Author: "White, S" - Searchworks@Jio Institute Digital Library Search Results

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15,117 results on '"White, S"'

1. Photocathode characterisation for robust PICOSEC Micromegas precise-timing detectors

Author: Lisowska, M., Aleksan, R., Angelis, Y., Aune, S., Bortfeldt, J., Brunbauer, F., Brunoldi, M., Chatzianagnostou, E., Datta, J., Dehmelt, K., Fanourakis, G., Ferry, S., Fiorina, D., Floethner, K. J., Gallinaro, M., Garcia, F., Giomataris, I., Gnanvo, K., Iguaz, F. J., Janssens, D., Kallitsopoulou, A., Kovacic, M., Kross, B., Lai, C. C., Legou, P., Liu, J., Lupberger, M., Maniatis, I., McKisson, J., Meng, Y., Muller, H., De Oliveira, R., Oliveri, E., Orlandini, G., Pandey, A., Papaevangelou, T., Pomorski, M., Robert, M., Ropelewski, L., Sampsonidis, D., Scharenberg, L., Schneider, T., Scorsone, E., Sohl, L., van Stenis, M., Tsipolitis, Y., Tzamarias, S., Utrobicic, A., Vai, I., Veenhof, R., Viezzi, L., Vitulo, P., Volpato, C., Wang, X., White, S., Xi, W., Zhang, Z., and Zhou, Y.
Subjects: Physics - Instrumentation and Detectors
Abstract: The PICOSEC Micromegas detector is a precise-timing gaseous detector based on a Cherenkov radiator coupled with a semi-transparent photocathode and a Micromegas amplifying structure, targeting a time resolution of tens of picoseconds for minimum ionising particles. Initial single-pad prototypes have demonstrated a time resolution below 25 ps, prompting ongoing developments to adapt the concept for applications. The achieved performance is being transferred to robust multi-channel detector modules suitable for large-area detection systems requiring excellent timing precision. To enhance the robustness and stability of the PICOSEC Micromegas detector, research on robust carbon-based photocathodes, including Diamond-Like Carbon (DLC) and Boron Carbide (B4C), is pursued. Results from prototypes equipped with DLC and B4C photocathodes exhibited a time resolution of approximately 32 ps and 34.5 ps, respectively. Efforts dedicated to improve detector robustness and stability enhance the feasibility of the PICOSEC Micromegas concept for large experiments, ensuring sustained performance while maintaining excellent timing precision.
Published: 2024

2. Centrality dependence of L\'evy-stable two-pion Bose-Einstein correlations in $\sqrt{s_{_{NN}}}=200$ GeV Au$+$Au collisions

Author: PHENIX Collaboration, Abdulameer, N. J., Acharya, U., Adare, A., Aidala, C., Ajitanand, N. N., Akiba, Y., Akimoto, R., Al-Ta'ani, H., Alexander, J., Angerami, A., Aoki, K., Apadula, N., Aramaki, Y., Asano, H., Aschenauer, E. C., Atomssa, E. T., Awes, T. C., Azmoun, B., Babintsev, V., Bai, M., Bannier, B., Barish, K. N., Bassalleck, B., Bathe, S., Baublis, V., Baumgart, S., Bazilevsky, A., Belmont, R., Berdnikov, A., Berdnikov, Y., Bichon, L., Blankenship, B., Blau, D. S., Bok, J. S., Borisov, V., Boyle, K., Brooks, M. L., Buesching, H., Bumazhnov, V., Butsyk, S., Campbell, S., Castera, P., Chen, C. -H., Chen, D., Chiu, M., Chi, C. Y., Choi, I. J., Choi, J. B., Choi, S., Choudhury, R. K., Christiansen, P., Chujo, T., Chvala, O., Cianciolo, V., Citron, Z., Cole, B. A., Connors, M., Corliss, R., Csanád, M., Csörgő, T., D'Orazio, L., Dairaku, S., Datta, A., Daugherity, M. S., David, G., Denisov, A., Deshpande, A., Desmond, E. J., Dharmawardane, K. V., Dietzsch, O., Ding, L., Dion, A., Donadelli, M., Doomra, V., Drapier, O., Drees, A., Drees, K. A., Durham, J. M., Durum, A., Edwards, S., Efremenko, Y. V., Engelmore, T., Enokizono, A., Esha, R., Eyser, K. O., Fadem, B., Fields, D. E., Finger, Jr., M., Finger, M., Firak, D., Fitzgerald, D., Fleuret, F., Fokin, S. L., Frantz, J. E., Franz, A., Frawley, A. D., Fukao, Y., Fusayasu, T., Gainey, K., Gal, C., Garishvili, A., Garishvili, I., Glenn, A., Gong, X., Gonin, M., Goto, Y., de Cassagnac, R. Granier, Grau, N., Greene, S. V., Perdekamp, M. Grosse, Gunji, T., Guo, L., Guo, T., Gustafsson, H. -Å., Hachiya, T., Haggerty, J. S., Hahn, K. I., Hamagaki, H., Hanks, J., Hashimoto, K., Haslum, E., Hayano, R., Hemmick, T. K., Hester, T., He, X., Hill, J. C., Hodges, A., Hollis, R. S., Homma, K., Hong, B., Horaguchi, T., Hori, Y., Ichihara, T., Iinuma, H., Ikeda, Y., Imrek, J., Inaba, M., Iordanova, A., Isenhower, D., Issah, M., Ivanishchev, D., Jacak, B. V., Javani, M., Jiang, X., Ji, Z., Johnson, B. M., Joo, K. S., Jouan, D., Jumper, D. S., Kamin, J., Kaneti, S., Kang, B. H., Kang, J. H., Kang, J. S., Kapustinsky, J., Karatsu, K., Kasai, M., Kasza, G., Kawall, D., Kazantsev, A. V., Kempel, T., Khanzadeev, A., Kijima, K. M., Kim, B. I., Kim, C., Kim, D. J., Kim, E. -J., Kim, H. J., Kim, K. -B., Kim, Y. -J., Kim, Y. K., Kinney, E., Kiss, Á., Kistenev, E., Klatsky, J., Kleinjan, D., Kline, P., Komatsu, Y., Komkov, B., Koster, J., Kotchetkov, D., Kotov, D., Kovacs, L., Krizek, F., Král, A., Kunde, G. J., Kurgyis, B., Kurita, K., Kurosawa, M., Kwon, Y., Kyle, G. S., Lai, Y. S., Lajoie, J. G., Lebedev, A., Lee, B., Lee, D. M., Lee, J., Lee, K. B., Lee, K. S., Lee, S. H., Lee, S. R., Leitch, M. J., Leite, M. A. L., Leitgab, M., Lewis, B., Lim, S. H., Levy, L. A. Linden, Liu, M. X., Lökös, S., Loomis, D. A., Love, B., Maguire, C. F., Makdisi, Y. I., Makek, M., Manion, A., Manko, V. I., Mannel, E., Masumoto, S., McCumber, M., McGaughey, P. L., McGlinchey, D., McKinney, C., Mendoza, M., Meredith, B., Miake, Y., Mibe, T., Mignerey, A. C., Milov, A., Mishra, D. K., Mitchell, J. T., Mitrankova, M., Mitrankov, Iu., Miyachi, Y., Miyasaka, S., Mohanty, A. K., Mohapatra, S., Moon, H. J., Morrison, D. P., Motschwiller, S., Moukhanova, T. V., Mulilo, B., Murakami, T., Murata, J., Mwai, A., Nagae, T., Nagamiya, S., Nagle, J. L., Nagy, M. I., Nakagawa, I., Nakamiya, Y., Nakamura, K. R., Nakamura, T., Nakano, K., Nattrass, C., Nederlof, A., Nihashi, M., Nouicer, R., Novák, T., Novitzky, N., Nukazuka, G., Nyanin, A. S., O'Brien, E., Ogilvie, C. A., Okada, K., Orosz, M., Oskarsson, A., Ouchida, M., Ozawa, K., Pak, R., Pantuev, V., Papavassiliou, V., Park, B. H., Park, I. H., Park, J. S., Park, S., Park, S. K., Patel, L., Pate, S. F., Pei, H., Peng, J. -C., Pereira, H., Peressounko, D. Yu., Petti, R., Pinkenburg, C., Pisani, R. P., Potekhin, M., Proissl, M., Purschke, M. L., Qu, H., Rak, J., Ravinovich, I., Read, K. F., Reynolds, D., Riabov, V., Riabov, Y., Richardson, E., Richford, D., Roach, D., Roche, G., Rolnick, S. D., Rosati, M., Sahlmueller, B., Saito, N., Sakaguchi, T., Samsonov, V., Sano, M., Sarsour, M., Sawada, S., Sedgwick, K., Seidl, R., Sen, A., Seto, R., Sharma, D., Shein, I., Shibata, T. -A., Shigaki, K., Shimomura, M., Shoji, K., Shukla, P., Sickles, A., Silva, C. L., Silvermyr, D., Sim, K. S., Singh, B. K., Singh, C. P., Singh, V., Slunečka, M., Smith, K. L., Soltz, R. A., Sondheim, W. E., Sorensen, S. P., Sourikova, I. V., Stankus, P. W., Stenlund, E., Stepanov, M., Ster, A., Stoll, S. P., Sugitate, T., Sukhanov, A., Sun, J., Sun, Z., Sziklai, J., Takagui, E. M., Takahara, A., Taketani, A., Tanaka, Y., Taneja, S., Tanida, K., Tannenbaum, M. J., Tarafdar, S., Taranenko, A., Tennant, E., Themann, H., Todoroki, T., Tomášek, L., Tomášek, M., Torii, H., Towell, R. S., Tserruya, I., Tsuchimoto, Y., Tsuji, T., Ujvari, B., Vale, C., van Hecke, H. W., Vargyas, M., Vazquez-Zambrano, E., Veicht, A., Velkovska, J., Virius, M., Vossen, A., Vrba, V., Vznuzdaev, E., Vértesi, R., Wang, X. R., Watanabe, D., Watanabe, K., Watanabe, Y., Watanabe, Y. S., Wei, F., Wei, R., White, S. N., Winter, D., Wolin, S., Woody, C. L., Wysocki, M., Xia, B., Yamaguchi, Y. L., Yang, R., Yanovich, A., Ying, J., Yokkaichi, S., Younus, I., You, Z., Yushmanov, I. E., Zajc, W. A., and Zelenski, A.
Subjects: Nuclear Experiment
Abstract: The PHENIX experiment measured the centrality dependence of two-pion Bose-Einstein correlation functions in $\sqrt{s_{_{NN}}}=200$~GeV Au$+$Au collisions at the Relativistic Heavy Ion Collider at Brookhaven National Laboratory. The data are well represented by L\'evy-stable source distributions. The extracted source parameters are the correlation-strength parameter $\lambda$, the L\'evy index of stability $\alpha$, and the L\'evy-scale parameter $R$ as a function of transverse mass $m_T$ and centrality. The $\lambda(m_T)$ parameter is constant at larger values of $m_T$, but decreases as $m_T$ decreases. The L\'evy scale parameter $R(m_T)$ decreases with $m_T$ and exhibits proportionality to the length scale of the nuclear overlap region. The L\'evy exponent $\alpha(m_T)$ is independent of $m_T$ within uncertainties in each investigated centrality bin, but shows a clear centrality dependence. At all centralities, the L\'evy exponent $\alpha$ is significantly different from that of Gaussian ($\alpha=2$) or Cauchy ($\alpha=1$) source distributions. Comparisons to the predictions of Monte-Carlo simulations of resonance-decay chains show that in all but the most peripheral centrality class (50%-60%), the obtained results are inconsistent with the measurements, unless a significant reduction of the in-medium mass of the $\eta'$ meson is included. In each centrality class, the best value of the in-medium $\eta'$ mass is compared to the mass of the $\eta$ meson, as well as to several theoretical predictions that consider restoration of $U_A(1)$ symmetry in hot hadronic matter., Comment: 401 authors from 75 institutions, 20 pages, 15 figures, 2 tables. v1 is version submitted to Physical Review C. HEPdata tables for the points plotted in figures for this and previous PHENIX publications are (or will be) publicly available at http://www.phenix.bnl.gov/papers.html
Published: 2024

3. Optical Tweezer Arrays of Erbium Atoms

Author: Grün, D. S., White, S. J. M., Ortu, A., Di Carli, A., Edri, H., Lepers, M., Mark, M. J., and Ferlaino, F.
Subjects: Physics - Atomic Physics, Condensed Matter - Quantum Gases
Abstract: We present the first successful trapping of single erbium atoms in an array of optical tweezers. Using a single narrow-line optical transition, we achieve deep cooling for direct tweezer loading, pairwise ejection, and continous imaging without additional recoil suppression techniques. Our tweezer wavelength choice enables us to reach the magic trapping condition by tuning the ellipticity of the trapping light. Additionally, we implement an ultrafast high-fidelity fluorescence imaging scheme using a broad transition, allowing time-resolved study of the tweezer population dynamics from many to single atoms during light-assisted collisions. In particular, we extract a pair-ejection rate that qualitatively agrees with the semiclassical predictions by the Gallagher-Pritchard model. This work represents a promising starting point for the exploration of erbium as a powerful resource for quantum simulation in optical tweezers.
Published: 2024

4. A Novel Diamond-like Carbon based photocathode for PICOSEC Micromegas detectors

Author: Wang, X., Aleksan, R., Angelis, Y., Bortfeldt, J., Brunbauer, F., Brunoldi, M., Chatzianagnostou, E., Datta, J., Degmelt, K., Fanourakis, G., Fiorina, D., Floethner, K. J., Gallinaro, M., Garcia, F., Giomataris, I., Gnanvo, K., Iguaz, F. J., Janssens, D., Kallitsopoulou, A., Kovacic, M., Kross, B., Legou, P., Lisowska, M., Liu, J., Maniatis, I., McKisson, J., Meng, Y., Muller, H., Oliveri, E., Orlandini, G., Pandey, A., Papaevangelou, T., Pomorski, M., Ropelewski, L., Sampsonidis, D., Scharenberg, L., Schneider, T., Shang, L., Shao, M., Sohl, L., van Stenis, M., Tsipolitis, Y., Tzamarias, S. E., Utrobicic, A., Vai, I., Veenhof, R., Vitulo, P., White, S., Xi, W., Zhang, Z., and Zhou, Y.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The PICOSEC Micromegas (MM) detector is a precise timing gaseous detector based on a MM detector operating in a two-stage amplification mode and a Cherenkov radiator. Prototypes equipped with cesium iodide (CsI) photocathodes have shown promising time resolutions as precise as 24 picoseconds (ps) for Minimum Ionizing Particles. However, due to the high hygroscopicity and susceptibility to ion bombardment of the CsI photocathodes, alternative photocathode materials are needed to improve the robustness of PICOSEC MM. Diamond-like Carbon (DLC) film have been introduced as a novel robust photocathode material, which have shown promising results. A batch of DLC photocathodes with different thicknesses were produced and evaluated using ultraviolet light. The quantum efficiency measurements indicate that the optimized thickness of the DLC photocathode is approximately 3 nm. Furthermore, DLC photocathodes show good resistance to ion bombardment in aging test compared to the CsI photocathode. Finally, a PICOSEC MM prototype equipped with DLC photocathodes was tested in muon beams. A time resolution of around 42 ps with a detection efficiency of 97% for 150 GeV/c muons were obtained. These results indicate the great potential of DLC as a photocathode for the PICOSEC MM detector.
Published: 2024

