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1. Development of the continuous monitoring of tritium water by mid-infrared laser spectroscopy (Contract research); FY2021 Nuclear Energy Science & Technology and Human Resource Development Project

Author: Collaborative Laboratories for Advanced Decommissioning Science and National Institutes of Natural Sciences
Abstract: 日本原子力研究開発機構(JAEA)廃炉環境国際共同研究センター(CLADS)では、令和3年度英知を結集した原子力科学技術・人材育成推進事業(以下、「本事業」という)を実施している。本事業は、東京電力ホールディングス株式会社福島第一原子力発電所の廃炉等を始めとした原子力分野の課題解決に貢献するため、国内外の英知を結集し、様々な分野の知見や経験を、従前の機関や分野の壁を越えて緊密に融合・連携させた基礎的・基盤的研究及び人材育成を推進することを目的としている。平成30年度の新規採択課題から実施主体を文部科学省からJAEAに移行することで、JAEAとアカデミアとの連携を強化し、廃炉に資する中長期的な研究開発・人材育成をより安定的かつ継続的に実施する体制を構築した。本研究は、研究課題のうち、令和3年度に採択された「中赤外レーザー分光によるトリチウム水連続モニタリング手法の開発」の令和3年度の研究成果について取りまとめたものである。本研究は、中赤外レーザーを用いたキャビティリングダウン計測システムによる「濃度60Bq/ccレベル」トリチウム水短時間計測の原理実証を成果目的とする。令和3年度は、上記目標を達成するため、(1)キャビティリングダウン装置に関する研究、及び(2)環境条件下における水素同位体組成評価と標準試料作製(再委託先: 弘前大学)を行った。(1)においては、中赤外キャビティリングダウン試験を行った。実験室に光学ベンチ(3m$\times$1.2m)を設置し、光学ベンチ上に設計した光キャビティを構築した。次に、キャビティリングダウン計測に必須なレーザー光源を開発した。波長4.34$\mu$mから4.72$\mu$mの範囲に可変可能で、最高出力22mW、ビーム品質M$^{2}$=1.1のレーザー開発に成功した。(2)においては、標準試料の作製として、複数の試薬会社より市販されている重水標準溶液を利用して水素同位体標準溶液作製を進め、安定同位体である重水試料の準備を行った。また市販の重水試薬を購入し、約100Bq/Lの標準試料作製準備が整った。さらに、屋内外の同位体比計測の測定準備を行った。低バックグラウンド液体シンチレーション計数装置の性能評価を行い、試料量10mLで2,400分計測すると検出下限値は約0.6Bq/Lであることを確認した。これにより一般環境中トリチウム濃度を計測する準備が整った。, The Collaborative Laboratories for Advanced Decommissioning Science (CLADS), Japan Atomic Energy Agency (JAEA), had been conducting the Nuclear Energy Science \& Technology and Human Resource Development Project (hereafter referred to "the Project") in FY2021. The Project aims to contribute to solving problems in the nuclear energy field represented by the decommissioning of the Fukushima Daiichi Nuclear Power Station, Tokyo Electric Power Company Holdings, Inc. (TEPCO). For this purpose, intelligence was collected from all over the world, and basic research and human resource development were promoted by closely integrating/collaborating knowledge and experiences in various fields beyond the barrier of conventional organizations and research fields. The sponsor of the Project was moved from the Ministry of Education, Culture, Sports, Science and Technology to JAEA since the newly adopted proposals in FY2018. On this occasion, JAEA constructed a new research system where JAEA-academia collaboration is reinforced and medium-to-long term research/development and human resource development contributing to the decommissioning are stably and consecutively implemented. Among the adopted proposals in FY2021, this report summarizes the research results of the "Development of the continuous monitoring of tritium water by mid-infrared laser spectroscopy" conducted in FY2021. The present study aims to demonstrate the principle of short-time measurement of tritiated water at the "60 Bq/cc level" using a cavity ring-down measurement system with a mid-infrared laser. In order to achieve the above goal, (1) research on the cavity ring-down system and (2) evaluation of hydrogen isotope composition under environmental conditions and preparation of standard samples (subcontractor: Hirosaki University) were conducted this fiscal year. In (1), a mid-infrared cavity ring-down test was conducted. An optical bench (3 m $\times$ 1.2 m) was set up in the laboratory, and a designed optical
Published: 2023

2. Energizing Star Formation: The Cosmic-Ray Ionization Rate in NGC 253 Derived from ALCHEMI Measurements of H3O+and SO

Author: European Commission, National Science Foundation (US), National Institutes of Natural Sciences (Japan), Japan Society for the Promotion of Science, Comunidad de Madrid, Agencia Estatal de Investigación (España), Holdship, Jonathan, Mangum, Jeffrey G., Viti, Serena, Behrens, Erica, Harada, Nanase, Martín, Sergio, Sakamoto, Kazushi, Müller, Sebastien, Tanaka, Kunihiko, Nakanishi, Kouichiro, Herrero-Illana, Rubén, Yoshimura, Yuki, Aladro, Rebeca, Colzi, Laura, Emig, Kimberly L., Henkel, Christian, Nishimura, Yuri, Rivilla, Victor M., Werf, Paul P. van der, European Commission, National Science Foundation (US), National Institutes of Natural Sciences (Japan), Japan Society for the Promotion of Science, Comunidad de Madrid, Agencia Estatal de Investigación (España), Holdship, Jonathan, Mangum, Jeffrey G., Viti, Serena, Behrens, Erica, Harada, Nanase, Martín, Sergio, Sakamoto, Kazushi, Müller, Sebastien, Tanaka, Kunihiko, Nakanishi, Kouichiro, Herrero-Illana, Rubén, Yoshimura, Yuki, Aladro, Rebeca, Colzi, Laura, Emig, Kimberly L., Henkel, Christian, Nishimura, Yuri, Rivilla, Victor M., and Werf, Paul P. van der
Abstract: The cosmic-ray ionization rate (CRIR) is a key parameter in understanding the physical and chemical processes in the interstellar medium. Cosmic rays are a significant source of energy in star formation regions, impacting the physical and chemical processes that drive the formation of stars. Previous studies of the circum-molecular zone of the starburst galaxy NGC 253 have found evidence for a high CRIR value: 103-106 times the average CRIR within the Milky Way. This is a broad constraint, and one goal of this study is to determine this value with much higher precision. We exploit ALMA observations toward the central molecular zone of NGC 253 to measure the CRIR. We first demonstrate that the abundance ratio of H3O+ and SO is strongly sensitive to the CRIR. We then combine chemical and radiative transfer models with nested sampling to infer the gas properties and CRIR of several star-forming regions in NGC 253 from emission from their transitions. We find that each of the four regions modeled has a CRIR in the range (1-80) × 10-14 s-1 and that this result adequately fits the abundances of other species that are believed to be sensitive to cosmic rays, including C2H, HCO+, HOC+, and CO. From shock and photon-dominated/X-ray dominated region models, we further find that neither UV-/X-ray-driven nor shock-dominated chemistry is a viable single alternative as none of these processes can adequately fit the abundances of all of these species.
Published: 2022

3. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Author: Centre National D'Etudes Spatiales (France), National Aeronautics and Space Administration (US), Indian Institue of Astrophysics, Canadian Space Agency, Korea Astronomy and Space Science Institute, National Institutes of Natural Sciences (Japan), Ministerio de Ciencia e Innovación (España), Australian Research Council, European Commission, Boselli, A., Fossati, M., Longobardi, A., Kianfar, K., Dametto, N.Z., Amram, P., Anderson, Joseph P., Andreani, P., Boissier, S., Boquien, Médéric, Buat, Véronique, Consolandi, G., Cortese, Luca, Côté, P., Cuillandre, Jean-Charles, Ferrarese, L., Galbany, Lluís, Gavazzi, G., Gwyn, Stephen, Hensler, G., Hutchings, J., Peng, E. W., Postma, J. F., Roediger, J., Roehlly, Y., Serra, P., Trinchieri, G., Centre National D'Etudes Spatiales (France), National Aeronautics and Space Administration (US), Indian Institue of Astrophysics, Canadian Space Agency, Korea Astronomy and Space Science Institute, National Institutes of Natural Sciences (Japan), Ministerio de Ciencia e Innovación (España), Australian Research Council, European Commission, Boselli, A., Fossati, M., Longobardi, A., Kianfar, K., Dametto, N.Z., Amram, P., Anderson, Joseph P., Andreani, P., Boissier, S., Boquien, Médéric, Buat, Véronique, Consolandi, G., Cortese, Luca, Côté, P., Cuillandre, Jean-Charles, Ferrarese, L., Galbany, Lluís, Gavazzi, G., Gwyn, Stephen, Hensler, G., Hutchings, J., Peng, E. W., Postma, J. F., Roediger, J., Roehlly, Y., Serra, P., and Trinchieri, G.
Abstract: As part of the Virgo Cluster Survey Tracing Ionised Gas Emission, a blind narrow-band H+[NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT, we discovered eight massive (1010 . Mstar . 1011 M) lenticular galaxies with prominent ionised gas emission features in their inner (a few kiloparsec) regions. These features are either ionised gas filaments similar to those observed in cooling flows (two galaxies), or they are thin discs with sizes 0:7 . R(H) . 2:0 kpc (six galaxies), thus significantly smaller than those of the stellar disc (R(H) ' 7 22%Riso(r)). The morphological properties of these discs are similar to those of the dust seen in absorption in high-resolution HST images. Using a unique set of multifrequency data, including new or archival ASTROSAT/UVIT, GALEX, HST, CFHT, Spitzer, and Herschel imaging data, combined with IFU (MUSE, ALMA) and long-slit (SOAR) spectroscopy, we show that while the gas that is located within these inner discs is photoionised by young stars, which signals ongoing star formation, the gas in the filamentary structures is shock ionised. The star formation surface brightness of these discs is similar to that observed in late-type galaxies. Because of their reduced size, however, these lenticular galaxies are located below the main sequence of unperturbed or cluster star-forming systems. By comparing the dust masses measured from absorption maps in optical images, from the Balmer decrement, or estimated by fitting the UV-to-far-IR spectral energy distribution of the target galaxies, we confirm that the dust masses derived from optical attenuation maps are heavily underestimated because of geometrical eects due to the relative distribution of the absorbing dust and the emitting stars. We also show that these galaxies have gas-to-dust ratios of G=D ' 80320 30 , and that the star formation within these discs follows the Schmidt relation, but with an eciency that is reduced by a factor of 2.5. Using our unique set
Published: 2022

4. Organic Molecules in Interstellar Space: Latest advances

Author: European Commission, Ministerio de Ciencia, Innovación y Universidades (España), European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Centre National de la Recherche Scientifique (France), Max Planck Society, Instituto Geográfico Nacional (España), Guélin, Michel, Cernicharo, José, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Centre National de la Recherche Scientifique (France), Max Planck Society, Instituto Geográfico Nacional (España), Guélin, Michel, and Cernicharo, José
Abstract: Although first considered as too diluted for the formation of molecules in-situ and too harsh an environment for their survival, the interstellar medium has turned out to host a rich palette of molecular species: to date, 256 species, not counting isotopologues, have been identified. The last decade, and more particularly the last 2 years, have seen an explosion of new detections, including those of a number of complex organic species, which may be dubbed as prebiotic. Organic molecules have been discovered not just in interstellar clouds from the Solar neighbourhood, but also throughout the Milky-Way, as well as in nearby galaxies, or some of the most distant quasars. These discoveries were made possible by the completion of large sub-millimetre and radio facilities. Equipped with new generation receivers, those instruments have provided the orders of magnitude leap in sensitivity required to detect the vanishingly weak rotational lines that allowed the molecule identifications. Last 2 years, 30 prebiotic molecules have been detected in TMC-1, a dustenshrouded gaseous cloud located at 400 light-years from the Sun in the Taurus constellation. Ten new molecular species, have been identified in the arm of a spiral galaxy seven billion light-yr distant, and 12 molecular species observed in a quasar at 11 billion light-yr. We present the latest spectral observations of this outlying quasar and discuss the implications of those detections in these 3 archetypal sources. The basic ingredients involved in the Miller-Urey experiment and related experiments (H2, H2O, CH4, NH3, CO, H2S, ... ) appeared early after the formation of the first galaxies and are widespread throughout the Universe. The chemical composition of the gas in distant galaxies seems not much different from that in the nearby interstellar clouds. It presumably comprises, like for TMC-1, aromatic rings and complex organic molecules putative precursors of the RNA nucleobases, except the lines of such complex s
Published: 2022

5. Structure and dynamics of the inner nebula around the symbiotic stellar system R Aquarii

Author: Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Centre (Poland), European Commission, National Research Foundation of Korea, European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Bujarrabal, V., Agúndez, Marcelino, Gómez-Garrido, M., Kim, H., Santander-García, M., Alcolea, J., Castro-Carrizo, A., Mikołajewska, J., Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Centre (Poland), European Commission, National Research Foundation of Korea, European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Bujarrabal, V., Agúndez, Marcelino, Gómez-Garrido, M., Kim, H., Santander-García, M., Alcolea, J., Castro-Carrizo, A., and Mikołajewska, J.
Abstract: Aims. We investigate the structure, dynamics, and chemistry of the molecule-rich nebula around the stellar symbiotic system R Aqr, which is significantly affected by the presence of a white dwarf (WD) companion. We study the effects of the strong dynamical interaction between the AGB wind and the WD and of photodissociation by the WD UV radiation on the circumstellar shells. Methods. We obtained high-quality ALMA maps of the 12CO J = 2-1, J = 3-2, and J = 6-5 lines and of 13CO J = 3-2. The maps were analyzed by means of a heuristic 3D model that is able to reproduce the observations. In order to interpret this description of the molecule-rich nebula, we performed sophisticated calculations of hydrodynamical interaction and photoinduced chemistry. Results. We find that the CO-emitting gas is distributed within a relatively small region â‰² 1.″5. Its structure consists of a central dense component plus strongly disrupted outer regions, which seem to be parts of spiral arms that are highly focused on the orbital plane. The structure and dynamics of these spiral arms are compatible with our hydrodynamical calculations. We argue that the observed nebula is the result of the dynamical interaction between the wind and the gravitational attraction of the WD. We also find that UV emission from the hot companion efficiently photodissociates molecules except in the densest and best-shielded regions, that is, in the close surroundings of the AGB star and some shreds of the spiral arms from which the detected lines come. We can offer a faithful description of the distribution of nebular gas in this prototypical source, which will be a useful template for studying material around other tight binary systems.
Published: 2021

6. DEATHSTAR: Nearby AGB stars with the Atacama Compact Array: II. CO envelope sizes and asymmetries: The S-type stars

Author: European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Swedish Research Council, Andriantsaralaza, M., Ramstedt, S., Vlemmings, W.H.T., Danilovich, T., Beck, E. de, Groenewegen, M.A.T., Höfner, S., Kerschbaum, F., Khouri, T., Lindqvist, M., Maercker, M., Olofsson, H., Quintana-Lacaci, G., Saberi, M., Sahai, R., Zijlstra, A., European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Swedish Research Council, Andriantsaralaza, M., Ramstedt, S., Vlemmings, W.H.T., Danilovich, T., Beck, E. de, Groenewegen, M.A.T., Höfner, S., Kerschbaum, F., Khouri, T., Lindqvist, M., Maercker, M., Olofsson, H., Quintana-Lacaci, G., Saberi, M., Sahai, R., and Zijlstra, A.
Abstract: Aims. We aim to constrain the sizes of, and investigate deviations from spherical symmetry in, the CO circumstellar envelopes (CSEs) of 16 S-type stars, along with an additional 7 and 4 CSEs of C-type and M-type AGB stars, respectively. Methods. We map the emission from the CO J = 2-1 and 3-2 lines observed with the Atacama Compact Array (ACA) and its total power (TP) antennas, and fit with a Gaussian distribution in the uv- and image planes for ACA-only and TP observations, respectively. The major axis of the fitted Gaussian for the CO(2-1) line data gives a first estimate of the size of the CO-line-emitting CSE. We investigate possible signs of deviation from spherical symmetry by analysing the line profiles and the minor-to-major axis ratio obtained from visibility fitting, and by investigating the deconvolved images. Results. The sizes of the CO-line-emitting CSEs of low-mass-loss-rate (low-MLR) S-type stars fall between the sizes of the CSEs of C-stars, which are larger, and those of M-stars, which are smaller, as expected because of the differences in their respective CO abundances and the dependence of the photodissociation rate on this quantity. The sizes of the low-MLR S-type stars show no dependence on circumstellar density, as measured by the ratio of the MLR to terminal outflow velocity, irrespective of variability type. The density dependence steepens for S-stars with higher MLRs. While the CO(2-1) brightness distribution size of the low-density S-stars is in general smaller than the predicted photodissociation radius (assuming the standard interstellar radiation field), the measured size of a few of the high-density sources is of the same order as the expected photodissociation radius. Furthermore, our results show that the CO CSEs of most of the S-stars in our sample are consistent with a spherically symmetric and smooth outflow. For some of the sources, clear and prominent asymmetric features are observed which are indicative of intrinsic circumstell
Published: 2021

7. Understanding the Origin of the Magnetic Field Morphology in the Wide-binary Protostellar System BHR 71

Author: ALMA Observatory, Japan Society for the Promotion of Science, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Hull, Charles L. H., Le Gouellec, Valentin J. M., Girart, Josep Miquel, Tobin, John J., Bourke, Tyler L., ALMA Observatory, Japan Society for the Promotion of Science, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Hull, Charles L. H., Le Gouellec, Valentin J. M., Girart, Josep Miquel, Tobin, John J., and Bourke, Tyler L.
Abstract: We present 1.3 mm Atacama Large Millimeter/submillimeter Array observations of polarized dust emission toward the wide-binary protostellar system BHR 71 IRS1 and IRS2. IRS1 features what appears to be a natal, hourglass-shaped magnetic field. In contrast, IRS2 exhibits a magnetic field that has been affected by its bipolar outflow. Toward IRS2, the polarization is confined mainly to the outflow cavity walls. Along the northern edge of the redshifted outflow cavity of IRS2, the polarized emission is sandwiched between the outflow and a filament of cold, dense gas traced by ND, toward which no dust polarization is detected. This suggests that the origin of the enhanced polarization in IRS2 is the irradiation of the outflow cavity walls, which enables the alignment of dust grains with respect to the magnetic field - but only to a depth of ∼300 au, beyond which the dust is cold and unpolarized. However, in order to align grains deep enough in the cavity walls, and to produce the high polarization fraction seen in IRS2, the aligning photons are likely to be in the mid- to far-infrared range, which suggests a degree of grain growth beyond what is typically expected in very young, Class 0 sources. Finally, toward IRS1 we see a narrow, linear feature with a high (10%-20%) polarization fraction and a well-ordered magnetic field that is not associated with the bipolar outflow cavity. We speculate that this feature may be a magnetized accretion streamer; however, this has yet to be confirmed by kinematic observations of dense-gas tracers.
Published: 2020

