C., Scarpelli, A., Schloesser, C., Sendai, K., Sergiampietri, F., Shahsavarani, S., Shoji, M., Sinclair, J., Soto-Oton, J., Stanca, D. I., Stefan, D., Sulej, R., Tanaka, M., Toboaru, V., Tonazzo, A., Tromeur, W., Trzaska, W. H., Uchida, T., Urda, L., Vannucci, F., Vasseur, G., Verdugo, A., Viant, T., Vihonen, S., Vilalte, S., Weber, M., Wu, S., Yu, J., Zambelli, L., and Zito, M.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The $3 \times 1 \times 1$ m$^3$ demonstrator is a dual phase liquid argon time projection chamber that has recorded cosmic rays events in 2017 at CERN. The light signal in these detectors is crucial to provide precise timing capabilities. The performances of the photon detection system, composed of five PMTs, are discussed. The collected scintillation and electroluminescence light created by passing particles has been studied in various detector conditions. In particular, the scintillation light production and propagation processes have been analyzed and compared to simulations, improving the understanding of some liquid argon properties., Comment: 30 pages, 26 figures
Published: 2020
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112. The great Kite in the sky: a LOFAR observation of the radio source in Abell 2626

Author: Ignesti, A., Shimwell, T., Brunetti, G., Gitti, M., Intema, H., van Weeren, R. J., Hardcastle, M. J., Clarke, A. O., Botteon, A., Di Gennaro, G., Brüggen, M., Browne, I., Mandal, S., Röttgering, H. J. A., Cuciti, V., de Gasperin, F., Cassano, R., and Scaife, A. M. M.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The radio source at the center of the galaxy cluster Abell 2626, also known as the Kite, stands out for its unique morphology composed of four, symmetric arcs. Previous studies have probed the properties of this source at different frequencies and its interplay with the surrounding thermal plasma, but the puzzle of its origin is still unsolved. We use new LOw Frequency ARray (LOFAR) observation from the LOFAR Two-meter Sky Survey at 144 MHz to investigate the origin of the Kite.} We present a detailed analysis of the new radio data which we combined with archival radio and X-ray observations. We have produced a new, resolved spectral index map of the source with a resolution of 7$''$ and we studied the spatial correlation of radio and X-ray emission to investigate the interplay between thermal and non-thermal plasma. The new LOFAR data have changed our view of the Kite by discovering two steep-spectrum ($\alpha<-1.5$) plumes of emission connected to the arcs. The spectral analysis shows, for the first time, a spatial trend of the spectrum along the arcs with evidence of curved synchrotron spectra and a spatial correlation with the X-ray surface brightness. On the basis of our results, we propose that the Kite was originally an X-shaped radio galaxy whose fossil radio plasma, after the end of the activity of the central active galactic nucleus, has been compressed due to motions of the thermal plasma in which it is encompassed. The interplay between the compression and advection of the fossil plasma, with the restarting of the nuclear activity of the central galaxy, could have enhanced the radio emission of the fossil plasma producing the arcs of the Kite. We present also the first, low-frequency observation of a jellyfish galaxy in the same field, in which we detect extended, low-frequency emission without a counterpart at higher frequencies., Comment: 10 pages, 7 figures. Accepted for publication on Astronomy & Astrophysics on 23/09/2020
Published: 2020
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113. Prospects for Beyond the Standard Model Physics Searches at the Deep Underground Neutrino Experiment

Author: DUNE Collaboration, Abi, B., Acciarri, R., Acero, M. A., Adamov, G., Adams, D., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Antonova, M., Antusch, S., Aranda-Fernandez, A., Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., Terrazas, I. Caro, Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. Cervera, Chalifour, M., Chang, C., Chardonnet, E., Chatterjee, A., Chattopadhyay, S., Chaves, J., Chen, H., Chen, M., Chen, Y., Cherdack, D., Chi, C., Childress, S., Chiriacescu, A., Cho, K., Choubey, S., Christensen, A., Christian, D., Christodoulou, G., Church, E., Clarke, P., Coan, T. E., Cocco, A. G., Coelho, J. A. B., Conley, E., Conrad, J. M., Convery, M., Corwin, L., Cotte, P., Cremaldi, L., Cremonesi, L., Crespo-Anadón, J. I., Cristaldo, E., Cross, R., Cuesta, C., Cui, Y., Cussans, D., Dabrowski, M., da Motta, H., Peres, L. Da Silva, David, C., David, Q., Davies, G. S., Davini, S., Dawson, J., De, K., De Almeida, R. M., Debbins, P., De Bonis, I., Decowski, M. P., de Gouvêa, A., De Holanda, P. C., Astiz, I. L. De Icaza, Deisting, A., De Jong, P., Delbart, A., Delepine, D., Delgado, M., Dell'Acqua, A., De Lurgio, P., Neto, J. R. T. de Mello, DeMuth, D. M., Dennis, S., Densham, C., Deptuch, G., De Roeck, A., De Romeri, V., De Vries, J. J., Dharmapalan, R., Dias, M., Diaz, F., Díaz, J. S., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Dokania, N., Dolinski, M. J., Domine, L., Douglas, D., Drielsma, F., Duchesneau, D., Duffy, K., Dunne, P., Durkin, T., Duyang, H., Dvornikov, O., Dwyer, D. A., Dyshkant, A. S., Eads, M., Edmunds, D., Eisch, J., Emery, S., Ereditato, A., Escobar, C. O., Sanchez, L. Escudero, Evans, J. J., Ewart, E., Ezeribe, A. C., Fahey, K., Falcone, A., Farnese, C., Farzan, Y., Felix, J., Fernandez-Martinez, E., Menendez, P. Fernandez, Ferraro, F., Fields, L., Filkins, A., Filthaut, F., Fitzpatrick, R. S., Flanagan, W., Fleming, B., Flight, R., Fowler, J., Fox, W., Franc, J., Francis, K., Franco, D., Freeman, J., Freestone, J., Fried, J., Friedland, A., Fuess, S., Furic, I., Furmanski, A. P., Gago, A., Gallagher, H., Gallego-Ros, A., Gallice, N., Galymov, V., Gamberini, E., Gamble, T., Gandhi, R., Gandrajula, R., Gao, S., Garcia-Gamez, D., García-Peris, M. Á., Gardiner, S., Gastler, D., Ge, G., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Gibin, D., Gil-Botella, I., Girerd, C., Giri, A. K., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Bermeo, L. V. Gomez, Fajardo, L. S. Gomez, Gonnella, F., Gonzalez-Cuevas, J. A., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Graham, M., Gramellini, E., Gran, R., Granados, E., Grant, A., Grant, C., Gratieri, D., Green, P., Green, S., Greenler, L., Greenwood, M., Greer, J., Griffith, W. C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guarino, V., Guenette, R., Guglielmi, A., Guo, B., Guthikonda, K. K., Gutierrez, R., Guzowski, P., Guzzo, M. M., Gwon, S., Habig, A., Hackenburg, A., Hadavand, H., Haenni, R., Hahn, A., Haigh, J., Haiston, J., Hamernik, T., Hamilton, P., Han, J., Harder, K., Harris, D. A., Hartnell, J., Hasegawa, T., Hatcher, R., Hazen, E., Heavey, A., Heeger, K. M., Heise, J., Hennessy, K., Henry, S., Morquecho, M. A. Hernandez, Herner, K., Hertel, L., Hesam, A. S., Hewes, V, Higuera, A., Hill, T., Hillier, S. J., Himmel, A., Hoff, J., Hohl, C., Holin, A., Hoppe, E., Horton-Smith, G. A., Hostert, M., Hourlier, A., Howard, B., Howell, R., Huang, J., Hugon, J., Iles, G., Ilic, N., Iliescu, A. M., Illingworth, R., Ioannisian, A., Itay, R., Izmaylov, A., James, E., Jargowsky, B., Jediny, F., Jesùs-Valls, C., Ji, X., Jiang, L., Jiménez, S., Jipa, A., Joglekar, A., Johnson, C., Johnson, R., Jones, B., Jones, S., Jung, C. K., Junk, T., Jwa, Y., Kabirnezhad, M., Kaboth, A., Kadenko, I., Kamiya, F., Karagiorgi, G., Karcher, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasetti, S. P., Kashur, L., Kazaryan, N., Kearns, E., Keener, P., Kelly, K. J., Kemp, E., Ketchum, W., Kettell, S. 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., Kordosky, M., Kosc, T., Kose, U., Kostelecký, V. A., Kothekar, K., Krennrich, F., Kreslo, I., Kudenko, Y., Kudryavtsev, V. A., Kulagin, S., Kumar, J., Kumar, R., Kuruppu, C., Kus, V., Kutter, T., Lambert, A., Lande, K., Lane, C. E., Lang, K., Langford, T., Lasorak, P., Last, D., Lastoria, C., Laundrie, A., Lawrence, A., Lazanu, I., LaZur, R., Le, T., Learned, J., LeBrun, P., Miotto, G. Lehmann, Lehnert, R., de Oliveira, M. A. Leigui, Leitner, M., Leyton, M., Li, L., Li, S., Li, S. W., Li, T., Li, Y., Liao, H., Lin, C. S., Lin, S., Lister, A., Littlejohn, B. R., Liu, J., Lockwitz, S., Loew, T., Lokajicek, M., Lomidze, I., Long, K., Loo, K., Lorca, D., Lord, T., LoSecco, J. M., Louis, W. C., Luk, K. B., Luo, X., Lurkin, N., Lux, T., Luzio, V. P., MacFarland, D., Machado, A. A., Machado, P., Macias, C. T., Macier, J. R., Maddalena, A., Madigan, P., Magill, S., Mahn, K., Maio, A., Maloney, J. A., Mandrioli, G., Maneira, J., Manenti, L., Manly, S., Mann, A., Manolopoulos, K., Plata, M. Manrique, Marchionni, A., Marciano, W., Marfatia, D., Mariani, C., Maricic, J., Marinho, F., Marino, A. D., Marshak, M., Marshall, C., Marshall, J., Marteau, J., Martin-Albo, J., Martinez, N., Caicedo, D. A. Martinez, Martynenko, S., Mason, K., Mastbaum, A., Masud, M., Matsuno, S., Matthews, J., Mauger, C., Mauri, N., Mavrokoridis, K., Mazza, R., Mazzacane, A., Mazzucato, E., McCluskey, E., McConkey, N., McFarland, K. S., McGrew, C., McNab, A., Mefodiev, A., Mehta, P., Melas, P., Mellinato, M., Mena, O., Menary, S., Mendez, H., Menegolli, A., Meng, G., Messier, M. D., Metcalf, W., Mewes, M., Meyer, H., Miao, T., Michna, G., Miedema, T., Migenda, J., Milincic, R., 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. Molina, Montanari, A., Montanari, C., Montanari, D., Zetina, L. M. Montano, Moon, J., Mooney, M., Moor, A., Moreno, D., Morgan, B., Morris, C., Mossey, C., Motuk, E., Moura, C. A., Mousseau, J., Mu, W., Mualem, L., Mueller, J., Muether, M., Mufson, S., Muheim, F., Muir, A., Mulhearn, M., Muramatsu, H., Murphy, S., Musser, J., Nachtman, J., Nagu, S., Nalbandyan, M., Nandakumar, R., Naples, D., Narita, S., Navas-Nicolás, D., Nayak, N., Nebot-Guinot, M., Necib, L., Negishi, K., Nelson, J. K., Nesbit, J., Nessi, M., Newbold, D., Newcomer, M., Newhart, D., Nichol, R., Niner, E., Nishimura, K., Norman, A., Norrick, A., Northrop, R., Novella, P., Nowak, J. A., Oberling, M., Del Campo, A. Olivares, Olivier, A., Onel, Y., Onishchuk, Y., Ott, J., Pagani, L., Pakvasa, S., Palamara, O., Palestini, S., Paley, J. M., Pallavicini, M., Palomares, C., Pantic, E., Paolone, V., Papadimitriou, V., Papaleo, R., Papanestis, A., Paramesvaran, S., Park, J. C., Parke, S., 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., Penichot, Y., 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., Pillow, J., Pinzino, J., Plunkett, R., Poling, R., Pons, X., Poonthottathil, N., Pordes, S., Potekhin, M., Potenza, R., Potukuchi, B. V. K. S., Pozimski, J., Pozzato, M., Prakash, S., Prakash, T., Prince, S., Prior, G., Pugnere, D., Qi, K., Qian, X., Raaf, J. L., Raboanary, R., Radeka, V., Rademacker, J., Radics, B., Rafique, A., Raguzin, E., Rai, M., Rajaoalisoa, M., Rakhno, I., Rakotondramanana, H. T., Rakotondravohitra, L., Ramachers, Y. A., Rameika, R., Delgado, M. A. Ramirez, Ramson, B., Rappoldi, A., Raselli, G., Ratoff, P., Ravat, S., Razafinime, H., Real, J. S., Rebel, B., Redondo, D., Reggiani-Guzzo, M., Rehak, T., Reichenbacher, J., Reitzner, S. D., Renshaw, A., Rescia, S., Resnati, F., Reynolds, A., Riccobene, G., Rice, L. C. J., Rielage, K., Rigaut, Y., Rivera, D., Rochester, L., Roda, M., Rodrigues, P., Alonso, M. J. Rodriguez, Rondon, J. Rodriguez, Roeth, A. J., Rogers, H., Rosauro-Alcaraz, S., Rossella, M., Rout, J., Roy, S., Rubbia, A., Rubbia, C., Russell, B., Russell, J., Ruterbories, D., Saakyan, R., Sacerdoti, S., Safford, T., Sahu, N., Sala, P., Samios, N., Sanchez, M. C., 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., Schlabach, P., Schmitz, D., Scholberg, K., Schukraft, A., Segreto, E., Sensenig, J., Seong, I., Sergi, A., Sergiampietri, F., Sgalaberna, D., Shaevitz, M. H., Shafaq, S., Shamma, M., Sharma, H. R., Sharma, R., Shaw, T., Shepherd-Themistocleous, C., Shin, S., Shooltz, D., Shrock, R., Simard, L., Simos, N., Sinclair, J., Sinev, G., Singh, J., Singh, V., Sipos, R., Sippach, F. W., Sirri, G., Sitraka, A., Siyeon, K., Smargianaki, D., Smith, A., Smith, E., Smith, P., Smolik, J., Smy, M., Snopok, P., Nunes, M. Soares, Sobel, H., Soderberg, M., Salinas, C. J. Solano, Söldner-Rembold, S., Solomey, N., Solovov, V., Sondheim, W. E., Sorel, M., 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., Steiner, H. M., Stewart, J., Stillwell, B., Stock, J., Stocker, F., Stocks, D., Stokes, T., Strait, M., Strauss, T., Striganov, S., Stuart, A., Summers, D., Surdo, A., Susic, V., Suter, L., Sutera, C. M., Svoboda, R., Szczerbinska, B., Szelc, A. M., Talaga, R., Tanaka, H. A., Oregui, B. Tapia, Tapper, A., Tariq, S., Tatar, E., Tayloe, R., Teklu, A. M., Tenti, M., Terao, K., Ternes, C. A., Terranova, F., Testera, G., Thea, A., Thompson, J. L., Thorn, C., Timm, S. C., Todd, J., Tonazzo, A., Torti, M., Tortola, M., Tortorici, F., Totani, D., Toups, M., Touramanis, C., Trevor, J., Trzaska, W. H., Tsai, Y. -T., Tsamalaidze, Z., Tsang, K. V., Tsverava, N., Tufanli, S., Tull, C., Tyley, E., Tzanov, M., Uchida, M. A., Urheim, J., Usher, T., Vagins, M. R., Vahle, P., Valdiviesso, G. A., Valencia, E., Vallari, Z., Valle, J. W. F., Vallecorsa, S., Van Berg, R., Van de Water, R. G., Forero, D. Vanegas, Varanini, F., Vargas, D., Varner, G., Vasel, J., Vasseur, G., Vaziri, K., Ventura, S., Verdugo, A., Vergani, S., Vermeulen, M. A., Verzocchi, M., de Souza, H. Vieira, Vignoli, C., Vilela, C., Viren, B., Vrba, T., Wachala, T., Waldron, A. V., Wallbank, M., Wang, H., Wang, J., 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., While, M. R., White, A., Whitehead, L. H., Whittington, D., Wilking, M. J., Wilkinson, C., Williams, Z., Wilson, F., Wilson, R. J., Wolcott, J., Wongjirad, T., Wood, K., Wood, L., Worcester, E., Worcester, M., Wret, C., Wu, W., Xiao, Y., Yang, G., Yang, T., Yershov, N., Yonehara, K., Young, T., Yu, B., Yu, J., Zaki, R., Zalesak, J., Zambelli, L., Zamorano, B., Zani, A., Zazueta, L., Zeller, G. P., Zennamo, J., Zeug, K., Zhang, C., Zhao, M., Zhao, Y., Zhivun, E., Zhu, G., Zimmerman, E. D., Zito, M., Zucchelli, S., Zuklin, J., Zutshi, V., and Zwaska, R.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: The Deep Underground Neutrino Experiment (DUNE) will be a powerful tool for a variety of physics topics. The high-intensity proton beams provide a large neutrino flux, sampled by a near detector system consisting of a combination of capable precision detectors, and by the massive far detector system located deep underground. This configuration sets up DUNE as a machine for discovery, as it enables opportunities not only to perform precision neutrino measurements that may uncover deviations from the present three-flavor mixing paradigm, but also to discover new particles and unveil new interactions and symmetries beyond those predicted in the Standard Model (SM). Of the many potential beyond the Standard Model (BSM) topics DUNE will probe, this paper presents a selection of studies quantifying DUNE's sensitivities to sterile neutrino mixing, heavy neutral leptons, non-standard interactions, CPT symmetry violation, Lorentz invariance violation, neutrino trident production, dark matter from both beam induced and cosmogenic sources, baryon number violation, and other new physics topics that complement those at high-energy colliders and significantly extend the present reach., Comment: 54 pages, 40 figures, paper based on the DUNE Technical Design Report (arXiv:2002.03005)
Published: 2020
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114. A giant radio bridge connecting two clusters in Abell 1758

Author: Botteon, A., van Weeren, R. J., Brunetti, G., de Gasperin, F., Intema, H. T., Osinga, E., Di Gennaro, G., Shimwell, T. W., Bonafede, A., Brüggen, M., Cassano, R., Cuciti, V., Dallacasa, D., Gastaldello, F., Mandal, S., Rossetti, M., and Röttgering, H. J. A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Collisions between galaxy clusters dissipate enormous amounts of energy in the intra-cluster medium (ICM) through turbulence and shocks. In the process, Mpc-scale diffuse synchrotron emission in form of radio halos and relics can form. However, little is known about the very early phase of the collision. We used deep radio observations from 53 MHz to 1.5 GHz to study the pre-merging galaxy clusters A1758N and A1758S that are $\sim2$ Mpc apart. We confirm the presence of a giant bridge of radio emission connecting the two systems that was reported only tentatively in our earlier work. This is the second large-scale radio bridge observed to date in a cluster pair. The bridge is clearly visible in the LOFAR image at 144 MHz and tentatively detected at 53 MHz. Its mean radio emissivity is more than one order of magnitude lower than that of the radio halos in A1758N and A1758S. Interestingly, the radio and X-ray emissions of the bridge are correlated. Our results indicate that non-thermal phenomena in the ICM can be generated also in the region of compressed gas in-between infalling systems., Comment: 6 pages, 4 figures, 1 table. Accepted for publication in MNRAS Letters
Published: 2020
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115. The LOFAR view of FR0 radio galaxies