5. Jet modification via $\pi^0$-hadron correlations in Au$+$Au collisions at $\sqrt{s_{_{NN}}}=200$ GeV

Author: PHENIX Collaboration, Abdulameer, N. J., Acharya, U., Adare, A., Afanasiev, S., Aidala, C., Ajitanand, N. N., Akiba, Y., Al-Bataineh, H., Alexander, J., Alfred, M., Aoki, K., Apadula, N., Aphecetche, L., Asai, J., Asano, H., Atomssa, E. T., Averbeck, R., Awes, T. C., Azmoun, B., Babintsev, V., Bai, M., Baksay, G., Baksay, L., Baldisseri, A., Bandara, N. S., Bannier, B., Barish, K. N., Barnes, P. D., Bassalleck, B., Basye, A. T., Bathe, S., Batsouli, S., Baublis, V., Baumann, C., Bazilevsky, A., Beaumier, M., Beckman, S., Belikov, S., Belmont, R., Bennett, R., Berdnikov, A., Berdnikov, Y., Bichon, L., Bickley, A. A., Blankenship, B., Blau, D. S., Boissevain, J. G., Bok, J. S., Borel, H., Borisov, V., Boyle, K., Brooks, M. L., Bryslawskyj, J., Buesching, H., Bumazhnov, V., Bunce, G., Butsyk, S., Camacho, C. M., Campbell, S., Chang, B. S., Chang, W. C., Charvet, J. L., Chen, C. -H., Chen, D., Chernichenko, S., Chiu, M., Chi, C. Y., Choi, I. J., Choi, J. B., Choudhury, R. K., Chujo, T., Chung, P., Churyn, A., Cianciolo, V., Citron, Z., Cole, B. A., Connors, M., Constantin, P., Corliss, R., Csanád, M., Csörgő, T., d'Enterria, D., Dahms, T., Dairaku, S., Danley, T. W., Das, K., Datta, A., Daugherity, M. S., David, G., DeBlasio, K., Dehmelt, K., Denisov, A., Deshpande, A., Desmond, E. J., Dietzsch, O., Dion, A., Diss, P. B., Donadelli, M., Doomra, V., Do, J. H., Drapier, O., Drees, A., Drees, K. A., Dubey, A. K., Durham, J. M., Durum, A., Dutta, D., Dzhordzhadze, V., Efremenko, Y. V., Ellinghaus, F., En'yo, H., Engelmore, T., Enokizono, A., Esha, R., Eyser, K. O., Fadem, B., Feege, N., Fields, D. E., Finger, Jr., M., Finger, M., Firak, D., Fitzgerald, D., Fleuret, F., Fokin, S. L., Fraenkel, Z., Frantz, J. E., Franz, A., Frawley, A. D., Fujiwara, K., Fukao, Y., Fusayasu, T., Gallus, P., Gal, C., Garg, P., Garishvili, I., Ge, H., Giordano, F., Glenn, A., Gong, H., Gonin, M., Gosset, J., Goto, Y., de Cassagnac, R. Granier, Grau, N., Greene, S. V., Perdekamp, M. Grosse, Gunji, T., Guo, T., Gustafsson, H. -Å., Hachiya, T., Henni, A. Hadj, Haggerty, J. S., Hahn, K. I., Hamagaki, H., Hamilton, H. F., Hanks, J., Han, R., Han, S. Y., Hartouni, E. P., Haruna, K., Hasegawa, S., Haseler, T. O. S., Hashimoto, K., Haslum, E., Hayano, R., Heffner, M., Hemmick, T. K., Hester, T., He, X., Hill, J. C., Hodges, A., Hohlmann, M., Hollis, R. S., Holzmann, W., Homma, K., Hong, B., Horaguchi, T., Hornback, D., Hoshino, T., Hotvedt, N., Huang, J., Ichihara, T., Ichimiya, R., Iinuma, H., Ikeda, Y., Imai, K., Imrek, J., Inaba, M., Iordanova, A., Isenhower, D., Ishihara, M., Isobe, T., Issah, M., Isupov, A., Ivanishchev, D., Jacak, B. V., Jezghani, M., Jiang, X., Jin, J., Ji, Z., Johnson, B. M., Joo, K. S., Jouan, D., Jumper, D. S., Kajihara, F., Kametani, S., Kamihara, N., Kamin, J., Kanda, S., Kang, J. H., Kapustinsky, J., Kawall, D., Kazantsev, A. V., Kempel, T., Key, J. A., Khachatryan, V., Khanzadeev, A., Kijima, K. M., Kikuchi, J., Kimelman, B., Kim, B. I., Kim, C., Kim, D. H., Kim, D. J., Kim, E., Kim, E. -J., Kim, G. W., Kim, M., Kim, S. H., Kinney, E., Kiriluk, K., Kiss, Á., Kistenev, E., Kitamura, R., Klatsky, J., Klay, J., Klein-Boesing, C., Kleinjan, D., Kline, P., Koblesky, T., Kochenda, L., Komkov, B., Konno, M., Koster, J., Kotov, D., Kovacs, L., Kozlov, A., Kravitz, A., Král, A., Kunde, G. J., Kurgyis, B., Kurita, K., Kurosawa, M., Kweon, M. J., Kwon, Y., Kyle, G. S., Lai, Y. S., Lajoie, J. G., Layton, D., Lebedev, A., Lee, D. M., Lee, K. B., Lee, S., Lee, S. H., Lee, T., Leitch, M. J., Leite, M. A. L., Lenzi, B., Liebing, P., Lim, S. H., Litvinenko, A., Liu, H., Liu, M. X., Liška, T., Li, X., Lokos, S., Loomis, D. A., Love, B., Lynch, D., Maguire, C. F., Makdisi, Y. I., Makek, M., Malakhov, A., Malik, M. D., Manion, A., Manko, V. I., Mannel, E., Mao, Y., Masui, H., Matathias, F., Mašek, L., McCumber, M., McGaughey, P. L., McGlinchey, D., McKinney, C., Means, N., Meles, A., Mendoza, M., Meredith, B., Miake, Y., Mignerey, A. C., Mikeš, P., Miki, K., Milov, A., Mishra, D. K., Mishra, M., Mitchell, J. T., Mitrankova, M., Mitrankov, Iu., Miyasaka, S., Mizuno, S., Mohanty, A. K., Montuenga, P., Moon, T., Morino, Y., Morreale, A., Morrison, D. P., Moukhanova, T. V., Mukhopadhyay, D., Mulilo, B., Murakami, T., Murata, J., Mwai, A., Nagamiya, S., Nagashima, K., Nagle, J. L., Naglis, M., Nagy, M. I., Nakagawa, I., Nakagomi, H., Nakamiya, Y., Nakamura, T., Nakano, K., Nattrass, C., Netrakanti, P. K., Newby, J., Nguyen, M., Niida, T., Nishimura, S., Nouicer, R., Novitzky, N., Novák, T., Nukazuka, G., Nyanin, A. S., O'Brien, E., Oda, S. X., Ogilvie, C. A., Okada, K., Oka, M., Onuki, Y., Koop, J. D. Orjuela, Orosz, M., Osborn, J. D., Oskarsson, A., Ouchida, M., Ozawa, K., Pak, R., Palounek, A. P. T., Pantuev, V., Papavassiliou, V., Park, J., Park, J. S., Park, S., Park, W. J., Patel, M., Pate, S. F., Pei, H., Peng, J. -C., Pereira, H., Perepelitsa, D. V., Perera, G. D. N., Peresedov, V., Peressounko, D. Yu., Perry, J., Petti, R., Pinkenburg, C., Pinson, R., Pisani, R. P., Potekhin, M., Purschke, M. L., Purwar, A. K., Qu, H., Rakotozafindrabe, A., Rak, J., Ramson, B. J., Ravinovich, I., Read, K. F., Rembeczki, S., Reygers, K., Reynolds, D., Riabov, V., Riabov, Y., Richford, D., Rinn, T., Roach, D., Roche, G., Rolnick, S. D., Rosati, M., Rosendahl, S. S. E., Rosnet, P., Rowan, Z., Rubin, J. G., Rukoyatkin, P., Ružička, P., Rykov, V. L., Sahlmueller, B., Saito, N., Sakaguchi, T., Sakai, S., Sakashita, K., Sako, H., Samsonov, V., Sarsour, M., Sato, S., Sato, T., Sawada, S., Schaefer, B., Schmoll, B. K., Sedgwick, K., Seele, J., Seidl, R., Semenov, A. Yu., Semenov, V., Sen, A., Seto, R., Sett, P., Sexton, A., Sharma, D., Shein, I., Shibata, T. -A., Shigaki, K., Shimomura, M., Shoji, K., Shukla, P., Sickles, A., Silva, C. L., Silvermyr, D., Silvestre, C., Sim, K. S., Singh, B. K., Singh, C. P., Singh, V., Slunečka, M., Smith, K. L., Snowball, M., Soldatov, A., Soltz, R. A., Sondheim, W. E., Sorensen, S. P., Sourikova, I. V., Staley, F., Stankus, P. W., Stenlund, E., Stepanov, M., Ster, A., Stoll, S. P., Sugitate, T., Suire, C., Sukhanov, A., Sumita, T., Sun, J., Sun, Z., Sziklai, J., Takagui, E. M., Taketani, A., Tanabe, R., Tanaka, Y., Tanida, K., Tannenbaum, M. J., Tarafdar, S., Taranenko, A., Tarján, P., Themann, H., Thomas, T. L., Tieulent, R., Timilsina, A., Todoroki, T., Togawa, M., Toia, A., Tomita, Y., Tomášek, L., Tomášek, M., Torii, H., Towell, C. L., Towell, R., Towell, R. S., Tram, V-N., Tserruya, I., Tsuchimoto, Y., Ujvari, B., Vale, C., Valle, H., van Hecke, H. W., Veicht, A., Velkovska, J., Vinogradov, A. A., Virius, M., Vrba, V., Vznuzdaev, E., Vértesi, R., Wang, X. R., Watanabe, Y., Watanabe, Y. S., Wei, F., Wessels, J., White, A. S., White, S. N., Winter, D., Woody, C. L., Wysocki, M., Xia, B., Xie, W., Xue, L., Yalcin, S., Yamaguchi, Y. L., Yamaura, K., Yang, R., Yanovich, A., Ying, J., Yokkaichi, S., Yoon, I., Yoo, J. H., Young, G. R., Younus, I., Yushmanov, I. E., Yu, H., Zajc, W. A., Zaudtke, O., Zelenski, A., Zhang, C., Zhou, S., Zolin, L., and Zou, L.
Subjects: Nuclear Experiment
Abstract: High-momentum two-particle correlations are a useful tool for studying jet-quenching effects in the quark-gluon plasma. Angular correlations between neutral-pion triggers and charged hadrons with transverse momenta in the range 4--12~GeV/$c$ and 0.5--7~GeV/$c$, respectively, have been measured by the PHENIX experiment in 2014 for Au$+$Au collisions at $\sqrt{s_{_{NN}}}=200$~GeV. Suppression is observed in the yield of high-momentum jet fragments opposite the trigger particle, which indicates jet suppression stemming from in-medium partonic energy loss, while enhancement is observed for low-momentum particles. The ratio and differences between the yield in Au$+$Au collisions and $p$$+$$p$ collisions, $I_{AA}$ and $\Delta_{AA}$, as a function of the trigger-hadron azimuthal separation, $\Delta\phi$, are measured for the first time at the Relativistic Heavy Ion Collider. These results better quantify how the yield of low-$p_T$ associated hadrons is enhanced at wide angle, which is crucial for studying energy loss as well as medium-response effects., Comment: 534 authors from 83 institutions, 12 pages, 7 figures. v1 is version submitted to Physical Review C. HEPdata tables for the points plotted in figures for this and previous PHENIX publications are (or will be) publicly available at http://www.phenix.bnl.gov/papers.html
Published: 2024

6. GaLactic and Extragalactic All-sky Murchison Widefield Array eXtended (GLEAM-X) survey II: Second Data Release

Author: Ross, K., Hurley-Walker, N., Galvin, T. J., Venville, B., Duchesne, S. W., Morgan, J., An, T., Gurkan, G., Hancock, P. J., Heald, G., Johnston-Hollitt, M., and White, S. V.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present the second data release for the GaLactic and Extragalactic All-sky Murchison Widefield Array eXtended (GLEAM-X) survey. This data release is an area of 12,892-deg^2 around the South Galactic Pole region covering 20h 40m <= RA <= 6h 40m, -90deg <= Dec <= +30deg. Observations were taken in 2020 using the Phase-II configuration of the Murchison Widefield Array (MWA) and covering a frequency range of 72-231MHz with twenty frequency bands. We produce a wideband source-finding mosaic over 170-231MHz with a median root mean squared noise of 1.5 (+1.5/-0.5) mJy beam^(-1). We present a catalogue of 624,866 components, including 562,302 components which are spectrally fit. This catalogue is 98% complete at 50mJy, and a reliability of 98.7% at a 5sigma level, consistent with expectations for this survey. The catalogue is made available via Vizier and the PASA datastore and accompanying mosaics for this data release are made available via AAO Data Central and SkyView., Comment: Accepted for publication in PASA; 24 pages, 15 figures
Published: 2024

7. Single channel PICOSEC Micromegas detector with improved time resolution

Author: Utrobicic, A., Aleksan, R., Angelis, Y., Bortfeldt, J., Brunbauer, F., Brunoldi, M., Chatzianagnostou, E., Datta, J., Dehmelt, K., Fanourakis, G., Fiorina, D., Floethner, K. J., Gallinaro, M., Garcia, F., Giomataris, I., Gnanvo, K., Iguaz, F. J., Janssens, D., Kallitsopoulou, A., Kovacic, M., Kross, B., Legou, P., Lisowska, M., Liu, J., Lupberger, M., Maniatis, I., McKisson, J., Meng, Y., Muller, H., Oliveri, E., Orlandini, G., Pandey, A., Papaevangelou, T., Pomorski, M., Ropelewski, L., Sampsonidis, D., Scharenberg, L., Schneider, T., Sohl, L., van Stenis, M., Tsipolitis, Y., Tzamarias, S. E., Vai, I., Veenhof, R., Vitulo, P., Wang, X., White, S., Xi, W., Zhang, Z., and Zhou, Y.
Subjects: Physics - Instrumentation and Detectors
Abstract: This paper presents design guidelines and experimental verification of a single-channel PICOSEC Micromegas (MM) detector with an improved time resolution. The design encompasses the detector board, vessel, auxiliary mechanical parts, and electrical connectivity for high voltage (HV) and signals, focusing on improving stability, reducing noise, and ensuring signal integrity to optimize timing performance. A notable feature is the simple and fast reassembly procedure, facilitating quick replacement of detector internal components that allows for an efficient measurement strategy involving different detector components. The paper also examines the influence of parasitics on the output signal integrity. To validate the design, a prototype assembly and three interchangeable detector boards with varying readout pad diameters were manufactured. The detectors were initially tested in the laboratory environment. Finally, the timing performance of detectors with different pad sizes was verified using a Minimum Ionizing Particle (MIP) beam test. Notably, a record time resolution for a PICOSEC Micromegas detector technology with a CsI photocathode of 12.5$\pm$0.8 ps was achieved with a 10 mm diameter readout pad size detector.
Published: 2024

8. TOFHIR2: The readout ASIC of the CMS Barrel MIP Timing Detector

Author: Albuquerque, E., Araújo, M., Benaglia, A., Boletti, A., Bugalho, R., Coutinho, T., De Guio, F., Faccioli, P., Ferramacho, L., Firlej, M., Fiutowski, T., Francisco, R., Gallinaro, M., Ghezzi, A., Hollar, J., Idzik, M., Legoinha, H., Leonardo, N., Leong, C., Lucchini, M. T., Malberti, M., Marozzo, G., Da Molin, G., Moron, J., Niknejad, T., Oliveira, L., Oliveira, N., Palluotto, S., Pisano, M., Redaelli, N., Silva, C., Silva, J. C., Silva, R., Silveira, M., Swientek, K., de Fatis, T. Tabarelli, Tavernier, S., Varela, J., Varela, V., White, S., and Wulff, J.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The CMS detector will be upgraded for the HL-LHC to include a MIP Timing Detector (MTD). The MTD will consist of barrel and endcap timing layers, BTL and ETL respectively, providing precision timing of charged particles. The BTL sensors are based on LYSO:Ce scintillation crystals coupled to SiPMs with TOFHIR2 ASICs for the front-end readout. A resolution of 30-60 ps for MIP signals at a rate of 2.5 Mhit/s per channel is expected along the HL-LHC lifetime. We present an overview of the TOFHIR2 requirements and design, simulation results and measurements with TOFHIR2 ASICs. The measurements of TOFHIR2 associated to sensor modules were performed in different test setups using internal test pulses or blue and UV laser pulses emulating the signals expected in the experiment. The measurements show a time resolution of 24 ps initially during Beginning of Operation (BoO) and 58 ps at End of Operation (EoO) conditions, matching well the BTL requirements. We also showed that the time resolution is stable up to the highest expected MIP rate. Extensive radiation tests were performed, both with x-rays and heavy ions, showing that TOFHIR2 is not affected by the radiation environment during the experiment lifetime., Comment: Editor: J. Varela
Published: 2024

9. MIGHTEE: multi-wavelength counterparts in the COSMOS field

Author: Whittam, I. H., Prescott, M., Hale, C. L., Jarvis, M . J., Heywood, I., An, Fangxia, Glowacki, M., Maddox, N., Marchetti, L., Morabito, L. K., Adams, N. J., Bowler, R. A. A., Hatfield, P. W., Varadaraj, R. G., Collier, J., Frank, B., Taylor, A. R., Santos, M. G., Vaccari, M., Afonso, J., Ao, Y., Delhaize, J., Knowles, K., Kolwa, S., Randriamampandry, S. M., Randriamanakoto, Z., Smirnov, O., Smith, D. J. B., and White, S. V.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: In this paper we combine the Early Science radio continuum data from the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) Survey, with optical and near-infrared data and release the cross-matched catalogues. The radio data used in this work covers $0.86$ deg$^2$ of the COSMOS field, reaches a thermal noise of $1.7$ $\mu$Jy/beam and contains $6102$ radio components. We visually inspect and cross-match the radio sample with optical and near-infrared data from the Hyper Suprime-Cam (HSC) and UltraVISTA surveys. This allows the properties of active galactic nuclei and star-forming populations of galaxies to be probed out to $z \approx 5$. Additionally, we use the likelihood ratio method to automatically cross-match the radio and optical catalogues and compare this to the visually cross-matched catalogue. We find that 94 per cent of our radio source catalogue can be matched with this method, with a reliability of $95$ per cent. We proceed to show that visual classification will still remain an essential process for the cross-matching of complex and extended radio sources. In the near future, the MIGHTEE survey will be expanded in area to cover a total of $\sim$20~deg$^2$; thus the combination of automated and visual identification will be critical. We compare redshift distribution of SFG and AGN to the SKADS and T-RECS simulations and find more AGN than predicted at $z \sim 1$., Comment: 15 pages, 15 figures. Accepted for publication in MNRAS
Published: 2023

10. Powerful Radio Sources in the Southern Sky. II. A SWIFT X-Ray Perspective

Author: Massaro, F., White, S. V., Paggi, A., Jimenez-Gallardo, A., Madrid, J. P., Mazzucchelli, C., Forman, W. R., Capetti, A., Leto, C., Garcia-Perez, A., Cheung, C. C., Chavushyan, V., Nesvadba, N. P. H., Andruchow, I., Pena-Herazo, H. A., Sani, E., Grossova, R., Reynaldi, V., Kraft, R. P., Balmaverde, B., and Cellone, S.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We recently constructed the G4Jy-3CRE, a catalog of extragalactic radio sources based on the GLEAM 4-Jy (G4Jy) sample, with the aim of increasing the number of powerful radio galaxies and quasars with similar selection criteria to those of the revised release of the Third Cambridge catalog (3CR). The G4Jy-3CRE consists of a total of 264 radio sources mainly visible from the Southern Hemisphere. Here, we present an initial X-ray analysis of 89 G4Jy-3CRE radio sources with archival X- ray observations from the Neil Gehrels Swift Observatory. We reduced a total of 615 Swift observations, for about 0.89 Msec of integrated exposure time, we found X-ray counterparts for 61 radio sources belonging to the G4Jy-3CRE, 11 of them showing extended X-ray emission. The remaining 28 sources do not show any X-ray emission associated with their radio cores. Our analysis demonstrates that X-ray snapshot observations, even if lacking uniform exposure times, as those carried out with Swift, allow us to (i) verify and/or re ne the host galaxy identi cation; (ii) discover the extended X-ray emission around radio galaxies of the intracluster medium when harbored in galaxy clusters, as the case of G4Jy 1518 and G4Jy 1664, and (iii) detect X-ray radiation arising from their radio lobes, as for G4Jy 1863., Comment: 35 pages, 17 figures, 2 tables; second paper of a series, pre-proof version
Published: 2023
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11. Generation of photoionized plasmas in the laboratory of relevance to accretion-powered x-ray sources using keV line radiation