8. Resolving Linear Polarization due to Emission and Extinction of Aligned Dust Grains on NGC 1333 IRAS4A with JVLA and ALMA

Author: National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Ministerio de Ciencia, Innovación y Universidades (España), Ko, Chialin, Liu, Hauyu Baobab, Lai, Shih-Ping, Ching, Taochung, Rao, Ramprasad, Girart, Josep Miquel, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Ministerio de Ciencia, Innovación y Universidades (España), Ko, Chialin, Liu, Hauyu Baobab, Lai, Shih-Ping, Ching, Taochung, Rao, Ramprasad, and Girart, Josep Miquel
Abstract: We report high angular resolution observations of linearly polarized dust emission toward the Class 0 young stellar object NGC1333 IRAS4A (hereafter IRAS4A) using the Karl G. Jansky Very Large Array at K (11.5-16.7 mm), Ka (8.1-10.3 mm), and Q bands (6.3-7.9 mm), and using the Atacama Large Millimeter Array (ALMA) at Band 6 (1.3 mm) and Band 7 (0.85-0.89 mm). On 100-1000 au scales, all of these observations consistently trace the hourglass-shaped magnetic field topology as shown in the previous studies. In the innermost 100 au region of IRAS4A1, the polarization position angles (E field) detected at 6.3-16.7 mm are consistent; however, they are nearly 90° offset from those detected at 1.3 mm and 0.85-0.89 mm. Such a 90° offset may be explained by the inner ∼100 au area being optically thick at wavelengths shorter than ∼1.5 mm, whereby the observations probe the absorption of aligned dust against the weakly or unpolarized warm dust emission from the innermost region. This can also consistently explain why the highest angular resolution ALMA images at Band 7 show that the polarization percentage increases with dust brightness temperature in the inner ∼100 au region of IRAS4A1. Following this interpretation and assuming that the dust grains are aligned with the magnetic fields, the inferred magnetic field position angle based on the 90° rotated at 6.3-7.9 mm in the central peak of IRAS4A1 is ∼-22°, which is approximately consistent with the outflow direction of ∼-9°.
Published: 2020

9. Magnetic Fields in the Early Stages of Massive Star Formation as Revealed by ALMA

Author: National Natural Science Foundation of China, China Scholarship Council, Ministerio de Economía y Competitividad (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Ministerio de Ciencia e Innovación (España), Liu, Junhao, Zhang, Qizhou, Qiu, Keping, Liu, Hauyu Baobab, Pillai, Thushara G. S., Girart, Josep Miquel, Li, Zhi-Yun, Wang, Ke, National Natural Science Foundation of China, China Scholarship Council, Ministerio de Economía y Competitividad (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Ministerio de Ciencia e Innovación (España), Liu, Junhao, Zhang, Qizhou, Qiu, Keping, Liu, Hauyu Baobab, Pillai, Thushara G. S., Girart, Josep Miquel, Li, Zhi-Yun, and Wang, Ke
Abstract: We present 1.3 mm ALMA dust polarization observations at a resolution of ∼0.02 pc for three massive molecular clumps, MM1, MM4, and MM9, in the infrared dark cloud G28.34+0.06. With these sensitive and high-resolution continuum data, MM1 is resolved into a cluster of condensations. The magnetic field structure in each clump is revealed by the polarized emission. We found a trend of decreasing polarized emission fraction with increasing Stokes I intensities in MM1 and MM4. Using the angular dispersion function method (a modified Davis-Chandrasekhar-Fermi method), the plane-of-sky magnetic field strengths in two massive dense cores, MM1-Core1 and MM4-Core4, are estimated to be ∼1.6 mG and ∼0.32 mG, respectively. The virial parameters in MM1-Core1 and MM4-Core4 are calculated to be ∼0.76 and ∼0.37, respectively, suggesting that massive star formation does not start in equilibrium. Using the polarization-intensity gradient-local gravity method, we found that the local gravity is closely aligned with intensity gradient in the three clumps, and the magnetic field tends to be aligned with the local gravity in MM1 and MM4 except for regions near the emission peak, which suggests that the gravity plays a dominant role in regulating the gas collapse. Half of the outflows in MM4 and MM9 are found to be aligned within 10 of the condensation-scale (<0.05 pc) magnetic field, indicating that the magnetic field could play an important role from condensation to disk scale in the early stage of massive star formation.
Published: 2020

10. ALMA observations of NGC 6334S. I. Forming massive stars and clusters in subsonic and transonic filamentary clouds

Author: National Natural Science Foundation of China, European Commission, Consejo Nacional de Ciencia y Tecnología (México), Ministerio de Ciencia e Innovación (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Academia Sinica (Taiwan), Li, Shanghuo, Zhang, Qizhou, Liu, Hauyu Baobab, Beuther, Henrik, Palau, Aina, Girart, Josep Miquel, Smith, Howard A., Hora, Joseph L., Lin, Yuxing, Qiu, Keping, Strom, Shaye, Wang, J., Li, Fei, Yue, Nannan, National Natural Science Foundation of China, European Commission, Consejo Nacional de Ciencia y Tecnología (México), Ministerio de Ciencia e Innovación (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Academia Sinica (Taiwan), Li, Shanghuo, Zhang, Qizhou, Liu, Hauyu Baobab, Beuther, Henrik, Palau, Aina, Girart, Josep Miquel, Smith, Howard A., Hora, Joseph L., Lin, Yuxing, Qiu, Keping, Strom, Shaye, Wang, J., Li, Fei, and Yue, Nannan
Abstract: We present Atacama Large Millimeter/submillimeter Array (ALMA) and Karl G. Jansky Very Large Array (JVLA) observations of the massive infrared dark cloud NGC 6334S (also known as IRDC G350.56+0.44), located at the southwestern end of the NGC 6334 molecular cloud complex. The HCO and NHD lines covered by the ALMA observations at a ∼3″ angular resolution (∼0.02 pc) reveal that the spatially unresolved nonthermal motions are predominantly subsonic and transonic, a condition analogous to that found in low-mass star-forming molecular clouds. The observed supersonic nonthermal velocity dispersions in massive star-forming regions, often reported in the literature, might be significantly biased by poor spatial resolutions that broaden the observed line widths owing to unresolved motions within the telescope beam. Our 3 mm continuum image resolves 49 dense cores, whose masses range from 0.17 to 14 M . The majority of them are resolved with multiple velocity components. Our analyses of these gas velocity components find an anticorrelation between the gas mass and the virial parameter. This implies that the more massive structures tend to be more gravitationally unstable. Finally, we find that the external pressure in the NGC 6334S cloud is important in confining these dense structures and may play a role in the formation of dense cores and, subsequently, the embedded young stars.
Published: 2020

11. Physical properties of the star-forming clusters in NGC 6334

Author: German Research Foundation, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Sadaghiani, M., Sánchez-Monge, Álvaro, Schilke, Peter, Liu, Hauyu Baobab, Clarke, S. D., Zhang, Qizhou, Girart, Josep Miquel, Seifried, D., Aghababaei, A., Li, Huabai, Juárez, Carmen, Tang, K. S., German Research Foundation, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Sadaghiani, M., Sánchez-Monge, Álvaro, Schilke, Peter, Liu, Hauyu Baobab, Clarke, S. D., Zhang, Qizhou, Girart, Josep Miquel, Seifried, D., Aghababaei, A., Li, Huabai, Juárez, Carmen, and Tang, K. S.
Abstract: [Aims] We aim to characterise certain physical properties of high-mass star-forming sites in the NGC 6334 molecular cloud, such as the core mass function (CMF), spatial distribution of cores, and mass segregation., [Methods] We used the Atacama Large Millimeter/sub-millimeter Array (ALMA) to image the embedded clusters NGC 6334-I and NGC 6334-I(N) in the continuum emission at 87.6 GHz. We achieved a spatial resolution of 1300 au, enough to resolve different compact cores and fragments, and to study the properties of the clusters., [Results] We detected 142 compact sources distributed over the whole surveyed area. The ALMA compact sources are clustered in different regions. We used different machine-learning algorithms to identify four main clusters: NGC 6334-I, NGC 6334-I(N), NGC 6334-I(NW), and NGC 6334-E. The typical separations between cluster members range from 4000 au to 12 000 au. These separations, together with the core masses (0.1–100 M⊙), are in agreement with the fragmentation being controlled by turbulence at scales of 0.1 pc. We find that the CMFs show an apparent excess of high-mass cores compared to the stellar initial mass function. We evaluated the effects of temperature and unresolved multiplicity on the derived slope of the CMF. Based on this, we conclude that the excess of high-mass cores might be spurious and due to inaccurate temperature determinations and/or resolution limitations. We searched for evidence of mass segregation in the clusters and we find that clusters NGC 6334-I and NGC 6334-I(N) show hints of segregation with the most massive cores located in the centre of the clusters., [Conclusions] We searched for correlations between the physical properties of the four embedded clusters and their evolutionary stage (based on the presence of H II regions and infrared sources). NGC 6334-E appears as the most evolved cluster, already harbouring a well-developed H II region. NGC 6334-I is the second-most evolved cluster with an ultra-compact H II region. NGC 6334-I(N) contains the largest population of dust cores distributed in two filamentary structures and no dominant H II region. Finally, NGC 6334-I(NW) is a cluster of mainly low-mass dust cores with no clear signs of massive cores or H II regions. We find a larger separation between cluster members in the more evolved clusters favouring the role of gas expulsion and stellar ejection with evolution. The mass segregation, seen in the NGC 6334-I and NGC 6334-I(N) clusters, suggests a primordial origin for NGC 6334-I(N). In contrast, the segregation in NGC 6334-I might be due to dynamical effects. Finally, the lack of massive cores in the most evolved cluster suggests that the gas reservoir is already exhausted, while the less evolved clusters still have a large gas reservoir along with the presence of massive cores. In general, the fragmentation process of NGC 6334 at large scales (from filament to clump, i.e. at about 1 pc) is likely governed by turbulent pressure, while at smaller scales (scale of cores and sub-fragments, i.e. a few hundred au) thermal pressure starts to be more significant.
Published: 2020

12. DEATHSTAR: Nearby AGB stars with the Atacama Compact Array: I. CO envelope sizes and asymmetries: A new hope for accurate mass-loss-rate estimates

Author: European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, European Space Agency, Ramstedt, S., Vlemmings, W.H.T., Doan, L., Danilovich, T., Lindqvist, M., Saberi, M., Olofsson, H., De Beck, E., Groenewegen, M.A.T., Höfner, S., Kastner, J.H., Kerschbaum, F., Khouri, T., Maercker, M., Montez, R., Quintana-Lacaci, G., Sahai, R., Tafoya, D., Zijlstra, A., European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, European Space Agency, Ramstedt, S., Vlemmings, W.H.T., Doan, L., Danilovich, T., Lindqvist, M., Saberi, M., Olofsson, H., De Beck, E., Groenewegen, M.A.T., Höfner, S., Kastner, J.H., Kerschbaum, F., Khouri, T., Maercker, M., Montez, R., Quintana-Lacaci, G., Sahai, R., Tafoya, D., and Zijlstra, A.
Abstract: Context. This is the first publication from the DEATHSTAR project. The overall goal of the project is to reduce the uncertainties of the observational estimates of mass-loss rates from evolved stars on the Asymptotic Giant Branch (AGB). Aim. The aim in this first publication is to constrain the sizes of the 12CO emitting region from the circumstellar envelopes around 42 mostly southern AGB stars, of which 21 are M-Type and 21 are C-Type, using the Atacama Compact Array (ACA) at the Atacama Large Millimeter/submillimeter Array. The symmetry of the outflows is also investigated. Methods. Line emission from 12CO J = 2→1 and 3→2 from all of the sources were mapped using the ACA. In this initial analysis, the emission distribution was fit to a Gaussian distribution in the uv-plane. A detailed radiative transfer analysis will be presented in a future publication. The major and minor axis of the best-fit Gaussian at the line center velocity of the 12CO J = 2→1 emission gives a first indication of the size of the emitting region. Furthermore, the fitting results, such as the Gaussian major and minor axis, center position, and the goodness of fit across both lines, constrain the symmetry of the emission distribution. For a subsample of sources, the measured emission distribution is compared to predictions from previous best-fit radiative transfer modeling results. Results. We find that the CO envelope sizes are, in general, larger for C-Type than for M-Type AGB stars, which is as expected if the CO/H2 ratio is larger in C-Type stars. Furthermore, the measurements show a relation between the measured (Gaussian) 12CO J = 2→1 size and circumstellar density that, while in broad agreement with photodissociation calculations, reveals large scatter and some systematic differences between the different stellar types. For lower mass-loss-rate irregular and semi-regular variables of both M-and C-Type AGB stars, the 12CO J = 2→1 size appears to be independent of the ratio of the mass-l
Published: 2020

13. Chromospheric LAyer SpectroPolarimeter (CLASP2)

Author: Centre National D'Etudes Spatiales (France), Japan Society for the Promotion of Science, Osaka University, Ministerio de Economía y Competitividad (España), National Aeronautics and Space Administration (US), National Astronomical Observatory of Japan, National Institutes of Natural Sciences (Japan), Narukage, N., Mckenzie, D. E., Asensio Ramos, Andrés, Pino Alemán, T. del, Larruquert, Juan Ignacio, Auchère, Frederic, Leenaarts, J., Carlsson, M. J. L., Centre National D'Etudes Spatiales (France), Japan Society for the Promotion of Science, Osaka University, Ministerio de Economía y Competitividad (España), National Aeronautics and Space Administration (US), National Astronomical Observatory of Japan, National Institutes of Natural Sciences (Japan), Narukage, N., Mckenzie, D. E., Asensio Ramos, Andrés, Pino Alemán, T. del, Larruquert, Juan Ignacio, Auchère, Frederic, Leenaarts, J., and Carlsson, M. J. L.
Abstract: The sounding rocket Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) was launched on September 3rd, 2015, and successfully detected (with a polarization accuracy of 0.1 %) the linear polarization signals (Stokes Q and U) that scattering processes were predicted to produce in the hydrogen Lyman-alpha line (Ly¿; 121.567 nm). Via the Hanle effect, this unique data set may provide novel information about the magnetic structure and energetics in the upper solar chromosphere. The CLASP instrument was safely recovered without any damage and we have recently proposed to dedicate its second flight to observe the four Stokes profiles in the spectral region of the Mg II h and k lines around 280 nm; in these lines the polarization signals result from scattering processes and the Hanle and Zeeman effects. Here we describe the modifications needed to develop this new instrument called the >Chromospheric LAyer SpectroPolarimeter> (CLASP2). © (2016) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Published: 2016