Author: Capetti, A., Brienza, M., Baldi, R. D., Giovannini, G., Morganti, R., Hardcastle, M. J., Rottgering, H. J. A., Brunetti, G. F., Best, P. N., and Miley, G.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We explore the low-frequency radio properties of the sources in the Fanaroff-Riley class 0 catalog (FR0CAT) as seen by the LOw Frequency ARray (LOFAR) observations at 150 MHz. This sample includes 104 compact radio active galactic nuclei (AGN) associated with nearby (z<0.05) massive early-type galaxies. Sixty-six FR0CAT sources are in the sky regions observed by LOFAR and all of them are detected, usually showing point-like structures with sizes smaller than 3-6 kpc. However, 12 FR0s present resolved emission of low surface brightness which contributes between 5% and 40% of the total radio power at 150 MHz, usually with a jetted morphology extending between 15 and 50 kpc. No extended emission is detected around the other FR0s, with a typical luminosity limit of 5 x 10$^{22}$ W/Hz over an area of 100 kpc x 100 kpc. The spectral slopes of FR0s between 150 MHz and 1.4 GHz span a broad range (-0.7 < $\alpha$ < 0.8) with a median value of $\overline\alpha \sim 0.1$; 20% of them have a steep spectrum ($\alpha$ > 0.5), an indication of the presence of substantial extended emission confined within the spatial resolution limit. The fraction of FR0s showing evidence for the presence of jets, by including both spectral and morphological information, is at least ~40%. This study confirms that FR0s and FRIs can be interpreted as two extremes of a continuous population of jetted sources, with the FR0s representing the low end in size and radio power., Comment: Pre-proofs version - Accepted for publication in A&A
Published: 2020
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116. Supernova Neutrino Burst Detection with the Deep Underground Neutrino Experiment

Author: DUNE collaboration, Abi, B., Acciarri, R., Acero, M. A., Adamov, G., Adams, D., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Antonova, M., Antusch, S., Aranda-Fernandez, A., Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., CaroTerrazas, I., Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. Cervera, Chalifour, M., Chang, C., Chardonnet, E., Chatterjee, A., Chattopadhyay, S., Chaves, J., Chen, H., Chen, M., Chen, Y., Cherdack, D., Chi, C., Childress, S., Chiriacescu, A., Cho, K., Choubey, S., Christensen, A., Christian, D., Christodoulou, G., Church, E., Clarke, P., Coan, T. E., Cocco, A. G., Coelho, J. A. B., Conley, E., Conrad, J. M., Convery, M., Corwin, L., Cotte, P., Cremaldi, L., Cremonesi, L., Crespo-Anadón, J. I., Cristaldo, E., Cross, R., Cuesta, C., Cui, Y., Cussans, D., Dabrowski, M., daMotta, H., Peres, L. Da Silva, David, C., David, Q., Davies, G. S., Davini, S., Dawson, J., De, K., De Almeida, R. M., Debbins, P., DeBonis, I., Decowski, M. P., de Gouvêa, A., De Holanda, P. C., Astiz, I. L. De Icaza, Deisting, A., De Jong, P., Delbart, A., Delepine, D., Delgado, M., Dell'Acqua, A., De Lurgio, P., Neto, J. R. T. de Mello, DeMuth, D. M., Dennis, S., Densham, C., Deptuch, G., DeRoeck, A., De Romeri, V., De Vries, J. J., Dharmapalan, R., Dias, M., Diaz, F., Díaz, J. S., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Dokania, N., Dolinski, M. J., Domine, L., Douglas, D., Drielsma, F., Duchesneau, D., Duffy, K., Dunne, P., Durkin, T., Duyang, H., Dvornikov, O., Dwyer, D. A., Dyshkant, A. S., Eads, M., Edmunds, D., Eisch, J., Emery, S., Ereditato, A., Escobar, C. O., Sanchez, L. Escudero, Evans, J. J., Ewart, E., Ezeribe, A. C., Fahey, K., Falcone, A., Farnese, C., Farzan, Y., Felix, J., Fernandez-Martinez, E., Menendez, P. Fernandez, Ferraro, F., Fields, L., Filkins, A., Filthaut, F., Fitzpatrick, R. S., Flanagan, W., Fleming, B., Flight, R., Fowler, J., Fox, W., Franc, J., Francis, K., Franco, D., Freeman, J., Freestone, J., Fried, J., Friedland, A., Fuess, S., Furic, I., Furmanski, A. P., Gago, A., Gallagher, H., Gallego-Ros, A., Gallice, N., Galymov, V., Gamberini, E., Gamble, T., Gandhi, R., Gandrajula, R., Gao, S., Garcia-Gamez, D., García-Peris, M. Á., Gardiner, S., Gastler, D., Ge, G., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Gibin, D., Gil-Botella, I., Girerd, C., Giri, A. K., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Bermeo, L. V. Gomez, Fajardo, L. S. Gomez, Gonnella, F., Gonzalez-Cuevas, J. A., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Graham, M., Gramellini, E., Gran, R., Granados, E., Grant, A., Grant, C., Gratieri, D., Green, P., Green, S., Greenler, L., Greenwood, M., Greer, J., Griffith, W. C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guarino, V., Guenette, R., Guglielmi, A., Guo, B., Guthikonda, K. K., Gutierrez, R., Guzowski, P., Guzzo, M. M., Gwon, S., Habig, A., Hackenburg, A., Hadavand, H., Haenni, R., Hahn, A., Haigh, J., Haiston, J., Hamernik, T., Hamilton, P., Han, J., Harder, K., Harris, D. A., Hartnell, J., Hasegawa, T., Hatcher, R., Hazen, E., Heavey, A., Heeger, K. M., Heise, J., Hennessy, K., Henry, S., Morquecho, M. A. Hernandez, Herner, K., Hertel, L., Hesam, A. S., Hewes, V, Higuera, A., Hill, T., Hillier, S. J., Himmel, A., Hoff, J., Hohl, C., Holin, A., Hoppe, E., Horton-Smith, G. A., Hostert, M., Hourlier, A., Howard, B., Howell, R., Huang, J., Hugon, J., Iles, G., Ilic, N., Iliescu, A. M., Illingworth, R., Ioannisian, A., Itay, R., Izmaylov, A., James, E., Jargowsky, B., Jediny, F., Jesùs-Valls, C., Ji, X., Jiang, L., Jiménez, S., Jipa, A., Joglekar, A., Johnson, C., Johnson, R., Jones, B., Jones, S., Jung, C. K., Junk, T., Jwa, Y., Kabirnezhad, M., Kaboth, A., Kadenko, I., Kamiya, F., Karagiorgi, G., Karcher, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasetti, S. P., Kashur, L., Kazaryan, N., Kearns, E., Keener, P., Kelly, K. J., Kemp, E., Ketchum, W., Kettell, S. 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., Kordosky, M., Kosc, T., Kose, U., Kostelecký, V. A., Kothekar, K., Krennrich, F., Kreslo, I., Kudenko, Y., Kudryavtsev, V. A., Kulagin, S., Kumar, J., Kumar, R., Kuruppu, C., Kus, V., Kutter, T., Lambert, A., Lande, K., Lane, C. E., Lang, K., Langford, T., Lasorak, P., Last, D., Lastoria, C., Laundrie, A., Lawrence, A., Lazanu, I., LaZur, R., Le, T., Learned, J., LeBrun, P., Miotto, G. Lehmann, Lehnert, R., de Oliveira, M. A. Leigui, Leitner, M., Leyton, M., Li, L., Li, S., Li, S. W., Li, T., Li, Y., Liao, H., Lin, C. S., Lin, S., Lister, A., Littlejohn, B. R., Liu, J., Lockwitz, S., Loew, T., Lokajicek, M., Lomidze, I., Long, K., Loo, K., Lorca, D., Lord, T., LoSecco, J. M., Louis, W. C., Luk, K. 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Subjects: High Energy Physics - Experiment, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Nuclear Experiment, Physics - Instrumentation and Detectors
Abstract: The Deep Underground Neutrino Experiment (DUNE), a 40-kton underground liquid argon time projection chamber experiment, will be sensitive to the electron-neutrino flavor component of the burst of neutrinos expected from the next Galactic core-collapse supernova. Such an observation will bring unique insight into the astrophysics of core collapse as well as into the properties of neutrinos. The general capabilities of DUNE for neutrino detection in the relevant few- to few-tens-of-MeV neutrino energy range will be described. As an example, DUNE's ability to constrain the $\nu_e$ spectral parameters of the neutrino burst will be considered., Comment: 29 pages, 17 figures; paper based on DUNE Technical Design Report. arXiv admin note: substantial text overlap with arXiv:2002.03005
Published: 2020
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117. Reaching thermal noise at ultra-low radio frequencies: the Toothbrush radio relic downstream of the shock front

Author: de Gasperin, F., Brunetti, G., Bruggen, M., van Weeren, R., Williams, W. L., Botteon, A., Cuciti, V., Dijkema, T. J., Edler, H., Iacobelli, M., Kang, H., Offringa, A., Orru, E., Pizzo, R., Rafferty, D., Rottgering, H., and Shimwell, T.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Ultra-low frequency observations (<100 MHz) are particularly challenging because they are usually performed in a low signal-to-noise ratio regime due to the high sky temperature and because of ionospheric disturbances whose effects are inversely proportional to the observing frequency. Nonetheless, these observations are crucial to study the emission from low-energy populations of cosmic rays. We aim to obtain the first thermal-noise limited (~ 1.5 mJy/beam) deep continuum radio map using the LOFAR Low Band Antenna (LBA) system. Our demonstration observation targeted the galaxy cluster RX J0603.3+4214 (the "Toothbrush" cluster). We used the resulting ultra-low frequency (58 MHz) image to study cosmic-ray acceleration and evolution in the post shock region, as well as their relation with the presence of a radio halo. We describe the data reduction we have used to calibrate LOFAR LBA observations. The resulting image is combined with observations at higher frequencies (LOFAR 150 MHz and VLA 1500 MHz) to extract spectral information. We obtained the first thermal-noise limited image from an observation carried out with the LOFAR LBA system using all Dutch stations at a central frequency of 58 MHz. With 8 hours of data, we reached an rms noise of 1.3 mJy/beam at a resolution of 18" x 11". The procedure we have developed is an important step forward towards routine high-fidelity imaging with the LOFAR LBA. The analysis of the radio spectra shows that the radio relic extends to distances of 800 kpc downstream from the shock front, larger than what allowed by electron cooling time. Furthermore, the shock wave started accelerating electrons already at a projected distance of <300 kpc from the crossing point of the two clusters. These results can be explained if electrons are reaccelerated downstream by background turbulence possibly combined with projection effects., Comment: 15 pages, 19 figures, accepted A&A
Published: 2020
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118. First results on ProtoDUNE-SP liquid argon time projection chamber performance from a beam test at the CERN Neutrino Platform

Author: DUNE Collaboration, Abi, B., Abud, A. Abed, Acciarri, R., Acero, M. A., Adamov, G., Adamowski, M., Adams, D., Adrien, P., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Antonova, M., Antusch, S., Aranda-Fernandez, A., Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Baller, B., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., Terrazas, I. Caro, Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. Cervera, Chalifour, M., Chang, C., Chardonnet, E., Charitonidis, N., Chatterjee, A., Chattopadhyay, S., Chatzidaki, P., Chaves, J., Chen, H., Chen, M., Chen, Y., Cherdack, D., Chi, C., Childress, S., Chiriacescu, A., Cho, K., Choubey, S., Christensen, A., Christian, D., Christodoulou, G., Church, E., Clarke, P., Coan, T. E., Cocco, A. G., Coelho, J. A. B., Conley, E., Conrad, J. M., Convery, M., Corwin, L., Cotte, P., Cremaldi, L., Cremonesi, L., Crespo-Anadón, J. I., Cristaldo, E., Cross, R., Cuesta, C., Cui, Y., Cussans, D., Dabrowski, M., da Motta, H., Peres, L. Da Silva, David, C., David, Q., Davies, G. S., Davini, S., Dawson, J., De, K., De Almeida, R. M., Debbins, P., De Bonis, I., Decowski, M. P., de Gouvêa, A., De Holanda, P. C., Astiz, I. L. De Icaza, Deisting, A., De Jong, P., Delbart, A., Delepine, D., Delgado, M., Dell'Acqua, A., De Lurgio, P., Neto, J. R. T. de Mello, DeMuth, D. M., Dennis, S., Densham, C., Deptuch, G., De Roeck, A., De Romeri, V., De Vries, J. J., Dharmapalan, R., Dias, M., Diaz, F., Díaz, J. S., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Dokania, N., Dolinski, M. J., Domine, L., Douglas, D., Drake, G., Drielsma, F., Duchesneau, D., Duffy, K., Dunne, P., Durkin, T., Duyang, H., Dvornikov, O., Dwyer, D. A., Dyshkant, A. S., Eads, M., Edmunds, D., Eisch, J., Emery, S., Ereditato, A., Escobar, C. O., Sanchez, L. Escudero, Evans, J. J., Ewart, E., Ezeribe, A. C., Fabre, C., Fahey, K., Falcone, A., Farnese, C., Farzan, Y., Felix, J., Fernandez-Martinez, E., Menendez, P. Fernandez, Ferraro, F., Fields, L., Filkins, A., Filthaut, F., Fitzpatrick, R. S., Flanagan, W., Fleming, B., Flight, R., Fowler, J., Fox, W., Franc, J., Francis, K., Franco, D., Freeman, J., Freestone, J., Fried, J., Friedland, A., Fuess, S., Furic, I., Furmanski, A. P., Gago, A., Gallagher, H., Gallego-Ros, A., Gallice, N., Galymov, V., Gamberini, E., Gamble, T., Gandhi, R., Gandrajula, R., Gao, S., Garcia-Gamez, D., García-Peris, M. Á., Gardiner, S., Gastler, D., Ge, G., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Gibin, D., Gil-Botella, I., Girerd, C., Giri, A. K., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Bermeo, L. V. Gomez, Fajardo, L. S. Gomez, Gonnella, F., Gonzalez-Cuevas, J. A., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Graham, M., Gramellini, E., Gran, R., Granados, E., Grant, A., Grant, C., Gratieri, D., Green, P., Green, S., Greenler, L., Greenwood, M., Greer, J., Griffith, W. C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guarino, V., Guenette, R., Guglielmi, A., Guo, B., Guthikonda, K. K., Gutierrez, R., Guzowski, P., Guzzo, M. 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D., Zito, M., Zucchelli, S., Zuklin, J., Zutshi, V., and Zwaska, R.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The ProtoDUNE-SP detector is a single-phase liquid argon time projection chamber with an active volume of $7.2\times 6.0\times 6.9$ m$^3$. It is installed at the CERN Neutrino Platform in a specially-constructed beam that delivers charged pions, kaons, protons, muons and electrons with momenta in the range 0.3 GeV$/c$ to 7 GeV/$c$. Beam line instrumentation provides accurate momentum measurements and particle identification. The ProtoDUNE-SP detector is a prototype for the first far detector module of the Deep Underground Neutrino Experiment, and it incorporates full-size components as designed for that module. This paper describes the beam line, the time projection chamber, the photon detectors, the cosmic-ray tagger, the signal processing and particle reconstruction. It presents the first results on ProtoDUNE-SP's performance, including noise and gain measurements, $dE/dx$ calibration for muons, protons, pions and electrons, drift electron lifetime measurements, and photon detector noise, signal sensitivity and time resolution measurements. The measured values meet or exceed the specifications for the DUNE far detector, in several cases by large margins. ProtoDUNE-SP's successful operation starting in 2018 and its production of large samples of high-quality data demonstrate the effectiveness of the single-phase far detector design., Comment: 93 pages, 70 figures
Published: 2020
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119. Long-baseline neutrino oscillation physics potential of the DUNE experiment

Author: DUNE Collaboration, Abi, B., Acciarri, R., Acero, M. A., Adamov, G., Adams, D., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Antonova, M., Antusch, S., Aranda-Fernandez, A., Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., Terrazas, I. Caro, Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. 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J., Dharmapalan, R., Dias, M., Diaz, F., Díaz, J. S., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Dokania, N., Dolinski, M. J., Domine, L., Douglas, D., Drielsma, F., Duchesneau, D., Duffy, K., Dunne, P., Durkin, T., Duyang, H., Dvornikov, O., Dwyer, D. A., Dyshkant, A. S., Eads, M., Edmunds, D., Eisch, J., Emery, S., Ereditato, A., Escobar, C. O., Sanchez, L. Escudero, Evans, J. J., Ewart, E., Ezeribe, A. C., Fahey, K., Falcone, A., Farnese, C., Farzan, Y., Felix, J., Fernandez-Martinez, E., Menendez, P. Fernandez, Ferraro, F., Fields, L., Filkins, A., Filthaut, F., Fitzpatrick, R. S., Flanagan, W., Fleming, B., Flight, R., Fowler, J., Fox, W., Franc, J., Francis, K., Franco, D., Freeman, J., Freestone, J., Fried, J., Friedland, A., Fuess, S., Furic, I., Furmanski, A. P., Gago, A., Gallagher, H., Gallego-Ros, A., Gallice, N., Galymov, V., Gamberini, E., Gamble, T., Gandhi, R., Gandrajula, R., Gao, S., Garcia-Gamez, D., García-Peris, M. Á., Gardiner, S., Gastler, D., Ge, G., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Gibin, D., Gil-Botella, I., Girerd, C., Giri, A. K., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Bermeo, L. V. Gomez, Fajardo, L. S. Gomez, Gonnella, F., Gonzalez-Cuevas, J. A., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Graham, M., Gramellini, E., Gran, R., Granados, E., Grant, A., Grant, C., Gratieri, D., Green, P., Green, S., Greenler, L., Greenwood, M., Greer, J., Griffith, W. C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guarino, V., Guenette, R., Guglielmi, A., Guo, B., Guthikonda, K. K., Gutierrez, R., Guzowski, P., Guzzo, M. M., Gwon, S., Habig, A., Hackenburg, A., Hadavand, H., Haenni, R., Hahn, A., Haigh, J., Haiston, J., Hamernik, T., Hamilton, P., Han, J., Harder, K., Harris, D. A., Hartnell, J., Hasegawa, T., Hatcher, R., Hazen, E., Heavey, A., Heeger, K. M., Heise, J., Hennessy, K., Henry, S., Morquecho, M. A. Hernandez, Herner, K., Hertel, L., Hesam, A. S., Hewes, V, Higuera, A., Hill, T., Hillier, S. J., Himmel, A., Hoff, J., Hohl, C., Holin, A., Hoppe, E., Horton-Smith, G. A., Hostert, M., Hourlier, A., Howard, B., Howell, R., Huang, J., Hugon, J., Iles, G., Ilic, N., Iliescu, A. M., Illingworth, R., Ioannisian, A., Itay, R., Izmaylov, A., James, E., Jargowsky, B., Jediny, F., Jesùs-Valls, C., Ji, X., Jiang, L., Jiménez, S., Jipa, A., Joglekar, A., Johnson, C., Johnson, R., Jones, B., Jones, S., Jung, C. K., Junk, T., Jwa, Y., Kabirnezhad, M., Kaboth, A., Kadenko, I., Kamiya, F., Karagiorgi, G., Karcher, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasetti, S. 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B., Luo, X., Lurkin, N., Lux, T., Luzio, V. P., MacFarland, D., Machado, A. A., Machado, P., Macias, C. T., Macier, J. R., Maddalena, A., Madigan, P., Magill, S., Mahn, K., Maio, A., Maloney, J. A., Mandrioli, G., Maneira, J., Manenti, L., Manly, S., Mann, A., Manolopoulos, K., Plata, M. Manrique, Marchionni, A., Marciano, W., Marfatia, D., Mariani, C., Maricic, J., Marinho, F., Marino, A. D., Marshak, M., Marshall, C., Marshall, J., Marteau, J., Martin-Albo, J., Martinez, N., Caicedo, D. A. Martinez, Martynenko, S., Mason, K., Mastbaum, A., Masud, M., Matsuno, S., Matthews, J., Mauger, C., Mauri, N., Mavrokoridis, K., Mazza, R., Mazzacane, A., Mazzucato, E., McCluskey, E., McConkey, N., McFarland, K. S., McGrew, C., McNab, A., Mefodiev, A., Mehta, P., Melas, P., Mellinato, M., Mena, O., Menary, S., Mendez, H., Menegolli, A., Meng, G., Messier, M. 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Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: The sensitivity of the Deep Underground Neutrino Experiment (DUNE) to neutrino oscillation is determined, based on a full simulation, reconstruction, and event selection of the far detector and a full simulation and parameterized analysis of the near detector. Detailed uncertainties due to the flux prediction, neutrino interaction model, and detector effects are included. DUNE will resolve the neutrino mass ordering to a precision of 5$\sigma$, for all $\delta_{\mathrm{CP}}$ values, after 2 years of running with the nominal detector design and beam configuration. It has the potential to observe charge-parity violation in the neutrino sector to a precision of 3$\sigma$ (5$\sigma$) after an exposure of 5 (10) years, for 50\% of all $\delta_{\mathrm{CP}}$ values. It will also make precise measurements of other parameters governing long-baseline neutrino oscillation, and after an exposure of 15 years will achieve a similar sensitivity to $\sin^{2} 2\theta_{13}$ to current reactor experiments., Comment: arXiv admin note: substantial text overlap with arXiv:2002.03005; Updated after referee comments
Published: 2020
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120. Neutrino interaction classification with a convolutional neural network in the DUNE far detector