Author: Riley, D., Singh, R. L., White, S, Charlwood, M., Bailie, D., Hyland, C., Audet, T., Sarri, G., Kettle, B., Gribakin, G., Rose, S. J., Hill, E. G., Ferland, G. J., Williams, R. J. R., and Keenan, F. P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We describe laboratory experiments to generate X-ray photoionized plasmas of relevance to accretion-powered X-ray sources such as neutron star binaries and quasars, with significant improvements over previous work. A key quantity is referenced, namely the photoionization parameter. This is normally meaningful in an astrophysical steady-state context, but is also commonly used in the literature as a figure of merit for laboratory experiments that are, of necessity, time-dependent. We demonstrate emission-weighted values of {\xi} > 50 ergcm/s using laser-plasma X-ray sources, with higher results at the centre of the plasma which are in the regime of interest for several astrophysical scenarios. Comparisons of laboratory experiments with astrophysical codes are always limited, principally by the many orders of magnitude differences in time and spatial scales, but also other plasma parameters. However useful checks on performance can often be made for a limited range of parameters. For example, we show that our use of a keV line source, rather than the quasi-blackbody radiation fields normally employed in such experiments, has allowed the generation of the ratio of inner-shell to outer-shell photoionization expected from a blackbody source with ~keV spectral temperature. We compare calculations from our in-house plasma modelling code with those from Cloudy and find moderately good agreement for the time evolution of both electron temperature and average ionisation. However, a comparison of code predictions for a K-beta argon X-ray spectrum with experimental data reveals that our Cloudy simulation overestimates the intensities of more highly ionised argon species. This is not totally surprising as the Cloudy model was generated for a single set of plasma conditions, while the experimental data are spatially integrated., Comment: High Energy Density Physics, in press; 21 pages, 10 figures
Published: 2023

12. Powerful Radio Sources in the Southern Sky. I. Optical Identifications

Author: Massaro, F., White, S. V., Garcia-Perez, A., Jimenez-Gallardo, A., Capetti, A., Cheung, C. C., Forman, W. R., Mazzucchelli, C., Paggi, A., Nesvadba, N. P. H., Madrid, J. P., Andruchow, I., Cellone, S., Pena-Herazo, H. A., Grossova, R., Balmaverde, B., Sani, E., Chavushyan, V., Kraft, R. P., Reynaldi, V., and Leto, C.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Since the early sixties, our view of radio galaxies and quasars has been drastically shaped by discoveries made thanks to observations of radio sources listed in the Third Cambridge catalog and its revised version (3CR). However, the largest fraction of data collected to date on 3CR sources was performed with relatively old instruments, rarely repeated and/or updated. Importantly, the 3CR contains only objects located in the Northern Hemisphere thus having limited access to new and innovative astronomical facilities. To mitigate these limitations we present a new catalog of powerful radio sources visible from the Southern Hemisphere, extracted from the GLEAM 4-Jy (G4Jy) catalog and based on equivalent selection criteria as the 3CR. This new catalog, named G4Jy- 3CRE, where the E stands for "equivalent", lists a total of 264 sources at declination below -5 degrees and with 9 Jy limiting sensitivity at ~178 MHz. We explored archival radio maps obtained with different surveys and compared then with optical images available in the Pan-STARRS, DES and DSS databases to search for optical counterparts of their radio cores. We compared mid-infrared counterparts, originally associated in the G4Jy, with the optical ones identified here and we present results of a vast literature search carried out to collect redshift estimates for all G4Jy-3CRE sources resulting in a total of 145 reliable z measurements., Comment: 72 pages, 35 figures, 5 Tables
Published: 2023
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13. Solar Radio Imaging at Arecibo: The Brightness Temperature and Magnetic Field of Active Regions

Author: Manoharan, P. K., Salter, C. J., White, S. M., Perillat, P., Fernandez, F., Perera, B., Venkataraman, A., and Brum, C.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Space Physics
Abstract: Strong solar magnetic fields are the energy source of intense flares and energetic coronal mass ejections of space weather importance. The key issue is the difficulty in predicting the occurrence time and location of strong solar eruptions, those leading to high impact space weather disturbances at the near-Earth environment. Here, we report regular solar mapping made at X-band (8.1 -- 9.2 GHz) with the Arecibo 12-m radio telescope. This has demonstrated its potential for identifying active regions, about one half to a day in advance, when they rotate on to the central meridian of the Sun, and predicting the strongest flares and coronal mass ejections directed towards the Earth. Results show (i) a good correlation between the temporal evolution of brightness temperature of active regions and their magnetic configurations; (ii) the ability of the mapping data to provide a better picture of the formation sites of active regions and to accurately track their evolution across the solar disk, giving forewarning of intense solar eruptions leading to severe space weather consequences; (iii) the importance of long-term monitoring of the Sun at X-band for understanding the complex three-dimensional evolution of solar features as a function of solar activity. The key point in this study is the identification of the magnetic properties of active regions on the solar disk to aid in improving forecast strategies for extreme space-weather events., Comment: 27 pages, 17 figures, submitted to Solar Physics
Published: 2023

14. Integration of thermo-electric coolers into the CMS MTD SiPM arrays for operation under high neutron fluence

Author: Bornheim, A., Lustermann, W., Stachon, K., Gutiérrez, G. Reales, Benaglia, A., De Guio, F., Ghezzi, A., Lucchini, M. T., Malberti, M., Palluotto, S., de Fatis, T. Tabarelli, Benettoni, M., Carlin, R., Tosi, M., Rossin, R., Meridiani, P., Paramatti, R., Santanastasio, F., Silva, J. C., Varela, J., Heering, A., Karneyeu, A., Musienko, Y., Wayne, M., Anderson, T., Cox, B., Lara, C. E. Perez, Ledovskoy, A., White, S., and Schmidt, I.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The barrel section of the novel MIP Timing Detector (MTD) will be constructed as part of the upgrade of the CMS experiment to provide a time resolution for single charged tracks in the range of $30-60$ ps using LYSO:Ce crystal arrays read out with Silicon Photomultipliers (SiPMs). A major challenge for the operation of such a detector is the extremely high radiation level, of about $2\times10^{14}$ 1 MeV(Si) Eqv. n/cm$^2$, that will be integrated over a decade of operation of the High Luminosity Large Hadron Collider (HL-LHC). Silicon Photomultipliers exposed to this level of radiation have shown a strong increase in dark count rate and radiation damage effects that also impact their gain and photon detection efficiency. For this reason during operations the whole detector is cooled down to about $-35^{\circ}$C. In this paper we illustrate an innovative and cost-effective solution to mitigate the impact of radiation damage on the timing performance of the detector, by integrating small thermo-electric coolers (TECs) on the back of the SiPM package. This additional feature, fully integrated as part of the SiPM array, enables a further decrease in operating temperature down to about $-45^{\circ}$C. This leads to a reduction by a factor of about two in the dark count rate without requiring additional power budget, since the power required by the TEC is almost entirely offset by a decrease in the power required for the SiPM operation due to leakage current. In addition, the operation of the TECs with reversed polarity during technical stops of the accelerator can raise the temperature of the SiPMs up to $60^{\circ}$C (about $50^{\circ}$C higher than the rest of the detector), thus accelerating the annealing of radiation damage effects and partly recovering the SiPM performance.
Published: 2023
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15. Precise timing and recent advancements with segmented anode PICOSEC Micromegas prototypes

Author: Manthos, I., Aune, S., Bortfeldt, J., Brunbauer, F., David, C., Desforge, D., Fanourakis, G., Gallinaro, M., García, F., Giomataris, I., Gustavsson, T., Iguaz, F. J., Kallitsopoulou, A., Kebbiri, M., Kordas, K., Lampoudis, C., Legou, P., Lisowska, M., Liu, J., Lupberger, M., Maillard, O., Maniatis, I., Müller, H., Oliveri, E., Papaevangelou, T., Paraschou, K., Pomorski, M., Qi, B., Resnati, F., Ropelewski, L., Sampsonidis, D., Scharenberg, L., Schneider, T., Sohl, L., van Stenis, M., Tsiamis, A., Tsipolitis, Y., Tzamarias, S. E., Utrobicic, A., Veenhof, R., Wang, X., White, S., Zhang, Z., and Zhou, Y.
Subjects: Physics - Instrumentation and Detectors
Abstract: Timing information in current and future accelerator facilities is important for resolving objects (particle tracks, showers, etc.) in extreme large particles multiplicities on the detection systems. The PICOSEC Micromegas detector has demonstrated the ability to time 150\,GeV muons with a sub-25\,ps precision. Driven by detailed simulation studies and a phenomenological model which describes stochastically the dynamics of the signal formation, new PICOSEC designs were developed that significantly improve the timing performance of the detector. PICOSEC prototypes with reduced drift gap size ($\sim$\SI{119}{\micro\metre}) achieved a resolution of 45\,ps in timing single photons in laser beam tests (in comparison to 76\,ps of the standard PICOSEC detector). Towards large area detectors, multi-pad PICOSEC prototypes with segmented anodes has been developed and studied. Extensive tests in particle beams revealed that the multi-pad PICOSEC technology provides also very precise timing, even when the induced signal is shared among several neighbouring pads. Furthermore, new signal processing algorithms have been developed, which can be applied during data acquisition and provide real time, precise timing., Comment: 5 pages, 3 figures, 12th International Conference on Position Sensitive Detectors
Published: 2022
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16. Subarcsecond imaging of a solar active region filament with ALMA and IRIS

Author: Santos, J. M. da Silva, White, S. M., Reardon, K., Cauzzi, G., Gunár, S., Heinzel, P., and Leenaarts, J.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Quiescent filaments appear as absorption features on the solar disk when observed in chromospheric lines and at continuum wavelengths in the millimeter (mm) range. Active region (AR) filaments are their small-scale, low-altitude analogues, but they could not be resolved in previous mm observations. This spectral diagnostic can provide insight into the details of the formation and physical properties of their fine threads, which are still not fully understood. Here, we shed light on the thermal structure of an AR filament using high-resolution brightness temperature ($T_{\rm b}$) maps taken with ALMA Band 6 complemented by simultaneous IRIS near-UV spectra, Hinode/SOT photospheric magnetograms, and SDO/AIA extreme-UV images. Some of the dark threads visible in the AIA 304 {\AA} passband and in the core of Mg II resonance lines have dark ($T_{\rm b}<5000$K) counterparts in the 1.25 mm maps, but their visibility significantly varies across the filament spine and in time. These opacity changes are possibly related to variations in temperature and electron density in filament fine structures. The coolest $T_{\rm b}$ values ($<$5000 K) coincide with regions of low integrated intensity in the Mg II h and k lines. ALMA Band 3 maps taken after the Band 6 ones do not clearly show the filament structure, contrary to the expectation that the contrast should increase at longer wavelengths based on previous observations of quiescent filaments. The ALMA maps are not consistent with isothermal conditions, but the temporal evolution of the filament may partly account for this., Comment: 15 pages, 4 figures. Accepted for publication in Front. Astron. Space Sci.; research topic: "The Sun Seen with the Atacama Large mm and sub-mm Array (ALMA) - First Results"
Published: 2022

17. L-shell X-ray conversion yields for laser-irradiated tin and silver foils

Author: Singh, R. L., White, S., Charlwood, M., Keenan, F. P., Hyland, C., Bailie, D., Audet, T., Sarri, G., Rose, S. J., Morton, J., Baird, C., Spindloe, C., and Riley, D.
Subjects: Physics - Plasma Physics
Abstract: We have employed the VULCAN laser facility to generate a laser plasma X-ray source for use in photoionisation experiments. A nanosecond laser pulse with an intensity of order ${10}^{15}$ W{cm}$^{-2}$ was used to irradiate thin Ag or Sn foil targets coated onto a parylene substrate, and the L-shell emission in the $3.3-4.4$ keV range was recorded for both the laser-irradiated and non-irradiated sides. Both the experimental and simulation results show higher laser to X-ray conversion yields for Ag compared with Sn, with our simulations indicating yields approximately a factor of two higher than found in the experiments. Although detailed angular data were not available experimentally, the simulations indicate that the emission is quite isotropic on the laser-irradiated side, but shows close to a cosine variation on the non-irradiated side of the target as seen experimentally in previous work., Comment: Number of papges: 14, Number of figures: 12
Published: 2022

18. Low-$p_T$ direct-photon production in Au$+$Au collisions at $\sqrt{s_{_{NN}}}=39$ and 62.4 GeV

Author: Abdulameer, N. J., Acharya, U., Adare, A., Aidala, C., Ajitanand, N. N., Akiba, Y., Akimoto, R., Al-Ta'ani, H., Alexander, J., Alfred, M., Angerami, A., Aoki, K., Apadula, N., Aramaki, Y., Asano, H., Aschenauer, E. C., Atomssa, E. T., Awes, T. C., Azmoun, B., Babintsev, V., Bai, M., Bannier, B., Barish, K. N., Bassalleck, B., Bathe, S., Baublis, V., Baumgart, S., Bazilevsky, A., Belmont, R., Berdnikov, A., Berdnikov, Y., Bichon, L., Blankenship, B., Blau, D. S., Bok, J. S., Borisov, V., Boyle, K., Brooks, M. L., Buesching, H., Bumazhnov, V., Butsyk, S., Campbell, S., Roman, V. Canoa, Castera, P., Chen, C. -H., Chiu, M., Chi, C. Y., Choi, I. J., Choi, J. B., Choi, S., Choudhury, R. K., Christiansen, P., Chujo, T., Chvala, O., Cianciolo, V., Citron, Z., Cole, B. A., Connors, M., Corliss, R., Morales, Y. Corrales, Csanád, M., Csörgő, T., D'Orazio, L., Dairaku, S., Datta, A., Daugherity, M. S., David, G., Dean, C. T., Denisov, A., Deshpande, A., Desmond, E. J., Dharmawardane, K. V., Dietzsch, O., Ding, L., Dion, A., Donadelli, M., Doomra, V., Drapier, O., Drees, A., Drees, K. A., Durham, J. M., Durum, A., Edwards, S., Efremenko, Y. V., Engelmore, T., Enokizono, A., Esha, R., Eyser, K. O., Fadem, B., Fan, W., Fields, D. E., Finger, Jr., M., Finger, M., Firak, D., Fitzgerald, D., Fleuret, F., Fokin, S. L., Frantz, J. E., Franz, A., Frawley, A. D., Fukao, Y., Fusayasu, T., Gainey, K., Gal, C., Garishvili, A., Garishvili, I., Giles, M., Glenn, A., Gong, X., Gonin, M., Goto, Y., de Cassagnac, R. Granier, Grau, N., Greene, S. V., Perdekamp, M. Grosse, Gunji, T., Guo, L., Gustafsson, H. -Å., Hachiya, T., Haggerty, J. S., Hahn, K. I., Hamagaki, H., Hanks, J., Harvey, M., Hasegawa, S., Hashimoto, K., Haslum, E., Hayano, R., Hemmick, T. K., Hester, T., He, X., Hill, J. C., Hodges, A., Hollis, R. S., Homma, K., Hong, B., Horaguchi, T., Hori, Y., Huang, J., Ichihara, T., Iinuma, H., Ikeda, Y., Imrek, J., Inaba, M., Iordanova, A., Isenhower, D., Issah, M., Ivanishchev, D., Jacak, B. V., Javani, M., Jiang, X., Ji, Z., Johnson, B. M., Joo, K. S., Jouan, D., Jumper, D. S., Kamin, J., Kaneti, S., Kang, B. H., Kang, J. H., Kang, J. S., Kapustinsky, J., Karatsu, K., Kasai, M., Kawall, D., Kazantsev, A. V., Kempel, T., Khachatryan, V., Khanzadeev, A., Khatiwada, A., Kijima, K. M., Kim, B. I., Kim, C., Kim, D. J., Kim, E. -J., Kim, H. J., Kim, K. -B., Kim, T., Kim, Y. -J., Kim, Y. K., Kincses, D., Kingan, A., Kinney, E., Kiss, Á., Kistenev, E., Klatsky, J., Kleinjan, D., Kline, P., Komatsu, Y., Komkov, B., Koster, J., Kotchetkov, D., Kotov, D., Kovacs, L., Krizek, F., Král, A., Kunde, G. J., Kurgyis, B., Kurita, K., Kurosawa, M., Kwon, Y., Kyle, G. S., Lai, Y. S., Lajoie, J. G., Larionova, D., Lebedev, A., Lee, B., Lee, D. M., Lee, J., Lee, K. B., Lee, K. S., Lee, S. H., Lee, S. R., Leitch, M. J., Leite, M. A. L., Leitgab, M., Lewis, B., Lewis, N. A., Lim, S. H., Levy, L. A. Linden, Liu, M. X., Li, X., Loomis, D. A., Love, B., Lökös, S., Maguire, C. F., Majoros, T., Makdisi, Y. I., Makek, M., Manion, A., Manko, V. I., Mannel, E., Masumoto, S., McCumber, M., McGaughey, P. L., McGlinchey, D., McKinney, C., Mendoza, M., Meredith, B., Miake, Y., Mibe, T., Mignerey, A. C., Milov, A., Mishra, D. K., Mitchell, J. T., Mitrankova, M., Mitrankov, Iu., Miyachi, Y., Miyasaka, S., Mohanty, A. K., Mohapatra, S., Mondal, M. M., Moon, H. J., Moon, T., Morrison, D. P., Motschwiller, S., Moukhanova, T. V., Muhammad, A., Mulilo, B., Murakami, T., Murata, J., Mwai, A., Nagae, T., Nagamiya, S., Nagle, J. L., Nagy, M. I., Nakagawa, I., Nakamiya, Y., Nakamura, K. R., Nakamura, T., Nakano, K., Nattrass, C., Nederlof, A., Nelson, S., Nihashi, M., Nouicer, R., Novák, T., Novitzky, N., Nukazuka, G., Nyanin, A. S., O'Brien, E., Ogilvie, C. A., Oh, J., Okada, K., Orosz, M., Osborn, J. D., Oskarsson, A., Ouchida, M., Ozawa, K., Pak, R., Pantuev, V., Papavassiliou, V., Park, B. H., Park, I. H., Park, J. S., Park, S., Park, S. K., Patel, L., Patel, M., Pate, S. F., Pei, H., Peng, J. -C., Peng, W., Pereira, H., Perepelitsa, D. V., Peressounko, D. Yu., PerezLara, C. E., Petti, R., Pinkenburg, C., Pisani, R. P., Potekhin, M., Proissl, M., Pun, A., Purschke, M. L., Qu, H., Radzevich, P. V., Rak, J., Ramasubramanian, N., Ravinovich, I., Read, K. F., Reynolds, D., Riabov, V., Riabov, Y., Richardson, E., Richford, D., Roach, D., Roche, G., Rolnick, S. D., Rosati, M., Runchey, J., Sahlmueller, B., Saito, N., Sakaguchi, T., Sako, H., Samsonov, V., Sano, M., Sarsour, M., Sato, S., Sawada, S., Sedgwick, K., Seidl, R., Sen, A., Seto, R., Sharma, D., Shein, I., Shi, Z., Shibata, M., Shibata, T. -A., Shigaki, K., Shimomura, M., Shoji, K., Shukla, P., Sickles, A., Silva, C. L., Silvermyr, D., Sim, K. S., Singh, B. K., Singh, C. P., Singh, V., Slunečka, M., Smith, K. L., Soltz, R. A., Sondheim, W. E., Sorensen, S. P., Sourikova, I. V., Stankus, P. W., Stenlund, E., Stepanov, M., Ster, A., Stoll, S. P., Sugitate, T., Sukhanov, A., Sun, J., Sun, Z., Sziklai, J., Takagui, E. M., Takahama, R., Takahara, A., Taketani, A., Tanaka, Y., Taneja, S., Tanida, K., Tannenbaum, M. J., Tarafdar, S., Taranenko, A., Tennant, E., Themann, H., Todoroki, T., Tomášek, L., Tomášek, M., Torii, H., Towell, R. S., Tserruya, I., Tsuchimoto, Y., Tsuji, T., Ueda, Y., Ujvari, B., Vale, C., van Hecke, H. W., Vargyas, M., Vazquez-Zambrano, E., Veicht, A., Vértesi, R., Velkovska, J., Virius, M., Vossen, A., Vrba, V., Vznuzdaev, E., Wang, X. R., Wang, Z., Watanabe, D., Watanabe, K., Watanabe, Y., Watanabe, Y. S., Wei, F., Wei, R., White, S. N., Winter, D., Wolin, S., Wong, C. P., Woody, C. L., Wysocki, M., Xia, B., Yamaguchi, Y. L., Yang, R., Yanovich, A., Ying, J., Yokkaichi, S., Younus, I., You, Z., Yushmanov, I. E., Zajc, W. A., Zelenski, A., and Zou, L.
Subjects: Nuclear Experiment
Abstract: The measurement of direct photons from Au$+$Au collisions at $\sqrt{s_{_{NN}}}=39$ and 62.4 GeV in the transverse-momentum range $0.4
Published: 2022
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19. Snowmass 2021 White Paper Instrumentation Frontier 05 -- White Paper 1: MPGDs: Recent advances and current R&D