14. Overview of the JET results in support to ITER

Author: Alfredo Pironti, J. Simpson-Hutchinson, Sean Conroy, J. Uljanovs, D. Middleton-Gear, G. Possnert, C. Angioni, R. McAdams, Nicholas Watkins, E. Fortuna-Zalesna, A. Garcia-Carrasco, K. Gałązka, D. Nodwell, Pasquale Gaudio, R.A. Pitts, Svetlana V. Ratynskaia, Seppo Koivuranta, O. J. Kwon, C. Boyd, A. Boboc, M. Reinhart, Igor Lengar, Jarrod Leddy, Hiroyasu Utoh, J. H. Ahn, A. Stevens, J. Lönnroth, U. Kruezi, C. Guillemaut, N. Fonnesu, W. Studholme, Marek Rubel, P. Cahyna, O. McCormack, A. S. Jacobsen, D. Mazon, Gunta Kizane, N. Ashikawa, William Tang, J. Goff, F. Nespoli, Thomas Giegerich, G. Petravich, Angela Busse, Corneliu Porosnicu, M. Bigi, M. Wheatley, Christopher N. Bowman, J. Zacks, Ivan Calvo, U. Losada, H. Weisen, B. Bauvir, Stanislas Pamela, Sylvain Brémond, M.F. Stamp, Scott W. McIntosh, A. Rakha, S. Glöggler, V. Braic, C. Bottereau, S. Murphy, S. Knott, Luigi Fortuna, P. Bunting, N. Vora, S. D. Scott, A. Lazaros, R. Dejarnac, P. Buratti, H.R. Strauss, Gabriele Croci, M. Nocente, A. Hollingsworth, S. Reynolds, D. J. Wilson, D. D. Brown, T.C. Luce, S. Zoletnik, E. Nilsson, L. Laguardia, O. Marchuk, F.P. Orsitto, E. Cecil, V. Huber, J. B. Girardo, Stylianos Varoutis, M. D. Axton, Hyun-Tae Kim, E. Safi, Ch. Day, S. Arshad, J. Rzadkiewicz, P. Prior, A. Meigs, S. Esquembri, P. Gohil, K. Purahoo, Torbjörn Hellsten, N. Tipton, R. Guirlet, E. Joffrin, V. Aldred, Calin Besliu, M. Valentinuzzi, G. T. Jones, J. Edwards, Giuseppe Ambrosino, Laurent Marot, N. Lam, F. Crisanti, G. Verona Rinati, R. Marshal, Michael L. Brown, D. Frigione, D. Chandra, Michaele Freisinger, R. Olney, Jari Varje, S. Whetham, F. Parra Diaz, M. R. Hough, P. Dinca, F. Salzedas, A. Goodyear, R. Gowland, J. A. Wilson, J. Horacek, D. King, K. Flinders, I. R. Merrigan, M. Ghate, R. Michling, F. Saint-Laurent, G. Kocsis, D. Van Eester, C. Young, R. O. Dendy, A. Meakins, N. Pace, C. L. Hunter, D. Alegre, S. Foster, V. Riccardo, M. Bulman, C. Jeong, Marek Szawlowski, B. D. Whitehead, Vasily Kiptily, James Harrison, Hiroshi Tojo, G. T. A. Huijsmans, J. W. Coenen, X. Litaudon, Justin Williams, C. Hidalgo, S. Lesnoj, I.E. Day, A. W. Morris, R. Mooney, Yann Corre, S. Brezinsek, B. Gonçalves, M. Kresina, D. Coombs, F. Köchl, J. L. Gardarein, W. Davis, Aqsa Shabbir, Kanti M. Aggarwal, L. Colas, A. B. Kukushkin, Seppo Sipilä, Elisabeth Rachlew, Leena Aho-Mantila, O. G. Pompilian, E. Viezzer, Shane Cooper, Fabio Villone, P. Blanchard, Patrick Tamain, P. Camp, T. Szabolics, C. Luna, Kalle Heinola, H. G. Esser, V. Bobkov, James Buchanan, Andrew West, Hajime Urano, Roberta Lima Gomes, J.P. Coad, Th. Pütterich, A. Sinha, S. Hollis, R. D. Wood, G. D. Ewart, F. S. Griph, T. Kobuchi, X. Lefebvre, S. Warder, A.J. Thornton, S. Peschanyi, B. Graham, Giuseppe Telesca, M. Kempenaars, J. Bernardo, M. Hughes, Eva Belonohy, S. Schmuck, Kai Nordlund, T. J. Smith, P. Hertout, K. D. Lawson, M. Brix, Matthew Sibbald, Grégoire Hornung, C. Tame, Matthew Carr, S. Wray, P. T. Doyle, A. Somers, Giuseppe Chitarin, D. C. Campling, Mitul Abhangi, I. Jepu, David A. Wood, J. Miettunen, A. Sopplesa, Raffaele Fresa, S. Saarelma, M. Bacharis, J. Pozzi, P. Vallejos Olivares, Teddy Craciunescu, Raffaele Albanese, S. Knipe, Jason P. Byrne, A. C. C. Sips, S. Hazel, V. Kazantzidis, G. Stankūnas, A. Kundu, J. Mailloux, C. Guerard, Pramit Dutta, J. E. Boom, Eduardo Alves, P. Grazier, Saskia Mordijck, V.S. Neverov, Kazuo Hoshino, A. P. Vadgama, P. D. Brennan, P. Innocente, Piergiorgio Sonato, M. Irishkin, M. Berry, D. W. Robson, Dieter Leichtle, Fabio Pisano, P. McCullen, T. M. Huddleston, Kensaku Kamiya, D. Pacella, Tommy Ahlgren, A. Kirschner, B. Magesh, A. Ash, J. Mlynář, C. Castaldo, C. Marchetto, D. L. Hillis, M. Incelli, B. Viola, R. J. Robins, E. Andersson Sundén, G. Ramogida, Matthew Reinke, Gerd Meisl, Yannis Kominis, R. Proudfoot, C. Noble, N. J. Conway, V. P. Lo Schiavo, Jorge Luis Rodriguez, Hugo Bufferand, C. H. A. Hogben, B. Evans, R. Sartori, H. Greuner, M. G. Dunne, K. Schöpf, M. I. K. Santala, E. Giovannozzi, A. E. Shevelev, C. Gil, P. Boulting, P. Sagar, A.E. Shumack, P. A. Coates, C. Ayres, R. Prakash, C. Giroud, M. Parsons, J. C. Giacalone, S. Meshchaninov, A. Peackoc, G. De Temmerman, A.C.A. Figueiredo, D. Gallart, P. Santa, Sergey Popovichev, Ivan Lupelli, M. Valovic, Thomas Johnson, Y. Martynova, M. Rack, Olivier Sauter, J. Garcia, P. Siren, I. Balboa, S. Lee, Hans Nordman, R. Roccella, M. Faitsch, Julien Hillairet, Patrick J. McCarthy, C. Reux, Irena Ivanova-Stanik, V. Coccorese, Ye. O. Kazakov, R. El-Jorf, C. Hamlyn-Harris, Matthias Weiszflog, C. F. Maggi, Panagiotis Tolias, N. C. Hawkes, E. Clark, Bruno Santos, B. Sieglin, R. Rodionov, Roch Kwiatkowski, P. Denner, C. Woodley, Hugh Summers, Francesco Pizzo, G. Pucella, D. Croft, F. Di Maio, M. Tomes, D. Molina, A. Fernades, L. Amicucci, Marco Cecconello, A. Bisoffi, Z. Ul-Abidin, J. Wilkinson, H. Maier, S. Rowe, M. Beckers, P.J. Knight, E. Pajuste, Choong-Seock Chang, K. Deakin, M. Enachescu, A. Cobalt, D. Tskhakaya Jun, Michela Gelfusa, Rémy Nouailletas, R. Ragona, N. Bonanomi, D. A. Homfray, K. Riddle, Yann Camenen, J. D. Thomas, R.P. Doerner, Timothy P. Robinson, Y. Miyoshi, Ph. Jacquet, H. T. Lambertz, D. Pulley, A. Bécoulet, E. Tholerus, O. Bogar, M. Peterka, R. Crowe, C. Sommariva, A. R. Talbot, N. K. Butler, N. Reid, R. Zagórski, Gerald Pintsuk, Juri Romazanov, Andre Neto, G. L. Ravera, Paolo Arena, A. Manning, F. Durodié, Maryna Chernyshova, D. Karkinsky, Štefan Matejčík, J. P. Thomas, A. Wilson, L. Joita, R. Naish, P. Strand, M. Balden, M. Kaufman, T. Powell, V. Schmidt, D. Barnes, José Vicente, S. Doswon, Daniel F. Valcarcel, Claudia Corradino, R. Warren, Annette M. Hynes, J. D. Strachan, A. M. Messiaen, M. Kovari, O. Omolayo, D. M. Witts, R. C. Felton, C. Fleming, C. A. Marren, Patrick Maget, J. Galdon-Quiroga, H. R. Koslowski, Bruce Lipschultz, Ana Elisa Bauer de Camargo Silva, J. Waterhouse, R. J. Dumont, M. Schneider, Sara Moradi, K. J. Nicholls, M. Beldishevski, Benedikt Geiger, A. Jardin, A. Ekedahl, A. Lyssoivan, C. Waldon, Davide Galassi, F. Jaulmes, A. Kirk, Yannick Marandet, F. Hasenbeck, Gabor Szepesi, R. C. Pereira, J. Juul Rasmussen, Nobuyuki Aiba, Michelle E. Walker, Gábor Cseh, Scott W. Mosher, R. Bastow, A. Di Siena, E. Lazzaro, M. Curuia, C. D. Challis, Z. Ghani, J. Deane, João M. C. Sousa, Henrik Sjöstrand, T. O'Gorman, H. R. Wilson, P. Devynck, M. Price, C. A. Thompson, Daniele Marocco, A. Cullen, M. Clark, M. Lennholm, D. Carralero, N. Balshaw, Roland Sabot, I. Stepanov, N. Petrella, Filippo Sartori, L. W. Packer, P. Thomas, M. Lungu, A. V. Krasilnikov, R. Young, Jonathan Graves, J. C. Hillesheim, Mǎdǎlina Vlad, Duccio Testa, Pierre Dumortier, Paulo Carvalho, M. Gosk, Yong-Su Na, M. Buckley, Carlos A. Silva, V. Fuchs, K. Vasava, P. A. Tigwell, B. Wakeling, M. Medland, M. Bellinger, K. Gal, Petter Ström, E. Veshchev, F. Nabais, A. Wynn, L. Lauro Taroni, B. Beckett, L. Gil, M. Towndrow, Brian Grierson, Harry M. Meyer, V. Philipps, A. de Castro, D. Kinna, D. Conka, Göran Ericsson, L. Piron, J. Hawkins, D. Cooper, Kenneth Hammond, V.V. Parail, Cristian Ruset, G.J. van Rooij, M. N. A. Beurskens, N. Fawlk, G. Evison, M. Van De Mortel, N. Marcenko, B. Slade, Th. Franke, Simone Peruzzo, N. den Harder, D. Baião, A. Martin de Aguilera, Frederic Imbeaux, Carlo Sozzi, J.L. de Pablos, J. Svensson, A. Withycombe, Ane Lasa, H. Sheikh, V.A. Yavorskij, Nick Walkden, E. Lerche, C. S. Gibson, Roberto Zanino, Y. Peysson, David Hatch, B. Bazylev, E. de la Cal, S. Hacquin, T. D. V. Haupt, S. A. Silburn, T.T.C. Jones, Maria Teresa Porfiri, Walid Helou, S. E. Sharapov, M. Zerbini, Ken W Bell, Marco Marinelli, Kyriakos Hizanidis, J. M. Fontdecaba, N. Teplova, K. K. Kirov, S. Vartanian, W. W. Pires de Sa, T. C. Hender, J. K. Blackburn, I. Monakhov, H. Patten, P. A. Simmons, Y. Austin, J. Regana, Stefano Coda, Amanda J. Page, D. Fuller, António J.N. Batista, A. Horton, P. Heesterman, S. Cramp, J. Hobirk, F. Clairet, A. Burckhart, M. Allinson, Larry R. Baylor, W. Leysen, D. B. Gin, P. Nielsen, A. Kantor, Yueqiang Liu, A.V. Stephen, Jose Ramon Martin-Solis, P. Mantica, B. C. Regan, Aleksander Drenik, A. Lukin, L. Thorne, G. Nemtsev, J. Denis, M. E. Graham, D. Rigamonti, W. Van Renterghem, M. Tardocchi, M. Koubiti, A. Malaquias, M. Tsalas, A. Cufar, Giuseppe Prestopino, D. Kogut, N. Pomaro, J. Keep, Jochen Linke, Shimpei Futatani, Boris Breizman, A. Sirinelli, M. Chandler, M. Fortune, F. Degli Agostini, I. Jenkins, T. Spelzini, G. Calabrò, O. N. Kent, A. Lunniss, Etienne Hodille, Z. Vizvary, Volker Naulin, T. Eich, F. Mink, A. Alkseev, P. W. Haydon, Massimo Angelone, Norberto Catarino, J. Lapins, Roberto Pasqualotto, R. Lawless, T. Schlummer, F. Bonelli, M. Wischmeier, Stéphane Devaux, G. Saibene, Dirk Reiser, Y. R. Martin, H. Bergsåker, Jon Godwin, Alessia Santucci, C. Lane, Justyna Grzonka, Ph. Mertens, Claudio Verona, David Moulton, E. Delabie, Anna Salmi, P. G. Smith, T. Bolzonella, Silvio Ceccuzzi, Ulrich Fischer, G. Liu, M. A. Henderson, M. Marinucci, T. Suzuki, Jakub Bielecki, João Figueiredo, M. Afzal, J. Cane, Robert Hager, Luciano Bertalot, M. Firdaouss, G. Tvalashvili, D. Hepple, D. Esteve, M. De Bock, Y. Baranov, R. D'Inca, G. De Tommasi, Ch. Linsmeier, T. Nicolas, I. J. Pearson, P. Finburg, Ireneusz Książek, S. Talebzadeh, A. Czarnecka, A. Botrugno, M. Gethins, Bohdan Bieg, R. Baughan, I. Borodkina, B. Kos, A. Muraro, T. Vasilopoulou, G. Hermon, S.J. Wukitch, Jari Likonen, D. P. Coster, Guglielmo Rubinacci, I. H. Coffey, Justine M. Kent, S. E. Dorling, J. Dankowski, Geert Verdoolaege, Daisuke Nishijima, R. Clarkson, E. R. Solano, M. Stephen, A. Lescinskis, P. Staniec, Karl Schmid, M. Mayer, Peter Lang, T. Franklin, M.I. Williams, C. G. Elsmore, F. Maviglia, C. Di Troia, C. Penot, A. Zarins, Pierre Manas, D. F. Gear, Yu Gao, Philipp Drews, E. Letellier, A. S. Thompson, L. Forsythe, I. Zychor, E. Khilkevich, A. Manzanares, T. Nakano, Paulo Rodrigues, J. Edmond, Sebastián Dormido-Canto, R. Dux, C. Appelbee, L. Moser, Angelo Cenedese, D. Fagan, N. Richardson, Giuseppe Gorini, V. Rohde, R. Paprok, João P. S. Bizarro, P. Aleynikov, M. Sertoli, Ł. Świderski, Simone Palazzo, O. W. Davies, D. Douai, N. Macdonald, M. Baruzzo, J. López-Razola, M. Lungaroni, D. Clatworthy, R. Bravanec, J. Lovell, Ambrogio Fasoli, S.-P. Pehkonen, M. E. Puiatti, P. Papp, G. Bodnar, V. Aslanyan, A. Weckmann, K. A. Taylor, R. Henriques, I. T. Chapman, Ewa Pawelec, Miles M. Turner, Steven J. Meitner, M. Bernert, Ph. Maquet, R. C. Meadows, A. Shaw, N. Vianello, L. Barrera Orte, Tomas Markovic, A. Fil, A. S. Couchman, Inessa Bolshakova, J. Fyvie, Konstantina Mergia, J. Gallagher, R.V. Budny, Frank Leipold, C. J. Rapson, R. C. Lobel, Gennady V. Miloshevsky, K.-D. Zastrow, Ph. Duckworth, Gianluca Rubino, G. Withenshaw, S. Maruyama, S. P. Hallworth Cook, M. Newman, Jérôme Bucalossi, P. Drewelow, Nuno Cruz, D. Iglesias, I. Nedzelski, T. Donne, P. Leichuer, R. Cesario, M. D. J. Bright, T. Boyce, N. Imazawa, Per Petersson, R. King, A. Loving, L. Garzotti, Jorge Ferreira, G. Corrigan, D. Sandiford, B. Tal, P. Puglia, Daniel Tegnered, J. Karhunen, James S. Wright, Tom Wauters, J. McKehon, K. Rathod, Olivier Février, Alessandro Formisano, Petra Bilkova, M. Groth, Ricardo Magnus Osorio Galvao, F. Medina, S. Collins, H. J. Boyer, Elena Bruno, Horacio Fernandes, M. J. Stead, R. Paccagnella, J. Kaniewski, Ion E. Stamatelatos, F. Causa, M. F. F. Nave, A. Patel, D. C. McDonald, L. Moreira, Mariano Ruiz, K. Dylst, Raymond A. Shaw, A. Brett, Jane Johnston, P. P. Pereira Puglia, J. Ongena, N. A. Benterman, V. N. Amosov, Christian Grisolia, J. Simpson, C. Perez von Thun, Jan Weiland, P. Tonner, F. Belli, T. Odupitan, T. Dittmar, Edmund Highcock, Taina Kurki-Suonio, I. Uytdenhouwen, Estelle Gauthier, M. Oberkofler, B. Alper, Iris D. Young, S. Soare, Yuji Hatano, D. Reece, D. Borodin, M. Moneti, W. Yanling, S. Mianowski, K. Fenton, Stephen J. Bailey, R. Coelho, Sandra C. Chapman, E. Łaszyńska, A. R. Field, F.J. Martínez, Anders Nielsen, M. Smithies, M. J. Mantsinen, A. J. Capel, N. D. Smith, A. Pires dos Reis, M.-L. Mayoral, T. Loarer, P. Carman, N. Grazier, S. Breton, J. M. A. Bradshaw, Alexandre C. Pereira, Fulvio Auriemma, Fulvio Militello, Barbara Cannas, D. Ulyatt, A. Kappatou, P. Blatchford, R. Scannell, B. I. Oswuigwe, Darren Price, Robert E. Grove, D. Guard, M. Leyland, G. Stubbs, J. W. Banks, V.V. Plyusnin, M. S. J. Rainford, Andrea Murari, Sanjeev Ranjan, A. Huber, V. Krasilnikov, C. Bower, H. Leggate, S. Abduallev, P. Tsavalas, G. Giruzzi, K. Maczewa, Colin Roach, P. Beaumont, R. P. Johnson, Anna Widdowson, L. A. Kogan, A. Baron Wiechec, Markus Airila, J. Morris, Robert Skilton, Katarzyna Słabkowska, M. A. Barnard, Jean-Paul Booth, Alessandro Pau, R. Price, R. Bament, M. Tokitani, I. Turner, T. Vu, P. Huynh, S.N. Gerasimov, D. I. Refy, Yunfeng Liang, Anders Hjalmarsson, S. Dalley, Roberto Ambrosino, O. Hemming, T. R. Blackman, Y. Zhou, Vasile Zoita, P. Vincenzi, A. Loarte, C. Rayner, Martin Imrisek, M. Tripsky, C. Mazzotta, A. Uccello, V. Basiuk, Lide Yao, V. Goloborod'ko, S. Villari, B. P. Duval, N. Bulmer, W. Zhang, L. Hackett, D. N. Borba, M. Halitovs, Mario Pillon, H. Arnichand, Alberto Alfier, A. Lawson, A. Masiello, T. Makkonen, A. Vitins, D. Rendell, D. Paton, L. Avotina, A. Krivska, M. Maslov, Richard Verhoeven, Marc Goniche, A. Broslawski, Marica Rebai, E. de la Luna, E. Militello-Asp, V. Cocilovo, L. Carraro, Michael Fitzgerald, Bernardo B. Carvalho, D. Young, C.G. Lowry, F. J. Casson, L.-G. Eriksson, T. M. Biewer, B. Esposito, F.G. Rimini, J. Fessey, G. Kaveney, S. Hall, Robin Barnsley, Michael Lehnen, N. Bekris, L. F. Ruchko, P. Batistoni, E. Alessi, M. G. O'Mullane, D. S. Darrow, C. N. Grundy, N. Hayter, Ivo S. Carvalho, M. Brombin, Enrico Zilli, M. Valisa, M. Reich, S. Panja, C. Gurl, Charles Harrington, Emmanuele Peluso, M. Porton, Michael Walsh, D. Falie, A. Reed, Jacob Eriksson, P. Macheta, J. M. Faustin, S. Cortes, S. Fietz, P. Piovesan, D. Ciric, Eric Nardon, R. Neu, Bojiang Ding, G.A. Rattá, F. Reimold, R. Craven, M. Cox, J. Orszagh, Aaro Järvinen, A. S. Thrysøe, A. Shepherd, I. Ďuran, Andrew M. Edwards, A. Kinch, J. Beal, M. Gherendi, Martin Köppen, D. Samaddar, P. Dalgliesh, I. Vinyar, J. Jansons, Nengchao Wang, J. Wu, John Wright, S. Wiesen, C. King, Alessandra Fanni, L. D. Horton, N. Krawczyk, J. Buch, K. Krieger, Václav Petržílka, D. Schworer, C. Watts, T. Keenan, Andrea Malizia, B. D. Stevens, P. Trimble, C. P. Lungu, V. Prajapati, Marco Ariola, C. Wellstood, S. Gilligan, Mirko Salewski, Michael Barnes, Florin Spineanu, H. Doerk, C. Kennedy, S. Jachmich, J. Caumont, Isabel L. Nunes, A. Petre, A. Kallenbach, M. Anghel, B. Lomanowski, Marco Riva, M. Romanelli, G. De Masi, T. May-Smith, T. Xu, A. Goussarov, S. Romanelli, M. Okabayashi, A. Baker, R. Salmon, T. Tala, Nicolas Fedorczak, S. Lanthaler, Giuliana Sias, J. Risner, Clarisse Bourdelle, M. E. Manso, Fabio Moro, R. Lucock, M. Bassan, M. T. Ogawa, V. Thompson, A. M. Whitehead, S. D. A. Reyes Cortes, Igor Bykov, Gennady Sergienko, E. Stefanikova, Mattia Frasca, H. Dabirikhah, Lorenzo Frassinetti, N. Dzysiuk, D. L. Keeling, Juan Manuel López, M. Turnyanskiy, Daniel Dunai, David Taylor, Arturo Buscarino, Carolina Björkas, A. Baciero, S. Meigh, M. Garcia-Munoz, Massimiliano Mattei, M. Hill, Gwyndaf Evans, S. Minucci, Xiang Gao, A. V. Chankin, Francesco Romanelli, A. Lahtinen, L. Giacomelli, A. Owen, Jesús Vega, Jonathan Citrin, Antti Hakola, Petr Vondracek, Sehyun Kwak, P. Abreu, L. Meneses, S. S. Medley, G. Gervasini, Surya K. Pathak, Kristel Crombé, M. Cleverly, H.S. Kim, C. Stan-Sion, Nobuyuki Asakura, E. Wang, A. Cardinali, L. Fazendeiro, R. Cavazzana, P. J. Lomas, J. Hawes, G. Stables, Silvia Spagnolo, S. P. Hotchin, N. R. Green, Slawomir Jednorog, Ewa Kowalska-Strzęciwilk, A. Martin, Linwei Li, Rajnikant Makwana, Richard Goulding, I. Voitsekhovitch, M. Bowden, I. Kodeli, Peter Hawkins, S. S. Henderson, Ondrej Ficker, Carl Hellesen, D. Yadikin, Fabio Subba, Luka Snoj, Anthony Laing, N. Ben Ayed, Mario Cavinato, M. Goodliffe, C. Clements, D. Kenny, Axel Klix, S. Gee, R. J. E. Smith, P. de Vries, L. Fittill, Min-Gu Yoo, S. Menmuir, K. Cave-Ayland, S. Potzel, D. Grist, K. Blackman, S. A. Robinson, Rodney Walker, David Pfefferlé, W. Broeckx, D. Harting, S. G. J. Tyrrell, F. Binda, L. Horvath, Davide Flammini, P. V. Edappala, Raul Moreno, G. M. D. Hogeweij, P. Card, A. Hagar, Ion Tiseanu, Rita Lorenzini, L. Appel, Jet Contributors, J. Flanagan, C. Paz Soldan, U. Samm, Otto Asunta, F. Eriksson, C. Taliercio, F. S. Zaitsev, G. F. Matthews, Tuomas Koskela, P. J. Howarth, D. Terranova, M. Skiba, Amanda Hubbard, R. Otin, K. G. McClements, M. Park, R. McKean, C. Christopher Klepper, I. Karnowska, Peter J. Pool, G. Ciraolo, Jennifer M. Lehmann, Institut de Mécanique des Fluides et des Solides (IMFS), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), VTT Technical Research Centre of Finland (VTT), Association EURATOM-TEKES, Association EURATOM-TEKES, Helsinki University of Technology, Finland, Assoc. Euratom-ENEA-CREATE, Universita Mediterranea of Reggio Calabria [Reggio Calabria], EURATOM/CCFE Fusion Association, Culham Science Centre [Abingdon], Instituto Tecnológico e Nuclear (ITN), ITN, University of Naples Federico II = Università degli studi di Napoli Federico II, Max-Planck-Institut für Plasmaphysik [Garching] (IPP), Università degli studi di Catania = University of Catania (Unict), National Institute for Fusion Science (NIFS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ITER organization (ITER), Karlsruhe Institute of Technology (KIT), Institut de Chimie des Substances Naturelles (ICSN), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche sur la Fusion par confinement Magnétique (IRFM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Fusion Development Agreement [Garching bei München] ( EFDA-CSU), Institut d'ophtalmologie Hédi-Rais de Tunis, Service Cardiologie [CHU Toulouse], Pôle Cardiovasculaire et Métabolique [CHU Toulouse], Centre Hospitalier Universitaire de Toulouse (CHU Toulouse)-Centre Hospitalier Universitaire de Toulouse (CHU Toulouse), H. Niewodniczanski Institute of Nuclear Physics, Polska Akademia Nauk = Polish Academy of Sciences (PAN), Laboratoire de recherche en Hydrodynamique, Énergétique et Environnement Atmosphérique (LHEEA), École Centrale de Nantes (ECN)-Centre National de la Recherche Scientifique (CNRS), Euratom/UKAEA Fusion Assoc., Magnetic Sensor laboratory [Lviv] (MSL), National Polytechnic University of Lviv (LPNU), The National Research Nuclear University MEPhI (Moscow Engineering Physics Institute) [Moscow, Russia], Institute of Energy and Climate Research - Plasma Physics (IEK-4), Forschungszentrum Jülich GmbH | Centre de recherche de Juliers, Helmholtz-Gemeinschaft = Helmholtz Association-Helmholtz-Gemeinschaft = Helmholtz Association, Institute for Problems of Material Science, National Academy of Sciences of Ukraine (NASU), Institute of Plasma Physics [Praha], Czech Academy of Sciences [Prague] (CAS), Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Département Méthodes et Modèles Mathématiques pour l'Industrie (3MI-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Centre G2I, Department of Hydraulics, Transportations and Roads, Laboratoire de microbiologie et génétique moléculaires - UMR5100 (LMGM), Centre de Biologie Intégrative (CBI), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Metallurgical & Materials Engineering Department (MS 388), University of Nevada [Reno], AUTRES, Institute of Plasma Physics and Laser Microfusion [Warsaw] (IPPLM), Culham Centre for Fusion Energy (CCFE), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), School of Mathematics [Cardiff], Cardiff University, Associazone EURATOM ENEA sulla Fusione, EURATOM, Laboratoire de physique des plasmas de l'ERM, Laboratorium voor plasmafysica van de KMS (LPP ERM KMS), Ecole Royale Militaire / Koninklijke Militaire School (ERM KMS), Paul-Drude-Institut für Festkörperelektronik (PDI), Institut für Physik, University of Basel (Unibas), Dutch Institute for Fundamental Energy Research [Nieuwegein] (DIFFER), Dutch Institute for Fundamental Energy Research [Eindhoven] (DIFFER), Institut Jean Lamour (IJL), Institut de Chimie du CNRS (INC)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), CEA Cadarache, Dipartimento di Energia [Milano], Politecnico di Milano [Milan] (POLIMI), Laboratoire de Mécanique, Modélisation et Procédés Propres (M2P2), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Lille économie management - UMR 9221 (LEM), Université d'Artois (UA)-Université catholique de Lille (UCL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Euratom research and training programme 633053, Institut de Mécanique des Fluides et des Solides ( IMFS ), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique ( CNRS ), VTT Technical Research Centre of Finland ( VTT ), Univ. Mediterranea RC, Culham Science Centre, Instituto Tecnológico e Nuclear ( ITN ), Università degli studi di Napoli Federico II, Max-Planck-Institut für Plasmaphysik [Garching] ( IPP ), Università degli studi di Catania [Catania], National Institute for Fusion Science, National Institutes of Natural Sciences, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), School of Geography, Earth and Environmental Sciences, ITER Organization, Karlsruhe Institute of Technology ( KIT ), Laboratoire de Nanotechnologie et d'Instrumentation Optique ( LNIO ), Institut Charles Delaunay ( ICD ), Université de Technologie de Troyes ( UTT ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Technologie de Troyes ( UTT ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Chimie des Substances Naturelles ( ICSN ), Centre National de la Recherche Scientifique ( CNRS ), Institut de Recherche sur la Fusion par confinement Magnétique ( IRFM ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), European Fusion Development Agreement [Garching bei München] ( EFDA-CSU ), Service de cardiologie [Toulouse], Université Paul Sabatier - Toulouse 3 ( UPS ) -CHU Toulouse [Toulouse]-Hôpital de Rangueil, ITER [St. Paul-lez-Durance], ITER, Polska Akademia Nauk ( PAN ), Laboratoire de recherche en Hydrodynamique, Énergétique et Environnement Atmosphérique ( LHEEA ), École Centrale de Nantes ( ECN ) -Centre National de la Recherche Scientifique ( CNRS ), MSL, Lviv Polytechnic National University ( MSL ), Lviv Polytechnic National University, Centre d'études et de recherches appliquées à la gestion ( CERAG ), Université Pierre Mendès France - Grenoble 2 ( UPMF ) -Centre National de la Recherche Scientifique ( CNRS ), Institute of Energy and Climate Research - Plasma Physics ( IEK-4 ), Forschungszentrum Jülich GmbH, National Academy of Sciences of Ukraine ( NASU ), Lille - Economie et Management ( LEM ), Université catholique de Lille ( UCL ) -Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Czech Academy of Sciences [Prague] ( ASCR ), Physique des interactions ioniques et moléculaires ( PIIM ), Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Département Méthodes et Modèles Mathématiques pour l'Industrie ( 3MI-ENSMSE ), École des Mines de Saint-Étienne ( Mines Saint-Étienne MSE ), Institut Mines-Télécom [Paris]-Institut Mines-Télécom [Paris]-Centre G2I, Laboratoire de microbiologie et génétique moléculaires ( LMGM ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ), University of Nevada, Institute of Plasma Physics and Laser Microfusion [Warsaw] ( IPPLM ), UCL Department of Space and Climate Physics, University College of London [London] ( UCL ), Astrophysics Research Centre [Belfast] ( ARC ), Queen's University [Belfast] ( QUB ), Laboratoire d'Electronique et des Technologies de l'Information ( CEA-LETI ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes [Saint Martin d'Hères], Cardiff School of Mathematics, Laboratoire de physique des plasmas de l'ERM, Laboratorium voor plasmafysica van de KMS ( LPP ERM KMS ), Ecole Royale Militaire / Koninklijke Militaire School ( ERM KMS ), Paul-Drude-Institut für Festkörperelektronik, University of Basel ( Unibas ), Dutch Institute for Fundamental Energy Research [Nieuwegein] ( DIFFER ), Dutch Institute for Fundamental Energy Research [Eindhoven] ( DIFFER ), Institut Jean Lamour ( IJL ), Centre National de la Recherche Scientifique ( CNRS ) -Université de Lorraine ( UL ), Dipartimento di Energia, Politecnico di Milano [Milan], Max Planck Institute for Plasma Physics, Laboratoire de Mécanique, Modélisation et Procédés Propres ( M2P2 ), Aix Marseille Université ( AMU ) -Ecole Centrale de Marseille ( ECM ) -Centre National de la Recherche Scientifique ( CNRS ), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. ANT - Advanced Nuclear Technologies Research Group, JET Contributors, Litaudon, X, Abduallev, S, Abhangi, M, Abreu, P, Afzal, M, Aggarwal, K, Ahlgren, T, Ahn, J, Aho Mantila, L, Aiba, N, Airila, M, Albanese, R, Aldred, V, Alegre, D, Alessi, E, Aleynikov, P, Alfier, A, Alkseev, A, Allinson, M, Alper, B, Alves, E, Ambrosino, G, Ambrosino, R, Amicucci, L, Amosov, V, Andersson SundÃ©n, E, Angelone, M, Anghel, M, Angioni, C, Appel, L, Appelbee, C, Arena, P, Ariola, M, Arnichand, H, Arshad, S, Ash, A, Ashikawa, N, Aslanyan, V, Asunta, O, Auriemma, F, Austin, Y, Avotina, L, Axton, M, Ayres, C, Bacharis, M, Baciero, A, Baiã¡o, D, Bailey, S, Baker, A, Balboa, I, Balden, M, Balshaw, N, Bament, R, Banks, J, Baranov, Y, Barnard, M, Barnes, D, Barnes, M, Barnsley, R, Baron Wiechec, A, Barrera Orte, L, Baruzzo, M, Basiuk, V, Bassan, M, Bastow, R, Batista, A, Batistoni, P, Baughan, R, Bauvir, B, Baylor, L, Bazylev, B, Beal, J, Beaumont, P, Beckers, M, Beckett, B, Becoulet, A, Bekris, N, Beldishevski, M, Bell, K, Belli, F, Bellinger, M, Belonohy, Ã, Ben Ayed, N, Benterman, N, Bergsã¥ker, H, Bernardo, J, Bernert, M, Berry, M, Bertalot, L, Besliu, C, Beurskens, M, Bieg, B, Bielecki, J, Biewer, T, Bigi, M, Bãlkovã¡, P, Binda, F, Bisoffi, A, Bizarro, J, Bjã¶rkas, C, Blackburn, J, Blackman, K, Blackman, T, Blanchard, P, Blatchford, P, Bobkov, V, Boboc, A, Bodnã¡r, G, Bogar, O, Bolshakova, I, Bolzonella, T, Bonanomi, N, Bonelli, F, Boom, J, Booth, J, Borba, D, Borodin, D, Borodkina, I, Botrugno, A, Bottereau, C, Boulting, P, Bourdelle, C, Bowden, M, Bower, C, Bowman, C, Boyce, T, Boyd, C, Boyer, H, Bradshaw, J, Braic, V, Bravanec, R, Breizman, B, Bremond, S, Brennan, P, Breton, S, Brett, A, Brezinsek, S, Bright, M, Brix, M, Broeckx, W, Brombin, M, Broså‚awski, A, Brown, D, Brown, M, Bruno, E, Bucalossi, J, Buch, J, Buchanan, J, Buckley, M, Budny, R, Bufferand, H, Bulman, M, Bulmer, N, Bunting, P, Buratti, P, Burckhart, A, Buscarino, A, Busse, A, Butler, N, Bykov, I, Byrne, J, Cahyna, P, Calabrã², G, Calvo, I, Camenen, Y, Camp, P, Campling, D, Cane, J, Cannas, B, Capel, A, Card, P, Cardinali, A, Carman, P, Carr, M, Carralero, D, Carraro, L, Carvalho, B, Carvalho, I, Carvalho, P, Casson, F, Castaldo, C, Catarino, N, Caumont, J, Causa, F, Cavazzana, R, Cave Ayland, K, Cavinato, M, Cecconello, M, Ceccuzzi, S, Cecil, E, Cenedese, A, Cesario, R, Challis, C, Chandler, M, Chandra, D, Chang, C, Chankin, A, Chapman, I, Chapman, S, Chernyshova, M, Chitarin, G, Ciraolo, G, Ciric, D, Citrin, J, Clairet, F, Clark, E, Clark, M, Clarkson, R, Clatworthy, D, Clements, C, Cleverly, M, Coad, J, Coates, P, Cobalt, A, Coccorese, V, Cocilovo, V, Coda, S, Coelho, R, Coenen, J, Coffey, I, Colas, L, Collins, S, Conka, D, Conroy, S, Conway, N, Coombs, D, Cooper, D, Cooper, S, Corradino, C, Corre, Y, Corrigan, G, Cortes, S, Coster, D, Couchman, A, Cox, M, Craciunescu, T, Cramp, S, Craven, R, Crisanti, F, Croci, G, Croft, D, Crombã©, K, Crowe, R, Cruz, N, Cseh, G, Cufar, A, Cullen, A, Curuia, M, Czarnecka, A, Dabirikhah, H, Dalgliesh, P, Dalley, S, Dankowski, J, Darrow, D, Davies, O, Davis, W, Day, C, Day, I, De Bock, M, De Castro, A, De La Cal, E, De La Luna, E, De Masi, G, De Pablos, J, De Temmerman, G, De Tommasi, G, De Vries, P, Deakin, K, Deane, J, Degli Agostini, F, Dejarnac, R, Delabie, E, Den Harder, N, Dendy, R, Denis, J, Denner, P, Devaux, S, Devynck, P, Di Maio, F, Di Siena, A, Di Troia, C, Dinca, P, D'Inca, R, Ding, B, Dittmar, T, Doerk, H, Doerner, R, Donnã©, T, Dorling, S, Dormido Canto, S, Doswon, S, Douai, D, Doyle, P, Drenik, A, Drewelow, P, Drews, P, Duckworth, P, Dumont, R, Dumortier, P, Dunai, D, Dunne, M, Äžuran, I, Durodiã©, F, Dutta, P, Duval, B, Dux, R, Dylst, K, Dzysiuk, N, Edappala, P, Edmond, J, Edwards, A, Edwards, J, Eich, T, Ekedahl, A, El Jorf, R, Elsmore, C, Enachescu, M, Ericsson, G, Eriksson, F, Eriksson, J, Eriksson, L, Esposito, B, Esquembri, S, Esser, H, Esteve, D, Evans, B, Evans, G, Evison, G, Ewart, G, Fagan, D, Faitsch, M, Falie, D, Fanni, A, Fasoli, A, Faustin, J, Fawlk, N, Fazendeiro, L, Fedorczak, N, Felton, R, Fenton, K, Fernades, A, Fernandes, H, Ferreira, J, Fessey, J, Fã©vrier, O, Ficker, O, Field, A, Fietz, S, Figueiredo, A, Figueiredo, J, Fil, A, Finburg, P, Firdaouss, M, Fischer, U, Fittill, L, Fitzgerald, M, Flammini, D, Flanagan, J, Fleming, C, Flinders, K, Fonnesu, N, Fontdecaba, J, Formisano, A, Forsythe, L, Fortuna, L, Fortuna Zalesna, E, Fortune, M, Foster, S, Franke, T, Franklin, T, Frasca, M, Frassinetti, L, Freisinger, M, Fresa, R, Frigione, D, Fuchs, V, Fuller, D, Futatani, S, Fyvie, J, Gã¡l, K, Galassi, D, Gaå‚azka, K, Galdon Quiroga, J, Gallagher, J, Gallart, D, Galvã¡o, R, Gao, X, Gao, Y, Garcia, J, Garcia Carrasco, A, GarcÃa MuÃ±oz, M, Gardarein, J, Garzotti, L, Gaudio, P, Gauthier, E, Gear, D, Gee, S, Geiger, B, Gelfusa, M, Gerasimov, S, Gervasini, G, Gethins, M, Ghani, Z, Ghate, M, Gherendi, M, Giacalone, J, Giacomelli, L, Gibson, C, Giegerich, T, Gil, C, Gil, L, Gilligan, S, Gin, D, Giovannozzi, E, Girardo, J, Giroud, C, Giruzzi, G, Glã¶ggler, S, Godwin, J, Goff, J, Gohil, P, Goloborod'Ko, V, Gomes, R, Goncalves, B, Goniche, M, Goodliffe, M, Goodyear, A, Gorini, G, Gosk, M, Goulding, R, Goussarov, A, Gowland, R, Graham, B, Graham, M, Graves, J, Grazier, N, Grazier, P, Green, N, Greuner, H, Grierson, B, Griph, F, Grisolia, C, Grist, D, Groth, M, Grove, R, Grundy, C, Grzonka, J, Guard, D, Guã©rard, C, Guillemaut, C, Guirlet, R, Gurl, C, Utoh, H, Hackett, L, Hacquin, S, Hagar, A, Hager, R, Hakola, A, Halitovs, M, Hall, S, Hallworth Cook, S, Hamlyn Harris, C, Hammond, K, Harrington, C, Harrison, J, Harting, D, Hasenbeck, F, Hatano, Y, Hatch, D, Haupt, T, Hawes, J, Hawkes, N, Hawkins, J, Hawkins, P, Haydon, P, Hayter, N, Hazel, S, Heesterman, P, Heinola, K, Hellesen, C, Hellsten, T, Helou, W, Hemming, O, Hender, T, Henderson, M, Henderson, S, Henriques, R, Hepple, D, Hermon, G, Hertout, P, Hidalgo, C, Highcock, E, Hill, M, Hillairet, J, Hillesheim, J, Hillis, D, 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A., Horáček, J., Hornung, G., Horton, A. R., Horton, L. D., Horvath, L., Hotchin, S. P., Hough, M. R., Howarth, P. J., Hubbard, A., Huber, A., Huber, V., Huddleston, T. M., Hughes, M., Huijsmans, G. T. A., Hunter, C. L., Huynh, P., Hynes, A. M., Iglesias, D., Imazawa, N., Imbeaux, F., Imríšek, M., Incelli, M., Innocente, P., Irishkin, M., Ivanova-Stanik, I., Jachmich, S., Jacobsen, A. S., Jacquet, P., Jansons, J., Jardin, A., Järvinen, A., Jaulmes, F., Jednoróg, S., Jenkins, I., Jeong, C., Jepu, I., Joffrin, E., Johnson, R., Johnson, T., Johnston, Jane, Joita, L., Jones, G., Jones, T. T. C., Hoshino, K. K., Kallenbach, A., Kamiya, K., Kaniewski, J., Kantor, A., Kappatou, A., Karhunen, J., Karkinsky, D., Karnowska, I., Kaufman, M., Kaveney, G., Kazakov, Y., Kazantzidis, V., Keeling, D. L., Keenan, T., Keep, J., Kempenaars, M., Kennedy, C., Kenny, D., Kent, J., Kent, O. N., Khilkevich, E., Kim, H. T., Kim, H. S., Kinch, A., King, C., King, D., King, R. F., Kinna, D. 