Author: DUNE Collaboration, Abi, B., Acciarri, R., Acero, M. A., Adamov, G., Adams, D., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Antonova, M., Antusch, S., Aranda-Fernandez, A., Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., Terrazas, I. Caro, Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. 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A., Oberling, M., Del Campo, A. Olivares, Olivier, A., Onel, Y., Onishchuk, Y., Ott, J., Pagani, L., Pakvasa, S., Palamara, O., Palestini, S., Paley, J. M., Pallavicini, M., Palomares, C., Pantic, E., Paolone, V., Papadimitriou, V., Papaleo, R., Papanestis, A., Paramesvaran, S., Parke, S., 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., Penichot, Y., 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., Pillow, J., Pinzino, J., Plunkett, R., Poling, R., Pons, X., Poonthottathil, N., Pordes, S., Potekhin, M., Potenza, R., Potukuchi, B. V. K. S., Pozimski, J., Pozzato, M., Prakash, S., Prakash, T., Prince, S., Prior, G., Pugnere, D., Qi, K., Qian, X., Raaf, J. L., Raboanary, R., Radeka, V., Rademacker, J., Radics, B., Radovic, A., Rafique, A., Raguzin, E., Rai, M., Rajaoalisoa, M., Rakhno, I., Rakotondramanana, H. T., Rakotondravohitra, L., Ramachers, Y. A., Rameika, R., Delgado, M. A. Ramirez, Ramson, B., Rappoldi, A., Raselli, G., Ratoff, P., Ravat, S., Razafinime, H., Real, J. S., Rebel, B., Redondo, D., Reggiani-Guzzo, M., Rehak, T., Reichenbacher, J., Reitzner, S. D., Renshaw, A., Rescia, S., Resnati, F., Reynolds, A., Riccobene, G., Rice, L. C. J., Rielage, K., Rigaut, Y., Rivera, D., Rochester, L., Roda, M., Rodrigues, P., Alonso, M. J. Rodriguez, Rondon, J. Rodriguez, Roeth, A. J., Rogers, H., Rosauro-Alcaraz, S., Rossella, M., Rout, J., Roy, S., Rubbia, A., Rubbia, C., Russell, B., Russell, J., Ruterbories, D., Saakyan, R., Sacerdoti, S., Safford, T., Sahu, N., Sala, P., Samios, N., Sanchez, M. C., 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., Schlabach, P., Schmitz, D., Scholberg, K., Schukraft, A., Segreto, E., Sensenig, J., Seong, I., Sergi, A., Sergiampietri, F., Sgalaberna, D., Shaevitz, M. H., Shafaq, S., Shamma, M., Sharma, H. R., Sharma, R., Shaw, T., Shepherd-Themistocleous, C., Shin, S., Shooltz, D., Shrock, R., Simard, L., Simos, N., Sinclair, J., Sinev, G., Singh, J., Singh, V., Sipos, R., Sippach, F. W., Sirri, G., Sitraka, A., Siyeon, K., Smargianaki, D., Smith, A., Smith, E., Smith, P., Smolik, J., Smy, M., Snopok, P., Nunes, M. Soares, Sobel, H., Soderberg, M., Salinas, C. J. Solano, Söldner-Rembold, S., Solomey, N., Solovov, V., Sondheim, W. E., Sorel, M., 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., Steiner, H. M., Stewart, J., Stillwell, B., Stock, J., Stocker, F., Stokes, T., Strait, M., Strauss, T., Striganov, S., Stuart, A., Summers, D., Surdo, A., Susic, V., Suter, L., Sutera, C. M., Svoboda, R., Szczerbinska, B., Szelc, A. M., Talaga, R., Tanaka, H. A., Oregui, B. Tapia, Tapper, A., Tariq, S., Tatar, E., Tayloe, R., Teklu, A. M., Tenti, M., Terao, K., Ternes, C. A., Terranova, F., Testera, G., Thea, A., Thompson, J. L., Thorn, C., Timm, S. C., Tonazzo, A., Torti, M., Tortola, M., Tortorici, F., Totani, D., Toups, M., Touramanis, C., Trevor, J., Trzaska, W. H., Tsai, Y. T., Tsamalaidze, Z., Tsang, K. V., Tsverava, N., Tufanli, S., Tull, C., Tyley, E., Tzanov, M., Uchida, M. A., Urheim, J., Usher, T., Vagins, M. R., Vahle, P., Valdiviesso, G. A., Valencia, E., Vallari, Z., Valle, J. W. F., Vallecorsa, S., Van Berg, R., Van de Water, R. G., Forero, D. Vanegas, Varanini, F., Vargas, D., Varner, G., Vasel, J., Vasseur, G., Vaziri, K., Ventura, S., Verdugo, A., Vergani, S., Vermeulen, M. A., Verzocchi, M., de Souza, H. Vieira, Vignoli, C., Vilela, C., Viren, B., Vrba, T., Wachala, T., Waldron, A. V., Wallbank, M., Wang, H., Wang, J., 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., While, M. R., White, A., Whitehead, L. H., Whittington, D., Wilking, M. J., Wilkinson, C., Williams, Z., Wilson, F., Wilson, R. J., Wolcott, J., Wongjirad, T., Wood, K., Wood, L., Worcester, E., Worcester, M., Wret, C., Wu, W., Xiao, Y., Yang, G., Yang, T., Yershov, N., Yonehara, K., Young, T., Yu, B., Yu, J., 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., Zimmerman, E. D., Zito, M., Zucchelli, S., Zuklin, J., Zutshi, V., and Zwaska, R.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The Deep Underground Neutrino Experiment is a next-generation neutrino oscillation experiment that aims to measure $CP$-violation in the neutrino sector as part of a wider physics program. A deep learning approach based on a convolutional neural network has been developed to provide highly efficient and pure selections of electron neutrino and muon neutrino charged-current interactions. The electron neutrino (antineutrino) selection efficiency peaks at 90% (94%) and exceeds 85% (90%) for reconstructed neutrino energies between 2-5 GeV. The muon neutrino (antineutrino) event selection is found to have a maximum efficiency of 96% (97%) and exceeds 90% (95%) efficiency for reconstructed neutrino energies above 2 GeV. When considering all electron neutrino and antineutrino interactions as signal, a selection purity of 90% is achieved. These event selections are critical to maximize the sensitivity of the experiment to $CP$-violating effects., Comment: 39 pages, 11 figures
Published: 2020
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121. LOFAR Observations of X-ray Cavity Systems

Author: Bîrzan, L., Rafferty, D. A., Brüggen, M., Botteon, A., Brunetti, G., Cuciti, V., Edge, A. C., Morganti, R., Röttgering, H. J. A., and Shimwell, T. W.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present LOFAR observations at 120-168 MHz of 42 systems with possible X-ray cavities in their hot atmosphere, of which 17 are groups or ellipticals, 19 are nearby clusters (z<0.3), and six are higher-redshift clusters (z>0.3). The X-ray cavities, formed by the radio lobes of the central active galactic nucleus (AGN), are evidence of radio-mode AGN feedback. In the groups and ellipticals sample, more than half of the systems have X-ray cavities for which no associated lobe emission was detected. Conversely, we report the discovery of large radio lobes in NGC 6338, extending far beyond the emission reported previously in the literature. In the case of the nearby clusters, our observations show that there is little low-frequency radio emission that extends beyond the cavities (e.g., MS 0735.6+7421 and A2052). For the first time, we report secure cavity-radio associations in 2A 0335+096, ZwCl 2701, and ZwCl 8276 that strengthens their interpretation as AGN-created cavities. However, in some known cavity systems (e.g., A1795 and ZwCl 3146) we report the lack of detectable low-frequency radio emission associated with the cavities. Our sample of higher-redshift systems is small, and unfortunately the present LOFAR observations are not able to resolve the lobes in many of them. Nevertheless, our sample represents one of the best available for investigating the connection between radio and jet power in radio-mode AGN feedback., Comment: 26 pages, 7 figures, 3 tables, MNRAS accepted. Revised to match published version
Published: 2020
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122. The ENUBET positron tagger prototype: construction and testbeam performance

Author: Acerbi, F., Bonesini, M., Bramati, F., Branca, A., Brizzolari, C., Brunetti, G., Capelli, S., Carturan, S., Catanesi, M. G., Cecchini, S., Cindolo, F., Collazuol, G., Conti, E., Corso, F. Dal, Delogu, C., De Rosa, G., Falcone, A., Gola, A., Jollet, C., Klicek, B., Kudenko, Y., Laveder, M., Longhin, A., Ludovici, L., Lutsenko, E., Magaletti, L., Mandrioli, G., Margotti, A., Mascagna, V., Mauri, N., Meazza, L., Meregaglia, A., Mezzetto, M., Paoloni, A., Pari, M., Parozzi, E., Pasqualini, L., Paternoster, G., Patrizii, L., Pozzato, M., Prest, M., Pupilli, F., Radicioni, E., Riccio, C., Ruggeri, A. C., Scian, C., Sirri, G., Stipcevic, M., Tenti, M., Terranova, F., Torti, M., Vallazza, E., and Votano, L.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: A prototype for the instrumented decay tunnel of ENUBET was tested in 2018 at the CERN East Area facility with charged particles up to 5 GeV. This detector is a longitudinal sampling calorimeter with lateral scintillation light readout. The calorimeter was equipped by an additional "$t_0$-layer" for timing and photon discrimination. The performance of this detector in terms of electron energy resolution, linearity, response to muons and hadron showers are presented in this paper and compared with simulation. The $t_0$-layer was studied both in standalone mode using pion charge exchange and in combined mode with the calorimeter to assess the light yield and the 1 mip/2 mip separation capability. We demonstrate that this system fulfills the requirements for neutrino physics applications and discuss performance and additional improvements., Comment: 23 pages, 20 figures, to appear in JINST
Published: 2020
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123. The beautiful mess in Abell 2255

Author: Botteon, A., Brunetti, G., van Weeren, R. J., Shimwell, T. W., Pizzo, R. F., Cassano, R., Iacobelli, M., Gastaldello, F., Bîrzan, L., Bonafede, A., Brüggen, M., Cuciti, V., Dallacasa, D., de Gasperin, F., Di Gennaro, G., Drabent, A., Hardcastle, M. J., Hoeft, M., Mandal, S., Röttgering, H. J. A., and Simionescu, A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present LOFAR observations of one of the most spectacular objects in the radio sky: Abell 2255. This is a nearby ($z = 0.0806$) merging galaxy cluster hosting one of the first radio halos ever detected in the intra-cluster medium (ICM). The deep LOFAR images at 144 MHz of the central $\sim10$ Mpc$^2$ region show a plethora of emission on different scales, from tens of kpc to above Mpc sizes. In this work, we focus on the innermost region of the cluster. Among the numerous interesting features observed, we discover remarkable bright and filamentary structures embedded in the radio halo. We incorporate archival WSRT 1.2 GHz data to study the spectral properties of the diffuse synchrotron emission and find a very complex spectral index distribution in the halo spanning a wide range of values. We combine the radio data with Chandra observations to investigate the connection between the thermal and non-thermal components by quantitatively comparing the radio and X-ray surface brightness and the spectral index of the radio emission with the thermodynamical quantities of the ICM. Despite the multitude of structures observed in the radio halo, we find that the X-ray and radio emission are overall well correlated. The fact that the steepest spectrum emission is located in the cluster center and traces regions with high entropy possibly suggests the presence of seed particles injected by radio galaxies that are spread in the ICM by turbulence generating the extended radio halo., Comment: 17 pages, 13 figures, 4 tables (including appendix). Accepted for publication in ApJ
Published: 2020
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124. Jansky VLA observations of synchrotron emitting optical hotspots of 3C 227 and 3C 445 radio galaxies

Author: Orienti, M., Migliori, G., Brunetti, G., Nagai, H., D'Ammando, F., Mack, K. -H., and Prieto, M. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report results on deep Jansky Very Large Array A-configuration observations at 22 GHz of the hotspots of the radio galaxies 3C227 and 3C445. Synchrotron emission in the optical on scales up to a few kpc was reported for the four hotspots. Our VLA observations point out the presence of unresolved regions with upper limit to their linear size of about 100 pc. This is the first time that such compact components in hotspots have been detected in a mini-sample, indicating that they are not a peculiar characteristic of a few individual hotspots. The polarization may reach values up to 70 per cent in compact (about 0.1 kpc scale) regions within the hotspot, indicating a highly ordered magnetic field with size up to a hundred parsecs. On larger scales, the average polarization of the hotspot component is about 30-45 per cent, suggesting the presence of a significant random field component, rather than an ordered magnetic field. This is further supported by the displacement between the peaks in polarized intensity and in total intensity images that is observed in all the four hotspots. The electric vector position angle is not constant, but changes arbitrarily in the central part of the hotspot regions, whereas it is usually perpendicular to the total intensity contours of the outermost edge of the hotspot structure, likely marking the large-scale shock front. The misalignment between X-ray and radio-to-optical emission suggests that the former is tracing the current particle acceleration, whereas the latter marks older shock fronts., Comment: 12 pages, 13 figures, published in MNRAS
Published: 2020
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125. Particle acceleration in low-power hotspots: modelling the broad-band spectral energy distribution

Author: Migliori, G., Orienti, M., Coccato, L., Brunetti, G., D'Ammando, F., Mack, K. -H., and Prieto, M. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The acceleration and radiative processes active in low-power radio hotspots are investigated by means of new deep near-infrared (NIR) and optical VLT observations, complemented with archival, high-sensitivity VLT, radio VLA and X-ray Chandra data. For the three studied radio galaxies (3C 105, 3C 195 and 3C 227), we confirm the detection of NIR/optical counterparts of the observed radio hotspots. We resolve multiple components in 3C 227 West and in 3C 105 South and characterize the diffuse NIR/optical emission of the latter. We show that the linear size of this component ($\gtrsim$4 kpc) makes 3C 105 South a compelling case for particles' re-acceleration in the post-shock region. Modeling of the radio-to-X-ray spectral energy distribution (SED) of 3C 195 South and 3C 227 W1 gives clues on the origin of the detected X-ray emission. In the context of inverse Compton models, the peculiarly steep synchrotron curve of 3C 195 South sets constraints on the shape of the radiating particles' spectrum that are testable with better knowledge of the SED shape at low ($\lesssim$GHz) radio frequencies and in X-rays. The X-ray emission of 3C 227 W1 can be explained with an additional synchrotron component originating in compact ($<$100 pc) regions, such those revealed by radio observations at 22 GHz, provided that efficient particle acceleration ($\gamma\gtrsim$10$^7$) is ongoing. The emerging picture is that of systems in which different acceleration and radiative processes coexist., Comment: 16 pages, 10 figures, accepted for publication in MNRAS
Published: 2020
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126. Low-frequency observations of the Giant Radio Galaxy NGC 6251

Author: Cantwell, T. M., Bray, J. D., Croston, J. H., Scaife, A. M. M., Mulcahy, D. D., Best, P. N., Bruggen, M., Brunetti, G., Callingham, J. R., Clarke, A. O., Hardcastle, M. J., Harwood, J. J., Heald, G., Heesen, V., Iacobelli, M., Jamrozy, M., Morganti, R., Orru, E., O'Sullivan, S. P., Riseley, C. J., Rottgering, H. J. A., Shulevski, A., Sridhar, S. S., Tasse, C., and Van Eck, C. L.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present LOFAR observations at 150 MHz of the borderline FRI/FRII giant radio galaxy NGC 6251. This paper presents the most sensitive and highest-resolution images of NGC 6251 at these frequencies to date, revealing for the first time a low-surface-brightness extension to the northern lobe, and a possible backflow associated with the southern lobe. The integrated spectra of components of NGC 6251 are consistent with previous measurements at higher frequencies, similar to results from other LOFAR studies of nearby radio galaxies. We find the outer structures of NGC 6251 to be either at equipartition or slightly electron dominated, similar to those of FRII sources rather than FRIs; but this conclusion remains tentative because of uncertainties associated with the geometry and the extrapolation of X-ray measurements to determine the external pressure distribution on the scale of the outer lobes. We place lower limits on the ages of the extension of the northern lobe and the backflow of the southern lobe of $t \gtrsim 250$ Myr and $t \gtrsim 210$ Myr respectively. We present the first detection of polarisation at 150 MHz in NGC 6251. Taking advantage of the high Faraday resolution of LOFAR, we place an upper limit on the magnetic field in the group of $B < 0.2 (\Lambda_B / 10 {\rm kpc})^{-0.5} \mu$G for a coherence scale of $\Lambda_B < 60 {\rm kpc}$ and $B < 13 \mu$G for $\Lambda_B = 240$ kpc., Comment: 19 pages, 17 figures; accepted by MNRAS
Published: 2020
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127. The hadronic beamline of the ENUBET neutrino beam

Author: ENUBET collaboration, Delogu, C., Acerbi, F., Berra, A., Bonesini, M., Branca, A., Brizzolari, C., Brunetti, G., Calviani, M., Capelli, S., Carturan, S., Catanesi, M. G., Cecchini, S., Charitonidis, N., Cindolo, F., Collazuol, G., Conti, E., Corso, F. Dal, De Rosa, G., Falcone, A., Gola, A., Jollet, C., Kain, V., Klicek, B., Kudenko, Y., Laveder, M., Longhin, A., Ludovici, L., Lutsenko, E., Magaletti, L., Mandrioli, G., Margotti, A., Mascagna, V., Mauri, N., Meazza, L., Meregaglia, A., Mezzetto, M., Nessi, M., Paoloni, A., Pari, M., Parozzi, E., Pasqualini, L., Paternoster, G., Patrizii, L., Pozzato, M., Prest, M., Pupilli, F., Radicioni, E., Riccio, C., Ruggeri, A. C., Scian, C., Sirri, G., Stipcevic, M., Tenti, M., Terranova, F., Torti, M., Vallazza, E., Velotti, F., Vesco, M., and Votano, L.
Subjects: Physics - Accelerator Physics, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract: The ENUBET ERC project (2016-2021) is studying a facility based on a narrow band beam capable of constraining the neutrino fluxes normalization through the monitoring of the associated charged leptons in an instrumented decay tunnel. A key element of the project is the design and optimization of the hadronic beamline. In this proceeding we present progress on the studies of the proton extraction schemes. We also show a realistic implementation and simulation of the beamline., Comment: Poster presented at NuPhys2019 (London, 16-18 December 2019). 4 pages, 4 figures. Typo in author list corrected
Published: 2020