Author: Dehmelt, K., Della Pietra, M., Muller, H., Tzamarias, S. E., White, A., White, S., Zhang, Z., Alviggi, M., Angelis, I., Aune, S., Bortfeldt, J., Bregant, M., Brunbauer, F., Camerlingo, M. T., Canale, V., D'Amico, V., Desforge, D., Di Donato, C., Di Nardo, R., Fanourakis, G., Floethner, K. J., Gallinaro, M., Garcia, F., Giomataris, I., Gnanvo, K., Gustavsson, T., Hall-Wilton, R., Iengo, P., Iguaz, F. J., Iodice, M., Janssens, D., Kallitsopoulou, A., Kebbiri, M., Kordas, K., Lampoudis, C., Legou, P., Lisowska, M., Liu, J., Lupberger, M., Malace, S., Maniatis, I., Manthos, I., Meng, Y., da Luz, H. Natal, Oliveri, E., Orlandini, G., Papaevangelou, T., Paraschou, K., Petrucci, F., Pfeiffer, D., Pomorski, M., Popescu, S., Resnati, F., Ropelewski, L., Rusu, A., Sampsonidis, D., Scharenberg, L., Schneider, T., Sekhniaidze, G., Sessa, M., Shao, M., Sohl, L., Toledo-Alarcon, J., Tsiamis, A., Tsipolitis, Y., Utrobicic, A., van Stenis, M., Veenhof, R., Wang, X., and Zhou, Y.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment, Nuclear Experiment
Abstract: This paper will review the origins, development, and examples of new versions of Micro-Pattern Gas Detectors. The goal for MPGD development was the creation of detectors that could cost-effectively cover large areas while offering excellent position and timing resolution, and the ability to operate at high incident particle rates. The early MPGD developments culminated in the formation of the RD51 collaboration which has become the critical organization for the promotion of MPGDs and all aspects of their production, characterization, simulation, and uses in an expanding array of experimental configurations. For the Snowmass 2021 study, a number of Letters of Interest were received that illustrate ongoing developments and expansion of the use of MPGDs. In this paper, we highlight high precision timing, high rate application, trigger capability expansion of the SRS readout system, and a structure designed for low ion backflow., Comment: Contribution to Snowmass 2021
Published: 2022

20. Heating of the solar chromosphere through current dissipation

Author: Santos, J. M. da Silva, Danilovic, S., Leenaarts, J., Rodríguez, J. de la Cruz, Zhu, X., White, S. M., Vissers, G. J. M., and Rempel, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: The solar chromosphere is heated to temperatures higher than predicted by radiative equilibrium. This excess heating is greater in active regions where the magnetic field is stronger. We aim to investigate the magnetic topology associated with an area of enhanced millimeter (mm) brightness temperatures in a solar active region mapped by the Atacama Large Millimeter/submillimeter Array (ALMA) using spectropolarimetric co-observations with the 1-m Swedish Solar Telescope (SST). We used Milne-Eddington inversions, nonlocal thermodynamic equilibrium (non-LTE) inversions, and a magnetohydrostatic extrapolation to obtain constraints on the three-dimensional stratification of temperature, magnetic field, and radiative energy losses. We compared the observations to a snapshot of a magnetohydrodynamics simulation and investigate the formation of the thermal continuum at 3 mm using contribution functions. We find enhanced heating rates in the upper chromosphere of up to $\sim 5\rm\,kW\,m^{-2}$, where small-scale emerging loops interact with the overlying magnetic canopy leading to current sheets as shown by the magnetic field extrapolation. Our estimates are about a factor of two higher than canonical values, but they are limited by the ALMA spatial resolution ($\sim 1.2^{\prime\prime}$). Band 3 brightness temperatures reach about $\sim10^{4}\,$K in the region, and the transverse magnetic field strength inferred from the non-LTE inversions is on the order of $\sim 500\,$G in the chromosphere. We are able to quantitatively reproduce many of the observed features, including the integrated radiative losses in our numerical simulation. We conclude that the heating is caused by dissipation in current sheets. However, the simulation shows a complex stratification in the flux emergence region where distinct layers may contribute significantly to the emission in the mm continuum., Comment: 18 pages, 13 figures. Accepted for publication in A&A. Typos and bibtex corrected
Published: 2022
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21. Pulsar Observations at Low Frequencies: Applications to Pulsar Timing and Solar Wind Models

Author: Kumar, P., White, S. M., Stovall, K., Dowell, J., and Taylor, G. B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: Efforts are underway to use high-precision timing of pulsars in order to detect low-frequency gravitational waves. A limit to this technique is the timing noise generated by dispersion in the plasma along the line of sight to the pulsar, including the solar wind. The effects due to the solar wind vary with time, influenced by the change in solar activity on different time scales, ranging up to $\sim 11$ years for a solar cycle. The solar wind contribution depends strongly on the angle between the pulsar line of sight and the solar disk, and is a dominant effect at small separations. Although solar wind models to mitigate these effects do exist, they do not account for all the effects of the solar wind and its temporal changes. Since low-frequency pulsar observations are most sensitive to these dispersive delays, they are most suited to test the efficacy of these models and identify alternative approaches. Here, we investigate the efficacy of some solar wind models commonly used in pulsar timing using long-term, high-cadence data on 6 pulsars taken with the Long Wavelength Array, and compare them with an operational solar wind model. Our results show that stationary models of the solar wind correction are insufficient to achieve the timing noise desired by pulsar timing experiments, and we need to use non-stationary models, which are informed by other solar wind observations, to obtain accurate timing residuals., Comment: Accepted for publication in MNRAS. 15 pages, 7 figures
Published: 2022
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22. Fractional cover mapping of wildland-urban interface fuels using Landsat, Sentinel 1 and PALSAR imagery

Author: Collins, L., Guindon, L., Lloyd, C., Taylor, S.W., and White, S.
Published: 2024
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23. Systematic study of nuclear effects in $p$$+$Al, $p$$+$Au, $d$$+$Au, and $^{3}$He$+$Au collisions at $\sqrt{s_{_{NN}}}=200$ GeV using $\pi^0$ production

Author: Acharya, U. A., Adare, A., Aidala, C., Ajitanand, N. N., Akiba, Y., Al-Bataineh, H., Alexander, J., Alfred, M., Andrieux, V., Angerami, A., Aoki, K., Apadula, N., Aramaki, Y., Asano, H., Atomssa, E. T., Averbeck, R., Awes, T. C., Azmoun, B., Babintsev, V., Bai, M., Baksay, G., Baksay, L., Bandara, N. S., Bannier, B., Barish, K. N., Bassalleck, B., Basye, A. T., Bathe, S., Baublis, V., Baumann, C., Bazilevsky, A., Beaumier, M., Beckman, S., Belikov, S., Belmont, R., Bennett, R., Berdnikov, A., Berdnikov, Y., Bhom, J. H., Bichon, L., Blankenship, B., Blau, D. S., Bok, J. S., Borisov, V., Boyle, K., Brooks, M. L., Bryslawskyj, J., Buesching, H., Bumazhnov, V., Bunce, G., Butsyk, S., Campbell, S., Roman, V. Canoa, Caringi, A., Cervantes, R., Chen, C. -H., Chiu, M., Chi, C. Y., Choi, I. J., Choi, J. B., Choudhury, R. K., Christiansen, P., Chujo, T., Chung, P., Chvala, O., Cianciolo, V., Citron, Z., Cole, B. A., del Valle, Z. Conesa, Connors, M., Corliss, R., Morales, Y. Corrales, Cronin, N., Csörgő, T., Csanád, M., D'Orazio, L., Dahms, T., Dairaku, S., Danchev, I., Danley, T. W., Das, K., Datta, A., Daugherity, M. S., David, G., Dayananda, M. K., DeBlasio, K., Dean, C. T., Dehmelt, K., Denisov, A., Deshpande, A., Desmond, E. J., Dharmawardane, K. V., Dietzsch, O., Dion, A., Diss, P. B., Dixit, D., Donadelli, M., Doomra, V., Do, J. H., Drapier, O., Drees, A., Drees, K. A., Durham, J. M., Durum, A., Dutta, D., Edwards, S., Efremenko, Y. V., Ellinghaus, F., En'yo, H., Engelmore, T., Enokizono, A., Esha, R., Esumi, S., Fadem, B., Fan, W., Feege, N., Fields, D. E., Finger, Jr., M., Finger, M., Fitzgerald, D., Fleuret, F., Fokin, S. L., Fraenkel, Z., Frantz, J. E., Franz, A., Frawley, A. D., Fujiwara, K., Fukao, Y., Fukuda, Y., Fusayasu, T., Gallus, P., Gal, C., Garg, P., Garishvili, I., Ge, H., Giles, M., Giordano, F., Glenn, A., Gong, H., Gonin, M., Goto, Y., de Cassagnac, R. Granier, Grau, N., Greene, S. V., Grim, G., Perdekamp, M. Grosse, Gunji, T., Guragain, H., Gustafsson, H. -Å., Hachiya, T., Haggerty, J. S., Hahn, K. I., Hamagaki, H., Hamblen, J., Hamilton, H. F., Hanks, J., Han, R., Han, S. Y., Harvey, M., Hasegawa, S., Haseler, T. O. S., Hashimoto, K., Haslum, E., Hayano, R., Heffner, M., Hemmick, T. K., Hester, T., He, X., Hill, J. C., Hill, K., Hodges, A., Hohlmann, M., Hollis, R. S., Holzmann, W., Homma, K., Hong, B., Horaguchi, T., Hornback, D., Hoshino, T., Hotvedt, N., Huang, J., Ichihara, T., Ichimiya, R., Ikeda, Y., Imai, K., Inaba, M., Iordanova, A., Isenhower, D., Ishihara, M., Issah, M., Ivanishchev, D., Iwanaga, Y., Jacak, B. V., Jezghani, M., Jiang, X., Jin, J., Ji, Z., Johnson, B. M., Jones, T., Joo, K. S., Jouan, D., Jumper, D. S., Kajihara, F., Kamin, J., Kanda, S., Kang, J. H., Kapukchyan, D., Kapustinsky, J., Karatsu, K., Karthas, S., Kasai, M., Kawall, D., Kawashima, M., Kazantsev, A. V., Kempel, T., Key, J. A., Khachatryan, V., Khanzadeev, A., Khatiwada, A., Kijima, K. M., Kikuchi, J., Kimelman, B., Kim, A., Kim, B. I., Kim, C., Kim, D. J., Kim, E. -J., Kim, G. W., Kim, M., Kim, T., Kim, Y. -J., Kincses, D., Kingan, A., Kinney, E., Kiss, Á., Kistenev, E., Kitamura, R., Klatsky, J., Kleinjan, D., Kline, P., Koblesky, T., Kochenda, L., Komkov, B., Konno, M., Koster, J., Kotov, D., Král, A., Kravitz, A., Kudo, S., Kunde, G. J., Kurita, K., Kurosawa, M., Kwon, Y., Kyle, G. S., Lai, Y. S., Lajoie, J. G., Larionova, D., Lebedev, A., Lee, D. M., Lee, J., Lee, K. B., Lee, K. S., Lee, S., Lee, S. H., Leitch, M. J., Leite, M. A. L., Leung, Y. H., Lewis, N. A., Liška, T., Lichtenwalner, P., Liebing, P., Lim, S. H., Levy, L. A. Linden, Liu, H., Liu, M. X., Li, X., Loggins, V. -R., Loomis, D. A., Lovasz, K., Love, B., Lynch, D., Lökös, S., Maguire, C. F., Majoros, T., Makdisi, Y. I., Makek, M., Malik, M. D., Manion, A., Manko, V. I., Mannel, E., Mao, Y., Masui, H., Matathias, F., McCumber, M., McGaughey, P. L., McGlinchey, D., McKinney, C., Means, N., Meles, A., Mendoza, M., Meredith, B., Miake, Y., Mibe, T., Mignerey, A. C., Miki, K., Milov, A., Mishra, D. K., Mitchell, J. T., Mitrankova, M., Mitrankov, Iu., Mitsuka, G., Miyasaka, S., Mizuno, S., Mohanty, A. K., Mondal, M. M., Montuenga, P., Moon, H. J., Moon, T., Morino, Y., Morreale, A., Morrison, D. P., Moukhanova, T. V., Mulilo, B., Murakami, T., Murata, J., Mwai, A., Nagai, K., Nagamiya, S., Nagashima, K., Nagashima, T., Nagle, J. L., Naglis, M., Nagy, M. I., Nakagawa, I., Nakagomi, H., Nakamiya, Y., Nakamura, K. R., Nakamura, T., Nakano, K., Nam, S., Nattrass, C., Nelson, S., Netrakanti, P. K., Newby, J., Nguyen, M., Nihashi, M., Niida, T., Nishimura, S., Nouicer, R., Novák, T., Novitzky, N., Nukazuka, G., Nyanin, A. S., O'Brien, E., Oakley, C., Oda, S. X., Ogilvie, C. A., Okada, K., Oka, M., Onuki, Y., Koop, J. D. Orjuela, Osborn, J. D., Oskarsson, A., Ottino, G. J., Ouchida, M., Ozawa, K., Pak, R., Pantuev, V., Papavassiliou, V., Park, I. H., Park, J. S., Park, S., Park, S. K., Park, W. J., Patel, M., Pate, S. F., Pei, H., Peng, J. -C., Peng, W., Pereira, H., Perepelitsa, D. V., Perera, G. D. N., Peressounko, D. Yu., PerezLara, C. E., Perry, J., Petti, R., Phipps, M., Pinkenburg, C., Pinson, R., Pisani, R. P., Potekhin, M., Proissl, M., Pun, A., Purschke, M. L., Qu, H., Radzevich, P. V., Rak, J., Ramasubramanian, N., Ramson, B. J., Ravinovich, I., Read, K. F., Rembeczki, S., Reygers, K., Reynolds, D., Riabov, V., Riabov, Y., Richardson, E., Richford, D., Rinn, T., Roach, D., Roche, G., Rolnick, S. D., Rosati, M., Rosendahl, S. S. E., Rosen, C. A., Rowan, Z., Ružička, P., Rubin, J. G., Runchey, J., Safonov, A. S., Sahlmueller, B., Saito, N., Sakaguchi, T., Sakashita, K., Sako, H., Samsonov, V., Sano, S., Sarsour, M., Sato, S., Sato, T., Sawada, S., Schaefer, B., Schmoll, B. K., Sedgwick, K., Seele, J., Seidl, R., Sen, A., Seto, R., Sett, P., Sexton, A., Sharma, D, Sharma, D., Shein, I., Shibata, M., Shibata, T. -A., Shigaki, K., Shimomura, M., Shioya, T., Shoji, K., Shukla, P., Sickles, A., Silva, C. L., Silvermyr, D., Silvestre, C., Sim, K. S., Singh, B. K., Singh, C. P., Singh, V., Slunečka, M., Smith, K. L., Snowball, M., Soltz, R. A., Sondheim, W. E., Sorensen, S. P., Sourikova, I. V., Stankus, P. W., Stenlund, E., Stepanov, M., Stoll, S. P., Sugitate, T., Sukhanov, A., Sumita, T., Sun, J., Sun, Z., Sziklai, J., Takagui, E. M., Takahama, R., Taketani, A., Tanabe, R., Tanaka, Y., Taneja, S., Tanida, K., Tannenbaum, M. J., Tarafdar, S., Taranenko, A., Tarnai, G., Themann, H., Thomas, D., Thomas, T. L., Tieulent, R., Timilsina, A., Todoroki, T., Togawa, M., Toia, A., Tomášek, L., Tomášek, M., Torii, H., Towell, C. L., Towell, R., Towell, R. S., Tserruya, I., Tsuchimoto, Y., Ueda, Y., Ujvari, B., Vértesi, R., Vale, C., Valle, H., van Hecke, H. W., Vazquez-Zambrano, E., Veicht, A., Velkovska, J., Virius, M., Vrba, V., Vukman, N., Vznuzdaev, E., Wang, X. R., Watanabe, D., Watanabe, K., Watanabe, Y., Watanabe, Y. S., Wei, F., Wei, R., Wessels, J., White, A. S., White, S. N., Winter, D., Wong, C. P., Woody, C. L., Wright, R. M., Wysocki, M., Xia, B., Xue, L., Xu, C., Xu, Q., Yalcin, S., Yamaguchi, Y. L., Yamamoto, H., Yamaura, K., Yang, R., Yanovich, A., Ying, J., Yokkaichi, S., Yoon, I., Yoo, J. H., Young, G. R., Younus, I., You, Z., Yushmanov, I. E., Yu, H., Zajc, W. A., Zelenski, A., Zhou, S., and Zou, L.
Subjects: Nuclear Experiment, High Energy Physics - Experiment
Abstract: The PHENIX collaboration presents a systematic study of $\pi^0$ production from $p$$+$$p$, $p$$+$Al, $p$$+$Au, $d$$+$Au, and $^{3}$He$+$Au collisions at $\sqrt{s_{_{NN}}}=200$ GeV. Measurements were performed with different centrality selections as well as the total inelastic, 0%--100%, selection for all collision systems. For 0%--100% collisions, the nuclear modification factors, $R_{xA}$, are consistent with unity for $p_T$ above 8 GeV/$c$, but exhibit an enhancement in peripheral collisions and a suppression in central collisions. The enhancement and suppression characteristics are similar for all systems for the same centrality class. It is shown that for high-$p_T$-$\pi^0$ production, the nucleons in the $d$ and $^3$He interact mostly independently with the Au nucleus and that the counter intuitive centrality dependence is likely due to a physical correlation between multiplicity and the presence of a hard scattering process. These observations disfavor models where parton energy loss has a significant contribution to nuclear modifications in small systems. Nuclear modifications at lower $p_T$ resemble the Cronin effect -- an increase followed by a peak in central or inelastic collisions and a plateau in peripheral collisions. The peak height has a characteristic ordering by system size as $p$$+$Au $>$ $d$$+$Au $>$ $^{3}$He$+$Au $>$ $p$$+$Al. For collisions with Au ions, current calculations based on initial state cold nuclear matter effects result in the opposite order, suggesting the presence of other contributions to nuclear modifications, in particular at lower $p_T$., Comment: 554 authors from 81 institutions, 21 pages, 13 figures, and 3 tables. Data from 2008, 2014, and 2015. v2 is version accepted for publication in Physical Review C. Plain text data tables for the points plotted in figures for this and previous PHENIX publications are (or will be) publicly available at http://www.phenix.bnl.gov/papers.html
Published: 2021
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24. Hygiene behaviour and hygiene behaviour change during humanitarian crises