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W., Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Hôpital de Rangueil, CHU Toulouse [Toulouse]-CHU Toulouse [Toulouse], Laboratoire de microbiologie et génétique moléculaires (LMGM), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Lorraine (UL)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Energia [Milano] (DENG), Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), Research Centre Julich (FZJ), Institute for Plasma Research, Instituto Superior Tecnico Lisboa, Queen's University Belfast, University of Helsinki, CEA, Department of Applied Physics, School services, SCI, National Institutes for Quantum and Radiological Science and Technology, VTT, University of Naples Federico II, Universidad Nacional de Educacion a Distancia, CNR, Russian Research Centre Kurchatov Institute, Universita degli Studi di Napoli Parthenope, Ente Per Le Nuove Tecnologie L'energia e l'ambiente, Troitsk Institute for Innovation and Fusion Research, Uppsala University, National Institute for Cryogenics and Isotopic Technology, Max-Planck-Institut fur Plasmaphysik, University of Catania, Fusion for Energy Joint Undertaking, National Institutes of Natural Sciences - National Institute for Fusion Science, Massachusetts Institute of Technology, University of Latvia, Imperial College London, CIEMAT, University of Oxford, EUROfusion Programme Management Unit, Oak Ridge National Laboratory, Karlsruhe Institute of Technology KIT, University of York, Royal Institute of Technology, Maritime University of Szczecin, H. Niewodniczanski Institute of Nuclear Physics of the Polish Academy of Sciences, Czech Academy of Sciences, University of Trento, Ecole Polytechnique Federale de Lausanne (EPFL), Wigner Research Centre for Physics, Comenius University, University of Milan - Bicocca, National Institute for Optoelectronics, Fourth State Research, University of Texas at Austin, Belgian Nuclear Research Center, National Centre for Nuclear Research (NCBJ), Princeton University, CNRS, University of Cagliari, University of Warwick, Soltan Institute for Nuclear Studies, FOM Institute DIFFER, National Institute for Laser, Plasma and Radiation Physics, Ghent University, J. Stefan Institute, Universite de Lorraine, CAS - Institute of Plasma Physics, University of California at San Diego, Koninklijke Militaire School - Ecole Royale Militaire, Horia Hulubei National Institute of Physics and Nuclear Engineering, Chalmers University of Technology, School services, ELEC, Department of Signal Processing and Acoustics, Automaatio- ja systeemitekniik, Universidad Politecnica de Madrid, Second University of Naples, Warsaw University of Technology, Universita della Basilicata, Barcelona Supercomp. Center, Universidad de Sevilla, Centro Brasileiro de Pesquisas Fisicas, Department of Electrical Engineering and Automation, Sähkötekniikan laitos, University of Rome Tor Vergata, RAS - Ioffe Physico Technical Institute, General Atomics, University of Innsbruck, Fusion and Plasma Physics, University of Toyama, University of Strathclyde, National Technical University of Athens, Universita della Tuscia, Technical University of Denmark, Korea Advanced Institute of Science and Technology, Seoul National University, University College Cork, Vienna University of Technology, University of Opole, Daegu University, National Fusion Research Institute, Dublin City University, Universidad Politécnica de Madrid, PELIN LLC, Arizona State University, Universidad Complutense, University of Basel, Universidad Carlos III de Madrid, Consorzio CREATE, Demokritos National Centre for Scientific Research, Purdue University, Universite Libre de Bruxelles, School Services, ARTS, Department of Design, University of California Office of the President, Universidade de Sao Paulo, School Services, BIZ, Department of Information and Service Management, Lithuanian Energy Institute, HRS Fusion, Politecnico di Torino, University of Cassino, University of Electronic Science and Technology of China, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, and Faculdade de Engenharia
Subjects: Technology, fusion, Física [Ciências exactas e naturais], Tokamak, Nuclear engineering, DIAGNOSTICS, 01 natural sciences, ILW, 010305 fluids & plasmas, law.invention, Ilw, [SPI.MECA.MEFL]Engineering Sciences [physics]/Mechanics [physics.med-ph]/Fluids mechanics [physics.class-ph], Plasma, H-Mode Plasmas, law, ITER, Disruption Prediction, COLLISIONALITY, EDGE LOCALIZED MODES, Diagnostics, Operation, JET, plasma, Nuclear and High Energy Physics, Condensed Matter Physics, Physics, Jet (fluid), JET, plasma, fusion, ITER, Divertor, Settore FIS/01 - Fisica Sperimentale, Fusion, Plasma and Space Physics, DENSITY PEAKING, Carbon Wall, H-MODE PLASMAS, [ SPI.MECA.MEFL ] Engineering Sciences [physics]/Mechanics [physics.med-ph]/Fluids mechanics [physics.class-ph], Density Peaking, Neutron transport, Facing Components, Collisionality, 114 Physical sciences, Física, Física, Nuclear physics, Physical sciences [Natural sciences], Fusion, plasma och rymdfysik, Pedestal, 0103 physical sciences, Nuclear fusion, ddc:530, Neutron, 010306 general physics, Fusion, Physics, Physical sciences, Nuclear and High Energy Physic, Edge Localized Modes, QC717, Física [Àrees temàtiques de la UPC], Reactors de fusió, Física, FACING COMPONENTS, Fusion reactors, Jet, CARBON WALL, DISRUPTION PREDICTION, OPERATION, ddc:600
Abstract: The 2014–2016 JET results are reviewed in the light of their significance for optimising the ITER research plan for the active and non-active operation. More than 60 h of plasma operation with ITER first wall materials successfully took place since its installation in 2011. New multi-machine scaling of the type I-ELM divertor energy flux density to ITER is supported by first principle modelling. ITER relevant disruption experiments and first principle modelling are reported with a set of three disruption mitigation valves mimicking the ITER setup. Insights of the L–H power threshold in Deuterium and Hydrogen are given, stressing the importance of the magnetic configurations and the recent measurements of fine-scale structures in the edge radial electric. Dimensionless scans of the core and pedestal confinement provide new information to elucidate the importance of the first wall material on the fusion performance. H-mode plasmas at ITER triangularity (H = 1 at ßN ~ 1.8 and n/nGW ~ 0.6) have been sustained at 2 MA during 5 s. The ITER neutronics codes have been validated on high performance experiments. Prospects for the coming D–T campaign and 14 MeV neutron calibration strategy are reviewed. This work has been carried out within the framework of the EUROfusion Consortium and has received funding from the Euratom research and training programme 2014–2018 under grant agreement No 633053. Peer Reviewed Article signat per 1.173 autors/es: X. Litaudon35, S. Abduallev39, M. Abhangi46, P. Abreu53, M. Afzal7, K.M. Aggarwal29, T. Ahlgren101, J.H. Ahn8, L. Aho-Mantila112, N. Aiba69, M. Airila112, R. Albanese105, V. Aldred7, D. Alegre93, E. Alessi45, P. Aleynikov55, A. Alfier12, A. Alkseev72, M. Allinson7, B. Alper7, E. Alves53, G. Ambrosino105, R. Ambrosino106, L. Amicucci90, V. Amosov88, E. Andersson Sundén22, M. Angelone90, M. Anghel85, C. Angioni62, L. Appel7, C. Appelbee7, P. Arena30, M. Ariola106, H. Arnichand8, S. Arshad41, A. Ash7, N. Ashikawa68, V. Aslanyan64, O. Asunta1, F. Auriemma12, Y. Austin7, L. Avotina103, M.D. Axton7, C. Ayres7, M. Bacharis24, A. Baciero57, D. Baião53, S. Bailey7, A. Baker7, I. Balboa7, M. Balden62, N. Balshaw7, R. Bament7, J.W. Banks7, Y.F. Baranov7, M.A. Barnard7, D. Barnes7, M. Barnes27, R. Barnsley55, A. Baron Wiechec7, L. Barrera Orte34, M. Baruzzo12, V. Basiuk8, M. Bassan55, R. Bastow7, A. Batista53, P. Batistoni90, R. Baughan7, B. Bauvir55, L. Baylor73, B. Bazylev56, J. Beal110, P.S. Beaumont7, M. Beckers39, B. Beckett7, A. Becoulet8, N. Bekris35, M. Beldishevski7, K. Bell7, F. Belli90, M. Bellinger7, É. Belonohy62, N. Ben Ayed7, N.A. Benterman7, H. Bergsåker42, J. Bernardo53, M. Bernert62, M. Berry7, L. Bertalot55, C. Besliu7, M. Beurskens63, B. Bieg61, J. Bielecki47, T. Biewer73, M. Bigi12, P. Bílková50, F. Binda22, A. Bisoffi31, J.P.S. Bizarro53, C. Björkas101, J. Blackburn7, K. Blackman7, T.R. Blackman7, P. Blanchard33, P. Blatchford7, V. Bobkov62, A. Boboc7, G. Bodnár113, O. Bogar18, I. Bolshakova60, T. Bolzonella12, N. Bonanomi97, F. Bonelli56, J. Boom62, J. Booth7, D. Borba35,53, D. Borodin39, I. Borodkina39, A. Botrugno90, C. Bottereau8, P. Boulting7, C. Bourdelle8, M. Bowden7, C. Bower7, C. Bowman110, T. Boyce7, C. Boyd7, H.J. Boyer7, J.M.A. Bradshaw7, V. Braic87, R. Bravanec40, B. Breizman107, S. Bremond8, P.D. Brennan7, S. Breton8, A. Brett7, S. Brezinsek39, M.D.J. Bright7, M. Brix7, W. Broeckx78, M. Brombin12, A. Brosławski65, D.P.D. Brown7, M. Brown7, E. Bruno55, J. Bucalossi8, J. Buch46, J. Buchanan7, M.A. Buckley7, R. Budny76, H. Bufferand8, M. Bulman7, N. Bulmer7, P. Bunting7, P. Buratti90, A. Burckhart62, A. Buscarino30, A. Busse7, N.K. Butler7, I. Bykov42, J. Byrne7, P. Cahyna50, G. Calabrò90, I. Calvo57, Y. Camenen4, P. Camp7, D.C. Campling7, J. Cane7, B. Cannas17, A.J. Capel7, P.J. Card7, A. Cardinali90, P. Carman7, M. Carr7, D. Carralero62, L. Carraro12, B.B. Carvalho53, I. Carvalho53, P. Carvalho53, F.J. Casson7, C. Castaldo90, N. Catarino53, J. Caumont7, F. Causa90, R. Cavazzana12, K. Cave-Ayland7, M. Cavinato12, M. Cecconello22, S. Ceccuzzi90, E. Cecil76, A. Cenedese12, R. Cesario90, C.D. Challis7, M. Chandler7, D. Chandra46, C.S. Chang76, A. Chankin62, I.T. Chapman7, S.C. Chapman28, M. Chernyshova49, G. Chitarin12, G. Ciraolo8, D. Ciric7, J. Citrin38, F. Clairet8, E. Clark7, M. Clark7, R. Clarkson7, D. Clatworthy7, C. Clements7, M. Cleverly7, J.P. Coad7, P.A. Coates7, A. Cobalt7, V. Coccorese105, V. Cocilovo90, S. Coda33, R. Coelho53, J.W. Coenen39, I. Coffey29, L. Colas8, S. Collins7, D. Conka103, S. Conroy22, N. Conway7, D. Coombs7, D. Cooper7, S.R. Cooper7, C. Corradino30, Y. Corre8, G. Corrigan7, S. Cortes53, D. Coster62, A.S. Couchman7, M.P. Cox7, T. Craciunescu86, S. Cramp7, R. Craven7, F. Crisanti90, G. Croci97, D. Croft7, K. Crombé15, R. Crowe7, N. Cruz53, G. Cseh113, A. Cufar81, A. Cullen7, M. Curuia85, A. Czarnecka49, H. Dabirikhah7, P. Dalgliesh7, S. Dalley7, J. Dankowski47, D. Darrow76, O. Davies7, W. Davis55,76, C. Day56, I.E. Day7, M. De Bock55, A. de Castro57, E. de la Cal57, E. de la Luna57, G. De Masi12, J. L. de Pablos57, G. De Temmerman55, G. De Tommasi105, P. de Vries55, K. Deakin7, J. Deane7, F. Degli Agostini12, R. Dejarnac50, E. Delabie73, N. den Harder38, R.O. Dendy7, J. Denis8, P. Denner39, S. Devaux62,104, P. Devynck8, F. Di Maio55, A. Di Siena62, C. Di Troia90, P. Dinca86, R. D’Inca62, B. Ding51, T. Dittmar39, H. Doerk62, R.P. Doerner9, T. Donné34, S.E. Dorling7, S. Dormido-Canto93, S. Doswon7, D. Douai8, P.T. Doyle7, A. Drenik62,81, P. Drewelow63, P. Drews39, Ph. Duckworth55, R. Dumont8, P. Dumortier58, D. Dunai113, M. Dunne62, I. Ďuran50, F. Durodié58, P. Dutta46, B. P. Duval33, R. Dux62, K. Dylst78, N. Dzysiuk22, P.V. Edappala46, J. Edmond7, A.M. Edwards7, J. Edwards7, Th. Eich62, A. Ekedahl8, R. El-Jorf7, C.G. Elsmore7, M. Enachescu84, G. Ericsson22, F. Eriksson16, J. Eriksson22, L.G. 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Rubino12, L. Ruchko52, M. Ruiz94, C. Ruset86, J. Rzadkiewicz65, S. Saarelma7, R. Sabot8, E. Safi101, P. Sagar7, G. Saibene41, F. Saint-Laurent8, M. Salewski83, A. Salmi112, R. Salmon7, F. Salzedas53, D. Samaddar7, U. Samm39, D. Sandiford7, P. Santa46, M.I.K. Santala1, B. Santos53, A. Santucci90, F. Sartori41, R. Sartori41, O. Sauter33, R. Scannell7, T. Schlummer39, K. Schmid62, V. Schmidt12, S. Schmuck7, M. Schneider8, K. Schöpf102, D. Schwörer32, S.D. Scott76, G. Sergienko39, M. Sertoli62, A. Shabbir15, S.E. Sharapov7, A. Shaw7, R. Shaw7, H. Sheikh7, A. Shepherd7, A. Shevelev54, A. Shumack38, G. Sias17, M. Sibbald7, B. Sieglin62, S. Silburn7, A. Silva53, C. Silva53, P.A. Simmons7, J. Simpson7, J. Simpson-Hutchinson7, A. Sinha46, S.K. Sipilä1, A.C.C. Sips36, P. Sirén112, A. Sirinelli55, H. Sjöstrand22, M. Skiba22, R. Skilton7, K. Slabkowska49, B. Slade7, N. Smith7, P.G. Smith7, R. Smith7, T.J. Smith7, M. Smithies110, L. Snoj81, S. Soare85, E. R. Solano35,57, A. Somers32, C. Sommariva8, P. Sonato12, A. Sopplesa12, J. Sousa53, C. Sozzi45, S. Spagnolo12, T. Spelzini7, F. Spineanu86, G. Stables7, I. Stamatelatos71, M.F. Stamp7, P. Staniec7, G. Stankūnas59, C. Stan-Sion84, M.J. Stead7, E. Stefanikova42, I. Stepanov58, A.V. Stephen7, M. Stephen46, A. Stevens7, B.D. Stevens7, J. Strachan76, P. Strand16, H.R. Strauss44, P. Ström42, G. Stubbs7, W. Studholme7, F. Subba75, H.P. Summers21, J. Svensson63, Ł. Świderski65, T. Szabolics113, M. Szawlowski49, G. Szepesi7, T.T. Suzuki69, B. Tál113, T. Tala112, A.R. Talbot7, S. Talebzadeh95, C. Taliercio12, P. Tamain8, C. Tame7, W. Tang76, M. Tardocchi45, L. Taroni12, D. Taylor7, K.A. Taylor7, D. Tegnered16, G. Telesca15, N. Teplova54, D. Terranova12, D. Testa33, E. Tholerus42, J. Thomas7, J.D. Thomas7, P. Thomas55, A. Thompson7, C.-A. Thompson7, V.K. Thompson7, L. Thorne7, A. Thornton7, A.S. Thrysøe83, P.A. Tigwell7, N. Tipton7, I. Tiseanu86, H. Tojo69, M. Tokitani67, P. Tolias82, M. Tomeš50, P. Tonner7, M. Towndrow7, P. Trimble7, M. Tripsky58, M. Tsalas38, P. Tsavalas71, D. Tskhakaya jun102, I. Turner7, M.M. Turner32, M. Turnyanskiy34, G. Tvalashvili7, S.G.J. Tyrrell7, A. Uccello45, Z. Ul-Abidin7, J. Uljanovs1, D. Ulyatt7, H. Urano69, I. Uytdenhouwen78, A.P. Vadgama7, D. Valcarcel7, M. Valentinuzzi8, M. Valisa12, P. Vallejos Olivares42, M. Valovic7, M. Van De Mortel7, D. Van Eester58, W. Van Renterghem78, G.J. van Rooij38, J. Varje1, S. Varoutis56, S. Vartanian8, K. Vasava46, T. Vasilopoulou71, J. Vega57, G. Verdoolaege58, R. Verhoeven7, C. Verona95, G. Verona Rinati95, E. Veshchev55, N. Vianello45, J. Vicente53, E. Viezzer62,92, S. Villari90, F. Villone100, P. Vincenzi12, I. Vinyar74, B. Viola90, A. Vitins103, Z. Vizvary7, M. Vlad86, I. Voitsekhovitch34, P. Vondráček50, N. Vora7, T. Vu8, W.W. Pires de Sa52, B. Wakeling7, C.W.F. Waldon7, N. Walkden7, M. Walker7, R. Walker7, M. Walsh55, E. Wang39, N. Wang39, S. Warder7, R.J. Warren7, J. Waterhouse7, N.W. Watkins28, C. Watts55, T. Wauters58, A. Weckmann42, J. Weiland23, H. Weisen33, M. Weiszflog22, C. Wellstood7, A.T. West7, M.R. Wheatley7, S. Whetham7, A.M. Whitehead7, B.D. Whitehead7, A.M. Widdowson7, S. Wiesen39, J. Wilkinson7, J. Williams7, M. Williams7, A.R. Wilson7, D.J. Wilson7, H.R. Wilson110, J. Wilson7, M. Wischmeier62, G. Withenshaw7, A. Withycombe7, D.M. Witts7, D. Wood7, R. Wood7, C. Woodley7, S. Wray7, J. Wright7, J.C. Wright64, J. Wu89, S. Wukitch64, A. Wynn110, T. Xu7, D. Yadikin16, W. Yanling39, L. Yao89, V. Yavorskij102, M.G. Yoo80, C. Young7, D. Young7, I.D. Young7, R. Young7, J. Zacks7, R. Zagorski49, F.S. Zaitsev18, R. Zanino75, A. Zarins103, K.D. Zastrow7, M. Zerbini90, W. Zhang62, Y. Zhou42, E. Zilli12, V. Zoita86, S. Zoletnik113, I. Zychor65 and JET Contributorsa // EUROfusion Consortium JET, Culham Science Centre, Abingdon, OX14 3DB, United Kingdom / 1 Aalto University, PO Box 14100, FIN-00076 Aalto, Finland / 2 Aix Marseille Université, CNRS, Centrale Marseille, M2P2 UMR 7340, 13451, Marseille, France / 3 Aix-Marseille Université, CNRS, IUSTI UMR 7343, 13013 Marseille, France / 4 Aix-Marseille Université, CNRS, PIIM, UMR 7345, 13013 Marseille, France / 5 Arizona State University, Tempe, AZ, United States of America / 6 Barcelona Supercomputing Center, Barcelona, Spain / 7 CCFE, Culham Science Centre, Abingdon, Oxon, OX14 3DB, United Kingdom / 8 CEA, IRFM, F-13108 Saint Paul Lez Durance, France / 9 Center for Energy Research, University of California at San Diego, La Jolla, CA 92093, United States of America / 10 Centro Brasileiro de Pesquisas Fisicas, Rua Xavier Sigaud, 160, Rio de Janeiro CEP 22290-180, Brazil / 11 Consorzio CREATE, Via Claudio 21, 80125 Napoli, Italy / 12 Consorzio RFX, corso Stati Uniti 4, 35127 Padova, Italy / 13 Daegu University, Jillyang, Gyeongsan, Gyeongbuk 712-174, Republic of Korea / 14 Departamento de Física, Universidad Carlos III de Madrid, 28911 Leganés, Madrid, Spain / 15 Department of Applied Physics UG (Ghent University) St-Pietersnieuwstraat 41 B-9000 Ghent, Belgium / 16 Department of Earth and Space Sciences, Chalmers University of Technology, SE-41296 Gothenburg, Sweden / 17 Department of Electrical and Electronic Engineering, University of Cagliari, Piazza d’Armi 09123, Cagliari, Italy / 18 Department of Experimental Physics, Faculty of Mathematics, Physics and Informatics Comenius University Mlynska dolina F2, 84248 Bratislava, Slovakia / 19 Department of Materials Science, Warsaw University of Technology, PL-01-152 Warsaw, Poland / 20 Department of Nuclear and Quantum Engineering, KAIST, Daejeon 34141, Korea / 21 Department of Physics and Applied Physics, University of Strathclyde, Glasgow, G4 ONG, United Kingdom / 22 Department of Physics and Astronomy, Uppsala University, SE-75120 Uppsala, Sweden / 23 Department of Physics, Chalmers University of Technology, SE-41296 Gothenburg, Sweden / 24 Department of Physics, Imperial College London, London, SW7 2AZ, United Kingdom / 25 Department of Physics, SCI, KTH, SE-10691 Stockholm, Sweden / 26 Department of Physics, University of Basel, Basel, Switzerland / 27 Department of Physics, University of Oxford, Oxford, OX1 2JD, United Kingdom / 28 Department of Physics, University of Warwick, Coventry, CV4 7AL, United Kingdom / 29 Department of Pure and Applied Physics, Queens University, Belfast, BT7 1NN, United Kingdom / 30 Dipartimento di Ingegneria Elettrica Elettronica e Informatica, Università degli Studi di Catania, 95125 Catania, Italy / 31 Dipartimento di Ingegneria Industriale, University of Trento, Trento, Italy / 32 Dublin City University (DCU), Dublin, Ireland / 33 Ecole Polytechnique Fédérale de Lausanne (EPFL), Swiss Plasma Center (SPC), CH-1015 Lausanne, Switzerland / 34 EUROfusion Programme Management Unit, Boltzmannstr. 2, 85748 Garching, Germany / 35 EUROfusion Programme Management Unit, Culham Science Centre, Culham, OX14 3DB, United Kingdom / 36 European Commission, B-1049 Brussels, Belgium / 37 Fluid and Plasma Dynamics, ULB—Campus Plaine—CP 231 Boulevard du Triomphe, 1050 Bruxelles, Belgium / 38 FOM Institute DIFFER, Eindhoven, Netherlands / 39 Forschungszentrum Jülich GmbH, Institut für Energie- und Klimaforschung—Plasmaphysik, 52425 Jülich, Germany / 40 Fourth State Research, 503 Lockhart Dr, Austin, TX, United States of America / 41 Fusion for Energy Joint Undertaking, Josep Pl. 2, Torres Diagonal Litoral B3, 08019, Barcelona, Spain / 42 Fusion Plasma Physics, EES, KTH, SE-10044 Stockholm, Sweden / 43 General Atomics, PO Box 85608, San Diego, CA 92186-5608, United States of America / 44 HRS Fusion, West Orange, NJ, United States of America / 45 IFP-CNR, via R. Cozzi 53, 20125 Milano, Italy / 46 Institute for Plasma Research, Bhat, Gandhinagar-382 428, Gujarat State, India / 47 Institute of Nuclear Physics, Radzikowskiego 152, 31-342 Kraków, Poland / 48 Institute of Physics, Opole University, Oleska 48, 45-052 Opole, Poland / 49 Institute of Plasma Physics and Laser Microfusion, Hery 23, 01-497 Warsaw, Poland / 50 Institute of Plasma Physics AS CR, Za Slovankou 1782/3, 182 00 Praha 8, Czechia / 51 Institute of Plasma Physics, Chinese Academy of Sciences, Hefei 230031, People’s Republic of China / 52 Instituto de Física, Universidade de São Paulo, Rua do Matão Travessa R Nr.187 CEP 05508-090 Cidade Universitária, São Paulo, Brasil / 53 Instituto de Plasmas e Fusão Nuclear, Instituto Superior Técnico, Universidade de Lisboa, Lisboa, Portugal / 54 Ioffe Physico-Technical Institute, 26 Politekhnicheskaya, St Petersburg 194021, Russian Federation / 55 ITER Organization, Route de Vinon, CS 90 046, 13067 Saint Paul Lez Durance, France / 56 Karlsruhe Institute of Technology, PO Box 3640, D-76021 Karlsruhe, Germany / 57 Laboratorio Nacional de Fusión, CIEMAT, Madrid, Spain / 58 Laboratory for Plasma Physics Koninklijke Militaire School—Ecole Royale Militaire, Renaissancelaan 30 Avenue de la Renaissance B-1000, Brussels, Belgium / 59 Lithuanian energy institute, Breslaujos g. 3, LT-44403, Kaunas, Lithuania / 60 Magnetic Sensor Laboratory, Lviv Polytechnic National University, Lviv, Ukraine / 61 Maritime University of Szczecin, Waly Chrobrego 1-2, 70-500 Szczecin, Poland / 62 Max-Planck-Institut für Plasmaphysik, D-85748 Garching, Germany / 63 Max-Planck-Institut für Plasmaphysik, Teilinsitut Greifswald, D-17491 Greifswald, Germany / 64 MIT Plasma Science and Fusion Centre, Cambridge, MA 02139, United States of America / 65 National Centre for Nuclear Research (NCBJ), 05-400 Otwock-Świerk, Poland / 66 National Fusion Research Institute (NFRI), 169-148 Gwahak-ro, Yuseong-gu, Daejeon 305-806, Republic of Korea / 67 National Institute for Fusion Science, Oroshi, Toki, Gifu 509-5292, Japan / 68 National Institute for Fusion Science, Toki, 509-5292, Japan / 69 National Institutes for Quantum and Radiological Science and Technology, Naka, Ibaraki 311-0193, Japan / 70 National Technical University of Athens, Iroon Politechniou 9, 157 73 Zografou, Athens, Greece / 71 NCSR ‘Demokritos’, 153 10, Agia Paraskevi Attikis, Greece / 72 NRC Kurchatov Institute, 1 Kurchatov Square, Moscow 123182, Russian Federation / 73 Oak Ridge National Laboratory, Oak Ridge, TN 37831-6169, United States of America / 74 PELIN LLC, 27a, Gzhatskaya Ulitsa, Saint Petersburg, 195220, Russian Federation / 75 Politecnico di Torino, Corso Duca degli Abruzzi 24, I-10129 Torino, Italy / 76 Princeton Plasma Physics Laboratory, James Forrestal Campus, Princeton, NJ 08543, United States of America / 77 Purdue University, 610 Purdue Mall, West Lafayette, IN 47907, United States of America / 78 SCK-CEN, Nuclear Research Centre, 2400 Mol, Belgium / 79 Second University of Napoli, Consorzio CREATE, Via Claudio 21, 80125 Napoli, Italy / 80 Seoul National University, Shilim-Dong, Gwanak-Gu, Republic of Korea / 81 Slovenian Fusion Association (SFA), Jozef Stefan Institute, Jamova 39, SI-1000 Ljubljana, Slovenia / 82 Space and Plasma Physics, EES, KTH SE-100 44 Stockholm, Sweden / 83 Technical University of Denmark, Department of Physics, Bldg 309, DK-2800 Kgs Lyngby, Denmark / 84 The ‘Horia Hulubei’ National Institute for Physics and Nuclear Engineering, Magurele-Bucharest, Romania / 85 The National Institute for Cryogenics and Isotopic Technology, Ramnicu Valcea, Romania / 86 The National Institute for Laser, Plasma and Radiation Physics, Magurele-Bucharest, Romania / 87 The National Institute for Optoelectronics, Magurele-Bucharest, Romania / 88 Troitsk Insitute of Innovating and Thermonuclear Research (TRINITI), Troitsk 142190, Moscow Region, Russian Federation / 89 University of Electronic Science and Technology of China, Chengdu, People’s Republic of China / 90 Unità Tecnica Fusione, ENEA C. R. Frascati, via E. Fermi 45, 00044 Frascati (Roma), Italy / 91 Universidad Complutense de Madrid, Madrid, Spain / 92 Universidad de Sevilla, Sevilla, Spain / 93 Universidad Nacional de Educación a Distancia, Madrid, Spain / 94 Universidad Politécnica de Madrid, Grupo I2A2, Madrid, Spain / 95 Università di Roma Tor Vergata, Via del Politecnico 1, Roma, Italy / 96 University College Cork (UCC), Ireland / 97 University Milano-Bicocca, piazza della Scienza 3, 20126 Milano, Italy / 98 University of Basilicata, Consorzio CREATE, Via Claudio 21, 80125 Napoli, Italy / 99 University of California, 1111 Franklin St., Oakland, CA 94607, United States of America / 100 University of Cassino, Consorzio CREATE, Via Claudio 21, 80125 Napoli, Italy / 101 University of Helsinki, PO Box 43, FI-00014 University of Helsinki, Finland / 102 University of Innsbruck, Fusion@Österreichische Akademie der Wissenschaften (ÖAW), Innsbruck, Austria / 103 University of Latvia, 19 Raina Blvd., Riga, LV 1586, Latvia / 104 University of Lorraine, CNRS, UMR7198, YIJL, Nancy, France / 105 University of Napoli ‘Federico II’, Consorzio CREATE, Via Claudio 21, 80125 Napoli, Italy / 106 University of Napoli Parthenope, Consorzio CREATE, Via Claudio 21, 80125 Napoli, Italy / 107 University of Texas at Austin, Institute for Fusion Studies, Austin, TX 78712, United States of America / 108 University of Toyama, Toyama, 930-8555, Japan / 109 University of Tuscia, DEIM, Via del Paradiso 47, 01100 Viterbo, Italy / 110 University of York, Heslington, York YO10 5DD, United Kingdom / 111 Vienna University of Technology, Fusion@Österreichische Akademie der Wissenschaften (ÖAW), Austria / 112 VTT Technical Research Centre of Finland, PO Box 1000, FIN-02044 VTT, Finland / 113 Wigner Research Centre for Physics, PO Box 49, H-1525 Budapest, Hungary
Published: 2017
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15. On the Impact Origin of Phobos and Deimos. IV. Volatile Depletion