128. Decay tunnel instrumentation for the ENUBET neutrino beam

Author: Acerbi, F., Berra, A., Bonesini, M., Branca, A., Brizzolari, C., Brunetti, G., Calviani, M., Capelli, S., Carturan, S., Catanesi, M. G., Cecchini, S., Charitonidis, N., Cindolo, F., Collazuol, G., Conti, E., Corso, F. Dal, Delogu, C., De Rosa, G., Falcone, A., Gola, A., Jollet, C., Kain, V., Klicek, B., Kudenko, Y., Laveder, M., Longhin, A., Ludovici, L., Lutsenko, E., Magaletti, L., Mandrioli, G., Margotti, A., Mascagna, V., Mauri, N., Meazza, L., Meregaglia, A., Mezzetto, M., Nessi, M., Paoloni, A., Pari, M., Parozzi, E., Pasqualini, L., Paternoster, G., Patrizii, L., Pozzato, M., Prest, M., Pupilli, F., Radicioni, E., Riccio, C., Ruggieri, A. C., Scian, C., Sirri, G., Stipcevic, M., Tenti, M., Terranova, F., Torti, M., Vallazza, E., Velotti, F., Vesco, M., and Votano, L.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The uncertainty in the initial neutrino flux is the main limitation for a precise determination of the absolute neutrino cross section. The ERC funded ENUBET project (2016-2021) is studying a facility based on a narrow band beam to produce an intense source of electron neutrinos with a ten-fold improvement in accuracy. Since March 2019 ENUBET is also a Neutrino Platform experiment at CERN: NP06/ENUBET. A key element of the project is the instrumentation of the decay tunnel to monitor large angle positrons produced together with $\nu_e$ in the three body decays of kaons ($K_{e3}$) and to discriminate them from neutral and charged pions. The need for an efficient and high purity e/$\pi$ separation over a length of several meters, and the requirements for fast response and radiation hardness imposed by the harsh beam environment, suggested the implementation of a longitudinally segmented Fe/scintillator calorimeter with a readout based on WLS fibers and SiPM detectors. An extensive experimental program through several test beam campaigns at the CERN-PS T9 beam line has been pursued on calorimeter prototypes, both with a shashlik and a lateral readout configuration. The latter, in which fibers collect the light from the side of the scintillator tiles, allows to place the light sensors away from the core of the calorimeter, thus reducing possible irradiation damages with respect to the shashlik design. This contribution will present the achievements of the prototyping activities carried out, together with irradiation tests made on the Silicon Photo-Multipliers. The results achieved so far pin down the technology of choice for the construction of the 3 m long demonstrator that will take data in 2021., Comment: Talk presented at the "15th Topical Seminar on Innovative Particle and Radiation Detectors (IPRD19)", 14-17 October 2019. Siena, Italy. 9 pages, 7 figures
Published: 2020
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129. Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume II: DUNE Physics

Author: Abi, B., Acciarri, R., Acero, Mario A., Adamov, G., Adams, D., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Anthony, J., Antonova, M., Antusch, S., Fernandez, A. Aranda, Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., Terrazas, I. Caro, Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. Cervera, Chalifour, M., Chang, C., Chardonnet, E., Chatterjee, A., Chattopadhyay, S., Chaves, J., Chen, H., Chen, M., Chen, Y., Cherdack, D., Chi, C., Childress, S., Chiriacescu, A., Cho, K., Choubey, S., Christensen, A., Christian, D., Christodoulou, G., Church, E., Clarke, P., Coan, T. E., Cocco, A. G., Coelho, J. A. B., Conley, E., Conrad, J. M., Convery, M., Corwin, L., Cotte, P., Cremaldi, L., Cremonesi, L., Crespo-Anadon, J. I., Cristaldo, E., Cross, R., Cuesta, C., Cui, Y., Cussans, D., Dabrowski, M., da Motta, H., Peres, L. Da Silva, David, Q., Davies, G. S., Davini, S., Dawson, J., De, K., De Almeida, R. M., Debbins, P., De Bonis, I., Decowski, M. P., de Gouvea, A., De Holanda, P. C., Astiz, I. L. De Icaza, Deisting, A., De Jong, P., Delbart, A., Delepine, D., Delgado, M., Dell'Acqua, A., De Lurgio, P., Neto, J. R. T. de Mello, DeMuth, D. M., Dennis, S., Densham, C., Deptuch, G., De Roeck, A., De Romeri, V., De Vries, J. J., Dharmapalan, R., Diaz, F., Diaz, J. S., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Dokania, N., Dolinski, M. J., Domine, L., Douglas, D., Drielsma, F., Duchesneau, D., Duffy, K., Dunne, P., Durkin, T., Duyang, H., Dvornikov, O., Dwyer, D. A., Dyshkant, A. S., Eads, M., Edmunds, D., Eisch, J., Emery, S., Ereditato, A., Escobar, C. O., Sanchez, L. Escudero, Evans, J. J., Ewart, E., Ezeribe, A. C., Fahey, K., Falcone, A., Farnese, C., Farzan, Y., Felix, J., Fernandez-Martinez, E., Menendez, P. Fernandez, Ferraro, F., Fields, L., Filkins, A., Filthaut, F., Fitzpatrick, R. S., Flanagan, W., Fleming, B., Flight, R., Fowler, J., Fox, W., Franc, J., Francis, K., Franco, D., Freeman, J., Freestone, J., Fried, J., Friedland, A., Fuess, S., Furic, I., Furmanski, A. P., Gago, A., Gallagher, H., Gallego-Ros, A., Gallice, N., Galymov, V., Gamberini, E., Gamble, T., Gandhi, R., Gandrajula, R., Gao, S., Garcia-Gamez, D., Garcia-Peris, M. Á., Gardiner, S., Gastler, D., Ge, G., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Gibin, D., Gil-Botella, I., Girerd, C., Giri, A. K., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Bermeo, L. V. Gomez, Fajardo, L. S. Gomez, Gonnella, F., Gonzalez-Cuevas, J. A., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Graham, M., Gramellini, E., Gran, R., Granados, E., Grant, A., Grant, C., Gratieri, D., Green, P., Green, S., Greenler, L., Greenwood, M., Greer, J., Griffith, W. C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guarino, V., Guenette, R., Guglielmi, A., Guo, B., Guthikonda, K. K., Gutierrez, R., Guzowski, P., Guzzo, M. M., Gwon, S., Habig, A., Hackenburg, A., Hadavand, H., Haenni, R., Hahn, A., Haigh, J., Haiston, J., Hamernik, T., Hamilton, P., Han, J., Harder, K., Harris, D. A., Hartnell, J., Hasegawa, T., Hatcher, R., Hazen, E., Heavey, A., Heeger, K. M., Hennessy, K., Henry, S., Morquecho, M. A. Hernandez, Herner, K., Hertel, L., Hesam, A. S., Hewes, V, Higuera, A., Hill, T., Hillier, S. J., Himmel, A., Hoff, J., Hohl, C., Holin, A., Hoppe, E., Horton-Smith, G. A., Hostert, M., Hourlier, A., Howard, B., Howell, R., Huang, J., Hugon, J., Iles, G., Iliescu, A. M., Illingworth, R., Ioannisian, A., Itay, R., Izmaylov, A., James, E., Jargowsky, B., Jediny, F., Jesus-Valls, C., Ji, X., Jiang, L., Jiménez, S., Jipa, A., Joglekar, A., Johnson, C., Johnson, R., Jones, B., Jones, S., Jung, C. K., Junk, T., Jwa, Y., Kabirnezhad, M., Kaboth, A., Kadenko, I., Kamiya, F., Karagiorgi, G., Karcher, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasetti, S. P., Kashur, L., Kazaryan, N., Kearns, E., Keener, P., Kelly, K. J., Kemp, E., Ketchum, W., Kettell, S. 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., Kordosky, M., Kosc, T., Kose, U., Kostelecky, V. 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Manrique, Marchionni, A., Marciano, W., Marfatia, D., Mariani, C., Maricic, J., Marinho, F., Marino, A. D., Marshak, M., Marshall, C., Marshall, J., Marteau, J., Martin-Albo, J., Martinez, N., Caicedo, D. A. Martinez, Martynenko, S., Mason, K., Mastbaum, A. T., Masud, M., Matsuno, S., Matthews, J., Mauger, C., Mauri, N., Mavrokoridis, K., Mazza, R., Mazzacane, A., Mazzucato, E., McCluskey, E., McConkey, N., McFarland, K. S., McGrew, C., McNab, A., Mefodiev, A., Mehta, P., Melas, P., Mellinato, M., Mena, O., Menary, S., Santos, L. Mendes, Mendez, H., Menegolli, A., Meng, G., Messier, M. D., Metcalf, W., Mewes, M., Meyer, H., Miao, T., Michna, G., Miedema, T., Migenda, J., Milincic, R., 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. Molina, Montanari, A., Montanari, C., Montanari, D., Zetina, L. M. 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Subjects: High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract: The preponderance of matter over antimatter in the early universe, the dynamics of the supernovae that produced the heavy elements necessary for life, and whether protons eventually decay -- these mysteries at the forefront of particle physics and astrophysics are key to understanding the early evolution of our universe, its current state, and its eventual fate. DUNE is an international world-class experiment dedicated to addressing these questions as it searches for leptonic charge-parity symmetry violation, stands ready to capture supernova neutrino bursts, and seeks to observe nucleon decay as a signature of a grand unified theory underlying the standard model. The DUNE far detector technical design report (TDR) describes the DUNE physics program and the technical designs of the single- and dual-phase DUNE liquid argon TPC far detector modules. Volume II of this TDR, DUNE Physics, describes the array of identified scientific opportunities and key goals. Crucially, we also report our best current understanding of the capability of DUNE to realize these goals, along with the detailed arguments and investigations on which this understanding is based. This TDR volume documents the scientific basis underlying the conception and design of the LBNF/DUNE experimental configurations. As a result, the description of DUNE's experimental capabilities constitutes the bulk of the document. Key linkages between requirements for successful execution of the physics program and primary specifications of the experimental configurations are drawn and summarized. This document also serves a wider purpose as a statement on the scientific potential of DUNE as a central component within a global program of frontier theoretical and experimental particle physics research. Thus, the presentation also aims to serve as a resource for the particle physics community at large., Comment: 357 pages, 165 figures (updated typos in Table 6.1 and corrected errors in author list)
Published: 2020

130. Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume IV: Far Detector Single-phase Technology

Author: Abi, B., Acciarri, R., Acero, Mario A., Adamov, G., Adams, D., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Anthony, J., Antonova, M., Antusch, S., Fernandez, A. Aranda, Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., Terrazas, I. Caro, Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. Cervera, Chalifour, M., Chang, C., Chardonnet, E., Chatterjee, A., Chattopadhyay, S., Chaves, J., Chen, H., Chen, M., Chen, Y., Cherdack, D., Chi, C., Childress, S., Chiriacescu, A., Cho, K., Choubey, S., Christensen, A., Christian, D., Christodoulou, G., Church, E., Clarke, P., Coan, T. E., Cocco, A. G., Coelho, J. A. B., Conley, E., Conrad, J. M., Convery, M., Corwin, L., Cotte, P., Cremaldi, L., Cremonesi, L., Crespo-Anadon, J. I., Cristaldo, E., Cross, R., Cuesta, C., Cui, Y., Cussans, D., Dabrowski, M., da Motta, H., Peres, L. Da Silva, David, Q., Davies, G. S., Davini, S., Dawson, J., De, K., De Almeida, R. M., Debbins, P., De Bonis, I., Decowski, M. P., de Gouvea, A., De Holanda, P. C., Astiz, I. L. De Icaza, Deisting, A., De Jong, P., Delbart, A., Delepine, D., Delgado, M., Dell'Acqua, A., De Lurgio, P., Neto, J. R. T. de Mello, DeMuth, D. M., Dennis, S., Densham, C., Deptuch, G., De Roeck, A., De Romeri, V., De Vries, J. J., Dharmapalan, R., Diaz, F., Diaz, J. S., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Dokania, N., Dolinski, M. J., Domine, L., Douglas, D., Drielsma, F., Duchesneau, D., Duffy, K., Dunne, P., Durkin, T., Duyang, H., Dvornikov, O., Dwyer, D. A., Dyshkant, A. S., Eads, M., Edmunds, D., Eisch, J., Emery, S., Ereditato, A., Escobar, C. O., Sanchez, L. Escudero, Evans, J. J., Ewart, E., Ezeribe, A. C., Fahey, K., Falcone, A., Farnese, C., Farzan, Y., Felix, J., Fernandez-Martinez, E., Menendez, P. Fernandez, Ferraro, F., Fields, L., Filkins, A., Filthaut, F., Fitzpatrick, R. S., Flanagan, W., Fleming, B., Flight, R., Fowler, J., Fox, W., Franc, J., Francis, K., Franco, D., Freeman, J., Freestone, J., Fried, J., Friedland, A., Fuess, S., Furic, I., Furmanski, A. P., Gago, A., Gallagher, H., Gallego-Ros, A., Gallice, N., Galymov, V., Gamberini, E., Gamble, T., Gandhi, R., Gandrajula, R., Gao, S., Garcia-Gamez, D., Garcia-Peris, M. Á., Gardiner, S., Gastler, D., Ge, G., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Gibin, D., Gil-Botella, I., Girerd, C., Giri, A. K., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Bermeo, L. V. Gomez, Fajardo, L. S. Gomez, Gonnella, F., Gonzalez-Cuevas, J. A., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Graham, M., Gramellini, E., Gran, R., Granados, E., Grant, A., Grant, C., Gratieri, D., Green, P., Green, S., Greenler, L., Greenwood, M., Greer, J., Griffith, W. C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guarino, V., Guenette, R., Guglielmi, A., Guo, B., Guthikonda, K. K., Gutierrez, R., Guzowski, P., Guzzo, M. M., Gwon, S., Habig, A., Hackenburg, A., Hadavand, H., Haenni, R., Hahn, A., Haigh, J., Haiston, J., Hamernik, T., Hamilton, P., Han, J., Harder, K., Harris, D. A., Hartnell, J., Hasegawa, T., Hatcher, R., Hazen, E., Heavey, A., Heeger, K. M., Hennessy, K., Henry, S., Morquecho, M. A. Hernandez, Herner, K., Hertel, L., Hesam, A. S., Hewes, V, Higuera, A., Hill, T., Hillier, S. J., Himmel, A., Hoff, J., Hohl, C., Holin, A., Hoppe, E., Horton-Smith, G. A., Hostert, M., Hourlier, A., Howard, B., Howell, R., Huang, J., Hugon, J., Iles, G., Iliescu, A. M., Illingworth, R., Ioannisian, A., Itay, R., Izmaylov, A., James, E., Jargowsky, B., Jediny, F., Jesus-Valls, C., Ji, X., Jiang, L., Jiménez, S., Jipa, A., Joglekar, A., Johnson, C., Johnson, R., Jones, B., Jones, S., Jung, C. K., Junk, T., Jwa, Y., Kabirnezhad, M., Kaboth, A., Kadenko, I., Kamiya, F., Karagiorgi, G., Karcher, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasetti, S. P., Kashur, L., Kazaryan, N., Kearns, E., Keener, P., Kelly, K. J., Kemp, E., Ketchum, W., Kettell, S. 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., Kordosky, M., Kosc, T., Kose, U., Kostelecky, V. A., Kothekar, K., Krennrich, F., Kreslo, I., Kudenko, Y., Kudryavtsev, V. A., Kulagin, S., Kumar, J., Kumar, R., Kuruppu, C., Kus, V., Kutter, T., Lambert, A., Lande, K., Lane, C. E., Lang, K., Langford, T., Lasorak, P., Last, D., Lastoria, C., Laundrie, A., Lawrence, A., Lazanu, I., LaZur, R., Le, T., Learned, J., LeBrun, P., Miotto, G. Lehmann, Lehnert, R., de Oliveira, M. A. Leigui, Leitner, M., Leyton, M., Li, L., Li, S., Li, S. W., Li, T., Li, Y., Liao, H., Lin, C. S., Lin, S., Lister, A., Littlejohn, B. R., Liu, J., Lockwitz, S., Loew, T., Lokajicek, M., Lomidze, I., Long, K., Loo, K., Lorca, D., Lord, T., LoSecco, J. M., Louis, W. C., Luk, K. B., Luo, X., Lurkin, N., Lux, T., Luzio, V. P., MacFarland, D., Machado, A. A., Machado, P., Macias, C. T., Macier, J. R., Maddalena, A., Madigan, P., Magill, S., Mahn, K., Maio, A., Maloney, J. A., Mandrioli, G., Maneira, J., Manenti, L., Manly, S., Mann, A., Manolopoulos, K., Plata, M. 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Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The preponderance of matter over antimatter in the early universe, the dynamics of the supernovae that produced the heavy elements necessary for life, and whether protons eventually decay -- these mysteries at the forefront of particle physics and astrophysics are key to understanding the early evolution of our universe, its current state, and its eventual fate. DUNE is an international world-class experiment dedicated to addressing these questions as it searches for leptonic charge-parity symmetry violation, stands ready to capture supernova neutrino bursts, and seeks to observe nucleon decay as a signature of a grand unified theory underlying the standard model. Central to achieving DUNE's physics program is a far detector that combines the many tens-of-kiloton fiducial mass necessary for rare event searches with sub-centimeter spatial resolution in its ability to image those events, allowing identification of the physics signatures among the numerous backgrounds. In the single-phase liquid argon time-projection chamber (LArTPC) technology, ionization charges drift horizontally in the liquid argon under the influence of an electric field towards a vertical anode, where they are read out with fine granularity. A photon detection system supplements the TPC, directly enhancing physics capabilities for all three DUNE physics drivers and opening up prospects for further physics explorations. The DUNE far detector technical design report (TDR) describes the DUNE physics program and the technical designs of the single- and dual-phase DUNE liquid argon TPC far detector modules. Volume IV presents an overview of the basic operating principles of a single-phase LArTPC, followed by a description of the DUNE implementation. Each of the subsystems is described in detail, connecting the high-level design requirements and decisions to the overriding physics goals of DUNE., Comment: Minor corrections made for JINST submission, 673 pages, 312 figures (corrected errors in author list)
Published: 2020

131. Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume III: DUNE Far Detector Technical Coordination