Author: White, S., Dreibelbis, R., Curtis, V., Palmer, J., and Blanchet, K.
Abstract: More than any other public health intervention, handwashing with soap can reduce the burden of faecal-oral diseases. Over the last decade substantial research and programmatic investment have gone into better understanding the determinants of people's handwashing behaviour. However, this research base is derived almost entirely from work conducted in stable settings. When a humanitarian crisis occurs, whether it be a disease outbreak, a disaster or a conflict, the social and physical environments of the affected population are disrupted. At the same time, disease risk related to faecal-oral pathogens substantially increases. Given that we currently lack an in-depth understanding of the factors that drive behaviour in crises, hygiene programmes in these settings typically rely on a narrow set of 'traditional' interventions such as health education and the distribution of hygiene kits. Although knowledge about handwashing and enabling products are likely to be important, these interventions alone have been shown to be insufficient to lead to meaningful and sustained changes in behaviour. Recent systematic reviews and research agenda setting activities within the humanitarian sector have suggested that research on hand hygiene behaviour and improved hygiene programme design in emergencies should prioritised. This thesis is grounded in a pragmatic epistemology and uses a mix of methods drawn from the disciples of cultural anthropology and behavioural science. It aims to better understand what influences hygiene behaviour during crises and outbreaks and identify opportunities for effective hygiene behaviour change in these settings. The thesis includes five manuscripts. The first is a literature review which aims to identify and categorise the determinants of handwashing behaviour in stable settings, crises and outbreaks and to appraise the quality of this evidence. The second assesses the strengths and limitations of a survey-based tool which is commonly used in humanitarian crises to understand behavioural determinants. The third and fourth paper are qualitative case studies set in Iraq and the Democratic Republic of the Congo. Both explore how the determinants of handwashing behaviour are shaped by different types of crises. The thesis concludes with a paper about experiences and challenges faced by humanitarians when designing hygiene programmes in emergencies. Prior research on behavioural determinants was found to be poor quality and limited by methodological challenges and inconsistent definitions of determinants. The literature review was unable to draw conclusions about the determinants of hygiene behaviour in crises or outbreaks due to a lack of evidence. Current approaches to assessing determinants in crises were feasible to conduct but were methodologically limited and unable to fully account for contextual factors and the impact of the crisis on behaviour. The qualitative case studies indicated that the relative importance of certain determinants is likely to vary during crises and outbreaks. The characteristics that appear to affect the variation of behavioural determinants include the type of crisis; the phase of the crisis or outbreak; the physical and social context; and the broader consequences of the crisis or outbreak on the lives of the affected population. The determinants that seem to be most influential in driving hygiene behaviour during crises and outbreaks included risk perceptions; the prioritisation of time and resources, daily routines; and factors within the behavioural settings where handwashing takes place (such as access to handwashing facilities, water and soap). Interviews with humanitarians indicated that the constraints humanitarians faced when designing hygiene programmes, and the way they made decisions, were remarkably similar across contexts, leading to programming that was also relatively de-contextualised. Hygiene programme design processes were considered sub-optimal, but humanitarians struggled to implement the more ideal principles and processes that they aspired to due to time pressures; financial constraints; limited capacities; the infeasibility of assessment tools; unequal partnerships organisations; and poor sector learning processes. Given these constraints, most programmatic decisions were based on the intuitions and past experiences of managerial staff. The findings presented in this thesis offer opportunities for strengthening the assessment of behavioural determinants and improving hygiene programme design so that it can be done rapidly, while still being contextualised and evidence-based.
Published: 2022
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25. AGN feeding and feedback in Fornax A: kinematical analysis of the multi-phase ISM

Author: Maccagni, F. M., Serra, P., Gaspari, M., Kleiner, D., Morokuma-Matsui, K., Oosterloo, T. A., Onodera, M., Kamphuis, P., Loi, F., Thorat, K., Ramatsoku, M., Smirnov, O., and White, S. V.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a multi-wavelength study of the gaseous medium surrounding the nearby active galactic nucleus (AGN) Fornax A. Using MeerKAT, ALMA and MUSE observations we reveal a complex distribution of the atomic (HI), molecular (CO), and ionised gas in its centre and along the radio jets. By studying the multi-scale kinematics of the multi-phase gas, we reveal the presence of concurrent AGN feeding and feedback phenomena. Several clouds and an extended 3 kpc filament -- perpendicular to the radio jets and the inner disk ($r\lesssim 4.5$ kpc) -- show highly-turbulent kinematics, which likely induces nonlinear condensation and subsequent Chaotic Cold Accretion (CCA) onto the AGN. In the wake of the radio jets and in an external ($r\gtrsim 4.5$ kpc) ring, we identify an entrained massive ($\sim$ $10^7$ M$_\odot$) multi-phase outflow ($v_{\rm OUT}\sim 2000$ km s$^{-1}$). The rapid flickering of the nuclear activity of Fornax A ($\sim$ 3 Myr) and the gas experiencing turbulent condensation raining onto the AGN provide quantitative evidence that a recurrent, tight feeding and feedback cycle may be self-regulating the activity of Fornax A, in agreement with CCA simulations. To date, this is one of the most in-depth probes of such a mechanism, paving the way to apply these precise diagnostics to a larger sample of nearby AGN hosts and their multi-phase ISM., Comment: 22 pages, 20 figures, accepted for publication on Astronomy & Astrophysics
Published: 2021
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26. CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope

Author: collaboration, CCAT-Prime, Aravena, M., Austermann, J. E., Basu, K., Battaglia, N., Beringue, B., Bertoldi, F., Bigiel, F., Bond, J. R., Breysse, P. C., Broughton, C., Bustos, R., Chapman, S. C., Charmetant, M., Choi, S. K., Chung, D. T., Clark, S. E., Cothard, N. F., Crites, A. T., Dev, A., Douglas, K., Duell, C. J., Dunner, R., Ebina, H., Erler, J., Fich, M., Fissel, L. M., Foreman, S., Gallardo, P. A., Gao, J., García, Pablo, Giovanelli, R., Golec, J. E., Groppi, C. E., Haynes, M. P., Henke, D., Hensley, B., Herter, T., Higgins, R., Hlozek, R., Huber, A., Huber, Z., Hubmayr, J., Jackson, R., Johnstone, D., Karoumpis, C., Keating, L. C., Komatsu, E., Li, Y., Magnelli, B., Matthews, B. C., Mauskopf, P., McMahon, J. J., Meerburg, P. D., Meyers, J., Muralidhara, V., Murray, N. W., Niemack, M. D., Nikola, T., Okada, Y., Puddu, R., Riechers, D. A., Rosolowsky, E., Rossi, K., Rotermund, K., Roy, A., Sadavoy, S. I., Schaaf, R., Schilke, P., Scott, D., Simon, R., Sinclair, Adrian K., Sivakoff, G. R., Stacey, G. J., Stutz, Amelia M., Stutzki, J., Tahani, M., Thanjavur, K., Timmermann, R. A., Ullom, J. N., van Engelen, A., Vavagiakis, E. M., Vissers, M. R., Wheeler, J. D., White, S. D. M., Zhu, Y., and Zou, B.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present a detailed overview of the science goals and predictions for the Prime-Cam direct detection camera/spectrometer being constructed by the CCAT-prime collaboration for dedicated use on the Fred Young Submillimeter Telescope (FYST). The FYST is a wide-field, 6-m aperture submillimeter telescope being built (first light in mid-2024) by an international consortium of institutions led by Cornell University and sited at more than 5600 meters on Cerro Chajnantor in northern Chile. Prime-Cam is one of two instruments planned for FYST and will provide unprecedented spectroscopic and broadband measurement capabilities to address important astrophysical questions ranging from Big Bang cosmology through reionization and the formation of the first galaxies to star formation within our own Milky Way galaxy. Prime-Cam on the FYST will have a mapping speed that is over ten times greater than existing and near-term facilities for high-redshift science and broadband polarimetric imaging at frequencies above 300 GHz. We describe details of the science program enabled by this system and our preliminary survey strategies., Comment: 61 pages, 16 figures. Resubmitted to ApJSS July 11, 2022
Published: 2021
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27. The GLEAM 200 MHz Local Radio Luminosity Function for AGN and Star-forming Galaxies

Author: Franzen, T. M. O., Seymour, N., Sadler, E. M., Mauch, T., White, S. V., Jackson, C. A., Chhetri, R., Quici, B., Bell, M. E., Callingham, J. R., Dwarakanath, K. S., For, B., Gaensler, B. M., Hancock, P. J., Hindson, L., Hurley-Walker, N., Johnston-Hollitt, M., Kapinska, A. D., Lenc, E., McKinley, B., Morgan, J., Offringa, A. R., Procopio, P., Staveley-Smith, L., Wayth, R. B., Wu, C., and Zheng, Q.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) is a radio continuum survey at 76-227 MHz of the entire southern sky (Declination $<+30\deg$) with an angular resolution of $\approx 2$ arcmin. In this paper, we combine GLEAM data with optical spectroscopy from the 6dF Galaxy Survey to construct a sample of 1,590 local (median $z \approx 0.064$) radio sources with $S_{200\,\mathrm{MHz}} > 55$ mJy across an area of $\approx 16,700~\mathrm{deg}^{2}$. From the optical spectra, we identify the dominant physical process responsible for the radio emission from each galaxy: 73 per cent are fuelled by an active galactic nucleus (AGN) and 27 per cent by star formation. We present the local radio luminosity function for AGN and star-forming galaxies at 200 MHz and characterise the typical radio spectra of these two populations between 76 MHz and $\sim 1$ GHz. For the AGN, the median spectral index between 200 MHz and $\sim 1$ GHz, $\alpha_{\mathrm{high}}$, is $-0.600 \pm 0.010$ (where $S \propto \nu^{\alpha}$) and the median spectral index within the GLEAM band, $\alpha_{\mathrm{low}}$, is $-0.704 \pm 0.011$. For the star-forming galaxies, the median value of $\alpha_{\mathrm{high}}$ is $-0.650 \pm 0.010$ and the median value of $\alpha_{\mathrm{low}}$ is $-0.596 \pm 0.015$. Among the AGN population, flat-spectrum sources are more common at lower radio luminosity, suggesting the existence of a significant population of weak radio AGN that remain core-dominated even at low frequencies. However, around 4 per cent of local radio AGN have ultra-steep radio spectra at low frequencies ($\alpha_{\mathrm{low}} < -1.2$). These ultra-steep-spectrum sources span a wide range in radio luminosity, and further work is needed to clarify their nature., Comment: 28 pages, 18 figures, accepted for publication in PASA
Published: 2021
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28. Real-time Electron Solvation Induced by Bursts of Laser-accelerated Protons in Liquid Water

Author: Prasselsperger, A., Coughlan, M., Breslin, N., Yeung, M., Arthur, C., Donnelly, H., White, S., Afshari, M., Speicher, M., Yang, R., Villagomez-Bernabe, B., Currell, F. J., Schreiber, J., and Dromey, B.
Subjects: Physics - Plasma Physics
Abstract: Understanding the mechanisms of proton energy deposition in matter and subsequent damage formation is fundamental to radiation science. Here we exploit the picosecond (10^-12 s) resolution of laser-driven accelerators to track ultra-fast solvation dynamics for electrons due to proton radiolysis in liquid water (H2O). Comparing these results with modelling that assumes initial conditions similar to those found in photolysis reveals that solvation time due to protons is extended by > 20 ps. Supported by magneto-hydrodynamic theory this indicates a highly dynamic phase in the immediate aftermath of the proton interaction that is not accounted for in current models., Comment: 6 pages, 3 figures
Published: 2021
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29. Generation of photoionized plasmas in the laboratory of relevance to accretion-powered x-ray sources using keV line radiation

Author: Riley, D., Singh, R.L., White, S., Charlwood, M., Bailie, D., Hyland, C., Audet, T., Sarri, G., Kettle, B., Gribakin, G., Rose, S.J., Hill, E.G., Ferland, G.J., Williams, R.J.R., and Keenan, F.P.
Published: 2024
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30. Principles of environmentally‐sustainable anaesthesia: a global consensus statement from the World Federation of Societies of Anaesthesiologists

Author: White, SM, Shelton, CL, Gelb, AW, Lawson, C, McGain, F, Muret, J, Sherman, JD, Shelton, C, White, S, Gelb, A, Sherman, J, Mejeni, N, Gathuya, Z, Ngumi, Z, Onajin‐Obembe, B, Farina, Z, Jendoubi, M, Tumukunde, J, Mansor, M, Peng, Z, Yang, L, Irwin, M, Kumar, N, Malhotra, N, Yamaura, K, Neupane, S, Kim, JH, Kayak, E, Story, D, Biribo, K, Karu, A, Burrell, R, Pecher, S, Malisiova, A, Drenger, B, Brazzi, L, Fernandes, T, Jovanovic, G, Bentzer, P, Allen, C, Montgomery, H, Pierce, T, Shinde, S, Ozelsel, T, Chesebro, B, McClain, C, Sondekoppam, R, Simoes, C, and Schultz, C Nilo
Subjects: Biomedical and Clinical Sciences, Clinical Sciences, Dentistry, Generic health relevance, Climate Action, Responsible Consumption and Production, Anesthesia, Anesthesiologists, Consensus Development Conferences as Topic, Delphi Technique, Environmental Exposure, Global Health, Global Warming, Humans, Scotland, Societies, Medical, anaesthesia, carbon, climate change, consensus, environment, sustainability, representing the World Federation of Societies of Anaesthesiologists Global Working Group on Environmental Sustainability in Anaesthesia, Neurosciences, Anesthesiology, Clinical sciences
Abstract: The Earth's mean surface temperature is already approximately 1.1°C higher than pre-industrial levels. Exceeding a mean 1.5°C rise by 2050 will make global adaptation to the consequences of climate change less possible. To protect public health, anaesthesia providers need to reduce the contribution their practice makes to global warming. We convened a Working Group of 45 anaesthesia providers with a recognised interest in sustainability, and used a three-stage modified Delphi consensus process to agree on principles of environmentally sustainable anaesthesia that are achievable worldwide. The Working Group agreed on the following three important underlying statements: patient safety should not be compromised by sustainable anaesthetic practices; high-, middle- and low-income countries should support each other appropriately in delivering sustainable healthcare (including anaesthesia); and healthcare systems should be mandated to reduce their contribution to global warming. We set out seven fundamental principles to guide anaesthesia providers in the move to environmentally sustainable practice, including: choice of medications and equipment; minimising waste and overuse of resources; and addressing environmental sustainability in anaesthetists' education, research, quality improvement and local healthcare leadership activities. These changes are achievable with minimal material resource and financial investment, and should undergo re-evaluation and updates as better evidence is published. This paper discusses each principle individually, and directs readers towards further important references.
Published: 2022

31. Threads, Ribbons, and Rings in the Radio Galaxy IC 4296

Author: Condon, J. J., Cotton, W. D., White, S. V., Legodi, S., Goedhart, S., McAlpine, K., Ratcliffe, S. M., and Camilo, F.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The nearby elliptical galaxy IC4296 has produced a large (510 kpc) low-luminosity radio source with typical FR I core/jet/lobe morphology. The unprecedented combination of brightness sensitivity, dynamic range, and angular resolution of a new 1.28 GHz MeerKAT continuum image reveals striking new morphological features which we call threads, ribbons, and rings. The threads are faint narrow emission features originating where helical Kelvin-Helmholtz instabilities disrupt the main radio jets. The ribbons are smooth regions between the jets and the lobes, and they appear to be relics of jets powered by earlier activity that have since come into pressure equilibrium. Vortex rings in the outer portions of the lobes and their backflows indicate that the straight outer jets and ribbons are inclined by $i = 60 \pm 5^\circ$ from the line-of-sight, in agreement with photometric, geometric, and gas-dynamical estimates of inclination angles near the nucleus., Comment: 14 pages, 12 figures ApJ accepted
Published: 2021
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32. A new look at old friends. I. Imaging classical radio galaxies with uGMRT and MeerKAT