Author: Sébastien Charnoz, Francesco C. Pignatale, Hidenori Genda, Ryuki Hyodo, Pascal Rosenblatt, Tokyo Institute of Technology [Tokyo] (TITECH), Earth-Life Science Institute [Tokyo] (ELSI), Institut de Physique du Globe de Paris (IPGP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceJP17J01269JSPS-MAEDI bilateral joint research project (SAKURA program) Astrobiolgy Center of the National Institutes of Natural Sciences, NINS AB291011Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)JP17H02990Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)JP17H06457, and Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science JP17J01269 JSPS-MAEDI bilateral joint research project (SAKURA program) Astrobiolgy Center of the National Institutes of Natural Sciences, NINS AB291011 Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research (KAKENHI) JP17H02990 Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research (KAKENHI) JP17H06457
Subjects: 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, 01 natural sciences, Astrobiology, Martian surface, 0103 physical sciences, planets and satellites: formation, 10. No inequality, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Volatiles, 0105 earth and related environmental sciences, Hydrodynamic escape, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Martian, planets and satellites: individual (Phobos Deimos), planets and satellites: composition, Astronomy and Astrophysics, Moons of Mars, Orbit, Radiation pressure, 13. Climate action, Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Recent works have shown that Martian moons Phobos and Deimos may have accreted within a giant impact-generated disk whose composition is about an equal mixture of Martian material and impactor material. Just after the giant impact, the Martian surface is heated up to $\sim3000-6000$ K and the building blocks of moons, including volatile-rich vapor, are heated up to $\sim2000$ K. In this paper, we investigate the volatile loss from the building blocks of Phobos and Deimos by hydrodynamic escape of vapor and radiation pressure on condensed particles. We show that a non-negligible amount of volatiles ($> 10\%$ of the vapor with temperature $> 1000$ K via hydrodynamic escape, and moderately volatile dusts that condense at $\sim700-2000$ K via radiation pressure) could be removed just after the impact during their first signle orbit from their pericenters to apocenters. Our results indicate that bulk Phobos and Deimos are depleted in volatile elements. Together with future explorations such as JAXA's MMX (Martian Moons eXploration) mission, our results would be used to constrain the origin of Phobos and Deimos., 15 pages, 8 figures. Accepted for publication in ApJ
Published: 2018
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16. On-surface synthesis of disilabenzene-bridged covalent organic frameworks