Author: Abi, B., Acciarri, R., Acero, Mario A., Adamov, G., Adams, D., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Anthony, J., Antonova, M., Antusch, S., Fernandez, A. Aranda, Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., Terrazas, I. Caro, Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. Cervera, Chalifour, M., Chang, C., Chardonnet, E., Chatterjee, A., Chattopadhyay, S., Chaves, J., Chen, H., Chen, M., Chen, Y., Cherdack, D., Chi, C., Childress, S., Chiriacescu, A., Cho, K., Choubey, S., Christensen, A., Christian, D., Christodoulou, G., Church, E., Clarke, P., Coan, T. E., Cocco, A. G., Coelho, J. A. B., Conley, E., Conrad, J. M., Convery, M., Corwin, L., Cotte, P., Cremaldi, L., Cremonesi, L., Crespo-Anadon, J. I., Cristaldo, E., Cross, R., Cuesta, C., Cui, Y., Cussans, D., Dabrowski, M., da Motta, H., Peres, L. Da Silva, David, Q., Davies, G. S., Davini, S., Dawson, J., De, K., De Almeida, R. M., Debbins, P., De Bonis, I., Decowski, M. P., de Gouvea, A., De Holanda, P. C., Astiz, I. L. De Icaza, Deisting, A., De Jong, P., Delbart, A., Delepine, D., Delgado, M., Dell'Acqua, A., De Lurgio, P., Neto, J. R. T. de Mello, DeMuth, D. M., Dennis, S., Densham, C., Deptuch, G., De Roeck, A., De Romeri, V., De Vries, J. J., Dharmapalan, R., Diaz, F., Diaz, J. S., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Dokania, N., Dolinski, M. J., Domine, L., Douglas, D., Drielsma, F., Duchesneau, D., Duffy, K., Dunne, P., Durkin, T., Duyang, H., Dvornikov, O., Dwyer, D. A., Dyshkant, A. S., Eads, M., Edmunds, D., Eisch, J., Emery, S., Ereditato, A., Escobar, C. O., Sanchez, L. Escudero, Evans, J. J., Ewart, E., Ezeribe, A. C., Fahey, K., Falcone, A., Farnese, C., Farzan, Y., Felix, J., Fernandez-Martinez, E., Menendez, P. Fernandez, Ferraro, F., Fields, L., Filkins, A., Filthaut, F., Fitzpatrick, R. S., Flanagan, W., Fleming, B., Flight, R., Fowler, J., Fox, W., Franc, J., Francis, K., Franco, D., Freeman, J., Freestone, J., Fried, J., Friedland, A., Fuess, S., Furic, I., Furmanski, A. P., Gago, A., Gallagher, H., Gallego-Ros, A., Gallice, N., Galymov, V., Gamberini, E., Gamble, T., Gandhi, R., Gandrajula, R., Gao, S., Garcia-Gamez, D., Garcia-Peris, M. Á., Gardiner, S., Gastler, D., Ge, G., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Gibin, D., Gil-Botella, I., Girerd, C., Giri, A. K., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Bermeo, L. V. Gomez, Fajardo, L. S. Gomez, Gonnella, F., Gonzalez-Cuevas, J. A., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Graham, M., Gramellini, E., Gran, R., Granados, E., Grant, A., Grant, C., Gratieri, D., Green, P., Green, S., Greenler, L., Greenwood, M., Greer, J., Griffith, W. C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guarino, V., Guenette, R., Guglielmi, A., Guo, B., Guthikonda, K. K., Gutierrez, R., Guzowski, P., Guzzo, M. M., Gwon, S., Habig, A., Hackenburg, A., Hadavand, H., Haenni, R., Hahn, A., Haigh, J., Haiston, J., Hamernik, T., Hamilton, P., Han, J., Harder, K., Harris, D. A., Hartnell, J., Hasegawa, T., Hatcher, R., Hazen, E., Heavey, A., Heeger, K. M., Hennessy, K., Henry, S., Morquecho, M. A. Hernandez, Herner, K., Hertel, L., Hesam, A. S., Hewes, V, Higuera, A., Hill, T., Hillier, S. J., Himmel, A., Hoff, J., Hohl, C., Holin, A., Hoppe, E., Horton-Smith, G. A., Hostert, M., Hourlier, A., Howard, B., Howell, R., Huang, J., Hugon, J., Iles, G., Iliescu, A. M., Illingworth, R., Ioannisian, A., Itay, R., Izmaylov, A., James, E., Jargowsky, B., Jediny, F., Jesus-Valls, C., Ji, X., Jiang, L., Jiménez, S., Jipa, A., Joglekar, A., Johnson, C., Johnson, R., Jones, B., Jones, S., Jung, C. K., Junk, T., Jwa, Y., Kabirnezhad, M., Kaboth, A., Kadenko, I., Kamiya, F., Karagiorgi, G., Karcher, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasetti, S. P., Kashur, L., Kazaryan, N., Kearns, E., Keener, P., Kelly, K. J., Kemp, E., Ketchum, W., Kettell, S. 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., Kordosky, M., Kosc, T., Kose, U., Kostelecky, V. A., Kothekar, K., Krennrich, F., Kreslo, I., Kudenko, Y., Kudryavtsev, V. A., Kulagin, S., Kumar, J., Kumar, R., Kuruppu, C., Kus, V., Kutter, T., Lambert, A., Lande, K., Lane, C. E., Lang, K., Langford, T., Lasorak, P., Last, D., Lastoria, C., Laundrie, A., Lawrence, A., Lazanu, I., LaZur, R., Le, T., Learned, J., LeBrun, P., Miotto, G. Lehmann, Lehnert, R., de Oliveira, M. A. Leigui, Leitner, M., Leyton, M., Li, L., Li, S., Li, S. W., Li, T., Li, Y., Liao, H., Lin, C. S., Lin, S., Lister, A., Littlejohn, B. R., Liu, J., Lockwitz, S., Loew, T., Lokajicek, M., Lomidze, I., Long, K., Loo, K., Lorca, D., Lord, T., LoSecco, J. M., Louis, W. C., Luk, K. B., Luo, X., Lurkin, N., Lux, T., Luzio, V. P., MacFarland, D., Machado, A. A., Machado, P., Macias, C. T., Macier, J. R., Maddalena, A., Madigan, P., Magill, S., Mahn, K., Maio, A., Maloney, J. A., Mandrioli, G., Maneira, J., Manenti, L., Manly, S., Mann, A., Manolopoulos, K., Plata, M. Manrique, Marchionni, A., Marciano, W., Marfatia, D., Mariani, C., Maricic, J., Marinho, F., Marino, A. D., Marshak, M., Marshall, C., Marshall, J., Marteau, J., Martin-Albo, J., Martinez, N., Caicedo, D. A. Martinez, Martynenko, S., Mason, K., Mastbaum, A. T., Masud, M., Matsuno, S., Matthews, J., Mauger, C., Mauri, N., Mavrokoridis, K., Mazza, R., Mazzacane, A., Mazzucato, E., McCluskey, E., McConkey, N., McFarland, K. S., McGrew, C., McNab, A., Mefodiev, A., Mehta, P., Melas, P., Mellinato, M., Mena, O., Menary, S., Santos, L. Mendes, Mendez, H., Menegolli, A., Meng, G., Messier, M. D., Metcalf, W., Mewes, M., Meyer, H., Miao, T., Michna, G., Miedema, T., Migenda, J., Milincic, R., 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. Molina, Montanari, A., Montanari, C., Montanari, D., Zetina, L. M. Montano, Moon, J., Mooney, M., Moor, A., Moreno, D., Morgan, B., Morris, C., Mossey, C., Motuk, E., Moura, C. A., Mousseau, J., Mu, W., Mualem, L., Mueller, J., Muether, M., Mufson, S., Muheim, F., Muir, A., Mulhearn, M., Muramatsu, H., Murphy, S., Musser, J., Nachtman, J., Nagu, S., Nalbandyan, M., Nandakumar, R., Naples, D., Narita, S., Navas-Nicolas, D., Nayak, N., Nebot-Guinot, M., Necib, L., Negishi, K., Nelson, J. K., Nesbit, J., Nessi, M., Newbold, D., Newcomer, M., Newhart, D., Nichol, R., Niner, E., Nishimura, K., Norman, A., Northrop, R., Novella, P., Nowak, J. A., Oberling, M., Del Campo, A. Olivares, Olivier, A., Onel, Y., Onishchuk, Y., Ott, J., Pagani, L., Pakvasa, S., Palamara, O., Palestini, S., Paley, J. M., Pallavicini, M., Palomares, C., Pantic, E., Paolone, V., Papadimitriou, V., Papaleo, R., Papanestis, A., Paramesvaran, S., Parke, S., 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., Penichot, Y., 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., Pillow, J., Plunkett, R., Poling, R., Pons, X., Poonthottathil, N., Pordes, S., Potekhin, M., Potenza, R., Potukuchi, B. V. K. S., Pozimski, J., Pozzato, M., Prakash, S., Prakash, T., Prince, S., Pugnere, D., Qi, K., Qian, X., Raaf, J. L., Raboanary, R., Radeka, V., Rademacker, J., Radics, B., Rafique, A., Raguzin, E., Rai, M., Rajaoalisoa, M., Rakhno, I., Rakotondramanana, H. T., Rakotondravohitra, L., Ramachers, Y. A., Rameika, R., Delgado, M. A. Ramirez, Ramson, B., Rappoldi, A., Raselli, G., Ratoff, P., Ravat, S., Razafinime, H., Real, J. S., Rebel, B., Redondo, D., Reggiani-Guzzo, M., Rehak, T., Reichenbacher, J., Reitzner, S. D., Renshaw, A., Rescia, S., Resnati, F., Reynolds, A., Riccobene, G., Rice, L. C. J., Rielage, K., Rigaut, Y., Rivera, D., Rochester, L., Roda, M., Rodrigues, P., Alonso, M. J. Rodriguez, Rondon, J. Rodriguez, Roeth, A. J., Rogers, H., Rosauro-Alcaraz, S., Rossella, M., Rout, J., Roy, S., Rubbia, A., Rubbia, C., Russell, B., Russell, J., Ruterbories, D., Saakyan, R., Sacerdoti, S., Safford, T., Sahu, N., Sala, P., Samios, N., Sanchez, M. C., 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., Schlabach, P., Schmitz, D., Scholberg, K., Schukraft, A., Segreto, E., Sensenig, J., Seong, I., Sergi, A., Sergiampietri, F., Sgalaberna, D., Shaevitz, M. H., Shafaq, S., Shamma, M., Sharma, H. 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Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The preponderance of matter over antimatter in the early universe, the dynamics of the supernovae that produced the heavy elements necessary for life, and whether protons eventually decay -- these mysteries at the forefront of particle physics and astrophysics are key to understanding the early evolution of our universe, its current state, and its eventual fate. The Deep Underground Neutrino Experiment (DUNE) is an international world-class experiment dedicated to addressing these questions as it searches for leptonic charge-parity symmetry violation, stands ready to capture supernova neutrino bursts, and seeks to observe nucleon decay as a signature of a grand unified theory underlying the standard model. The DUNE far detector technical design report (TDR) describes the DUNE physics program and the technical designs of the single- and dual-phase DUNE liquid argon TPC far detector modules. Volume III of this TDR describes how the activities required to design, construct, fabricate, install, and commission the DUNE far detector modules are organized and managed. This volume details the organizational structures that will carry out and/or oversee the planned far detector activities safely, successfully, on time, and on budget. It presents overviews of the facilities, supporting infrastructure, and detectors for context, and it outlines the project-related functions and methodologies used by the DUNE technical coordination organization, focusing on the areas of integration engineering, technical reviews, quality assurance and control, and safety oversight. Because of its more advanced stage of development, functional examples presented in this volume focus primarily on the single-phase (SP) detector module., Comment: Minor corrections made for JINST submission, 209 pages, 55 figures (updated typos in Table A.5; corrected errors in author list)
Published: 2020

132. Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume I: Introduction to DUNE