Author: Fanaroff, B., Lal, D. V., Venturi, T., Smirnov, O., Bondi, M., Thorat, K., Bester, L., Jozsa, G., Kleiner, D., Loi, F., Makhathini, S., and White, S. V.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We have undertaken a systematic study of FRI and FRII radio galaxies with the upgraded Giant Metrewave Radio Telescope (uGMRT) and MeerKAT. The main goal is to explore whether the unprecedented few $\mu$Jy sensitivity reached in the range 550-1712 MHz at the resolution of $\sim4^{\prime\prime}-7^{\prime\prime}$ reveals new features in the radio emission which might need us to revise our current classification scheme for classical radio galaxies. In this paper we present the results for the first set of four radio galaxies, i.e. 4C 12.02, 4C 12.03, CGCG 044-046 and CGCG 021-063. The sources have been selected from the 4C sample with well-defined criteria, and have been imaged with the uGMRT in the range 550-850 MHz (band 4) and with the MeerKAT in the range 856-1712 MHz (L-band). Full resolution images are presented for all sources in the sample, together with MeerKAT in-band spectral images. Additionally, the uGMRT-MeerKAT spectral image and MeerKAT L-band polarisation structure are provided for CGCG 044-046. Our images contain a wealth of morphological details, such as filamentary structure in the emission from the lobes, radio emission beyond the hot-spots in three sources, and misalignments. We briefly discuss the overall properties of CGCG 044-046 in the light of the local environment as well, and show possible restarted activity in 4C 12.03 which needs to be confirmed. We conclude that at least for the sources presented here, the classical FRI/FRII morphological classification still holds with the current improved imaging capabilities, but the richness in details also suggests caution in the systematic morphological classification carried out with automatic procedures in surveys with poorer sensitivity and angular resolution., Comment: 16 pages, 8 figures, and 3 tables; accepted for publication in MNRAS
Published: 2021
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33. Test beam characterization of sensor prototypes for the CMS Barrel MIP Timing Detector

Author: Abbott, R., Abreu, A., Addesa, F., Alhusseini, M., Anderson, T., Andreev, Y., Apresyan, A., Arcidiacono, R., Arenton, M., Auffray, E., Bastos, D., Bauerdick, L. A. T., Bellan, R., Bellato, M., Benaglia, A., Benettoni, M., Bertoni, R., Besancon, M., Bharthuar, S., Bornheim, A., Brücken, E., Butler, J. N., Campagnari, C., Campana, M., Carlin, R., Carniti, P., Cartiglia, N., Casarsa, M., Cerri, O., Checchia, P., Chen, H., Chidzik, S., Chlebana, F., Cossutti, F., Costa, M., Cox, B., Dafinei, I., De Guio, F., Debbins, P., del Re, D., Dermenev, A., Di Marco, E., Dilsiz, K., Di Petrillo, K. F., Dissertori, G., Dogra, S., Dosselli, U., Dutta, I., Caleb, F., Madrazo, C. Fernandez, Fernandez, M., Ferrero, M., Flowers, Z., Funk, W., Gallinaro, M., Ganjour, S., Gardner, M., Geurts, F., Ghezzi, A., Gninenko, S., Golf, F., Gonzalez, J., Gotti, C., Gray, L., Guilloux, F., Gundacker, S., Hazen, E., Hedia, S., Heering, A., Heller, R., Isidori, T., Isocrate, R., Jaramillo, R., Joyce, M., Kaadze, K., Karneyeu, A., Kim, H., King, J., Kopp, G., Korjik, M., Koseyan, O. K., Kozyrev, A., Kratochwil, N., Lazarovits, M., Ledovskoy, A., Lee, H., Lee, J., Li, A., Li, S., Li, W., Liu, T., Lu, N., Lucchini, M., Lustermann, W., Madrid, C., Malberti, M., Mandjavize, I., Mao, J., Maravin, Y., Marlow, D., Marsh, B., del Arbol, P. Martinez, Marzocchi, B., Mazza, R., McMahon, C., Mechinsky, V., Meridiani, P., Mestvirishvili, A., Minafra, N., Mohammadi, A., Monti, F., Moon, C. S., Mulargia, R., Murray, M., Musienko, Y., Nachtman, J., Nargelas, S., Narvaez, L., Neogi, O., Neu, C., Niknejad, T., Obertino, M., Ogul, H., Oh, G., Ojalvo, I., Onel, Y., Organtini, G., Orimoto, T., Ott, J., Ovtin, I., Paganoni, M., Pandolfi, F., Paramatti, R., Peck, A., Perez, C., Pessina, G., Pena, C., Pigazzini, S., Radchenko, O., Redaelli, N., Rigoni, D., Robutti, E., Rogan, C., Rossin, R., Rovelli, C., Royon, C., Sahin, M. Ö., Sands, W., Santanastasio, F., Sarica, U., Schmidt, I., Schmitz, R., Sheplock, J., Silva, J. C., Siviero, F., Soffi, L., Sola, V., Sorrentino, G., Spiropulu, M., Spitzbart, D., Leiton, A. G. Stahl, Staiano, A., Stuart, D., Suarez, I., de Fatis, T. Tabarelli, Tamulaitis, G., Tang, Y., Tannenwald, B., Taylor, R., Tiras, E., Titov, M., Tkaczyk, S., Tlisov, D., Tlisova, I., Tornago, M., Tosi, M., Tramontano, R., Trevor, J., Tully, C. G., Ujvari, B., Varela, J., Ventura, S., Vila, I., Wamorkar, T., Wang, C., Wang, X., Wayne, M., Wetzel, J., White, S., Winn, D., Wu, S., Xie, S., Ye, Z., Yu, G. B., Zhang, G., Zhang, L., Zhang, Y., Zhang, Z., and Zhu, R.
Subjects: Physics - Instrumentation and Detectors
Abstract: The MIP Timing Detector will provide additional timing capabilities for detection of minimum ionizing particles (MIPs) at CMS during the High Luminosity LHC era, improving event reconstruction and pileup rejection. The central portion of the detector, the Barrel Timing Layer (BTL), will be instrumented with LYSO:Ce crystals and Silicon Photomultipliers (SiPMs) providing a time resolution of about 30 ps at the beginning of operation, and degrading to 50-60 ps at the end of the detector lifetime as a result of radiation damage. In this work, we present the results obtained using a 120 GeV proton beam at the Fermilab Test Beam Facility to measure the time resolution of unirradiated sensors. A proof-of-concept of the sensor layout proposed for the barrel region of the MTD, consisting of elongated crystal bars with dimensions of about 3 x 3 x 57 mm$^3$ and with double-ended SiPM readout, is demonstrated. This design provides a robust time measurement independent of the impact point of the MIP along the crystal bar. We tested LYSO:Ce bars of different thickness (2, 3, 4 mm) with a geometry close to the reference design and coupled to SiPMs manufactured by Hamamatsu and Fondazione Bruno Kessler. The various aspects influencing the timing performance such as the crystal thickness, properties of the SiPMs (e.g. photon detection efficiency), and impact angle of the MIP are studied. A time resolution of about 28 ps is measured for MIPs crossing a 3 mm thick crystal bar, corresponding to an MPV energy deposition of 2.6 MeV, and of 22 ps for the 4.2 MeV MPV energy deposition expected in the BTL, matching the detector performance target for unirradiated devices.
Published: 2021
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34. Immunomodulatory therapy in children with paediatric inflammatory multisystem syndrome temporally associated with SARS-CoV-2 (PIMS-TS, MIS-C; RECOVERY): a randomised, controlled, open-label, platform trial

Author: Faust, Saul N, Haynes, Richard, Jones, Christine E, Staplin, Natalie, Whittaker, Elizabeth, Jaki, Thomas, Juszczak, Ed, Spata, Enti, Wan, Mandy, Bamford, Alasdair, Dimitri, Paul, Finn, Adam, Furness, John, Ramanan, Athimalaipet V, Gale, Christopher, Cathie, Katrina, Drysdale, Simon, Bernatoniene, Jolanta, Murray, Clare, Roehr, Charles C, Fleming, Paul, Riordan, Andrew, Bandi, Srini, Jyothish, Deepthi, Evans, Jennifer, Emonts, Marieke, Kelly, Dominic, Pathan, Nazima, Davies, Patrick, Hague, Rosie, Pollock, Louisa, Semple, Malcolm G, Peto, Leon, Baillie, J Kenneth, Buch, Maya, Jeffery, Katie, Knight, Marian, Lim, Wei Shen, Montgomery, Alan, Mukherjee, Aparna, Mumford, Andrew, Rowan, Kathryn, Thwaites, Guy, Mafham, Marion, Emberson, Jonathan, Landray, Martin J, Horby, Peter W, Chappell, Lucy, Day, Jeremy, Dung, DV, Quang, NN, Binh, Prof, Burhan, E, Alisjahbana, B, Koirala, J, Basnet, S, Kestelyn, E, Basnyat, B, Gyanwali, P, Hamers, RL, Sandercock, P, Darbyshire, J, DeMets, D, Fowler, R, Lalloo, D, Munavvar, M, Roberts, I, Warris, A, Wittes, J, Craddock-Bamford, A, Barton, J, Basoglu, A, Brown, R, Brudlo, W, Denis, E, Fletcher, L, Howard, S, Musini, S, Taylor, K, Cui, G, Goodenough, B, King, A, Lay, M, Murray, D, Stevens, W, Wallendszus, K, Welsh, R, Crichton, C, Davies, J, Goldacre, R, Harper, C, Knight, F, Nunn, M, Salih, H, Welch, J, Campbell, M, Pessoa-Amorim, G, Zayed, M, Wiles, J, Bagley, G, Cameron, S, Chamberlain, S, Farrell, B, Freeman, H, Kennedy, A, Whitehouse, A, Wilkinson, S, Wood, C, Reith, C, Davies, K, Halls, H, Holland, L, Truell, R, Wilson, K, Lingwood, Emma, Howie, L, Lunn, M, Rodgers, Penelope, Amuasi, J, Baird, K, Bao, T, Bittaye, M, Bonney, J, D'Alessandro, U, Dhimal, M, Huyen, T, Jagne, A, Karkey, A, Maiga, O, Matey, E, Nadjm, B, Nel, J, Pant, S, Puspatriani, K, Rahardjani, M, Raijal, S, Rees, H, Rimainar, A, Roberts, C, Rocca, A, Shrestha, S, Usuf, E, Vidaillic, C, Wulandari, F, Alexander, A, Amezaga, M, Armah, C, Asghar, A, Aubrey, P, Barker-Williams, K, Barnard, A, Bartholomew, J, Beaumont-Jewell, D, Beddows, S, Beety, J, Birch, C, Boyle, P, Brend, M, Brookes, M, Callens, C, Campbell, D, Campbell, H, Cate, H, Chambers, E, Chapman, K, Coe, A, Collins, J, Crawshaw, S, Das, S, De Soyza, A, Denton, E, Dicks, P, Dolman, M, Donaldson, K, Dowden, L, Dowling, S, Drake, C, Duckles-Leech, H, Duffy, H, Gerdes, L, Gibbons, K, Gill, L, Gilmour, K, Goodwin, J, Graham, J, Green, C, Hall, C, Hall, A, Hampshire, K, Hanson, J, Harman, T, Harper, H, Harrison, S, Hicks, J, Hodgson, H, Hough, M, Jackson, S, Johnson, G, Kirk, J, Lemoine, N, Levett, C, Lock, S, Lockett, T, Logan, M, Lomme, K, Luo, J, McMillan, N, Membrey, H, Mguni, N, Minton, J, Monaghan, H, Murphy, S, Muzengi, N, Naz, M, Nickson, I, Odam, M, Ohia, U, Okell, E, Oliver, A, Pearson, K, Pine, K, Pleass, R, Porter, D, Porter, L, Potter, A, Poustie, V, Pratt, S, Price, A, Priest, A, Rodgers, A, Rook, C, Ryan, P, Sam, S, Sharratt, P, Sheffield, J, Shenton, J, Shirley, K, Skinner, T, Slade, H, Sutu, M, Taylor, J, Thomas, E, Tinkler, H, Unsworth, A, Usher, R, van't Hoff, W, Walker, S, Walters, J, Walton, E, Warmington, J, Wayman, E, Williams, P, Williamson, J, Williamson, D, Yelnoorkar, F, Knight, M, Hodson, K, Pavord, S, Williamson, C, Bowman, L, Chen, F, Clarke, R, Goonasekara, M, Herrington, W, Judge, P, Ng, S, Preiss, D, Sammons, E, Zhu, D, Arkley, C, Bowker, P, Bruce, J, Byrne-Watts, V, Chapman, G, Coleman, G, Denwood, T, Gray, J, Harrison, D, Mather, N, Pinches, H, Rees, A, Rees, S, Turner, G, Abani, O, Abbas, A, Abbas, F, Abbas, J, Abbas, K, Abbas, M, Abbasi, S, Abbass, H, Abbott, A, Abdallah, N, Abdelaziz, A, Abdelfattah, M, Abdelqader, B, Abdul, A, Abdul, B, Abdul, S, Abdul Rasheed, A, Abdulakeem, A, Abdul-Kadir, R, Abdullah, A, Abdulmumeen, A, Abdul-Raheem, R, Abdulshukkoor, N, Abdusamad, K, Abed El Khaleq, Y, Abedalla, M, Abeer Ul Amna, A, Abel, L, Abernethy, K, Abeywickrema, M, Abhinaya, C, Aboaba, A, Aboagye-Odei, A, Aboelela, H, Abo-Leyah, H, Abouelela, K, Abou-Haggar, A, Abouibrahim, M, Abousamra, A, Abouzaid, M, Abraham, M, Abraham, T, Abraheem, A, Abrams, J, Abrams, R, Abu, H, Abu-Arafeh, A, Abubacker, S, Abung, A, Abusamra, Y, Aceampong, Y, Achara, A, Acharya, D, Acheampong, S, Acheampong, P, Acheson, J, Achieng, S, Acosta, A, Acquah, R, Acton, C, Adabie-Ankrah, J, Adair, P, Adam, F, Adam, M, Adamali, H, Adamczyk, M, Adams, C, Adams, D, Adams, K, Adams, L, Adams, N, Adams, R, Adams, T, Adamu-Ikeme, L, Adati, K, Adcock, K, Addo, A, Adeagbo, O, Adebiyi, A, Adedeji, O, Adegeye, Y, Adegoke, K, Adell, V, Adenwalla, S, Adeoye, F, Adesemoye, O, Adewunmi, E, Adeyanju, A, Adeyemi, J, Adeyemo, T, Adhikary, R, Aditya, A, Adkins, G, Adnan, A, Aeron-Thomas, J, Affleck, D, Afnan, C, Afridi, M, Aftab, Z, Agarwal, M, Agbeko, R, Agbo, C, Aggarwal, S, Aghababaie, A, Aguilar Jimenez, L, Ahamed Sadiq, S, Ahammed Nazeer, M, Ahmed, A, Ahmed, B, Ahmed, F, Ahmed, H, Ahmed, I, Ahmed, K, Ahmed, L, Ahmad, M, Ahmed, N, Ahmed, O, Ahmed, R, 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Winslow, H, Winter, H, Winter, J, Winter-Goodwin, B, Winterton, J, Winwood, H, Wischhusen, J, Wisdom, S, Wise, M, Wiselka, M, Wiseman, R, Wiseman, S, Wishart, S, Wishlade, T, Witele, E, Withers, N, Wixted, D, Wodehouse, T, Wolf, W, Wolff, N, Wolffsohn, K, Wolf-Roberts, R, Wolodimeroff, E, Wolstencroft, A, Wong, A, Wong, C, Wong, C H, Wong, E, Wong, J, Wong, K, Wong, M, Wong, N, Wong, S, Wong, T, Wood, A, Wood, D, Wood, F, Wood, G, Wood, H, Wood, J, Wood, L, Wood, M, Wood, S, Wood, T, Woodall, K, Woodfield, R, Woodford, C, Woodford, E, Woodford, J, Woodhead, L, Woodhead, T, Woodland, P, Woodman, M, Woodmansey, S, Woods, C, Woods, J, Woods, K, Woods, S, Woodward, Z, Woolcock, M, Wooldridge, G, Woolf, R, Woollard, C, Woollen, L, Woolley, E, Woolley, J, Woosey, D, Wootton, D, Wootton, J, Worley, D, Worton, S, Wraight, J, Wray, M, Wren, K, Wren, L, Wrey Brown, C, Wright, C, Wright, D, Wright, F, Wright, H, Wright, I, Wright, L, Wright, R, Wright, S, Wright, T, Wroe, C, Wroe, H, Wu, H, Wu, P, Wubetu, J, Wulandari, R, Wurie, S, Wyatt, C, Wyn-Griffiths, F, Wynter, I, Xavier, B, Xhikola, A, Xia, B, Xia, Z, Y Ellis, T, Yacoba, E, Yakubi, M, Yan, M, Yanagisawa, Y, Yang, F, Yang, Y, Yanney, M, Yap, W, Yaqoob, N, Yasmin, S, Yates, B, Yates, D, Yates, E, Yates, H, Yates, M, Yates, T, Ye, J, Yearwood Martin, C, Yein, K, Yeoh, A, Yeung, C, Yew, P, Yewatkar, D, Ylquimiche Melly, L, Ynter, I, Yong, H, Yorke, J, Youens, J, Younes Ibrahim, A, Young, E, Young, G, Young, L, Yousafzar, A, Youssouf, S, Yousuf, A, Yu, C, Yuan, J, Yung, B, Yusef, D, Yusef, S, Yusuf, I, Zafar, A-M, Zagalo, S, Zaher, S, Zahoor, A, Zainab, M, Zak, T, Zaki, K, Zakir, N, Zalewska, K, Zamalloa, A, Zaman, M, Zaman, S, Zamikula, J, Zammit, L, Zammit-Mangion, M, Zawadzka, M, Zebracki, E, Zehnder, D, Zeidan, L, Zeinali, D, Zhang, J, Zhao, X, Zheng, D, Zia, M, Zibdeh, O, Zill-E-Huma, R, Zin, E, Zincone, E, Zindoga, G, Zinkin, E, Zinyemba, V, Zipitis, C, Zitter, L, Zmierczak, A, Zubikarai, G, Zubir, A, Zuhra, N, Zulaikha, R, Zulfikar, S, Zullo, C, and Zuriaga-Alvaro, A
Published: 2024
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35. Reduced Microwave Brightness Temperature in a Sunspot Atmosphere due to Open Magnetic Fields

Author: Vrublevskis, A., Ryabov, B. I., and White, S. M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Motivated by dark coronal lanes in SOHO / EIT 284 {\AA} EUV observations we construct and optimize an atmosphere model of the AR 8535 sunspot by adding a cool and dense component in the volume of plasma along open field lines determined using the Potential Field Source Surface (PFSS) extrapolation. Our model qualitatively reproduces the observed reduced microwave brightness temperature in the northern part of the sunspot in the VLA observations from 13 May 1999 and provides a physical explanation for the coronal dark lanes. We propose application of this method to other sunspots with such observed dark regions in EUV or soft X-rays and with concurrent microwave observations to determine the significance of open field regions. The connection between open fields and the resulting plasma temperature and density change is of relevance for slow solar wind source investigations., Comment: 26 pages, 12 figures. [v1] replaced to include journal reference after publication. This preprint has not undergone peer review or any post-submission improvements or corrections. The Version of Record of this article is published in Solar Physics, and is available online at https://doi.org/10.1007/s11207-021-01891-5
Published: 2021
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36. GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey III: South Galactic Pole data release