Author: Kewei Sun, Orlando J. Silveira, Yujing Ma, Yuri Hasegawa, Michio Matsumoto, Satoshi Kera, Ondřej Krejčí, Adam S. Foster, Shigeki Kawai, National Institute for Materials Science, Surfaces and Interfaces at the Nanoscale, National Institutes of Natural Sciences, Institute for Molecular Science, Computational Electronic Structure Theory, University of Tsukuba, Department of Applied Physics, Aalto-yliopisto, and Aalto University
Subjects: General Chemical Engineering, General Chemistry
Abstract: Substituting carbon with silicon in organic molecules and materials has long been an attractive way to modify their electronic structure and properties. Silicon-doped graphene-based materials are known to exhibit exotic properties, yet conjugated organic materials with atomically precise Si substitution have remained difficult to prepare. Here we present the on-surface synthesis of one- and two-dimensional covalent organic frameworks whose backbones contain 1,4-disilabenzene (C4Si2) linkers. Silicon atoms were first deposited on a Au(111) surface, forming a AuSix film on annealing. The subsequent deposition and annealing of a bromo-substituted polyaromatic hydrocarbon precursor (triphenylene or pyrene) on this surface led to the formation of the C4Si2-bridged networks, which were characterized by a combination of high-resolution scanning tunnelling microscopy and photoelectron spectroscopy supported by density functional theory calculations. Each Si in a hexagonal C4Si2 ring was found to be covalently linked to one terminal Br atom. For the linear structure obtained with the pyrene-based precursor, the C4Si2 rings were converted into C4Si pentagonal siloles by further annealing.
Published: 2023

17. Rotational spectroscopy of oxirane-2,2-d2, c-CD2CH2O, and its tentative detection toward IRAS 16293-2422 B

Author: Müller, Holger S. P., Jørgensen, Jes K., Guillemin, Jean-Claude, Lewen, Frank, Schlemmer, Stephan, Universität zu Köln = University of Cologne, University of Copenhagen = Københavns Universitet (UCPH), Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), National Science Foundation, NSF, National Aeronautics and Space Administration, NASA, National Radio Astronomy Observatory, NRAO, Associated Universities, AUI, Centre national d'études spatiales, CNES, National Research Council Canada, NRC, Deutsche Forschungsgemeinschaft, DFG: 184018867, SCHL 341/15-1, National Science Council, NSC, Centre National d’Etudes Spatiales, CNES: 4500065585, Korea Astronomy and Space Science Institute, KASI, National Institutes of Natural Sciences, NINS, National Astronomical Observatory of Japan, NAOJ, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, CEA, and Danmarks Frie Forskningsfond, DFF: 0135-00123B
Subjects: Rotational spectroscopy, Reduced Hamiltonian, FOS: Physical sciences, Interstellar molecule, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), [CHIM]Chemical Sciences, Physics - Atomic and Molecular Clusters, Submillimeter spectroscopy, Astrophysics - Instrumentation and Methods for Astrophysics, Atomic and Molecular Clusters (physics.atm-clus), Molecular symmetry, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We prepared a sample of oxirane doubly deuterated at one C atom and studied its rotational spectrum in the laboratory for the first time between 120~GHz and 1094~GHz. Accurate spectroscopic parameters up to eighth order were determined, and the calculated rest frequencies were used to identify $c$-CD$_2$CH$_2$O tentatively in the interstellar medium in the Atacama Large Millimeter/submillimeter Array Protostellar Interferometric Line Survey (PILS) of the Class 0 protostellar system IRAS 16293$-$2422. The $c$-CD$_2$CH$_2$O to $c$-C$_2$H$_4$O ratio was estimated to be $\sim$0.054 with $T_{\rm rot} = 125$ K. This value translates to a D-to-H ratio of $\sim$0.16 per H atom which is higher by a factor of 4.5 than the $\sim$0.036 per H atom obtained for $c$-C$_2$H$_3$DO. Such increase in the degree of deuteration referenced to one H atom in multiply deuterated isotopologs compared to their singly deuterated variants have been observed commonly in recent years., Comment: Journal of Molecular Spectroscopy, in press; Per Jensen special issue. 12 pages here
Published: 2023
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18. General Relativistic Radiation MHD Simulations of Supercritical Accretion onto a Magnetized Neutron Star: Modeling of Ultraluminous X-Ray Pulsars