Author: Abi, B., Acciarri, R., Acero, Mario A., Adamov, G., Adams, D., Adinolfi, M., Ahmad, Z., Ahmed, J., Alion, T., Monsalve, S. Alonso, Alt, C., Anderson, J., Andreopoulos, C., Andrews, M. P., Andrianala, F., Andringa, S., Ankowski, A., Anthony, J., Antonova, M., Antusch, S., Fernandez, A. Aranda, Ariga, A., Arnold, L. O., Arroyave, M. A., Asaadi, J., Aurisano, A., Aushev, V., Autiero, D., Azfar, F., Back, H., Back, J. J., Backhouse, C., Baesso, P., Bagby, L., Bajou, R., Balasubramanian, S., Baldi, P., Bambah, B., Barao, F., Barenboim, G., Barker, G. J., Barkhouse, W., Barnes, C., Barr, G., Monarca, J. Barranco, Barros, N., Barrow, J. L., Bashyal, A., Basque, V., Bay, F., Alba, J. L. Bazo, Beacom, J. F., Bechetoille, E., Behera, B., Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Belver, D., Benekos, N., Neves, F. Bento, Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Berns, H., Bertolucci, S., Betancourt, M., Bezawada, Y., Bhattacharjee, M., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Siffert, B. Blanco, Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bonesini, M., Bongrand, M., Bonini, F., Booth, A., Booth, C., Bordoni, S., Borkum, A., Boschi, T., Bostan, N., Bour, P., Boyd, S. B., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Brandt, A., Bremer, J., Brew, C., Brianne, E., Brice, S. J., Brizzolari, C., Bromberg, C., Brooijmans, G., Brooke, J., Bross, A., Brunetti, G., Buchanan, N., Budd, H., Caiulo, D., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Camilleri, L., Caminata, A., Campanelli, M., Caratelli, D., Carini, G., Carlus, B., Carniti, P., Terrazas, I. Caro, Carranza, H., Castillo, A., Castromonte, C., Cattadori, C., Cavalier, F., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Villanueva, A. Cervera, Chalifour, M., Chang, C., Chardonnet, E., Chatterjee, A., Chattopadhyay, S., Chaves, J., Chen, H., Chen, M., Chen, Y., Cherdack, D., Chi, C., Childress, S., Chiriacescu, A., Cho, K., Choubey, S., Christensen, A., Christian, D., Christodoulou, G., Church, E., Clarke, P., Coan, T. E., Cocco, A. G., Coelho, J. A. B., Conley, E., Conrad, J. M., Convery, M., Corwin, L., Cotte, P., Cremaldi, L., Cremonesi, L., Crespo-Anadon, J. I., Cristaldo, E., Cross, R., Cuesta, C., Cui, Y., Cussans, D., Dabrowski, M., da Motta, H., Peres, L. Da Silva, David, Q., Davies, G. S., Davini, S., Dawson, J., De, K., De Almeida, R. M., Debbins, P., De Bonis, I., Decowski, M. P., de Gouvea, A., De Holanda, P. C., Astiz, I. L. De Icaza, Deisting, A., De Jong, P., Delbart, A., Delepine, D., Delgado, M., Dell'Acqua, A., De Lurgio, P., Neto, J. R. T. de Mello, DeMuth, D. M., Dennis, S., Densham, C., Deptuch, G., De Roeck, A., De Romeri, V., De Vries, J. J., Dharmapalan, R., Diaz, F., Diaz, J. S., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Dokania, N., Dolinski, M. J., Domine, L., Douglas, D., Drielsma, F., Duchesneau, D., Duffy, K., Dunne, P., Durkin, T., Duyang, H., Dvornikov, O., Dwyer, D. A., Dyshkant, A. S., Eads, M., Edmunds, D., Eisch, J., Emery, S., Ereditato, A., Escobar, C. O., Sanchez, L. Escudero, Evans, J. J., Ewart, E., Ezeribe, A. C., Fahey, K., Falcone, A., Farnese, C., Farzan, Y., Felix, J., Fernandez-Martinez, E., Menendez, P. Fernandez, Ferraro, F., Fields, L., Filkins, A., Filthaut, F., Fitzpatrick, R. S., Flanagan, W., Fleming, B., Flight, R., Fowler, J., Fox, W., Franc, J., Francis, K., Franco, D., Freeman, J., Freestone, J., Fried, J., Friedland, A., Fuess, S., Furic, I., Furmanski, A. P., Gago, A., Gallagher, H., Gallego-Ros, A., Gallice, N., Galymov, V., Gamberini, E., Gamble, T., Gandhi, R., Gandrajula, R., Gao, S., Garcia-Gamez, D., Garcia-Peris, M. Á., Gardiner, S., Gastler, D., Ge, G., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Gibin, D., Gil-Botella, I., Girerd, C., Giri, A. K., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Bermeo, L. V. Gomez, Fajardo, L. S. Gomez, Gonnella, F., Gonzalez-Cuevas, J. A., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Graham, M., Gramellini, E., Gran, R., Granados, E., Grant, A., Grant, C., Gratieri, D., Green, P., Green, S., Greenler, L., Greenwood, M., Greer, J., Griffith, W. C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guarino, V., Guenette, R., Guglielmi, A., Guo, B., Guthikonda, K. K., Gutierrez, R., Guzowski, P., Guzzo, M. M., Gwon, S., Habig, A., Hackenburg, A., Hadavand, H., Haenni, R., Hahn, A., Haigh, J., Haiston, J., Hamernik, T., Hamilton, P., Han, J., Harder, K., Harris, D. A., Hartnell, J., Hasegawa, T., Hatcher, R., Hazen, E., Heavey, A., Heeger, K. M., Hennessy, K., Henry, S., Morquecho, M. A. Hernandez, Herner, K., Hertel, L., Hesam, A. S., Hewes, V, Higuera, A., Hill, T., Hillier, S. J., Himmel, A., Hoff, J., Hohl, C., Holin, A., Hoppe, E., Horton-Smith, G. A., Hostert, M., Hourlier, A., Howard, B., Howell, R., Huang, J., Hugon, J., Iles, G., Iliescu, A. M., Illingworth, R., Ioannisian, A., Itay, R., Izmaylov, A., James, E., Jargowsky, B., Jediny, F., Jesus-Valls, C., Ji, X., Jiang, L., Jiménez, S., Jipa, A., Joglekar, A., Johnson, C., Johnson, R., Jones, B., Jones, S., Jung, C. K., Junk, T., Jwa, Y., Kabirnezhad, M., Kaboth, A., Kadenko, I., Kamiya, F., Karagiorgi, G., Karcher, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasetti, S. P., Kashur, L., Kazaryan, N., Kearns, E., Keener, P., Kelly, K. J., Kemp, E., Ketchum, W., Kettell, S. 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., Kordosky, M., Kosc, T., Kose, U., Kostelecky, V. A., Kothekar, K., Krennrich, F., Kreslo, I., Kudenko, Y., Kudryavtsev, V. A., Kulagin, S., Kumar, J., Kumar, R., Kuruppu, C., Kus, V., Kutter, T., Lambert, A., Lande, K., Lane, C. E., Lang, K., Langford, T., Lasorak, P., Last, D., Lastoria, C., Laundrie, A., Lawrence, A., Lazanu, I., LaZur, R., Le, T., Learned, J., LeBrun, P., Miotto, G. Lehmann, Lehnert, R., de Oliveira, M. A. Leigui, Leitner, M., Leyton, M., Li, L., Li, S., Li, S. W., Li, T., Li, Y., Liao, H., Lin, C. S., Lin, S., Lister, A., Littlejohn, B. R., Liu, J., Lockwitz, S., Loew, T., Lokajicek, M., Lomidze, I., Long, K., Loo, K., Lorca, D., Lord, T., LoSecco, J. M., Louis, W. C., Luk, K. B., Luo, X., Lurkin, N., Lux, T., Luzio, V. P., MacFarland, D., Machado, A. A., Machado, P., Macias, C. T., Macier, J. R., Maddalena, A., Madigan, P., Magill, S., Mahn, K., Maio, A., Maloney, J. A., Mandrioli, G., Maneira, J., Manenti, L., Manly, S., Mann, A., Manolopoulos, K., Plata, M. Manrique, Marchionni, A., Marciano, W., Marfatia, D., Mariani, C., Maricic, J., Marinho, F., Marino, A. D., Marshak, M., Marshall, C., Marshall, J., Marteau, J., Martin-Albo, J., Martinez, N., Caicedo, D. A. Martinez, Martynenko, S., Mason, K., Mastbaum, A. T., Masud, M., Matsuno, S., Matthews, J., Mauger, C., Mauri, N., Mavrokoridis, K., Mazza, R., Mazzacane, A., Mazzucato, E., McCluskey, E., McConkey, N., McFarland, K. S., McGrew, C., McNab, A., Mefodiev, A., Mehta, P., Melas, P., Mellinato, M., Mena, O., Menary, S., Santos, L. Mendes, Mendez, H., Menegolli, A., Meng, G., Messier, M. D., Metcalf, W., Mewes, M., Meyer, H., Miao, T., Michna, G., Miedema, T., Migenda, J., Milincic, R., 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. Molina, Montanari, A., Montanari, C., Montanari, D., Zetina, L. M. Montano, Moon, J., Mooney, M., Moor, A., Moreno, D., Morgan, B., Morris, C., Mossey, C., Motuk, E., Moura, C. A., Mousseau, J., Mu, W., Mualem, L., Mueller, J., Muether, M., Mufson, S., Muheim, F., Muir, A., Mulhearn, M., Muramatsu, H., Murphy, S., Musser, J., Nachtman, J., Nagu, S., Nalbandyan, M., Nandakumar, R., Naples, D., Narita, S., Navas-Nicolas, D., Nayak, N., Nebot-Guinot, M., Necib, L., Negishi, K., Nelson, J. K., Nesbit, J., Nessi, M., Newbold, D., Newcomer, M., Newhart, D., Nichol, R., Niner, E., Nishimura, K., Norman, A., Northrop, R., Novella, P., Nowak, J. A., Oberling, M., Del Campo, A. Olivares, Olivier, A., Onel, Y., Onishchuk, Y., Ott, J., Pagani, L., Pakvasa, S., Palamara, O., Palestini, S., Paley, J. M., Pallavicini, M., Palomares, C., Pantic, E., Paolone, V., Papadimitriou, V., Papaleo, R., Papanestis, A., Paramesvaran, S., Parke, S., 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., Penichot, Y., 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., Pillow, J., Plunkett, R., Poling, R., Pons, X., Poonthottathil, N., Pordes, S., Potekhin, M., Potenza, R., Potukuchi, B. V. K. S., Pozimski, J., Pozzato, M., Prakash, S., Prakash, T., Prince, S., Pugnere, D., Qi, K., Qian, X., Raaf, J. L., Raboanary, R., Radeka, V., Rademacker, J., Radics, B., Rafique, A., Raguzin, E., Rai, M., Rajaoalisoa, M., Rakhno, I., Rakotondramanana, H. T., Rakotondravohitra, L., Ramachers, Y. A., Rameika, R., Delgado, M. A. Ramirez, Ramson, B., Rappoldi, A., Raselli, G., Ratoff, P., Ravat, S., Razafinime, H., Real, J. S., Rebel, B., Redondo, D., Reggiani-Guzzo, M., Rehak, T., Reichenbacher, J., Reitzner, S. D., Renshaw, A., Rescia, S., Resnati, F., Reynolds, A., Riccobene, G., Rice, L. C. J., Rielage, K., Rigaut, Y., Rivera, D., Rochester, L., Roda, M., Rodrigues, P., Alonso, M. J. Rodriguez, Rondon, J. Rodriguez, Roeth, A. J., Rogers, H., Rosauro-Alcaraz, S., Rossella, M., Rout, J., Roy, S., Rubbia, A., Rubbia, C., Russell, B., Russell, J., Ruterbories, D., Saakyan, R., Sacerdoti, S., Safford, T., Sahu, N., Sala, P., Samios, N., Sanchez, M. C., 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., Schlabach, P., Schmitz, D., Scholberg, K., Schukraft, A., Segreto, E., Sensenig, J., Seong, I., Sergi, A., Sergiampietri, F., Sgalaberna, D., Shaevitz, M. H., Shafaq, S., Shamma, M., Sharma, H. R., Sharma, R., Shaw, T., Shepherd-Themistocleous, C., Shin, S., Shooltz, D., Shrock, R., Simard, L., Simos, N., Sinclair, J., Sinev, G., Singh, J., Sipos, R., Sippach, F. W., Sirri, G., Sitraka, A., Siyeon, K., Smargianaki, D., Smith, A., Smith, E., Smith, P., Smolik, J., Smy, M., Snopok, P., Nunes, M. Soares, Sobel, H., Soderberg, M., Salinas, C. J. Solano, Soldner-Rembold, S., Solomey, N., Solovov, V., Sondheim, W. E., Sorel, M., Soto-Oton, J., Sousa, A., Soustruznik, K., Spagliardi, F., Spanu, M., Spitz, J., Spooner, N. J., Spurgeon, K., Staley, R., Stancari, M., Stanco, L., Steiner, H. M., Stewart, J., Stillwell, B., Stock, J., Stocker, F., Stokes, T., Strait, M., Strauss, T., Striganov, S., Stuart, A., Summers, D., Surdo, A., Susic, V., Suter, L., Sutera, C. M., Svoboda, R., Szczerbinska, B., Szelc, A., Talaga, R., Tanaka, H. A., Oregui, B. Tapia, Tapper, A., Tariq, S., Tatar, E., Tayloe, R., Teklu, A. M., Tenti, M., Terao, K., Ternes, C. A., Terranova, F., Testera, G., Thea, A., Thompson, J. L., Thorn, C., Timm, S. C., Tonazzo, A., Torti, M., Tortola, M., Tortorici, F., Totani, D., Toups, M., Touramanis, C., Trevor, J., Trzaska, W. H., Tsai, Y. T., Tsamalaidze, Z., Tsang, K. V., Tsverava, N., Tufanli, S., Tull, C., Tyley, E., Tzanov, M., Uchida, M. A., Urheim, J., Usher, T., Vagins, M. R., Vahle, P., Valdiviesso, G. A., Valencia, E., Vallari, Z., Valle, J. W. F., Vallecorsa, S., Van Berg, R., Van de Water, R. G., Forero, D. Vanegas, Varanini, F., Vargas, D., Varner, G., Vasel, J., Vasseur, G., Vaziri, K., Ventura, S., Verdugo, A., Vergani, S., Vermeulen, M. A., Verzocchi, M., de Souza, H. Vieira, Vignoli, C., Vilela, C., Viren, B., Vrba, T., Wachala, T., Waldron, A. V., Wallbank, M., Wang, H., Wang, J., 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., While, M. R., White, A., Whitehead, L. H., Whittington, D., Wilking, M. J., Wilkinson, C., Williams, Z., Wilson, F., Wilson, R. J., Wolcott, J., Wongjirad, T., Wood, K., Wood, L., Worcester, E., Worcester, M., Wret, C., Wu, W., Xiao, Y., Yang, G., Yang, T., Yershov, N., Yonehara, K., Young, T., Yu, B., Yu, J., 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., Zimmerman, E. D., Zito, M., Zucchelli, S., Zuklin, J., Zutshi, V., and Zwaska, R.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The preponderance of matter over antimatter in the early universe, the dynamics of the supernovae that produced the heavy elements necessary for life, and whether protons eventually decay -- these mysteries at the forefront of particle physics and astrophysics are key to understanding the early evolution of our universe, its current state, and its eventual fate. The Deep Underground Neutrino Experiment (DUNE) is an international world-class experiment dedicated to addressing these questions as it searches for leptonic charge-parity symmetry violation, stands ready to capture supernova neutrino bursts, and seeks to observe nucleon decay as a signature of a grand unified theory underlying the standard model. The DUNE far detector technical design report (TDR) describes the DUNE physics program and the technical designs of the single- and dual-phase DUNE liquid argon TPC far detector modules. This TDR is intended to justify the technical choices for the far detector that flow down from the high-level physics goals through requirements at all levels of the Project. Volume I contains an executive summary that introduces the DUNE science program, the far detector and the strategy for its modular designs, and the organization and management of the Project. The remainder of Volume I provides more detail on the science program that drives the choice of detector technologies and on the technologies themselves. It also introduces the designs for the DUNE near detector and the DUNE computing model, for which DUNE is planning design reports. Volume II of this TDR describes DUNE's physics program in detail. Volume III describes the technical coordination required for the far detector design, construction, installation, and integration, and its organizational structure. Volume IV describes the single-phase far detector technology. A planned Volume V will describe the dual-phase technology., Comment: Minor corrections made for JINST submission; 244 pages, 114 figures
Published: 2020

133. Second order Fermi reacceleration mechanisms and large scale synchrotron radio emission in intra-cluster bridges

Author: Brunetti, G. and Vazza, F.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Radio observations at low frequencies with the Low Frequency Array (LOFAR) start discovering gigantic radio bridges connecting pairs of massive galaxy clusters. These observations probe unexplored mechanisms of in situ particle acceleration that operate on volumes of several Mpc$^3$. Numerical simulations suggest that such bridges are dynamically complex and that weak shocks and super-Alfv\'{e}nic turbulence can be driven across the entire volume of these regions. In this Letter we explore, for the first time, the role of second order Fermi mechanisms for the reacceleration of relativistic electrons interacting with turbulence in these peculiar regions. We assume the turbulent energy flux measured in simulations and adopt a scenario in which relativistic particles scatter with magnetic field lines diffusing in super-Alfv\'enic turbulence and magnetic fields are amplified by the same turbulence. We show that steep spectrum and volume filling synchrotron emission can be generated in the entire intra-cluster bridge region thus providing a natural explanation for radio bridges. Consequently, radio observations have the potential to probe the dissipation of energy on scales larger than galaxy clusters and second order Fermi mechanisms operating in physical regimes that are still poorly explored. This has a potential impact on several branches of astrophysics and cosmology., Comment: 5 pages, 3 figures (+ Supplementary Material). Physical Review Letters, in press
Published: 2020
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134. Polysiloxane-based scintillators for shashlik calorimeters

Author: Acerbi, F., Branca, A., Brizzolari, C., Brunetti, G., Carturan, S., Catanesi, M. G., Cecchini, S., Cindolo, F., Collazuol, G., Corso, F. Dal, De Rosa, G., Delogu, C., Falcone, A., Gola, A., Jollet, C., Kliček, B., Kudenko, Y., Laveder, M., Longhin, A., Ludovici, L., Lutsenko, E., Magaletti, L., Mandrioli, G., Marchi, T., Margotti, A., Mascagna, V., Meregaglia, A., Mezzetto, M., Nessi, M., Pari, M., Parozzi, E., Pasqualini, L., Paternoster, G., Patrizii, L., Piemonte, C., Pozzato, M., Prest, M., Pupilli, F., Radicioni, E., Riccio, C., Ruggeri, A. C., Scian, C., Sirri, G., Stipčevic, M., Tenti, M., Terranova, F., Torti, M., Vallazza, E., and Vesco, M.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: We present the first application of polysiloxane-based scintillators as active medium in a shashlik sampling calorimeter. These results were obtained from a testbeam campaign of a $\sim$6$\times$6$\times$45 cm$^3$ (13 $X_0$ depth) prototype. A Wavelength Shifting fiber array of 36 elements runs perpendicularly to the stack of iron (15 mm) and polysiloxane scintillator (15 mm) tiles with a density of about one over cm$^2$. Unlike shashlik calorimeters based on plastic organic scintillators, here fibers are optically matched with the scintillator without any intermediate air gap. The prototype features a compact light readout based on Silicon Photo-Multipliers embedded in the bulk of the detector. The detector was tested with electrons, pions and muons with energies ranging from 1 to 7 GeV at the CERN-PS. This solution offers a highly radiation hard detector to instrument the decay region of a neutrino beam, providing an event-by-event measurement of high-angle decay products associated with neutrino production (ENUBET, Enhanced NeUtrino BEams from kaon Tagging, ERC project). The results in terms of light yield, uniformity and energy resolution, are compared to a similar calorimeter built with ordinary plastic scintillators., Comment: 28 pages, 16 figures. To appear in NIM-A
Published: 2020
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135. Validation of a sub-epidermal moisture scanner for early detection of pressure ulcers in an ex vivo porcine model of localized oedema

Author: Brunetti, G., Patton, D., Moore, Z., Palomeque-Chavez, J.C., O'Brien, F.J., and Boyle, C.J.
Published: 2023
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136. Revived Fossil Plasma Sources in Galaxy Clusters

Author: Mandal, S., Intema, H. T., van Weeren, R. J., Shimwell, T. W., Botteon, A., Brunetti, G., de Gasperin, F., Brüggen, M., Di Gennaro, G., Kraft, R., Röttgering, H. J. A., Hardcastle, M., and Tasse, C.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: It is well established that particle acceleration by shocks and turbulence in the intra-cluster medium can produce cluster-scale synchrotron emitting sources. However, the detailed physics of these particle acceleration processes is still not well understood. One of the main open questions is the role of fossil relativistic electrons that have been deposited in the intra-cluster medium by radio galaxies. These synchrotron-emitting electrons are very difficult to study, as their radiative life time is only tens of Myrs at GHz frequencies, and are therefore a relatively unexplored population. Despite the typical steep radio spectrum due to synchrotron losses, these fossil electrons are barely visible even at radio frequencies well below a GHz. However, when a pocket of fossil radio plasma is compressed, it boosts the visibility at sub-GHz frequencies, creating so-called radio phoenices. This compression can be the result of bulk motion and shocks in the ICM due to merger activity. In this paper, we demonstrate the discovery potential of low frequency radio sky surveys to find and study revived fossil plasma sources in galaxy clusters. We used the 150~MHz TGSS and 1.4 GHz NVSS sky surveys to identify candidate radio phoenices. A subset of three candidates were studied in detail using deep multi-band radio observations (LOFAR and GMRT), X-ray (\textit{Chandra} or \textit{XMM-Newton}) and archival optical observations. Two of the three sources are new discoveries. Using these observations, we identified common observational properties (radio morphology, ultra-steep spectrum, X-ray luminosity, dynamical state) that will enable us to identify this class of sources more easily, and help to understand the physical origin of these sources., Comment: 12 pages, 5 figures; Accepted for publication in Astronomy and Astrophysics
Published: 2019
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137. Particle acceleration in a nearby galaxy cluster pair: the role of cluster dynamics

Author: Botteon, A., Cassano, R., Eckert, D., Brunetti, G., Dallacasa, D., Shimwell, T. W., van Weeren, R. J., Gastaldello, F., Bonafede, A., Brüggen, M., Bîrzan, L., Clavico, S., Cuciti, V., de Gasperin, F., De Grandi, S., Ettori, S., Ghizzardi, S., Rossetti, M., Röttgering, H. J. A., and Sereno, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Diffuse radio emission associated with the intra-cluster medium (ICM) is observed in a number of merging galaxy clusters. It is currently believed that in mergers a fraction of the kinetic energy is channeled into non-thermal components, such as turbulence, cosmic rays and magnetic fields, that may lead to the formation of giant synchrotron sources in the ICM. Studying merging galaxy clusters in different evolutionary phases is fundamental to understanding the origin of radio emission in the ICM. We observed the nearby galaxy cluster pair RXC J1825.3+3026 ($z\sim0.065$) and CIZA J1824.1+3029 ($z\sim0.071$) at 120-168 MHz with the LOw Frequency ARray (LOFAR) and made use of a deep (240 ks) XMM-Newton dataset to study the non-thermal and thermal properties of the system. RXC J1825.3+3026 is in a complex dynamical state, with a primary on-going merger in the E-W direction and a secondary later stage merger with a group of galaxies in the SW, while CIZA J1824.1+3029 is dynamically relaxed. These two clusters are in a pre-merger phase. We report the discovery of a Mpc-scale radio halo with a low surface brightness extension in RXC J1825.3+3026 that follows the X-ray emission from the cluster center to the remnant of a galaxy group in the SW. This is among the least massive systems and the faintest giant radio halo known to date. Contrary to this, no diffuse radio emission is observed in CIZA J1824.1+3029 nor in the region between the pre-merger cluster pair. The power spectra of the X-ray surface brightness fluctuations of RXC J1825.3+3026 and CIZA J1824.1+3029 are in agreement with the findings for clusters exhibiting a radio halo and the ones where no radio emission has been detected, respectively. We provide quantitative support to the idea that cluster mergers play a crucial role in the generation of non-thermal components in the ICM., Comment: 7 pages, 5 figures, 1 table, accepted for publication in A&A
Published: 2019
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138. Growth and disruption in the Lyra complex

Author: Clavico, S., De Grandi, S., Ghizzardi, S., Rossetti, M., Molendi, S., Gastaldello, F., Girardi, M., Boschin, W., Botteon, A., Cassano, R., Bruggen, M., Brunetti, G., Dallacasa, D., Eckert, D., Ettori, S., Gaspari, M., Sereno, M., Shimwell, T., and van Weeren, R. J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Nearby clusters of galaxies, z<0.1, are cosmic structures still under formation. Understanding the thermodynamic properties of merging clusters can provide crucial information on how they grow in the local universe. A detailed study of the intra-cluster medium (ICM) properties of un-relaxed systems is essential to understand the fate of in-falling structures and, more generally, the virialization process. We analyzed a mosaic of XMM-Newton observations (240 ks) of the Lyra system (z=0.067) that shows a complex dynamical state. We find the main cluster RXC J1825.3+3026 to be in a late merger phase, whereas its companion CIZA J1824.1+3029 is a relaxed cool-core cluster. We estimate a mass ratio of ~1:2 for the pair. No diffuse X-ray emission is found in the region between them, indicating that these clusters are in a pre-merger phase. We found evidence of a galaxy group infalling on RXC J1825.3+3026 in an advanced state of disruption. The Southern Galaxy, one of the brightest galaxies in the Lyra complex, was very likely at the center of the infalling group. This galaxy has a gaseous corona indicating that it was able to retain some of its gas after the ram-pressure stripping of the intra-group medium. In this scenario the diffuse emission excess observed southwest of RXC J1825.3+3026 could be due to gas once belonging to the group and/or to cluster ICM dislocated by the passage of the group. Finally, we identified three high-velocity galaxies aligned between RXC J1825.3+3026 and the SG, two of these showing evidence of gas stripped from them during infall. We estimate them to be currently falling onto the main cluster at an infall velocity of ~ 3000 km/s. Our study of the Lyra complex provides important clues about the processes presiding over the virialization of massive clusters in the local Universe., Comment: A&A accepted, 17 pages, 19 figures
Published: 2019
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139. LOFAR discovery of a radio halo in the high-redshift galaxy cluster PSZ2 G099.86+58.45

