2016, Li, Y., Zhao, M., Mildrexler, D.J., Motesharrei, S., Mu, Q., Kalnay, E., Zhao, F., Li, S., Wang, K.

2014, Wang, K., Gu, Y., Zhou, H.F., Zhang, L.Y., Kang, C.Z., Wu, M.J., Pan, W.W., Lu, P.F., Gong, Q., Wang, S.M.

InPBi was predicted to be the most robust infrared optoelectronic material but also the most difficult to synthesize within In-VBi (V = P, As and Sb) 25 years ago. We report the first successful growth of InPBi single crystals with Bi concentration far beyond the doping level by gas source molecular beam epitaxy. The InPBi thin films reveal excellent surface, structural and optical qualities making it a promising new III–V compound family member for heterostructures. The Bi concentration is found to be 2.4 ± 0.4% with 94 ± 5% Bi atoms at substitutional sites. Optical absorption indicates a band gap of 1.23 eV at room temperature while photoluminescence shows unexpectedly strong and broad light emission at 1.4–2.7 μm which can't be explained by the existing theory.

2020, Assmann, R. W., Weikum, M. K., Akhter, T., Alesini, D., Alexandrova, A. S., Anania, M. P., Andreev, N. E., Andriyash, I., Artioli, M., Aschikhin, A., Audet, T., Jafarinia, F. J., Jakobsson, O., Jaroszynski, D. A., Jaster-Merz, S., Joshi, C., Kaluza, M., Kando, M., Karger, O. S., Karsch, S., Khazanov, E., Bacci, A., Khikhlukha, D., Kirchen, M., Kirwan, G., Kitégi, C., Knetsch, A., Kocon, D., Koester, P., Kononenko, O. S., Korn, G., Kostyukov, I., Barna, I. F., Kruchinin, K. O., Labate, L., Le Blanc, C., Lechner, C., Lee, P., Leemans, W., Lehrach, A., Li, X., Li, Y., Libov, V., Bartocci, S., Lifschitz, A., Lindstrøm, C. A., Litvinenko, V., Lu, W., Lundh, O., Maier, A. R., Malka, V., Manahan, G. G., Mangles, S. P. D., Marcelli, A., Bayramian, A., Marchetti, B., Marcouillé, O., Marocchino, A., Marteau, F., Martinez de la Ossa, A., Martins, J. L., Mason, P. D., Massimo, F., Mathieu, F., Maynard, G., Beaton, A., Mazzotta, Z., Mironov, S., Molodozhentsev, A. Y., Morante, S., Mosnier, A., Mostacci, A., Müller, A. -S., Murphy, C. D., Najmudin, Z., Nghiem, P. A. P., Beck, A., Nguyen, F., Niknejadi, P., Nutter, A., Osterhoff, J., Oumbarek Espinos, D., Paillard, J. -L., Papadopoulos, D. N., Patrizi, B., Pattathil, R., Pellegrino, L., Bellaveglia, M., Petralia, A., Petrillo, V., Piersanti, L., Pocsai, M. A., Poder, K., Pompili, R., Pribyl, L., Pugacheva, D., Reagan, B. A., Resta-Lopez, J., Beluze, A., Ricci, R., Romeo, S., Rossetti Conti, M., Rossi, A. R., Rossmanith, R., Rotundo, U., Roussel, E., Sabbatini, L., Santangelo, P., Sarri, G., Bernhard, A., Schaper, L., Scherkl, P., Schramm, U., Schroeder, C. B., Scifo, J., Serafini, L., Sharma, G., Sheng, Z. M., Shpakov, V., Siders, C. W., Biagioni, A., Silva, L. O., Silva, T., Simon, C., Simon-Boisson, C., Sinha, U., Sistrunk, E., Specka, A., Spinka, T. M., Stecchi, A., Stella, A., Bielawski, S., Stellato, F., Streeter, M. J. V., Sutherland, A., Svystun, E. N., Symes, D., Szwaj, C., Tauscher, G. E., Terzani, D., Toci, G., Tomassini, P., Bisesto, F. G., Torres, R., Ullmann, D., Vaccarezza, C., Valléau, M., Vannini, M., Vannozzi, A., Vescovi, S., Vieira, J. M., Villa, F., Wahlström, C. -G., Bonatto, A., Walczak, R., Walker, P. A., Wang, K., Welsch, A., Welsch, C. P., Weng, S. M., Wiggins, S. M., Wolfenden, J., Xia, G., Yabashi, M., Boulton, L., Zhang, H., Zhao, Y., Zhu, J., Zigler, A., Brandi, F., Brinkmann, R., Briquez, F., Brottier, F., Bründermann, E., Büscher, M., Buonomo, B., Bussmann, M. H., Bussolino, G., Campana, P., Cantarella, S., Cassou, K., Chancé, A., Chen, M., Chiadroni, E., Cianchi, A., Cioeta, F., Clarke, J. A., Cole, J. M., Costa, G., Couprie, M. -E., Cowley, J., Croia, M., Cros, B., Crump, P. A., D’Arcy, R., Dattoli, G., Del Dotto, A., Delerue, N., Del Franco, M., Delinikolas, P., De Nicola, S., Dias, J. M., Di Giovenale, D., Diomede, M., Di Pasquale, E., Di Pirro, G., Di Raddo, G., Dorda, U., Erlandson, A. C., Ertel, K., Esposito, A., Falcoz, F., Falone, A., Fedele, R., Ferran Pousa, A., Ferrario, M., Filippi, F., Fils, J., Fiore, G., Fiorito, R., Fonseca, R. A., Franzini, G., Galimberti, M., Gallo, A., Galvin, T. C., Ghaith, A., Ghigo, A., Giove, D., Giribono, A., Gizzi, L. A., Grüner, F. J., Habib, A. F., Haefner, C., Heinemann, T., Helm, A., Hidding, B., Holzer, B. J., Hooker, S. M., Hosokai, T., Hübner, M., Ibison, M., Incremona, S., Irman, A., Iungo, F.