Author: Ohsuga, Ken [Division of Theoretical Astronomy, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Mitaka, Tokyo 181-8588 (Japan)]
Published: 2017
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19. Fluorescent H{sub 2} Emission Lines from the Reflection Nebula NGC 7023 Observed with IGRINS

Author: Pyo, Tae-Soo [Subaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NINS), 650 North Aohoku Place, Hilo, HI 96720 (United States)]
Published: 2017
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20. Three-sided pyramid wavefront sensor, part II: preliminary demonstration on the new comprehensive adaptive optics and coronagraph test instrument testbed

Author: Schatz, Lauren, Codona, Johanan, Long, Joseph D., Males, Jared R., Pullen, Weslin, Lumbres, Jennifer, Van Gorkom, Kyle, Chambouleyron, Vincent, Close, Laird M., Correia, Carlos, Fauvarque, Olivier, Fusco, Thierry, Guyon, Olivier, Hart, Michael, Janin-potiron, Pierre, Johnson, Robert, Jovanovic, Nemanja, Mateen, Mala, Sauvage, Jean-francois, Neichel, Benoit, Wyant College of Optical Sciences [University of Arizona], University of Arizona, Hart Scientific Consulting International LLC, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Astrobiology Center of NINS (ABC), National Institutes of Natural Sciences [Tokyo] (NINS), Air Force Research Laboratory (AFRL), United States Air Force (USAF), California Institute of Technology (CALTECH), DOTA, ONERA [Salon], and ONERA
Subjects: instrumentation, [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], Mechanical Engineering, ANALYSE FRONT ONDE, Astronomy and Astrophysics, OPTIQUE ADAPTATIVE, adaptive optics, testbed, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Electronic, Optical and Magnetic Materials, Space and Planetary Science, Control and Systems Engineering, pyramid wavefront sensor, wavefront sensing, Instrumentation
Abstract: International audience; The next generation of giant ground and space telescopes will have the light-collect-ing power to detect and characterize potentially habitable terrestrial exoplanets using high-contrast imaging for the first time. This will only be achievable if the performance of the Giant Segment Mirror Telescopes (GSMTs) extreme adaptive optics (ExAO) systems are opti-mized to their full potential. A key component of an ExAO system is the wavefront sensor (WFS), which measures aberrations from atmospheric turbulence. A common choice in current and next-generation instruments is the pyramid wavefront sensor (PWFS). ExAO systems require high spatial and temporal sampling of wavefronts to optimize performance and, as a result, require large detectors for the WFS. We present a closed-loop testbed demonstration of a three-sided pyramid wavefront sensor (3PWFS) as an alternative to the conventional four-sided pyramid wavefront (4PWFS) sensor for GSMT-ExAO applications on the innovative comprehensive adaptive optics and coronagraph test instrument (CACTI). The 3PWFS is less sensitive to read noise than the 4PWFS because it uses fewer detector pixels. The 3PWFS has further benefits: a high-quality three-sided pyramid optic is easier to manufacture than a four-sided pyramid. We describe the design of the two components of the CACTI system, the adaptive optics simulator and the PWFS testbed that includes both a 3PWFS and 4PWFS. We detail the error budget of the CACTI system, review its operation and calibration procedures, and discuss its current status. A preliminary experiment was performed on CACTI to study the performance of the 3PWFS to the 4PWFS in varying strengths of turbulence using both the raw intensity and slopes map signal processing methods. This experiment was repeated for a modulation radius of 1.6 and 3.25 λ∕D. We found that the performance of the two wavefront sensors is comparable if modal loop gains are tuned.; La prochaine génération de télescopes terrestres et spatiaux géants aura la capacité de collecter la lumière pour détecter et caractériser des exoplanètes terrestres potentiellement habitables en utilisant pour la première fois une imagerie à contraste élevée. Cela ne sera réalisable que si les performances des systèmes d'optique adaptative extrême (ExAO) des télescopes à miroir à segmentés géants (GSMT) sont optimisées à leur plein potentiel. Un composant clé d'un système ExAO est le senseur de front d'onde (WFS), qui mesure les aberrations de la turbulence atmosphérique. Un choix courant dans les instruments actuels et de prochaine génération est le senseur de front d'onde pyramidal (PWFS). Les systèmes ExAO nécessitent un échantillonnage spatial et temporel élevé des fronts d'onde pour optimiser les performances et en conséquence nécessitent des détecteurs de grande taille pour le WFS. Nous présentons une démonstration de banc d'essai en boucle fermée d'un capteur de front d'onde pyramidal à trois côtés (3PWFS) comme alternative au capteur conventionnel de front d'onde pyramidal à quatre côtés (4PWFS) pour les applications GSMT-ExAO sur l'optique adaptative complète innovante et l'instrument de test coronographe ( CACTUS). Le 3PWFS est moins sensible au bruit de lecture que le 4PWFS car il utilise moins de pixels détecteurs. Le 3PWFS a un avantages supplémentaire : une optique pyramidale à trois côtés de haute qualité est plus facile à fabriquer qu'une pyramide à quatre côtés. Nous décrivons la conception des deux composants du système CACTI, le simulateur d'optique adaptative et le banc d'essai PWFS qui comprend à la fois un 3PWFS et un 4PWFS. Nous détaillons le budget d'erreur du système CACTI, passons en revue ses procédures de fonctionnement et d'étalonnage, et discutons de son état actuel. Une expérience préliminaire a été réalisée sur CACTI pour étudier les performances de la 3PWFS à la 4PWFS dans différentes forces de turbulence en utilisant à la fois l'intensité brute et les méthodes de traitement du signal de la carte des pentes. Cette expérience a été répétée pour un rayon de modulation de 1,6 et 3,25 λ∕D. Nous avons constaté que les performances des deux capteurs de front d'onde sont comparables si les gains de boucle modale sont réglés.
Published: 2022
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21. MAPPING THE POLARIZATION OF THE RADIO-LOUD Ly α NEBULA B3 J2330+3927

Author: Matsuda, Yuichi [National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)]
Published: 2017
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22. Upgraded millimeter-wave interferometer for measuring the electron density during the beam extraction in the negative ion source

Author: Kaneko, O. [National Institutes of Natural Sciences, 4-3-13 Toranomon, Minato-ku, Tokyo 105-0001 (Japan)]
Published: 2016
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23. Faraday-cup-type lost fast ion detector on Heliotron J

Author: Kemmochi, N. [National Institute for Fusion Science, National Institutes of Natural Sciences, 322-6 Oroshi, Toki, Gifu 509-5292 (Japan)]
Published: 2016
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24. Energizing Star Formation: The Cosmic-Ray Ionization Rate in NGC 253 Derived from ALCHEMI Measurements of H3O+and SO

Author: Jonathan Holdship, Jeffrey G. Mangum, Serena Viti, Erica Behrens, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, Rebeca Aladro, Laura Colzi, Kimberly L. Emig, Christian Henkel, Yuri Nishimura, Víctor M. Rivilla, Paul P. van der Werf, European Commission, National Science Foundation (US), National Institutes of Natural Sciences (Japan), Japan Society for the Promotion of Science, Comunidad de Madrid, and Agencia Estatal de Investigación (España)
Subjects: Starbust galaxies, Interstellar abundances, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Starburst Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Active galaxies, Astrophysics::Galaxy Astrophysics, Interstellar Medium, Insterstellar medium
Abstract: The cosmic ray ionization rate (CRIR) is a key parameter in understanding the physical and chemical processes in the interstellar medium. Cosmic rays are a significant source of energy in star formation regions, which impacts the physical and chemical processes which drive the formation of stars. Previous studies of the circum-molecular zone (CMZ) of the starburst galaxy NGC 253 have found evidence for a high CRIR value; $10^3-10^6$ times the average cosmic ray ionization rate within the Milky Way. This is a broad constraint and one goal of this study is to determine this value with much higher precision. We exploit ALMA observations towards the central molecular zone of NGC 253 to measure the CRIR. We first demonstrate that the abundance ratio of H$_3$O$^+$ and SO is strongly sensitive to the CRIR. We then combine chemical and radiative transfer models with nested sampling to infer the gas properties and CRIR of several star-forming regions in NGC 253 due to emission from their transitions. We find that each of the four regions modelled has a CRIR in the range $(1-80)\times10^{-14}$ s$^{-1}$ and that this result adequately fits the abundances of other species that are believed to be sensitive to cosmic rays including C$_2$H, HCO$^+$, HOC$^+$, and CO. From shock and PDR/XDR models, we further find that neither UV/X-ray driven nor shock dominated chemistry are a viable single alternative as none of these processes can adequately fit the abundances of all of these species., 24 pages, 15 figures, accepted for publication in ApJ, updated to include changes made for proofs
Published: 2022

25. Organic Molecules in Interstellar Space: Latest advances

Author: Michel Guélin, Jose Cernicharo, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Centre National de la Recherche Scientifique (France), Max Planck Society, and Instituto Geográfico Nacional (España)
Subjects: Prebiotic molecules, Astronomy and Astrophysics, Molecules—ISM, Radio astronomy, Galaxies, Interstellar matter (ISM), Astrochemistry
Abstract: 16 pags., 14 figs., Although first considered as too diluted for the formation of molecules in-situ and too harsh an environment for their survival, the interstellar medium has turned out to host a rich palette of molecular species: to date, 256 species, not counting isotopologues, have been identified. The last decade, and more particularly the last 2 years, have seen an explosion of new detections, including those of a number of complex organic species, which may be dubbed as prebiotic. Organic molecules have been discovered not just in interstellar clouds from the Solar neighbourhood, but also throughout the Milky-Way, as well as in nearby galaxies, or some of the most distant quasars. These discoveries were made possible by the completion of large sub-millimetre and radio facilities. Equipped with new generation receivers, those instruments have provided the orders of magnitude leap in sensitivity required to detect the vanishingly weak rotational lines that allowed the molecule identifications. Last 2 years, 30 prebiotic molecules have been detected in TMC-1, a dustenshrouded gaseous cloud located at 400 light-years from the Sun in the Taurus constellation. Ten new molecular species, have been identified in the arm of a spiral galaxy seven billion light-yr distant, and 12 molecular species observed in a quasar at 11 billion light-yr. We present the latest spectral observations of this outlying quasar and discuss the implications of those detections in these 3 archetypal sources. The basic ingredients involved in the Miller-Urey experiment and related experiments (H2, H2O, CH4, NH3, CO, H2S, ... ) appeared early after the formation of the first galaxies and are widespread throughout the Universe. The chemical composition of the gas in distant galaxies seems not much different from that in the nearby interstellar clouds. It presumably comprises, like for TMC-1, aromatic rings and complex organic molecules putative precursors of the RNA nucleobases, except the lines of such complex species are too weak to be detected that far., J. Cernicharo thanks ERC for funding support through grant ERC-2013-Syg-610256-NANOCOSMOS, and the Ministerio de Ciencia e Innovación of Spain (MICIU) for funding support through projects PID2019-106110GB-I00, PID2019-107115GBC21/AEI/10.130 39/501 100 011 033, and PID2019-106235GB-I00. This paper makes use of ALMA data from project 2017.1.01 232.S, of IRAM NOEMA interferometer data from projects V03E, W19DA and S20BY, and of Yebes 40-m telescope data from projects 19A003, 20A014, 20A017, 20D023, and 21A011. ALMA is a partnership of ESO (representing its member states), NSF (United States) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The Yebes 40-m telescope belongs to Instituto Geografico Nacional (Spain).
Published: 2022

26. Ion-coincidence momentum imaging of three-body Coulomb explosion of formaldehyde in ultrashort intense laser fields

Author: Tseng, C. [Institute for Molecular Science, National Institutes of Natural Sciences, Okazaki, Aichi 444-8585 (Japan)]
Published: 2015
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27. Influence of weak vibrational-electronic couplings on 2D electronic spectra and inter-site coherence in weakly coupled photosynthetic complexes

Author: Ishizaki, Akihito [Institute for Molecular Science, National Institutes of Natural Sciences, Okazaki 444-8585 (Japan)]
Published: 2015
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28. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Author: Boselli, A., Fossati, M., Longobardi, A., Kianfar, K., Dametto, N.Z., Amram, P., Anderson, J. P., Andreani, P., Boissier, S., Boquien, Médéric, Buat, Véronique, Consolandi, G., Cortese, L., Côté, P., Cuillandre, J.C., Ferrarese, L., Galbany, Lluís, Gavazzi, G., Gwyn, Stephen, Hensler, G., Hutchings, J., Peng, E. W., Postma, J. F., Roediger, J., Roehlly, Y., Serra, P., Trinchieri, G., Centre National D'Etudes Spatiales (France), National Aeronautics and Space Administration (US), Indian Institue of Astrophysics, Canadian Space Agency, Korea Astronomy and Space Science Institute, National Institutes of Natural Sciences (Japan), Ministerio de Ciencia e Innovación (España), Australian Research Council, and European Commission
Subjects: Galaxies: elliptical and lenticular, clusters: individual: Virgo [Galaxies], Galaxies: evolution, interactions [Galaxies], clusters: general [Galaxies], Galaxies: clusters: individual: Virgo, evolution [Galaxies], Galaxies: interactions, cD, elliptical and lenticular [Galaxies], Galaxies: ISM, ISM [Galaxies], Galaxies: clusters: general
Abstract: As part of the Virgo Cluster Survey Tracing Ionised Gas Emission, a blind narrow-band H+[NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT, we discovered eight massive (1010 . Mstar . 1011 M) lenticular galaxies with prominent ionised gas emission features in their inner (a few kiloparsec) regions. These features are either ionised gas filaments similar to those observed in cooling flows (two galaxies), or they are thin discs with sizes 0:7 . R(H) . 2:0 kpc (six galaxies), thus significantly smaller than those of the stellar disc (R(H) ' 7 22%Riso(r)). The morphological properties of these discs are similar to those of the dust seen in absorption in high-resolution HST images. Using a unique set of multifrequency data, including new or archival ASTROSAT/UVIT, GALEX, HST, CFHT, Spitzer, and Herschel imaging data, combined with IFU (MUSE, ALMA) and long-slit (SOAR) spectroscopy, we show that while the gas that is located within these inner discs is photoionised by young stars, which signals ongoing star formation, the gas in the filamentary structures is shock ionised. The star formation surface brightness of these discs is similar to that observed in late-type galaxies. Because of their reduced size, however, these lenticular galaxies are located below the main sequence of unperturbed or cluster star-forming systems. By comparing the dust masses measured from absorption maps in optical images, from the Balmer decrement, or estimated by fitting the UV-to-far-IR spectral energy distribution of the target galaxies, we confirm that the dust masses derived from optical attenuation maps are heavily underestimated because of geometrical eects due to the relative distribution of the absorbing dust and the emitting stars. We also show that these galaxies have gas-to-dust ratios of G=D ' 80320 30 , and that the star formation within these discs follows the Schmidt relation, but with an eciency that is reduced by a factor of 2.5. Using our unique set of multifrequency data, we discuss the possible origin of the ionised gas in these objects, which suggests multiple and complex formation scenarios for massive lenticular galaxies in clusters., We acknowledge financial support from “Programme National de Cosmologie and Galaxies” (PNCG) funded by CNRS/INSU-IN2P3-INP, CEA and CNES, France, and from “Projet International de Coopération Scientifique” (PICS) with Canada funded by the CNRS, France. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration and of the GOLDMine database (http://goldmine.mib.infn.it/) (Gavazzi et al. 2003). The UVIT project is collaboration between the following institutes from India: Indian Institute of Astrophysics (IIA), Bengaluru, Inter University Centre for Astronomy and Astrophysics (IUCAA), Pune, and National Centre for Radioastrophysics (NCRA) (TIFR), Pune, and the Canadian Space Agency (CSA). This paper makes use of the following ALMA data: ADS/JAO.ALMA 2013.1.00493.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M.F. has received funding from the European Research Council (ERC) (grant agreement No 757535). N.Z.D. acknowledges partial support from FONDECYT through project 3190769. L.G. acknowledges financial support from the Spanish Ministry of Science and Innovation (MCIN) under the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MCIN project HOSTFLOWS PID2020-115253GA-I00. M.B. gratefully acknowledges support by the ANID BASAL project FB210003 and the FONDECYT regular grant 1211000. L.C. acknowledges support from the Australian Research Council Discovery Project and Future Fellowship funding schemes (DP210100337, FT180100066). Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013.
Published: 2022