Author: Cassano, R., Botteon, A., Di Gennaro, G., Brunetti, G., Sereno, M., Shimwell, T. W., van Weeren, R. J., Brüggen, M., Gastaldello, F., Izzo, L., Bîrzan, L., Bonafede, A., Cuciti, V., de Gasperin, F., Rötttgering, H. J. A., Hardcastle, M., Mechev, A. P., and Tasse, C.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In this Letter, we report the discovery of a radio halo in the high-redshift galaxy cluster PSZ2 G099.86+58.45 ($z=0.616$) with the LOw Frequency ARray (LOFAR) at 120-168 MHz. This is one of the most distant radio halos discovered so far. The diffuse emission extends over $\sim$ 1 Mpc and has a morphology similar to that of the X-ray emission as revealed by XMM-Newton data. The halo is very faint at higher frequencies and is barely detected by follow-up 1-2 GHz Karl G.~Jansky Very Large Array (JVLA) observations, which enable us to constrain the radio spectral index to be $\alpha\leq 1.5-1.6$, i.e.; with properties between canonical and ultra-steep spectrum radio halos. Radio halos are currently explained as synchrotron radiation from relativistic electrons that are re-accelerated in the intra-cluster medium (ICM) by turbulence driven by energetic mergers. We show that in such a framework radio halos are expected to be relatively common at $\sim150$ MHz ($\sim30-60\%$) in clusters with mass and redshift similar to PSZ2 G099.86+58.45; however, at least 2/3 of these radio halos should have steep spectrum and thus be very faint above $\sim 1$ GHz frequencies. Furthermore, since the luminosity of radio halos at high redshift depends strongly on the magnetic field strength in the hosting clusters, future LOFAR observations will also provide vital information on the origin and amplification of magnetic fields in galaxy clusters., Comment: 6 pages, 3 figures, accepted (2019, July 17) for publication in ApJ Letter
Published: 2019
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140. Shock acceleration efficiency in radio relics

Author: Botteon, A., Brunetti, G., Ryu, D., and Roh, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Radio relics in galaxy clusters are giant diffuse synchrotron sources powered in cluster outskirts by merger shocks. Although the relic-shock connection has been consolidated in recent years by a number of observations, the details of the mechanisms leading to the formation of relativistic particles in this environment are still not well understood. The diffusive shock acceleration (DSA) theory is a commonly adopted scenario to explain the origin of cosmic rays at astrophysical shocks, including those in radio relics in galaxy clusters. However, in a few specific cases it has been shown that the energy dissipated by cluster shocks is not enough to reproduce the luminosity of the relics via DSA of thermal particles. Studies based on samples of radio relics are required to further address this limitation of the mechanism. In this paper, we focus on ten well-studied radio relics with underlying shocks observed in the X-rays and calculate the electron acceleration efficiency of these shocks that is necessary to reproduce the observed radio luminosity of the relics. We find that in general the standard DSA cannot explain the origin of the relics if electrons are accelerated from the thermal pool with an efficiency significantly smaller than 10%. Our results show that other mechanisms, such as shock re-acceleration of supra-thermal seed electrons or a modification of standard DSA, are required to explain the formation of radio relics., Comment: Matched to the A&A published version, minor grammar and typo fixes
Published: 2019
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141. A radio ridge connecting two galaxy clusters in a filament of the cosmic web

Author: Govoni, F., Orrù, E., Bonafede, A., Iacobelli, M., Paladino, R., Vazza, F., Murgia, M., Vacca, V., Giovannini, G., Feretti, L., Loi, F., Bernardi, G., Ferrari, C., Pizzo, R. F., Gheller, C., Manti, S., Brüggen, M., Brunetti, G., Cassano, R., de Gasperin, F., Enßlin, T. A., Hoeft, M., Horellou, C., Junklewitz, H., Röttgering, H. J. A., Scaife, A. M. M., Shimwell, T. W., van Weeren, R. J., and Wise, M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Galaxy clusters are the most massive gravitationally bound structures in the Universe. They grow by accreting smaller structures in a merging process that produces shocks and turbulence in the intra-cluster gas. We observed a ridge of radio emission connecting the merging galaxy clusters Abell 0399 and Abell 0401 with the Low Frequency Array (LOFAR) at 140 MHz. This emission requires a population of relativistic electrons and a magnetic field located in a filament between the two galaxy clusters. We performed simulations to show that a volume-filling distribution of weak shocks may re-accelerate a pre-existing population of relativistic particles, producing emission at radio wavelengths that illuminates the magnetic ridge., Comment: Published in Science
Published: 2019
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142. Signatures from a merging galaxy cluster and its AGN population: LOFAR observations of Abell 1682

Author: Clarke, A. O., Scaife, A. M. M., Shimwell, T., van Weeren, R. J., Bonafede, A., Heald, G., Brunetti, G., Cantwell, T. M., de Gasperin, F., Brüggen, M., Botteon, A., Hoeft, M., Horellou, C., Cassano, R., Harwood, J. J., and Röttgering, H. J. A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present LOFAR data from 110--180~MHz of the merging galaxy cluster Abell 1682, alongside archival optical, radio and X-ray data. Our 6 arc-second resolution images at low frequencies reveal new structures associated with numerous radio galaxies in the cluster. At 20 arc-second resolution we see diffuse emission throughout the cluster over hundreds of kpc, indicating particle acceleration mechanisms are in play as a result of the cluster merger event and powerful active galactic nuclei. We show that a significant part of the cluster emission is from an old radio galaxy with very steep spectrum emission (having a spectral index of $\alpha < -2.5$). Furthermore we identify a new region of diffuse steep spectrum emission ($\alpha < -1.1$) as a candidate for a radio halo which is co-spatial with the centre of the cluster merger. We suggest its origin as a population of old and mildly relativistic electrons left over from radio galaxies throughout the cluster which have been re-accelerated to higher energies by shocks and turbulence induced by the cluster merger event. We also note the discovery of six new giant radio galaxies in the vicinity of Abell 1682., Comment: Accepted in A&A; see journal version for uncompressed figures
Published: 2019
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143. A joint XMM-NuSTAR observation of the galaxy cluster Abell 523: constraints on Inverse Compton emission

Author: Cova, F., Gastaldello, F., Wik, D. R., Boschin, W., Botteon, A., Brunetti, G., Buote, D. A., De Grandi, S., Eckert, D., Ettori, S., Feretti, L., Gaspari, M., Ghizzardi, S., Giovannini, G., Ghirardi, M., Govoni, F., Molendi, S., Murgia, M., Rossetti, M., and Vacca, V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the results of a joint XMM-Newton and NuSTAR observation (200 ks) of the galaxy cluster Abell 523 at $z=0.104$. The peculiar morphology of the cluster radio halo and its outlier position in the radio power P(1.4 GHz) - X-ray luminosity plane make it an ideal candidate for the study of radio-X-ray correlations and for the search of inverse Compton (IC) emission. We constructed thermodynamic maps derived from the XMM observations to describe in detail the physical and dynamical state of the ICM. We performed a point-to-point comparison in terms of surface brightness between the X-ray and radio emissions, to quantify their morphological discrepancies. Making use of NuSTAR's hard X-ray focusing capability, we looked for IC emission both globally and locally, after modeling the purely thermal component with a multi-temperature description. The thermodynamic maps suggest the presence of a secondary merging process that could be responsible for the peculiar radio halo morphology. This hypothesis is supported by the comparison between the X-ray and radio surface brightnesses, which shows a broad intrinsic scatter and a series of outliers. The global NuSTAR spectrum can be explained by purely thermal gas emission, and there is no convincing evidence that an IC component is needed. The $3\sigma$ upper limit on the IC flux in the 20-80 keV band is in the range $\left[2.2 - 4.0\right] \times 10^{-13} \, \mathrm{erg} \, \mathrm{s}^{-1} \, \mathrm{cm}^{-2}$, implying a lower limit on the magnetic field strength in the range $B > [0.23 - 0.31] \, \mu G$. Locally, we looked for IC emission in the central region of the cluster radio halo finding a $3\sigma$ upper limit on the 20-80 keV non-thermal flux of $3.17 \times 10^{-14} \, \mathrm{erg} \, \mathrm{s}^{-1} \, \mathrm{cm}^{-2}$, corresponding to a lower limit on the magnetic field strength of $B \gtrsim 0.81 \, \mu G$., Comment: 20 pages, 37 figures, 6 tables; accepted for publication in A&A
Published: 2019
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144. A Massive Cluster at z = 0.288 Caught in the Process of Formation: The Case of Abell 959

Author: Bîrzan, L., Rafferty, D. A., Cassano, R., Brunetti, G., van Weeren, R. J., Brüggen, M., Intema, H. T., de Gasperin, F., Andrade-Santos, F., Botteon, A., Röttgering, H. J. A., and Shimwell, T. W.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The largest galaxy clusters are observed still to be forming through major cluster-cluster mergers, often showing observational signatures such as radio relics and giant radio haloes. Using LOFAR Two-meter Sky Survey data, we present new detections of both a radio halo (with a spectral index of $\alpha_{143}^{1400}=1.48^{+0.06}_{-0.23}$) and a likely radio relic in Abell 959, a massive cluster at a redshift of z=0.288. Using a sample of clusters with giant radio haloes from the literature (80 in total), we show that the radio halo in A959 lies reasonably well on the scaling relations between the thermal and non-thermal power of the system. Additionally, we find evidence that steep-spectrum haloes tend to reside in clusters with high X-ray luminosities relative to those expected from cluster LM scaling relations, indicating that such systems may preferentially lie at an earlier stage of the merger, consistent with the theory that some steep-spectrum haloes result from low-turbulence mergers. Lastly, we find that halo systems containing radio relics tend to lie at lower X-ray luminosities, relative to those expected from cluster LM scaling relations, for a given halo radio power than those without relics, suggesting that the presence of relics indicates a later stage of the merger, in line with simulations., Comment: 17 pages, 5 figures, accepted for publication in MNRAS
Published: 2019
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145. Turbulent pressure support and hydrostatic mass-bias in the intracluster medium

Author: Angelinelli, M., Vazza, F., Giocoli, C., Ettori, S., Jones, T. W., Brunetti, G., Brüggen, M., and Eckert, D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The degree of turbulent pressure support by residual gas motions in galaxy clusters is not well known. Mass modelling of combined X-ray and Sunyaev Zel'dovich observations provides an estimate of turbulent pressure support in the outer regions of several galaxy clusters. Here, we test two different filtering techniques to disentangle bulk from turbulent motions in non-radiative high-resolution cosmological simulations of galaxy clusters using the cosmological hydro code ENZO. We find that the radial behavior of the ratio of non-thermal pressure to total gas pressure as a function of cluster-centric distance can be described by a simple polynomial function. The typical non-thermal pressure support in the centre of clusters is $\sim$5%, increasing to $\sim$15% in the outskirts, in line with the pressure excess found in recent X-ray observations. While the complex dynamics of the ICM makes it impossible to reconstruct a simple correlation between turbulent motions and hydrostatic bias, we find that a relation between them can be established using the median properties of a sample of objects. Moreover, we estimate the contribution of radial accelerations to the non-thermal pressure support and conclude that it decreases moving outwards from 40% (in the core) to 15% (in the cluster's outskirts). Adding this contribution to one provided by turbulence, we show that it might account for the entire observed hydrostatic bias in the innermost regions of the clusters, and for less than 80% of it at $r > 0.8 r_{200, m}$., Comment: 20 pages; 21 figures; Substantial Revision; MNRAS in press
Published: 2019
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146. The ENUBET Beamline

Author: ENUBET Collaboration, Brunetti, G., Acerbi, F., Ballerini, G., Bonesini, M., Branca, A., Brizzolari, C., Calviani, M., Carturan, S., Catanesi, M. G., Cecchini, S., Cindolo, F., Collazuol, G., Conti, E., Corso, F. Dal, De Rosa, G., Delogu, C., Falcone, A., Goddard, B., Gola, A., Intonti, R. A., Jollet, C., Kain, V., Klicek, B., Kudenko, Y., Laveder, M., Longhin, A., Ludovici, L., Magaletti, L., Mandrioli, G., Margotti, A., Mascagna, V., Mauri, N., Meregaglia, A., Mezzetto, M., Nessi, M., Paoloni, A., Pari, M., Parozzi, E., Pasqualini, L., Paternoster, G., Patrizii, L., Piemonte, C., Pozzato, M., Prest, M., Pupilli, F., Radicioni, E., Riccio, C., Ruggeri, A. C., Sirri, G., Soldani, M., Stipcevic, M., Tenti, M., Terranova, F., Torti, M., Vallazza, E., Velotti, F., Vesco, M., and Votano, L.
Subjects: Physics - Accelerator Physics, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract: The ENUBET ERC project (2016-2021) is studying a narrow band neutrino beam where lepton production can be monitored at single particle level in an instrumented decay tunnel. This would allow to measure $\nu_{\mu}$ and $\nu_{e}$ cross sections with a precision improved by about one order of magnitude compared to present results. In this proceeding we describe a first realistic design of the hadron beamline based on a dipole coupled to a pair of quadrupole triplets along with the optimisation guidelines and the results of a simulation based on G4beamline. A static focusing design, though less efficient than a horn-based solution, results several times more efficient than originally expected. It works with slow proton extractions reducing drastically pile-up effects in the decay tunnel and it paves the way towards a time-tagged neutrino beam. On the other hand a horn-based transferline would ensure higher yields at the tunnel entrance. The first studies conducted at CERN to implement the synchronization between a few ms proton extraction and a horn pulse of 2-10 ms are also described., Comment: Poster presented at NuPhys2018 (London 19-21 December 2018). 4 pages, 3 figures
Published: 2019

147. Evidence for a merger induced shock wave in ZwCl\,0008.8+5215 with {\it Chandra} and {\it Suzaku}

Author: Di Gennaro, G., van Weeren, R. J., Andrade-Santos, F., Akamatsu, H., Randall, S. W., Forman, W., Kraft, R. P., Brunetti, G., Dawson, W. A., Golovich, N., and Jones, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the results from new deep {\it Chandra} ($\sim410$~ks) and {\it Suzaku} ($\sim180$ ks) observations of the merging galaxy cluster ZwCl\,0008.8+5215 ($z=0.104$). Previous radio observations revealed the presence of a double radio relic located diametrically west and east of the cluster center. Using our new {\it Chandra} data, we find evidence for the presence of a shock at the location of the western relic, RW, with a Mach number $\mathcal{M}_{S_X}=1.48^{+0.50}_{-0.32}$ from the density jump. We also measure $\mathcal{M}_{T_X}=2.35^{+0.74}_{-0.55}$ and $\mathcal{M}_{T_X}=2.02^{+0.74}_{-0.47}$ from the temperature jump, with {\it Chandra} and {\it Suzaku} respectively. These values are consistent with the Mach number estimate from a previous study of the radio spectral index, under the assumption of diffusive shock acceleration ($\mathcal{M}_{\rm RW}=2.4^{+0.4}_{-0.2}$). Interestingly, the western radio relic does not entirely trace the X-ray shock. A possible explanation is that the relic traces fossil plasma from nearby radio galaxies which is re-accelerated at the shock. For the eastern relic we do not detect an X-ray surface brightness discontinuity, despite the fact that radio observations suggest a shock with $\mathcal{M}_{\rm RE}=2.2^{+0.2}_{-0.1}$. The low surface brightness and reduced integration time for this region might have prevented the detection. {\it Chandra} surface brightness profile suggests $\mathcal{M}\lesssim1.5$, while {\it Suzaku} temperature measurements found $\mathcal{M}_{T_X}=1.54^{+0.65}_{-0.47}$. Finally, we also detect a merger induced cold front on the western side of the cluster, behind the shock that traces the western relic., Comment: 21 pages, 15 figures, 4 tables; accepted for publication in ApJ
Published: 2019
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148. Irradiation and performance of RGB-HD Silicon Photomultipliers for calorimetric applications

Author: Acerbi, F., Ballerini, G., Berra, A., Brizzolari, C., Brunetti, G., Catanesi, M. G., Cecchini, S., Cindolo, F., Coffani, A., Collazuol, G., Conti, E., Corso, F. Dal, Delogu, C., De Rosa, G., Gola, A., Intonti, R. A., Jollet, C., Kudenko, Y., Longhin, A., Ludovici, L., Magaletti, L., Mandrioli, G., Margotti, A., Mascagna, V., Mauri, N., Meregaglia, A., Pari, M., Pasqualini, L., Paternoster, G., Patrizii, L., Piemonte, C., Pozzato, M., Pupilli, F., Prest, M., Radicioni, E., Riccio, C., Ruggeri, A. C., Scian, C., Sirri, G., Soldani, M., Tenti, M., Torti, M., Terranova, F., and Vallazza, E.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: Silicon Photomultipliers with cell-pitch ranging from 12 $\mu$m to 20 $\mu$m were tested against neutron irradiation at moderate fluences to study their performance for calorimetric applications. The photosensors were developed by FBK employing the RGB-HD technology. We performed irradiation tests up to $2 \times 10^{11}$ n/cm$^2$ (1 MeV eq.) at the INFN-LNL Irradiation Test facility. The SiPMs were characterized on-site (dark current and photoelectron response) during and after irradiations at different fluences. The irradiated SiPMs were installed in the ENUBET compact calorimetric modules and characterized with muons and electrons at the CERN East Area facility. The tests demonstrate that both the electromagnetic response and the sensitivity to minimum ionizing particles are retained after irradiation. Gain compensation can be achieved increasing the bias voltage well within the operation range of the SiPMs. The sensitivity to single photoelectrons is lost at $\sim 10^{10}$ n/cm$^2$ due to the increase of the dark current., Comment: 14 pages, 13 figures. To appear in JINST
Published: 2019
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149. A high precision neutrino beam for a new generation of short baseline experiments

Author: Acerbi, F., Ballerini, G., Bolognesi, S., Bonesini, M., Brizzolari, C., Brunetti, G., Carturan, S., Catanesi, M. G., Cecchini, S., Cindolo, F., Collazuol, G., Conti, E., Corso, F. Dal, De Rosa, G., Di Lodovico, F., Delogu, C., Falcone, A., Gola, A., Intonti, R. A., Jollet, C., Klicek, B., Kudenko, Y., Laveder, M., Longhin, A., Ludovici, L., Magaletti, L., Mandrioli, G., Margotti, A., Mascagna, V., Mauri, N., Meregaglia, A., Mezzetto, M., Nessi, M., Paoloni, A., Pari, M., Parozzi, E., Pasqualini, L., Paternoster, G., Patrizii, L., Piemonte, C., Pozzato, M., Pupilli, F., Prest, M., Radicioni, E., Riccio, C., Ruggeri, A. C., Nieto, F. Sanchez, Sirri, G., Soldani, M., Stipcevic, M., Tenti, M., Terranova, F., Torti, M., Vallazza, E., Vesco, M., and Votano, L.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment, Physics - Accelerator Physics
Abstract: The current generation of short baseline neutrino experiments is approaching intrinsic source limitations in the knowledge of flux, initial neutrino energy and flavor. A dedicated facility based on conventional accelerator techniques and existing infrastructures designed to overcome these impediments would have a remarkable impact on the entire field of neutrino oscillation physics. It would improve by about one order of magnitude the precision on $\nu_\mu$ and $\nu_e$ cross sections, enable the study of electroweak nuclear physics at the GeV scale with unprecedented resolution and advance searches for physics beyond the three-neutrino paradigm. In turn, these results would enhance the physics reach of the next generation long baseline experiments (DUNE and Hyper-Kamiokande) on CP violation and their sensitivity to new physics. In this document, we present the physics case and technology challenge of high precision neutrino beams based on the results achieved by the ENUBET Collaboration in 2016-2018. We also set the R&D milestones to enable the construction and running of this new generation of experiments well before the start of the DUNE and Hyper-Kamiokande data taking. We discuss the implementation of this new facility at three different level of complexity: $\nu_\mu$ narrow band beams, $\nu_e$ monitored beams and tagged neutrino beams. We also consider a site specific implementation based on the CERN-SPS proton driver providing a fully controlled neutrino source to the ProtoDUNE detectors at CERN., Comment: 13 pages, 3 figures, submitted as an input document for the European Particle Physics Strategy. Dec. 2018
Published: 2019