This report presents the conceptual design of a new European research infrastructure EuPRAXIA. The concept has been established over the last four years in a unique collaboration of 41 laboratories within a Horizon 2020 design study funded by the European Union. EuPRAXIA is the first European project that develops a dedicated particle accelerator research infrastructure based on novel plasma acceleration concepts and laser technology. It focuses on the development of electron accelerators and underlying technologies, their user communities, and the exploitation of existing accelerator infrastructures in Europe. EuPRAXIA has involved, amongst others, the international laser community and industry to build links and bridges with accelerator science — through realising synergies, identifying disruptive ideas, innovating, and fostering knowledge exchange. The Eu-PRAXIA project aims at the construction of an innovative electron accelerator using laser- and electron-beam-driven plasma wakefield acceleration that offers a significant reduction in size and possible savings in cost over current state-of-the-art radiofrequency-based accelerators. The foreseen electron energy range of one to five gigaelectronvolts (GeV) and its performance goals will enable versatile applications in various domains, e.g. as a compact free-electron laser (FEL), compact sources for medical imaging and positron generation, table-top test beams for particle detectors, as well as deeply penetrating X-ray and gamma-ray sources for material testing. EuPRAXIA is designed to be the required stepping stone to possible future plasma-based facilities, such as linear colliders at the high-energy physics (HEP) energy frontier. Consistent with a high-confidence approach, the project includes measures to retire risk by establishing scaled technology demonstrators. This report includes preliminary models for project implementation, cost and schedule that would allow operation of the full Eu-PRAXIA facility within 8—10 years.

2021, Schuller, F., Urquhart, J.S., Csengeri, T., Colombo, D., Duarte-Cabral, A., Mattern, M., Ginsburg, A., Pettitt, A.R., Wyrowski, F., Anderson, L., Azagra, F., Barnes, P., Beltran, M., Beuther, H., Billington, S., Bronfman, L., Cesaroni, R., Dobbs, C., Eden, D., Lee, M.-Y., Medina, S.-N.X., Menten, K.M., Moore, T., Montenegro-Montes, F.M., Ragan, S., Rigby, A., Riener, M., Russeil, D., Schisano, E., Sanchez-Monge, A., Traficante, A., Zavagno, A., Agurto, C., Bontemps, S., Finger, R., Giannetti, A., Gonzalez, E., Hernandez, A.K., Henning, T., Kainulainen, J., Kauffmann, J., Leurini, S., Lopez, S., Mac-Auliffe, F., Mazumdar, P., Molinari, S., Motte, F., Muller, E., Nguyen-Luong, Q., Parra, R., Perez-Beaupuits, J.-P., Schilke, P., Schneider, N., Suri, S., Testi, L., Torstensson, K., Veena, V.S., Venegas, P., Wang, K., Wienen, M.

The SEDIGISM (Structure, Excitation and Dynamics of the Inner Galactic Interstellar Medium) survey used the APEX telescope to map 84 deg2 of the Galactic plane between ℓ = −60° and +31° in several molecular transitions, including 13CO (2 – 1) and C18O (2 – 1), thus probing the moderately dense (∼103 cm−3) component of the interstellar medium. With an angular resolution of 30 arcsec and a typical 1σ sensitivity of 0.8–1.0 K at 0.25 km s−1 velocity resolution, it gives access to a wide range of structures, from individual star-forming clumps to giant molecular clouds and complexes. The coverage includes a good fraction of the first and fourth Galactic quadrants, allowing us to constrain the large-scale distribution of cold molecular gas in the inner Galaxy. In this paper, we provide an updated overview of the full survey and the data reduction procedures used. We also assess the quality of these data and describe the data products that are being made publicly available as part of this First Data Release (DR1). We present integrated maps and position–velocity maps of the molecular gas and use these to investigate the correlation between the molecular gas and the large-scale structural features of the Milky Way such as the spiral arms, Galactic bar and Galactic Centre. We find that approximately 60 per cent of the molecular gas is associated with the spiral arms and these appear as strong intensity peaks in the derived Galactocentric distribution. We also find strong peaks in intensity at specific longitudes that correspond to the Galactic Centre and well-known star-forming complexes, revealing that the 13CO emission is concentrated in a small number of complexes rather than evenly distributed along spiral arms.