Author: Franzen, T., Hurley-Walker, N., White, S., Hancock, P., Seymour, N., Kapińska, A., Staveley-Smith, L., and Wayth, R.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present the South Galactic Pole (SGP) data release from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey. These data combine both years of GLEAM observations at 72-231 MHz conducted with the Murchison Widefield Array (MWA) and cover an area of 5,113 $\mathrm{deg}^2$ centred on the SGP at 20$^\mathrm{h}$40$^\mathrm{m}$ < RA < 05$^\mathrm{h}$04$^\mathrm{m}$ and $-48\deg$ < Dec < $-2\deg$. At 216 MHz, the typical rms noise is $\approx 5$ mJy/beam and the angular resolution $\approx 2$ arcmin. The source catalogue contains a total of 108,851 components above $5\sigma$, of which 77 per cent have measured spectral indices between 72 and 231 MHz. Improvements to the data reduction in this release include the use of the GLEAM Extragalactic catalogue as a sky model to calibrate the data, a more efficient and automated algorithm to deconvolve the snapshot images, and a more accurate primary beam model to correct the flux scale. This data release enables more sensitive large-scale studies of extragalactic source populations as well as spectral variability studies on a one-year timescale., Comment: 13 pages, 7 figures, accepted for publication in PASA. Added link to images and source catalogue from GLEAM SGP data release in section 5. Corrected some mistakes in column numbers in section 4.5 describing catalogue. The catalogue is now also available on VizieR
Published: 2021
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37. Commissioning the HI Observing Mode of the Beamformer for the Cryogenically Cooled Focal L-band Array for the GBT (FLAG)

Author: Pingel, N. M., Pisano, D. J., Ruzindana, M., Burnett, M., Rajwade, K. M., Black, R., Jeffs, B., Lorimer, D. R., Roshi, D. Anish, Prestage, R., McLaughlin, M. A., Agarwal, D., Chamberlin, T., Hawkins, L., Jensen, L., Marganian, P., Nelson, J. D., Shillue, W., Smith, E., Simon, B., Van Tonder, V., and White, S.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present the results of commissioning observations for a new digital beamforming back end for the Focal plane L-band Array for the Robert C. Byrd Green Bank Telescope (FLAG), a cryogenically cooled Phased Array Feed (PAF) with the lowest measured T_sys/eta of any PAF outfitted on a radio telescope to date. We describe the custom software used to apply beamforming weights to the raw element covariances to create research quality spectral line images for the new fine-channel mode, study the stability of the beam weights over time, characterize FLAG's sensitivity over a frequency range of 150 MHz, and compare the measured noise properties and observed distribution of neutral hydrogen emission from several extragalactic and Galactic sources with data obtained with the current single-pixel L-band receiver. These commissioning runs establish FLAG as the preeminent PAF receiver currently available for spectral line observations on the world's major radio telescopes., Comment: 28 ages, 18 figures. Accepted for publication in the Astronomical Journal
Published: 2021
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38. Remnant Radio Galaxies Discovered in a Multi-frequency Survey

Author: Quici, B., Hurley-Walker, N., Seymour, N., Turner, R. J., Shabala, S. S., Huynh, M., Andernach, H., Kapińska, A. D., Collier, J. D., Johnston-Hollitt, M., White, S. V., Prandoni, I., Galvin, T. J., Franzen, T., Ishwara-Chandra, C. H., Bellstedt, S., Tingay, S. J., Gaensler, B. M., O'Brien, A., Rogers, J., Chow, K., Driver, S., and Robotham, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The remnant phase of a radio galaxy begins when the jets launched from an active galactic nucleus are switched off. To study the fraction of radio galaxies in a remnant phase, we take advantage of a $8.31$\,deg$^2$ sub-region of the GAMA~23~field which comprises of surveys covering the frequency range 0.1--9\,GHz. We present a sample of 104 radio galaxies compiled from observations conducted by the Murchison Wide-field Array (216\,MHz), the Australia Square Kilometer Array Pathfinder (887\,MHz), and the Australia Telescope Compact Array (5.5\,GHz). We adopt an `absent radio core' criterion to identify 10 radio galaxies showing no evidence for an active nucleus. We classify these as new candidate remnant radio galaxies. Seven of these objects still display compact emitting regions within the lobes at 5.5\,GHz; at this frequency the emission is short-lived, implying a recent jet switch-off. On the other hand, only three show evidence of aged lobe plasma by the presence of an ultra-steep spectrum ($\alpha<-1.2$) and a diffuse, low surface-brightness radio morphology. The predominant fraction of young remnants is consistent with a rapid fading during the remnant phase. Within our sample of radio galaxies, our observations constrain the remnant fraction to $4\%\lesssim f_{\mathrm{rem}} \lesssim 10\%$; the lower limit comes from the limiting case in which all remnant candidates with hotspots are simply active radio galaxies with faint, undetected radio cores. Finally, we model the synchrotron spectrum arising from a hotspot to show they can persist for 5--10\,Myr at 5.5\,GHz after the jets switch off -- radio emission arising from such hotspots can therefore be expected in an appreciable fraction of genuine remnants.
Published: 2021
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39. Untangling the global coronal magnetic field with multiwavelength observations

Author: Gibson, S. E., Malanushenko, A., de Toma, G., Tomczyk, S., Reeves, K., Tian, H., Yang, Z., Chen, B., Fleishman, G., Gary, D., Nita, G., Pillet, V. M., White, S., Bąk-Stęślicka, U., Dalmasse, K., Kucera, T., Rachmeler, L. A., Raouafi, N. E., and Zhao, J.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Magnetism defines the complex and dynamic solar corona. Coronal mass ejections (CMEs) are thought to be caused by stresses, twists, and tangles in coronal magnetic fields that build up energy and ultimately erupt, hurling plasma into interplanetary space. Even the ever-present solar wind possesses a three-dimensional morphology shaped by the global coronal magnetic field, forming geoeffective corotating interaction regions. CME evolution and the structure of the solar wind depend intimately on the coronal magnetic field, so comprehensive observations of the global magnetothermal atmosphere are crucial both for scientific progress and space weather predictions. Although some advances have been made in measuring coronal magnetic fields locally, synoptic measurements of the global coronal magnetic field are not yet available. We conclude that a key goal for 2050 should be comprehensive, ongoing 3D synoptic maps of the global coronal magnetic field. This will require the construction of new telescopes, ground and space-based, to obtain complementary, multiwavelength observations sensitive to the coronal magnetic field. It will also require development of inversion frameworks capable of incorporating multi-wavelength data, and forward analysis tools and simulation testbeds to prioritize and establish observational requirements on the proposed telescopes., Comment: Helio2050 white paper
Published: 2020

40. MIGHTEE: Are giant radio galaxies more common than we thought?

Author: Delhaize, J., Heywood, I., Prescott, M., Jarvis, M. J., Delvecchio, I., Whittam, I. H., White, S. V., Hardcastle, M. J., Hale, C. L., Afonso, J., Ao, Y., Brienza, M., Brueggen, M., Collier, J. D., Daddi, E., Glowacki, M., Maddox, N., Morabito, L. K., Prandoni, I., Randriamanakoto, Z., Sekhar, S., An, Fangxia, Adams, N. J., Blyth, S., Bowler, R. A. A., Leeuw, L., Marchetti, L., Randriamampandry, S. M., Thorat, K., Seymour, N., Smirnov, O., Taylor, A. R., Tasse, C., and Vaccari, M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report the discovery of two new giant radio galaxies (GRGs) using the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) survey. Both GRGs were found within a 1 deg^2 region inside the COSMOS field. They have redshifts of z=0.1656 and z=0.3363 and physical sizes of 2.4Mpc and 2.0Mpc, respectively. Only the cores of these GRGs were clearly visible in previous high resolution VLA observations, since the diffuse emission of the lobes was resolved out. However, the excellent sensitivity and uv coverage of the new MeerKAT telescope allowed this diffuse emission to be detected. The GRGs occupy a unpopulated region of radio power - size parameter space. Based on a recent estimate of the GRG number density, the probability of finding two or more GRGs with such large sizes at z<0.4 in a ~1deg^2 field is only 2.7x10^-6, assuming Poisson statistics. This supports the hypothesis that the prevalence of GRGs has been significantly underestimated in the past due to limited sensitivity to low surface brightness emission. The two GRGs presented here may be the first of a new population to be revealed through surveys like MIGHTEE which provide exquisite sensitivity to diffuse, extended emission., Comment: 15 pages; 8 figures, accepted for publication in MNRAS on 2020 Dec 9
Published: 2020
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41. Spectral Variability of Radio Sources at Low Frequencies

Author: Ross, K., Callingham, J. R., Hurley-Walker, N., Seymour, N., Hancock, P., Franzen, T. M. O., Morgan, J., White, S. V., Bell, M. E., and Patil, P.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Spectral variability of radio sources encodes information about the conditions of intervening media, source structure, and emission processes. With new low-frequency radio interferometers observing over wide fractional bandwidths, studies of spectral variability for a large population of extragalactic radio sources are now possible. Using two epochs of observations from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey that were taken one year apart, we search for spectral variability across 100--230 MHz for 21,558 sources. We present methodologies for detecting variability in the spectrum between epochs and for classifying the type of variability: either as a change in spectral shape or as a uniform change in flux density across the bandwidth. We identify 323 sources with significant spectral variability over a year-long timescale. Of the 323 variable sources, we classify 51 of these as showing a significant change in spectral shape. Variability is more prevalent in peaked-spectrum sources, analogous to gigahertz-peaked spectrum and compact steep-spectrum sources, compared to typical radio galaxies. We discuss the viability of several potential explanations of the observed spectral variability, such as interstellar scintillation and jet evolution. Our results suggest that the radio sky in the megahertz regime is more dynamic than previously suggested., Comment: Accepted for publication in MNRAS
Published: 2020
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42. Timing performance of a multi-pad PICOSEC-Micromegas detector prototype

Author: Aune, S., Bortfeldt, J., Brunbauer, F., David, C., Desforge, D., Fanourakis, G., Gallinaro, M., García, F., Giomataris, I., Gustavsson, T., Iguaz, F. J., Kebbiri, M., Kordas, K., Lampoudis, C., Legou, P., Lisowska, M., Liu, J., Lupberger, M., Maillard, O., Manthos, I., Müller, H., Oliveri, E., Papaevangelou, T., Paraschou, K., Pomorski, M., Qi, B., Resnati, F., Ropelewski, L., Sampsonidis, D., Scharenberg, L., Schneider, T., Sohl, L., van Stenis, M., Tsiamis, A., Tsipolitis, Y., Tzamarias, S. E., Utrobicic, A., Veenhof, R., Wang, X., White, S., Zhang, Z., and Zhou, Y.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract: The multi-pad PICOSEC-Micromegas is an improved detector prototype with a segmented anode, consisting of 19 hexagonal pads. Detailed studies are performed with data collected in a muon beam over four representative pads. We demonstrate that such a device, scalable to a larger area, provides excellent time resolution and detection efficiency. As expected from earlier single-cell device studies, we measure a time resolution of approximately 25 picoseconds for charged particles hitting near the anode pad centers, and up to 30 picoseconds at the pad edges. Here, we study in detail the effect of drift gap thickness non-uniformity on the timing performance and evaluate impact position based corrections to obtain a uniform timing response over the full detector coverage., Comment: 29 pages, 20 figures
Published: 2020
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43. The infrared-radio correlation of star-forming galaxies is strongly M$_{\star}$-dependent but nearly redshift-invariant since z$\sim$4

Author: Delvecchio, I., Daddi, E., Sargent, M. T., Jarvis, M. J., Elbaz, D., Jin, S., Liu, D., Whittam, I. H., Algera, H., Carraro, R., D'Eugenio, C., Delhaize, J., Kalita, B. S., Leslie, S., Molnar, D. Cs., Novak, M., Prandoni, I., Smolcic, V., Ao, Y., Aravena, M., Bournaud, F., Collier, J. D., Randriamampandry, S. M., Randriamanakoto, Z., Rodighiero, G., Schober, J., White, S. V., and Zamorani, G.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Several works in the past decade have used the ratio between total (rest 8-1000$\mu$m) infrared and radio (rest 1.4~GHz) luminosity in star-forming galaxies (q$_{IR}$), often referred to as the "infrared-radio correlation" (IRRC), to calibrate radio emission as a star formation rate (SFR) indicator. Previous studies constrained the evolution of q$_{IR}$ with redshift, finding a mild but significant decline, that is yet to be understood. For the first time, we calibrate q$_{IR}$ as a function of \textit{both} stellar mass (M$_{\star}$) and redshift, starting from an M$_{\star}$-selected sample of $>$400,000 star-forming galaxies in the COSMOS field, identified via (NUV-r)/(r-J) colours, at redshifts 0.1$<$z$<$4.5. Within each (M$_{\star}$,z) bin, we stack the deepest available infrared/sub-mm and radio images. We fit the stacked IR spectral energy distributions with typical star-forming galaxy and IR-AGN templates, and carefully remove radio AGN candidates via a recursive approach. We find that the IRRC evolves primarily with M$_{\star}$, with more massive galaxies displaying systematically lower q$_{IR}$. A secondary, weaker dependence on redshift is also observed. The best-fit analytical expression is the following: q$_{IR}$(M$_{\star}$,z)=(2.646$\pm$0.024)$\times$(1+z)$^{(-0.023\pm0.008)}$-(0.148$\pm$0.013)$\times$($\log~M_{\star}$/M$_{\odot}$-10). The lower IR/radio ratios seen in more massive galaxies are well described by their higher observed SFR surface densities. Our findings highlight that using radio-synchrotron emission as a proxy for SFR requires novel M$_{\star}$-dependent recipes, that will enable us to convert detections from future ultra deep radio surveys into accurate SFR measurements down to low-SFR, low-M$_{\star}$ galaxies., Comment: Accepted for publication in A&A. 22 pages + Appendices. 24 figures, 4 tables
Published: 2020
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44. MeerKAT's discovery of a radio relic in the bimodal merging cluster A2384

Author: Parekh, V., Thorat, K., Kale, R., Hugo, B., Oozeer, N., Makhathini, S., Kleiner, D., White, S. V., Józsa, G. I. G., Smirnov, O., van der Heyden, K., Perkins, S., Andati, L., Ramaila, A., and Ramatsoku, M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present the discovery of a single radio relic located at the edge of the galaxy cluster A2384, using the MeerKAT radio telescope. A2384 is a nearby ($z$ = 0.092), low mass, complex bimodal, merging galaxy cluster that displays a dense X-ray filament ($\sim$ 700 kpc in length) between A2384(N) (Northern cluster) and A2384(S) (Southern cluster). The origin of the radio relic is puzzling. By using the MeerKAT observation of A2384, we estimate that the physical size of the radio relic is 824 $\times$ 264 kpc$^{2}$ and that it is a steep spectrum source. The radio power of the relic is $P_{1.4\mathrm{GHz}}$ $\sim$ (3.87 $\pm$ 0.40) $\times$ 10$^{23}$ W Hz$^{-1}$. This radio relic could be the result of shock wave propagation during the passage of the low-mass A2384(S) cluster through the massive A2384(N) cluster, creating a trail appearing as a hot X-ray filament. In the previous GMRT 325 MHz observation we detected a peculiar FR I radio galaxy interacting with the hot X-ray filament of A2384, but the extended radio relic was not detected; it was confused with the southern lobe of the FR I galaxy. This newly detected radio relic is elongated and perpendicular to the merger axis, as seen in other relic clusters. In addition to the relic, we notice a candidate radio ridge in the hot X-ray filament. The physical size of the radio ridge source is $\sim$ 182 $\times$ 129 kpc$^{2}$. Detection of the diffuse radio sources in the X-ray filament is a rare phenomenon, and could be a new class of radio source found between the two merging clusters of A2384(N) and A2384(S)., Comment: 12 pages, 6 figures, accepted in MNRAS
Published: 2020
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45. A dynamically cold disk galaxy in the early Universe

Author: Rizzo, F., Vegetti, S., Powell, D., Fraternali, F., McKean, J. P., Stacey, H. R., and White, S. D. M.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The extreme astrophysical processes and conditions that characterize the early Universe are expected to result in young galaxies that are dynamically different from those observed today. This is because the strong effects associated with galaxy mergers and supernova explosions would lead to most young star-forming galaxies being dynamically hot, chaotic and strongly unstable. Here we report the presence of a dynamically cold, but highly star-forming, rotating disk in a galaxy at redshift ($z$) 4.2, when the Universe was just 1.4 billion years old. Galaxy SPT-S J041839-4751.9 is strongly gravitationally lensed by a foreground galaxy at $z = 0.263$, and it is a typical dusty starburst, with global star-forming and dust properties that are in agreement with current numerical simulations and observations of its galaxy population. Interferometric imaging at a spatial resolution of about 60 pc reveals a ratio of rotational-to-random motions of $V/\sigma = 9.7\pm 0.4$, which is at least four times larger than expected from any galaxy evolution model at this epoch, but similar to the ratios of spiral galaxies in the local Universe. We derive a rotation curve with the typical shape of nearby massive spiral galaxies, which demonstrates that at least some young galaxies are dynamically akin to those observed in the local Universe, and only weakly affected by extreme physical processes., Comment: Published in Nature on 12 August 2020. The published version is available at http://www.nature.com/articles/s41586-020-2572-6
Published: 2020
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46. ALMA observations of transient heating in a solar active region