150. Reconstruction of interactions in the ProtoDUNE-SP detector with Pandora

Author: Abud, A. Abed, Abi, B., Acciarri, R., Acero, M. A., Adames, M. R., Adamov, G., Adamowski, M., Adams, D., Adinolfi, M., Adriano, C., Aduszkiewicz, A., Aguilar, J., Ahmad, Z., Ahmed, J., Aimard, B., Akbar, F., Ali-Mohammadzadeh, B., Allison, K., Monsalve, S. Alonso, AlRashed, M., Alt, C., Alton, A., Alvarez, R., 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., Arellano, L., Arnold, L. O., Arroyave, M. A., Asaadi, J., Asquith, L., Aurisano, A., Aushev, V., Autiero, D., Ayala Lara, V., Ayala-Torres, M., Azfar, F., Back, A., Back, H., Back, J. J., Backhouse, C., 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. Barranco, Barros, A., Barros, N., Barrow, J. L., Basharina-Freshville, A., Bashyal, A., Basque, V., Batchelor, C., Battat, J., Battisti, F., Bay, F., Bazetto, M. C. Q., Bazo Alba, J. L., Beacom, J. F., Bechetoille, E., Behera, B., das Chagas, E. Belchior Batista, Bellantoni, L., Bellettini, G., Bellini, V., Beltramello, O., Benekos, N., Benitez Montiel, C., Bento Neves, F., Berger, J., Berkman, S., Bernardini, P., Berner, R. M., Bersani, A., Bertolucci, S., Betancourt, M., Rodríguez, A. Betancur, Bevan, A., Bezawada, Y., Bezerra, A. T., Bezerra, T. J., Bhardwaj, A., Bhatnagar, V., Bhattacharjee, M., Bhattarai, D., Bhuller, S., Bhuyan, B., Biagi, S., Bian, J., Biassoni, M., Biery, K., Bilki, B., Bishai, M., Bitadze, A., Blake, A., Blaszczyk, F. D. M., Blazey, G. C., Blucher, E., Boissevain, J., Bolognesi, S., Bolton, T., Bomben, L., Bonesini, M., Bonilla-Diaz, C., Bonini, F., Booth, A., Boran, F., Bordoni, S., Borkum, A., Bostan, N., Bour, P., Boyden, D., Bracinik, J., Braga, D., Brailsford, D., Branca, A., Brandt, A., Bremer, J., Brew, C., Brice, S. J., Brizzolari, C., Bromberg, C., Brooke, J., Bross, A., Brunetti, G., Brunetti, M., Buchanan, N., Budd, H., Butorov, I., Cagnoli, I., Cai, T., Caiulo, D., Calabrese, R., Calafiura, P., Calcutt, J., Calin, M., Calvez, S., Calvo, E., Caminata, A., Campos Benitez, A., Caratelli, D., Carber, D., Carceller, J. M., Carini, G., Carlus, B., Carneiro, M. F., Carniti, P., Terrazas, I. Caro, Carranza, H., Carroll, T., Forero, J. F. Castaño, Castillo, A., Castromonte, C., Catano-Mur, E., Cattadori, C., Cavalier, F., Cavallaro, G., Cavanna, F., Centro, S., Cerati, G., Cervelli, A., Cervera Villanueva, A., Chalifour, M., Chappell, A., Chardonnet, E., Charitonidis, N., Chatterjee, A., Chattopadhyay, S., Chavarry Neyra, M. S., Chen, H., Chen, M., Chen, Y., Chen, Z., Chen-Wishart, Z., Cheon, Y., Cherdack, D., Chi, C., Childress, S., Chirco, R., Chiriacescu, A., Cho, K., Choate, S., Chokheli, D., Chong, P. S., Christensen, A., Christian, D., Christodoulou, G., Chukanov, A., Chung, M., Church, E., Cicero, V., Clarke, P., Cline, G., Coan, T. E., Cocco, A. G., Coelho, J., Collot, J., Colton, N., Conley, E., Conley, R., Conrad, J., Convery, M., Copello, S., Cova, P., Cremaldi, L., Cremonesi, L., Crespo-Anadón, J. I., Crisler, M., Cristaldo, E., Crnkovic, J., Cross, R., Cudd, A., Cuesta, C., Cui, Y., Cussans, D., Dai, J., Dalager, O., Da Motta, H., Da Silva Peres, L., David, C., David, Q., Davies, G. S., Davini, S., Dawson, J., De, K., De, S., Debbins, P., De Bonis, I., Decowski, M., De Gouvea, A., De Holanda, P. C., De Icaza Astiz, I. L., Deisting, A., De Jong, P., Delbart, A., De Leo, V., Delepine, D., Delgado, M., Dell’Acqua, A., Delmonte, N., De Lurgio, P., De Mello Neto, J. R., DeMuth, D. M., Dennis, S., Densham, C., Deptuch, G. W., De Roeck, A., De Romeri, V., De Souza, G., Devi, R., Dharmapalan, R., Dias, M., Diaz, J., Díaz, F., Di Capua, F., Di Domenico, A., Di Domizio, S., Di Giulio, L., Ding, P., Di Noto, L., Dirkx, G., Distefano, C., Diurba, R., Diwan, M., Djurcic, Z., Doering, D., Dolan, S., Dolek, F., Dolinski, M., Domine, L., Donon, Y., Douglas, D., Dragone, A., Drake, G., Drielsma, F., Duarte, L., Duchesneau, D., Duffy, K., Dunne, P., Dutta, B., Duyang, H., Dvornikov, O., Dwyer, D., Dyshkant, A., Eads, M., Earle, A., Edmunds, D., Eisch, J., Emberger, L., Emery, S., Englezos, P., Ereditato, A., Erjavec, T., Escobar, C., Escudero Sanchez, L., Eurin, G., Evans, J. 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Á., Gardiner, S., Gastler, D., Gauvreau, J., Gauzzi, P., Ge, G., Geffroy, N., Gelli, B., Gendotti, A., Gent, S., Ghorbani-Moghaddam, Z., Giammaria, P., Giammaria, T., Giangiacomi, N., Gibin, D., Gil-Botella, I., Gilligan, S., Girerd, C., Giri, A., Gnani, D., Gogota, O., Gold, M., Gollapinni, S., Gollwitzer, K., Gomes, R. A., Gomez Bermeo, L., Gomez Fajardo, L. S., Gonnella, F., González Caamaño, D., Gonzalez-Diaz, D., Gonzalez-Lopez, M., Goodman, M. C., Goodwin, O., Goswami, S., Gotti, C., Goudzovski, E., Grace, C., Gran, R., Granados, E., Granger, P., Grant, C., Gratieri, D., Green, P., Green, S., Greenberg, S., Greenler, L., Greer, J., Grenard, J., Griffith, C., Groh, M., Grudzinski, J., Grzelak, K., Gu, W., Guardincerri, E., Guarino, V., Guarise, M., Guenette, R., Guerard, E., Guerzoni, M., Guffanti, D., Guglielmi, A., Guo, B., Gupta, A., Gupta, V., Guthikonda, K., Guzowski, P., Guzzo, M. M., Gwon, S., Ha, C., Haaf, K., Habig, A., Hadavand, H., Haenni, R., Hahn, A., Haiston, J., Hamacher-Baumann, P., Hamernik, T., Hamilton, P., Han, J., Harris, D. A., Hartnell, J., Hartnett, T., Harton, J., Hasegawa, T., Hasnip, C., Hatcher, R., Hatfield, K. W., Hatzikoutelis, A., Hayes, C., Hayrapetyan, K., Hays, J., Hazen, E., He, M., Heavey, A., Heeger, K. M., Heise, J., Henry, S., Morquecho, M. Hernandez, Herner, K., Hewes, J., Hilgenberg, C., Hill, T., Hillier, S. J., Himmel, A., Hinkle, E., Hirsch, L. R., Ho, J., Hoff, J., Holin, A., Hoppe, E., Horton-Smith, G. A., Hostert, M., Hourlier, A., Howard, B., Howell, R., Hristova, I., Hronek, M. S., Huang, J., Hulcher, Z., Iles, G., Ilic, N., Iliescu, A. M., Illingworth, R., Ingratta, G., Ioannisian, A., Irwin, B., Isenhower, L., Itay, R., Jackson, C. M., Jain, V., James, E., Jang, W., Jargowsky, B., Jediny, F., Jena, D., Jeong, Y., Jesús-Valls, C., Ji, X., Jiang, J., Jiang, L., Jiménez, S., Jipa, A., Joaquim, F., Johnson, W., Johnston, N., Jones, B., Judah, M., Jung, C., Junk, T., Jwa, Y., Kabirnezhad, M., Kaboth, A., Kadenko, I., Kakorin, I., Kalitkina, A., Kalra, D., Kamiya, F., Kaplan, D. M., Karagiorgi, G., Karaman, G., Karcher, A., Karolak, M., Karyotakis, Y., Kasai, S., Kasetti, S. P., Kashur, L., Kazaryan, N., Kearns, E., Keener, P., Kelly, K. J., Kemp, E., Kemularia, O., Ketchum, W., Kettell, S. H., Khabibullin, M., Khotjantsev, A., Khvedelidze, A., Kim, D., King, B., Kirby, B., Kirby, M., Klein, J., Klustova, A., Kobilarcik, T., Koehler, K., Koerner, L. W., Koh, D. H., Kohn, S., Koller, P. P., Kolupaeva, L., Korablev, D., Kordosky, M., Kosc, T., Kose, U., Kostelecky, V., Kothekar, K., Kralik, R., Kreczko, L., Krennrich, F., Kreslo, I., Kropp, W., Kroupova, T., Kubota, S., Kudenko, Y., Kudryavtsev, V. A., Kuhlmann, S., Kulagin, S., Kumar, J., Kumar, P., Kunze, P., Kuravi, R., Kurita, N., Kuruppu, C., Kus, V., Kutter, T., Kvasnicka, J., Kwak, D., Lambert, A., Land, B., Lane, C. E., Lang, K., Langford, T., Langstaff, M., Larkin, J., Lasorak, P., Last, D., 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., Lehmann Miotto, G., Lehnert, R., de Oliveira, M. Leigui, Leitner, M., Lepin, L. M., Li, S., Li, Y., Liao, H., Lin, C., Lin, Q., Lin, S., Lineros, R. A., Ling, J., Lister, A., Littlejohn, B. R., Liu, J., Liu, Y., Lockwitz, S., Loew, T., Lokajicek, M., Lomidze, I., Long, K., Lord, T., LoSecco, J., Louis, W. C., Lu, X., Luk, K., Lunday, B., Luo, X., Luppi, E., Lux, T., Luzio, V. P., Maalmi, J., 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. A., Mandrioli, G., Mandujano, R. C., Maneira, J. C., Manenti, L., Manly, S., Mann, A., Manolopoulos, K., Manrique Plata, M., Manyam, V. N., Marchan, M., Marchionni, A., Marciano, W., Marfatia, D., Mariani, C., Maricic, J., Marie, R., Marinho, F., Marino, A. D., Markiewicz, T., Marsden, D., Marshak, M., Marshall, C., Marshall, J., Marteau, J., Martín-Albo, J., Martinez, N., Martinez Caicedo, D. A., Miravé, P. Martínez, Martynenko, S., Mascagna, V., Mason, K., Mastbaum, A., 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., Mendez, H., Mendez, P., Méndez, D. P., Menegolli, A., Meng, G., Messier, M., Metcalf, W., Mewes, M., Meyer, H., Miao, T., Michna, G., Mikola, V., Milincic, R., Miller, G., Miller, W., Mills, J., Mineev, O., Minotti, A., Miranda, O. G., Miryala, S., Mishra, C., Mishra, S., Mislivec, A., Mitchell, M., Mladenov, D., Mocioiu, I., Moffat, K., Moggi, N., Mohanta, R., Mohayai, T. A., Mokhov, N., Molina, J. A., Molina Bueno, L., Montagna, E., Montanari, A., Montanari, C., Montanari, D., Montanino, D., Zetina, L. M. Montaño, Moon, S., Mooney, M., Moor, A. F., Moreno, D., Moretti, D., Morris, C., Mossey, C., Mote, M., 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, M., Murphy, S., Musser, J., Nachtman, J., Nagai, Y., Nagu, S., Nalbandyan, M., Nandakumar, R., Naples, D., Narita, S., Nath, A., Navrer-Agasson, A., Nayak, N., Nebot-Guinot, M., Negishi, K., Nelson, J. K., Nesbit, J., Nessi, M., Newbold, D., Newcomer, M., Newton, H., Nichol, R., Nicolas-Arnaldos, F., Nikolica, A., Niner, E., Nishimura, K., Norman, A., Norrick, A., Northrop, R., Novella, P., Nowak, J. A., Oberling, M., Ochoa-Ricoux, J., Olivier, A., Olshevskiy, A., Onel, Y., Onishchuk, Y., Ott, J., Pagani, L., Palacio, G., Palamara, O., Palestini, S., Paley, J. M., Pallavicini, M., Palomares, C., Panduro 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. B., Patton, S., Patzak, T., Paudel, A., Paulos, B., Paulucci, L., Pavlovic, Z., Pawloski, G., Payne, D., Pec, V., Peeters, S. J., Pena Perez, A., Pennacchio, E., Penzo, A., Peres, O. L., Perry, J., Pershey, D., Pessina, G., Petrillo, G., Petta, C., Petti, R., Pia, V., Piastra, F., Pickering, L., Pietropaolo, F., Pimentel, V. L., Pinaroli, G., Plows, K., Plunkett, R., Pompa, F., Pons, X., Poonthottathil, N., Poppi, F., Pordes, S., Porter, J., Porzio, S., Potekhin, M., Potenza, R., Potukuchi, B. V., Pozimski, J., Pozzato, M., Prakash, S., Prakash, T., Prest, M., Prince, S., Psihas, F., Pugnere, D., Qian, X., Raaf, J., Radeka, V., Rademacker, J., Radics, B., Rafique, A., Raguzin, E., Rai, M., Rajaoalisoa, M., Rakhno, I., Rakotonandrasana, A., Rakotondravohitra, L., Rameika, R., Ramirez Delgado, M., Ramson, B., Rappoldi, A., Raselli, G., Ratoff, P., Raut, S., Razafinime, H., Razakamiandra, R., Rea, E. M., Real, J. S., Rebel, B., Rechenmacher, R., Reggiani-Guzzo, M., Reichenbacher, J., Reitzner, S. D., Rejeb Sfar, H., Renshaw, A., Rescia, S., Resnati, F., Ribas, M., Riboldi, S., Riccio, C., Riccobene, G., Rice, L. C., Ricol, J. S., Rigamonti, A., Rigaut, Y., Rincón, E. V., Ritchie-Yates, H., Rivera, D., Robert, A., Rocabado Rocha, J., Rochester, L., Roda, M., Rodrigues, P., da Silva Leite, J. V. Rodrigues, Alonso, M. J. Rodriguez, Rondon, J. Rodriguez, Rosauro-Alcaraz, S., Rosier, P., Roskovec, B., Rossella, M., Rossi, M., Rout, J., Roy, P., Rubbia, A., Rubbia, C., Russell, B., Ruterbories, D., Rybnikov, A., Saa-Hernandez, A., Saakyan, R., Sacerdoti, S., Sahu, N., Sala, P., Samios, N., Samoylov, O., Sanchez, M., Sandberg, V., Sanders, D. A., Sankey, D., Saoulidou, N., Sapienza, P., Sarasty, C., Sarcevic, I., Savage, G., Savinov, V., Scaramelli, A., Scarff, A., Scarpelli, A., Schefke, T., Schellman, H., Schifano, S., Schlabach, P., Schmitz, D., Schneider, A. W., Scholberg, K., Schukraft, A., Segreto, E., Selyunin, A., Senise, Jr., C. R., Sensenig, J., Sgalaberna, D., Shaevitz, M., Shafaq, S., Shaker, F., Shamma, M., Sharankova, R., Sharma, H. R., Sharma, R., Sharma, R. K., Shaw, K., Shaw, T., Shchablo, K., Shepherd-Themistocleous, C., Sheshukov, A., Shin, S., Shoemaker, I., Shooltz, D., Shrock, R., Siegel, H., Simard, L., Sinclair, J., Sinev, G., Singh, J., Singh, J., Singh, L., Singh, P., Singh, V., Sipos, R., Sippach, F., Sirri, G., Sitraka, A., Siyeon, K., Skarpaas, K., Smith, E., Smith, P., Smolik, J., Smy, M., Snider, E., Snopok, P., Snowden-Ifft, D., Nunes, M. Soares, Sobel, H., Soderberg, M., Sokolov, S., Salinas, C. J. Solano, Söldner-Rembold, S., Soleti, S., Solomey, N., Solovov, V., Sondheim, W. E., Sorel, M., Sotnikov, A., Soto-Oton, J., Ugaldi, F. Soto, Sousa, A., Soustruznik, K., Spagliardi, F., Spanu, M., Spitz, J., Spooner, N. J. C., Spurgeon, K., Stancari, M., Stanco, L., Stanford, C., Stein, R., Steiner, H., Lisbôa, A. F. Steklain, Stewart, J., Stillwell, B., Stock, J., Stocker, F., Stokes, T., Strait, M., Strauss, T., Strigari, L., Stuart, A., Suarez, J. G., Sunción, J. Suárez, Sullivan, H., Surdo, A., Susic, V., Suter, L., Sutera, C., Suvorov, Y., Svoboda, R., Szczerbinska, B., Szelc, A. M., Talukdar, N., Tanaka, H., Tang, S., Oregui, B. Tapia, Tapper, A., Tariq, S., Tarpara, E., Tata, N., Tatar, E., Tayloe, R., Teklu, A., Tennessen, P., Tenti, M., Terao, K., Ternes, C. A., Terranova, F., Testera, G., Thakore, T., Thea, A., Thorn, C., Timm, S., Tishchenko, V., 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., Tsamalaidze, Z., Tsang, K., Tsverava, N., Tu, S. Z., Tufanli, S., Tull, C., Tyler, J., Tyley, E., Tzanov, M., Uboldi, L., Uchida, M. A., Urheim, J., Usher, T., Uzunyan, S., Vagins, M. R., Vahle, P., Valder, S., Valdiviesso, G. D., Valencia, E., Valentim, R., Vallari, Z., Vallazza, E., Valle, J. W., Vallecorsa, S., Van Berg, R., Van de Water, R. G., Vanegas Forero, D., Vannerom, D., Varanini, F., Vargas Oliva, 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., Vieira de Souza, H., Vignoli, C., Vilela, C., Viren, B., Vrba, T., Wachala, T., Waldron, A. V., Wallbank, M., Wallis, C., Walton, T., Wang, H., Wang, J., Wang, L., Wang, M. H., Wang, X., Wang, Y., Wang, Y., Warburton, K., Warner, D., Wascko, M., Waters, D., Watson, A., Wawrowska, K., 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, A., Wilkinson, C., Williams, Z., Wilson, F., Wilson, R. J., Wisniewski, W., Wolcott, J., Wongjirad, T., Wood, A., Wood, K., Worcester, E., Worcester, M., Wresilo, K., Wret, C., Wu, W., Wu, W., Xiao, Y., Yaeggy, B., Yandel, E., Yang, G., Yang, K., Yang, T., Yankelevich, A., Yershov, N., Yonehara, K., Yoon, Y., Young, T., Yu, B., Yu, H., Yu, H., Yu, J., Yu, Y., Yuan, W., Zaki, R., Zalesak, J., Zambelli, L., Zamorano, B., Zani, A., Zazueta, L., Zeller, G., Zennamo, J., Zeug, K., Zhang, C., Zhang, S., Zhang, Y., Zhao, M., Zhivun, E., Zhu, G., Zimmerman, E. D., Zucchelli, S., Zuklin, J., Zutshi, V., and Zwaska, R.
Published: 2023
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