Author: Santos, J. M. da Silva, Rodríguez, J. de la Cruz, White, S. M., Leenaarts, J., Vissers, G. J. M., and Hansteen, V. H.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We aim to investigate the temperature enhancements and formation heights of impulsive heating phenomena in solar active-regions such as Ellerman bombs (EBs), ultraviolet bursts (UVBs), and flaring active-region fibrils (FAFs) using interferometric observations in the millimeter (mm) continuum provided by the Atacama Large Millimeter/submillimeter Array (ALMA). We examined 3 mm signatures of heating events identified in Solar Dynamics Observatory (SDO) observations of an active region and compared the results with synthetic spectra from a 3D radiative magnetohydrodynamic simulation. We estimated the contribution from the corona to the mm brightness using differential emission measure analysis. We report the null detection of EBs in the 3 mm continuum at $\sim1.2$" spatial resolution, which is evidence that they are sub-canopy events that do not significantly contribute to heating the upper chromosphere. In contrast, we find the active region to be populated with multiple compact, bright, flickering mm bursts -- reminiscent of UVBs. The high brightness temperatures of up to $\sim14200$ K in some events have a significant contribution (up to $\sim$7%) from the corona. We also detect FAF-like events in the 3 mm continuum that show rapid motions of $>10000\,$K plasma launched with high plane-of-sky velocities ($37-340\rm\,km\,s^{-1}$) from bright kernels. The mm FAFs are the brightest class of warm canopy fibrils that connect magnetic regions of opposite polarities. The simulation confirms that ALMA should be able to detect the mm counterparts of UVBs and small flares and thus provide a complementary diagnostic for localized heating in the solar chromosphere., Comment: revised; accepted in Astronomy & Astrophysics
Published: 2020
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47. Measurement of jet-medium interactions via direct photon-hadron correlations in Au$+$Au and $d$$+$Au collisions at $\sqrt{s_{_{NN}}}=200$ GeV

Author: Acharya, U., Adare, A., Afanasiev, S., Aidala, C., Ajitanand, N. N., Akiba, Y., Akimoto, R., Al-Bataineh, H., Alexander, J., Al-Ta'ani, H., Angerami, A., Aoki, K., Apadula, N., Aramaki, Y., Asano, H., Aschenauer, E. C., Atomssa, E. T., Averbeck, R., Awes, T. C., Azmoun, B., Babintsev, V., Bai, M., Baksay, G., Baksay, L., Bannier, B., Barish, K. N., Bassalleck, B., Basye, A. T., Bathe, S., Baublis, V., Baumann, C., Baumgart, S., Bazilevsky, A., Belikov, S., Belmont, R., Bennett, R., Berdnikov, A., Berdnikov, Y., Bhom, J. H., Bichon, L., Bickley, A. A., Black, D., Blankenship, B., Blau, D. S., Bok, J. S., Borisov, V., Boyle, K., Brooks, M. L., Bryslawskyj, J., Buesching, H., Bumazhnov, V., Bunce, G., Butsyk, S., Camacho, C. M., Campbell, S., Roman, V. Canoa, Caringi, A., Castera, P., Chen, C. -H., Chi, C. Y., Chiu, M., Choi, I. J., Choi, J. B., Choi, S., Choudhury, R. K., Christiansen, P., Chujo, T., Chung, P., Chvala, O., Cianciolo, V., Citron, Z., Cole, B. A., del Valle, Z. Conesa, Connors, M., Constantin, P., Cronin, N., Crossette, N., Csanád, M., Csörgő, T., Dahms, T., Dairaku, S., Danchev, I., Das, K., Datta, A., Daugherity, M. S., David, G., Dayananda, M. K., DeBlasio, K., Dehmelt, K., Denisov, A., Deshpande, A., Desmond, E. J., Dharmawardane, K. V., Dietzsch, O., Ding, L., Dion, A., Do, J. H., Donadelli, M., D'Orazio, L., Drapier, O., Drees, A., Drees, K. A., Durham, J. M., Durum, A., Dutta, D., Edwards, S., Efremenko, Y. V., Ellinghaus, F., Engelmore, T., Enokizono, A., En'yo, H., Esha, R., Esumi, S., Eyser, K. O., Fadem, B., Fan, W., Fields, D. E., Finger, M., Finger, Jr., M., Firak, D., Fitzgerald, D., Fleuret, F., Fokin, S. L., Fraenkel, Z., Frantz, J. E., Franz, A., Frawley, A. D., Fujiwara, K., Fukao, Y., Fusayasu, T., Gainey, K., Gal, C., Garg, P., Garishvili, A., Garishvili, I., Giordano, F., Glenn, A., Gong, H., Gong, X., Gonin, M., Goto, Y., de Cassagnac, R. Granier, Grau, N., Greene, S. V., Grim, G., Perdekamp, M. Grosse, Gu, Y., Gunji, T., Guo, L., Gustafsson, H. -Å., Hachiya, T., Haggerty, J. S., Hahn, K. I., Hamagaki, H., Hamblen, J., Han, R., Han, S. Y., Hanks, J., Hartouni, E. P., Hasegawa, S., Hashimoto, K., Haslum, E., Hayano, R., Hayashi, S., He, X., Heffner, M., Hemmick, T. K., Hester, T., Hill, J. C., Hodges, A., Hohlmann, M., Hollis, R. S., Holzmann, W., Homma, K., Hong, B., Horaguchi, T., Hori, Y., Hornback, D., Huang, J., Huang, S., Ichihara, T., Ichimiya, R., Ide, J., Iinuma, H., Ikeda, Y., Imai, K., Imazu, Y., Imrek, J., Inaba, M., Iordanova, A., Isenhower, D., Ishihara, M., Isinhue, A., Isobe, T., Issah, M., Isupov, A., Ivanishchev, D., Iwanaga, Y., Jacak, B. V., Javani, M., Ji, Z., Jia, J., Jiang, X., Jin, J., Johnson, B. M., Jones, T., Joo, K. S., Jouan, D., Jumper, D. S., Kajihara, F., Kametani, S., Kamihara, N., Kamin, J., Kaneti, S., Kang, B. H., Kang, J. H., Kang, J. S., Kapustinsky, J., Karatsu, K., Kasai, M., Kawall, D., Kawashima, M., Kazantsev, A. V., Kempel, T., Key, J. A., Khachatryan, V., Khandai, P. K., Khanzadeev, A., Khatiwada, A., Kijima, K. M., Kikuchi, J., Kim, A., Kim, B. I., Kim, C., Kim, D. H., Kim, D. J., Kim, E., Kim, E. -J., Kim, H. J., Kim, K. -B., Kim, S. H., Kim, Y. -J., Kim, Y. K., Kincses, D., Kinney, E., Kiriluk, K., Kiss, Á., Kistenev, E., Klatsky, J., Kleinjan, D., Kline, P., Kochenda, L., Komatsu, Y., Komkov, B., Konno, M., Koster, J., Kotchetkov, D., Kotov, D., Kozlov, A., Král, A., Kravitz, A., Krizek, F., Kunde, G. J., Kurgyis, B., Kurita, K., Kurosawa, M., Kwon, Y., Kyle, G. S., Lacey, R., Lai, Y. S., Lajoie, J. G., Larionova, D., Larionova, M., Lebedev, A., Lee, B., Lee, D. M., Lee, J., Lee, K., Lee, K. B., Lee, K. S., Lee, S. H., Lee, S. R., Leitch, M. J., Leite, M. A. L., Leitgab, M., Leitner, E., Lenzi, B., Lewis, B., Lewis, N. A., Li, X., Lichtenwalner, P., Liebing, P., Lim, S. H., Levy, L. A. Linden, Liška, T., Litvinenko, A., Liu, H., Liu, M. X., Lökös, S., Love, B., Luechtenborg, R., Lynch, D., Maguire, C. F., Majoros, T., Makdisi, Y. I., Makek, M., Malakhov, A., Malik, M. D., Manion, A., Manko, V. I., Mannel, E., Mao, Y., Masui, H., Masumoto, S., Matathias, F., McCumber, M., McGaughey, P. L., McGlinchey, D., McKinney, C., Means, N., Meles, A., Mendoza, M., Meredith, B., Metzger, W. J., Miake, Y., Mibe, T., Midori, J., Mignerey, A. C., Mikeš, P., Miki, K., Milov, A., Mishra, D. K., Mishra, M., Mitchell, J. T., Mitrankov, Iu., Miyachi, Y., Miyasaka, S., Mohanty, A. K., Mohapatra, S., Moon, H. J., Moon, T., Morino, Y., Morreale, A., Morrison, D. P., Morrow, S. I., Moskowitz, M., Motschwiller, S., Moukhanova, T. V., Mulilo, B., Murakami, T., Murata, J., Mwai, A., Nagae, T., Nagamiya, S., Nagle, J. L., Naglis, M., Nagy, M. I., Nakagawa, I., Nakamiya, Y., Nakamura, K. R., Nakamura, T., Nakano, K., Nam, S., Nattrass, C., Nederlof, A., Nelson, S., Netrakanti, P. K., Newby, J., Nguyen, M., Nihashi, M., Niida, T., Nouicer, R., Novitzky, N., Nukariya, A., Nyanin, A. S., Oakley, C., Obayashi, H., O'Brien, E., Oda, S. X., Ogilvie, C. A., Oka, M., Okada, K., Onuki, Y., Osborn, J. D., Oskarsson, A., Ouchida, M., Ozawa, K., Pak, R., Pantuev, V., Papavassiliou, V., Park, B. H., Park, I. H., Park, J., Park, S., Park, S. K., Park, W. J., Pate, S. F., Patel, L., Patel, M., Pei, H., Peng, J. -C., Peng, W., Pereira, H., Perepelitsa, D. V., Peresedov, V., Peressounko, D. Yu., PerezLara, C. E., Petti, R., Pinkenburg, C., Pisani, R. P., Proissl, M., Pun, A., Purschke, M. L., Purwar, A. K., Qu, H., Radzevich, P. V., Rak, J., Rakotozafindrabe, A., Ramasubramanian, N., Ravinovich, I., Read, K. F., Rembeczki, S., Reygers, K., Reynolds, D., Riabov, V., Riabov, Y., Richardson, E., Richford, D., Rinn, T., Riveli, N., Roach, D., Roche, G., Rolnick, S. D., Rosati, M., Rosen, C. A., Rosendahl, S. S. E., Rosnet, P., Rukoyatkin, P., Runchey, J., Ružička, P., Ryu, M. S., Sahlmueller, B., Saito, N., Sakaguchi, T., Sakashita, K., Sako, H., Samsonov, V., Sano, M., Sano, S., Sarsour, M., Sato, S., Sato, T., Sawada, S., Sedgwick, K., Seele, J., Seidl, R., Semenov, A. Yu., Sen, A., Seto, R., Sett, P., Sharma, D., Shein, I., Shibata, T. -A., Shigaki, K., Shimomura, M., Shoji, K., Shukla, P., Sickles, A., Silva, C. L., Silvermyr, D., Silvestre, C., Sim, K. S., Singh, B. K., Singh, C. P., Singh, V., Skolnik, M., Slunečka, M., Smith, K. L., Solano, S., Soltz, R. A., Sondheim, W. E., Sorensen, S. P., Sourikova, I. V., Sparks, N. A., Stankus, P. W., Steinberg, P., Stenlund, E., Stepanov, M., Ster, A., Stoll, S. P., Sugitate, T., Sukhanov, A., Sun, J., Sun, X., Sun, Z., Sziklai, J., Takagui, E. M., Takahara, A., Taketani, A., Tanabe, R., Tanaka, Y., Taneja, S., Tanida, K., Tannenbaum, M. J., Tarafdar, S., Taranenko, A., Tarján, P., Tennant, E., Themann, H., Thomas, D., Thomas, T. L., Todoroki, T., Togawa, M., Toia, A., Tomášek, L., Tomášek, M., Torii, H., Towell, R. S., Tserruya, I., Tsuchimoto, Y., Tsuji, T., Ueda, Y., Ujvari, B., Vale, C., Valle, H., van Hecke, H. W., Vargyas, M., Vazquez-Zambrano, E., Veicht, A., Velkovska, J., Vértesi, R., Vinogradov, A. A., Virius, M., Voas, B., Vossen, A., Vrba, V., Vznuzdaev, E., Wang, X. R., Watanabe, D., Watanabe, K., Watanabe, Y., Watanabe, Y. S., Wei, F., Wei, R., Wessels, J., Whitaker, S., White, S. N., Winter, D., Wolin, S., Wong, C. P., Wood, J. P., Woody, C. L., Wright, R. M., Wu, Y., Wysocki, M., Xia, B., Xie, W., Xu, Q., Yamaguchi, Y. L., Yamaura, K., Yang, R., Yanovich, A., Ying, J., Yokkaichi, S., Yoon, I., You, Z., Young, G. R., Younus, I., Yushmanov, I. E., Zajc, W. A., Zelenski, A., Zhai, Y., Zhang, C., Zharko, S., Zhou, S., Zolin, L., and Zou, L.
Subjects: High Energy Physics - Experiment, Nuclear Experiment
Abstract: We present direct photon-hadron correlations in 200 GeV/A Au$+$Au, $d$$+$Au and $p$$+$$p$ collisions, for direct photon $p_T$ from 5--12 GeV/$c$, collected by the PHENIX Collaboration in the years from 2006 to 2011. We observe no significant modification of jet fragmentation in $d$$+$Au collisions, indicating that cold nuclear matter effects are small or absent. Hadrons carrying a large fraction of the quark's momentum are suppressed in Au$+$Au compared to $p$$+$$p$ and $d$$+$Au. As the momentum fraction decreases, the yield of hadrons in Au$+$Au increases to an excess over the yield in $p$$+$$p$ collisions. The excess is at large angles and at low hadron $p_T$ and is most pronounced for hadrons associated with lower momentum direct photons. Comparison to theoretical calculations suggests that the hadron excess arises from medium response to energy deposited by jets., Comment: 578 authors from 80 institutions, 11 pages, 7 figures, data from 2007, 2008, 2010, and 2011. v2 is version accepted for publication in Physical Review C. Plain text data tables for the points plotted in figures for this and previous PHENIX publications are (or will be) publicly available at http://www.phenix.bnl.gov/papers.html
Published: 2020
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48. The POlarised GLEAM Survey (POGS) II: Results from an All-Sky Rotation Measure Synthesis Survey at Long Wavelengths

Author: Riseley, C. J., Galvin, T. J., Sobey, C., Vernstrom, T., White, S. V., Zhang, X., Gaensler, B. M., Heald, G., Anderson, C. S., Franzen, T. M. O., Hancock, P. J., Hurley-Walker, N., Lenc, E., and Van Eck, C. L.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The low-frequency linearly-polarised radio source population is largely unexplored. However, a renaissance in low-frequency polarimetry has been enabled by pathfinder and precursor instruments for the Square Kilometre Array. In this second paper from the POlarised GaLactic and Extragalactic All-Sky Murchison Widefield Array (MWA) Survey -- the POlarised GLEAM Survey, or POGS -- we present the results from our all-sky MWA Phase I Faraday Rotation Measure survey. Our survey covers nearly the entire Southern sky in the Declination range $-82^{\circ}$ to $+30^{\circ}$ at a resolution between around three and seven arcminutes (depending on Declination) using data in the frequency range 169$-$231 MHz. We have performed two targeted searches: the first covering 25,489 square degrees of sky, searching for extragalactic polarised sources; the second covering the entire sky South of Declination $+30^{\circ}$, searching for known pulsars. We detect a total of 517 sources with 200 MHz linearly-polarised flux densities between 9.9 mJy and 1.7 Jy, of which 33 are known radio pulsars. All sources in our catalogues have Faraday rotation measures in the range $-328.07$ rad m$^{-2}$ to $+279.62$ rad m$^{-2}$. The Faraday rotation measures are broadly consistent with results from higher-frequency surveys, but with typically more than an order of magnitude improvement in the precision, highlighting the power of low-frequency polarisation surveys to accurately study Galactic and extragalactic magnetic fields. We discuss the properties of our extragalactic and known-pulsar source population, how the sky distribution relates to Galactic features, and identify a handful of new pulsar candidates among our nominally extragalactic source population., Comment: Replacement of previous version. Only change is minor updates to catalogues (see ancillary files) which now contain bib code of finalised manuscript (published in PASA). Manuscript has 31 pages, 10 figures, 5 tables. Four Appendices are included in the ancillary material, showing further Figures, continuum spectra for a handful of selected sources, and RM spectra for all 517 sources
Published: 2020
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49. Hydrodynamical Backflow in X-shaped Radio Galaxy PKS 2014-55

Author: Cotton, W. D., Thorat, K., Condon, J. J., Frank, B . S., Józsa, G . I. G., White, S. V., Deane, R ., Oozeer, N., Atemkeng, M., Bester, L., Fanaroff, B., Kupa, R. S., Smirnov, O. M., Mauch, T., Krishnan, V., and Camilo, F.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present MeerKAT 1.28 GHz total-intensity, polarization, and spectral-index images covering the giant (projected length $l \approx 1.57$~Mpc) X-shaped radio source PKS~2014$-$55 with an unprecedented combination of brightness sensitivity and angular resolution. They show the clear "double boomerang" morphology of hydrodynamical backflows from the straight main jets deflected by the large and oblique hot-gas halo of the host galaxy PGC~064440. The magnetic field orientation in PKS~2014$-$55 follows the flow lines from the jets through the secondary wings. The radio source is embedded in faint ($T_\mathrm{b} \approx 0.5 \mathrm{\,K}$) cocoons having the uniform brightness temperature and sharp outer edges characteristic of subsonic expansion into the ambient intra-group medium. The position angle of the much smaller ($l \sim 25$~kpc) restarted central source is within $5^\circ$ of the main jets, ruling out models that invoke jet re-orientation or two independent jets. Compression and turbulence in the backflows probably produce the irregular and low polarization bright region behind the apex of each boomerang as well as several features in the flow with bright heads and dark tails., Comment: 13 pages, 11 figures
Published: 2020
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50. Collimated synchrotron threads linking the radio lobes of ESO137-006

Author: Ramatsoku, M., Murgia, M., Vacca, V., Serra, P., Makhathini, S., Govoni, F., Smirnov, O., Andati, L. A. L., de Blok, E., Józsa, G. I. G., Kamphuis, P., Kleiner, D., Maccagni, F. M., Molnár, D. Cs., Ramaila, A. J. T., Thorat, K., and White, S. V.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present MeerKAT 1000 MHz and 1400 MHz observations of a bright radio galaxy in the southern hemisphere, ESO~137-006. The galaxy lies at the centre of the massive and merging Norma galaxy cluster. The MeerKAT continuum images (rms ~0.02 mJy/beam at ~10" resolution) reveal new features that have never been seen in a radio galaxy before: collimated synchrotron threads of yet unknown origin, which link the extended and bent radio lobes of ESO~137-006. The most prominent of these threads stretches in projection for about 80 kpc and is about 1 kpc in width. The radio spectrum of the threads is steep, with a spectral index of up to $\alpha\simeq 2$ between 1000 MHz and 1400 MHz., Comment: 5 pages, 4 figures, accepted for publication in A&A letters
Published: 2020
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