29. DEATHSTAR: nearby AGB stars with the Atacama Compact Array II. CO envelope sizes and asymmetries: the S-type stars

Author: M. Andriantsaralaza, Raghvendra Sahai, Taissa Danilovich, Sofia Ramstedt, Hans Olofsson, Martin Groenewegen, Maryam Saberi, Susanne Höfner, Franz Kerschbaum, E. De Beck, Albert A. Zijlstra, Matthias Maercker, Theo Khouri, G. Quintana-Lacaci, Wouter Vlemmings, Michael Lindqvist, European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, and Swedish Research Council
Subjects: SAMPLE, CIRCUMSTELLAR ENVELOPES, Gaussian, Astrophysics, 7. Clean energy, 01 natural sciences, circumstellar matter [Stars], MASS-LOSS RATES, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, winds, outflows [stars], 010303 astronomy & astrophysics, Line (formation), Envelope (waves), Physics, Astrophysics::Instrumentation and Methods for Astrophysics, mass-loss [stars], AGB and post-AGB [stars], Stars: AGB and post AGB, RADIO LINE EMISSION, Astrophysics - Solar and Stellar Astrophysics, Physical Sciences, symbols, Stars: winds, outflows, Circular symmetry, Stars: mass loss, MODELS, FOS: Physical sciences, Astronomy & Astrophysics, Computer Science::Digital Libraries, circumstellar matter, symbols.namesake, 0103 physical sciences, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Science & Technology, 010308 nuclear & particles physics, Astronomy and Astrophysics, PHOTODISSOCIATION, Astrophysics - Astrophysics of Galaxies, Physics::History of Physics, EVOLUTION, Stars, Distribution (mathematics), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), AGB and post AGB [Stars], Stars: circumstellar matter, Outflow, mass loss [Stars]
Abstract: 25 pags., 15 figs., 4 tabs., Aims. We aim to constrain the sizes of, and investigate deviations from spherical symmetry in, the CO circumstellar envelopes (CSEs) of 16 S-type stars, along with an additional 7 and 4 CSEs of C-type and M-type AGB stars, respectively. Methods. We map the emission from the CO J = 2-1 and 3-2 lines observed with the Atacama Compact Array (ACA) and its total power (TP) antennas, and fit with a Gaussian distribution in the uv- and image planes for ACA-only and TP observations, respectively. The major axis of the fitted Gaussian for the CO(2-1) line data gives a first estimate of the size of the CO-line-emitting CSE. We investigate possible signs of deviation from spherical symmetry by analysing the line profiles and the minor-to-major axis ratio obtained from visibility fitting, and by investigating the deconvolved images. Results. The sizes of the CO-line-emitting CSEs of low-mass-loss-rate (low-MLR) S-type stars fall between the sizes of the CSEs of C-stars, which are larger, and those of M-stars, which are smaller, as expected because of the differences in their respective CO abundances and the dependence of the photodissociation rate on this quantity. The sizes of the low-MLR S-type stars show no dependence on circumstellar density, as measured by the ratio of the MLR to terminal outflow velocity, irrespective of variability type. The density dependence steepens for S-stars with higher MLRs. While the CO(2-1) brightness distribution size of the low-density S-stars is in general smaller than the predicted photodissociation radius (assuming the standard interstellar radiation field), the measured size of a few of the high-density sources is of the same order as the expected photodissociation radius. Furthermore, our results show that the CO CSEs of most of the S-stars in our sample are consistent with a spherically symmetric and smooth outflow. For some of the sources, clear and prominent asymmetric features are observed which are indicative of intrinsic circumstellar anisotropy. Conclusions. As the majority of the S-type CSEs of the stars in our sample are consistent with a spherical geometry, the CO envelope sizes obtained in this paper will be used to constrain detailed radiative transfer modelling to directly determine more accurate MLR estimates for the stars in our sample. For several of our sources that present signs of deviation from spherical symmetry, further high-resolution observations would be necessary to investigate the nature of, and the physical processes behind, these asymmetrical structures. This will provide further insight into the mass-loss process and its related chemistry in S-type AGB stars., This paper makes use of the following ALMA data: ADS/JAO.ALMA#2018.1.01434.S; ADS/JAO.ALMA#2017.1.00595.S and ADS/JAO.ALMA#2012.1.00524.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. MA acknowledges support from the Nordic ALMA Regional Centre (ARC) node based at Onsala Space Observatory. The Nordic ARC node is funded through Swedish Research Council grant No 2017-00648. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme under grant agreements No. 883867 [EXWINGS] and 730562 [RadioNet].
Published: 2021

30. Photon-induced positron annihilation lifetime spectroscopy using ultrashort laser-Compton-scattered gamma-ray pulses

Author: Katoh, M. [UVSOR, Institute for Molecular Science, National Institutes of Natural Sciences, Myodaiji-cho, Okazaki, Aichi 444-8585 (Japan)]
Published: 2013
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31. Ten years of collaborative progress in the Quest for Orthologs

Author: Linard, B. (Benjamin), Ebersberger, I. (Ingo), McGlynn, S. (SE), Glover, N. (Natacha M), Mochizuki, T. (T), Patricio, M. (Mateus), Lecompte, O. (Odile), Nevers, Y. (Yannis), Thomas, P. (Paul D), Gabaldon, T., Sonnhammer, E. (Erik), Dessimoz, C., Uchiyama, I. (I), Méthodes et Algorithmes pour la Bioinformatique (MAB), Laboratoire d'Informatique de Robotique et de Microélectronique de Montpellier (LIRMM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), Goethe-University Frankfurt am Main, Tokyo Institute of Technology [Tokyo] (TITECH), University of Lausanne (UNIL), European Bioinformatics Institute [Hinxton] (EMBL-EBI), EMBL Heidelberg, Université de Strasbourg (UNISTRA), University of Southern California (USC), Barcelona Institute of Science and Technology (BIST), Stockholm University, National Institutes of Natural Sciences [Tokyo] (NINS), and QFO Consortium
Subjects: AcademicSubjects/SCI01130, gene models, Review, AcademicSubjects/SCI01180, [SDV.BID.SPT]Life Sciences [q-bio]/Biodiversity/Systematics, Phylogenetics and taxonomy, Informatique [cs]/Intelligence artificielle [cs.AI], phylogenetic profiling, ddc:570, [SDV.BBM.GTP]Life Sciences [q-bio]/Biochemistry, Molecular Biology/Genomics [q-bio.GN], viruses, orthology, xenology, [INFO.INFO-BI]Computer Science [cs]/Bioinformatics [q-bio.QM], [SDE.BE]Environmental Sciences/Biodiversity and Ecology, paralogy
Abstract: International audience; Accurate determination of the evolutionary relationships between genes is a foundational challenge in biology. Homology — evolutionary relatedness — is in many cases readily determined based on sequence similarity analysis. By contrast, whether or not two genes directly descended from a common ancestor by a speciation event (orthologs) or duplication event (paralogs) is more challenging, yet provides critical information on the history of a gene. Since 2009, this task has been the focus of the Quest for Orthologs (QFO) consortium. The 6th QFO meeting took place in Okazaki, Japan in conjunction with the 67th National Institute for Basic Biology conference. Here we report recent advances, applications, and oncoming challenges that were discussed during the conference. Steady progress has been made toward standardisation and scalability of new and existing tools. A feature of the conference was the presentation of a panel of accessible tools for phylogenetic profiling and several developments to bring orthology beyond the gene unit—from domains to networks. This meeting brought into light several challenges to come: leveraging orthology computations to get the most of the incoming avalanche of genomic data, integrating orthology from domain to biological network levels, building better gene models, and adapting orthology approaches to the broad evolutionary and genomic diversity recognized in different forms of life and viruses.
Published: 2021
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32. Origin of Intense Electron Heating in Relativistic Blast Waves

Author: Arno Vanthieghem, Martin Lemoine, Laurent Gremillet, Institut Lagrange de Paris, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), National Institutes of Natural Sciences [Tokyo] (NINS), Department of Astrophysical Sciences [Princeton], Princeton University, SLAC National Accelerator Laboratory (SLAC), Stanford University, DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire Matière sous Conditions Extrêmes (LMCE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, the NSF grants PHY-1804048 and AST-1814708, A0030407666 made by GENCI and on CORI at the National Energy Research Scientific Computing Center (NERSC) through ALCC award, ANR-10-LABX-0063,ILP,Institute Lagrange of Paris(2010), ANR-11-IDEX-0004,SUPER,Sorbonne Universités à Paris pour l'Enseignement et la Recherche(2011), ANR-14-CE33-0019,MACH,Micro-Astro-CHocs(2014), and ANR-20-CE30-0030,UnRIP,Vers la compréhension des instabilités plasma relativistes(2020)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Plasma Physics (physics.plasm-ph), Physics::Plasma Physics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, FOS: Physical sciences, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], Physics - Plasma Physics
Abstract: The modeling of gamma-ray burst afterglow emission bears witness to strong electron heating in the precursor of Weibel-mediated, relativistic collisionless shock waves propagating in unmagnetized electron-ion plasmas. In this Letter, we propose a theoretical model, which describes electron heating via a Joule-like process caused by pitch-angle scattering in the decelerating, self-induced microturbulence and the coherent charge-separation field induced by the difference in inertia between electrons and ions. The emergence of this electric field across the precursor of electron-ion shocks is confirmed by large-scale particle-in-cell (PIC) simulations. Integrating the model using a Monte Carlo-Poisson method, we compare the main observables to the PIC simulations to conclude that the above mechanism can indeed account for the bulk of electron heating., Comment: 9 pages, 8 figures; to be published in Astrophysical Journal Letters
Published: 2022
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33. Structure and dynamics of the inner nebula around the symbiotic stellar system R Aqr

Author: M. Santander-García, A. Castro-Carrizo, Hyosun Kim, M. Gómez-Garrido, Valentin Bujarrabal, Marcelino Agúndez, J. Alcolea, Joanna Mikolajewska, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), National Science Centre (Poland), European Commission, National Research Foundation of Korea, European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Academia Sinica (Taiwan), and Korea Astronomy and Space Science Institute
Subjects: symbiotic [Binaries], R Aquarii, Structure (category theory), FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, Binaries: close, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Nebula, 010308 nuclear & particles physics, Binaries: symbiotic, Dynamics (mechanics), Stars: AGB and post-AGB, Astronomy and Astrophysics, AGB and post-AGB [Stars], Circumstellar matter, Astrophysics - Astrophysics of Galaxies, Stars: individual: R Aqr, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), individual: R Aqr [Stars], Astrophysics::Earth and Planetary Astrophysics, close [Binaries]
Abstract: 17 pags., 16 figs., Aims. We investigate the structure, dynamics, and chemistry of the molecule-rich nebula around the stellar symbiotic system R Aqr, which is significantly affected by the presence of a white dwarf (WD) companion. We study the effects of the strong dynamical interaction between the AGB wind and the WD and of photodissociation by the WD UV radiation on the circumstellar shells. Methods. We obtained high-quality ALMA maps of the 12CO J = 2-1, J = 3-2, and J = 6-5 lines and of 13CO J = 3-2. The maps were analyzed by means of a heuristic 3D model that is able to reproduce the observations. In order to interpret this description of the molecule-rich nebula, we performed sophisticated calculations of hydrodynamical interaction and photoinduced chemistry. Results. We find that the CO-emitting gas is distributed within a relatively small region â‰² 1.″5. Its structure consists of a central dense component plus strongly disrupted outer regions, which seem to be parts of spiral arms that are highly focused on the orbital plane. The structure and dynamics of these spiral arms are compatible with our hydrodynamical calculations. We argue that the observed nebula is the result of the dynamical interaction between the wind and the gravitational attraction of the WD. We also find that UV emission from the hot companion efficiently photodissociates molecules except in the densest and best-shielded regions, that is, in the close surroundings of the AGB star and some shreds of the spiral arms from which the detected lines come. We can offer a faithful description of the distribution of nebular gas in this prototypical source, which will be a useful template for studying material around other tight binary systems., This work has been supported by the Spanish MICINN, grants AYA2016-78994-P, AYA2016-75066-C2-1-P, PID2019- 105203GB-C2, PID2019-106110GB-I00, and PID2019-107115GB-C21, and by the National Science Centre, Poland, grant OPUS 2017/27/B/ST9/01940. M.A. acknowledges funding support from the Ramón y Cajal programme of Spanish MICIU (grant RyC-2014-16277) and from the European Research Council (ERC Grant 610256: NANOCOSMOS). H.K. acknowledges support by the National Research Foundation of Korea (NRF), grant funded by the Korea government (MIST) (No. 2021R1A2C1008928). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.00363.S and 2018.1.00638.S. ALMA is a partnership of ESO (representing its member more states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.
Published: 2021
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34. Origin of subgap current in an SIS junction

Author: Matsuo, Hiroshi [National Institutes of Natural Sciences/National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588 (Japan)]
Published: 2009
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35. Rotational spectroscopic study of S-methyl thioformate: A global laboratory analysis of ground and excited torsional states up to 660 GHz

Author: Isabelle Kleiner, Roman A. Motiyenko, Jean-Claude Guillemin, Laurent Margulès, Belén Tercero, José Cernicharo, Eugene A. Alekseev, Atef Jabri, Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique des Lasers, Atomes et Molécules - UMR 8523 (PhLAM), Université de Lille-Centre National de la Recherche Scientifique (CNRS), Physique Moléculaire aux Interfaces (PMI), Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université de Lille, Institut des Sciences Chimiques de Rennes (ISCR), Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA), Grant, Centre National d’Etudes Spatiales, ERC-2013Syg-610256-NANOCOSMOS, ERC, AYA2012-32032, MINECO, ASTROMOL CSD 2009-00038, CONSOLIDER-Ingenio, SPECTRORIMI, PCMI/CEA/CNRS, travel Grants, GDR SPECMO 3152, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), National Science Foundation (US), European Southern Observatory, National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, ALMA Observatory, National Astronomical Observatory of Japan, National Radio Astronomy Observatory (US), Institut national des sciences de l'Univers (France), Centre National de la Recherche Scientifique (France), Max Planck Society, Instituto Geográfico Nacional (España), European Commission, Ministerio de Economía y Competitividad (España), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), and Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Methyl formate, laboratory: molecular [Methods], methods: laboratory: molecular, Context (language use), Astrophysics, 7. Clean energy, 01 natural sciences, Molecular physics, Article, ISM: abundances, chemistry.chemical_compound, 0103 physical sciences, identification [Line], Spectroscopy, 010303 astronomy & astrophysics, Physics, abundances [ISM], [PHYS]Physics [physics], 010304 chemical physics, Spectrometer, ISM [Submillimeter], Astronomy and Astrophysics, Catalogues, Interstellar medium, chemistry, Space and Planetary Science, Excited state, submillimeter: ISM, Ground state, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Microwave, line: identification, catalogs
Abstract: 9 pags., 3 figs., 6 tabs., Context. S-methyl thioformate CH3SC(O)H is a monosulfur derivative of methyl formate, a relatively abundant component of the interstellar medium (ISM). S-methyl thioformate being, thermodynamically, the most stable isomer, it can be reasonably proposed for detection in the ISM. Aims. This work aims to experimentally study and theoretically analyze the ground and first torsional excited states for CH3SC(O)H in a large spectral range for astrophysical use. Methods. S-methyl thioformate was synthesized as a result of a reaction of methyl mercaptan with acetic-formic anhydride. The millimeter-wave spectrum was then recorded for the first time from 150 to 660 GHz with the solid-state spectrometer located at Lille. Results. A set of 3545 lines is determined and combined with 54 previously measured lines in the microwave region, belonging to ground state νt = 0 as well as 1391 transitions in the first excited state of torsion ν18 = 1. Some 164 lines were also assigned to ν18 = 2 for the A-species. A global fit was performed using the BELGI-Cs code taking into account the large splitting of A and E lines due to methyl internal rotation motion with a relatively low barrier, V3 = 127.4846(15) cm-1. Conclusions. Using our spectroscopy work, a deep search of S-methyl thioformate was carried out in the IRAM 30 m and ALMA data of different high-mass star-forming regions (Orion KL and Sgr B2). We derived an upper limit to the CH3SC(O)H column density in these regions., This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00009.SV. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The results are also based on observations obtained with the IRAM 30 m telescope supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). This work was supported by the Programme National Physique et Chimie du Milieu Intestellaire (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES. B.T. and J.C. thank the ERC for support under grant ERC-2013-Syg-610 256- NANOCOSMOS and the Spanish MINECO for funding support under grants AYA2012-32032 and FIS2014-52172-C2, and the CONSOLIDER-Ingenio program “ASTROMOL” CSD 2009-00038. J.-C.G. thanks the Centre National d’Etudes Spatiales (CNES) for a grant.
Published: 2020
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36. DEATHSTAR: Nearby AGB stars with the Atacama Compact Array: I. CO envelope sizes and asymmetries: A new hope for accurate mass-loss-rate estimates

Author: Matthias Maercker, Franz Kerschbaum, Martin Groenewegen, Hans Olofsson, Susanne Höfner, Daniel Tafoya, L. Doan, Rodolfo Montez, Theo Khouri, Taissa Danilovich, Wouter Vlemmings, E. De Beck, Raghvendra Sahai, Albert A. Zijlstra, Sofia Ramstedt, G. Quintana-Lacaci, Maryam Saberi, Michael Lindqvist, Joel H. Kastner, European Southern Observatory, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, and European Space Agency
Subjects: CIRCUMSTELLAR ENVELOPES, PERIOD, FOS: Physical sciences, Context (language use), Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, 01 natural sciences, Submillimeter Array, outflows, 0103 physical sciences, Radiative transfer, Asymptotic giant branch, Astrophysics::Solar and Stellar Astrophysics, winds [stars], winds, outflows [Stars], Stars: mass-loss, GIANT BRANCH STARS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Envelope (waves), Line (formation), Physics, Science & Technology, mass-loss [Stars], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Stars: AGB and post-AGB, Astronomy and Astrophysics, AGB and post-AGB [Stars], Circumstellar matter, Astrophysics - Astrophysics of Galaxies, Physics::History of Physics, RADIO LINE EMISSION, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, Outflow, Stars: winds, outflows
Abstract: 28 pags., 10 figs., 7 tabs., Context. This is the first publication from the DEATHSTAR project. The overall goal of the project is to reduce the uncertainties of the observational estimates of mass-loss rates from evolved stars on the Asymptotic Giant Branch (AGB). Aim. The aim in this first publication is to constrain the sizes of the 12CO emitting region from the circumstellar envelopes around 42 mostly southern AGB stars, of which 21 are M-Type and 21 are C-Type, using the Atacama Compact Array (ACA) at the Atacama Large Millimeter/submillimeter Array. The symmetry of the outflows is also investigated. Methods. Line emission from 12CO J = 2→1 and 3→2 from all of the sources were mapped using the ACA. In this initial analysis, the emission distribution was fit to a Gaussian distribution in the uv-plane. A detailed radiative transfer analysis will be presented in a future publication. The major and minor axis of the best-fit Gaussian at the line center velocity of the 12CO J = 2→1 emission gives a first indication of the size of the emitting region. Furthermore, the fitting results, such as the Gaussian major and minor axis, center position, and the goodness of fit across both lines, constrain the symmetry of the emission distribution. For a subsample of sources, the measured emission distribution is compared to predictions from previous best-fit radiative transfer modeling results. Results. We find that the CO envelope sizes are, in general, larger for C-Type than for M-Type AGB stars, which is as expected if the CO/H2 ratio is larger in C-Type stars. Furthermore, the measurements show a relation between the measured (Gaussian) 12CO J = 2→1 size and circumstellar density that, while in broad agreement with photodissociation calculations, reveals large scatter and some systematic differences between the different stellar types. For lower mass-loss-rate irregular and semi-regular variables of both M-and C-Type AGB stars, the 12CO J = 2→1 size appears to be independent of the ratio of the mass-loss rate to outflow velocity, which is a measure of circumstellar density. For the higher mass-loss-rate Mira stars, the 12CO J = 2→1 size clearly increases with circumstellar density, with larger sizes for the higher CO-Abundance C-Type stars. The M-Type stars appear to be consistently smaller than predicted from photodissociation theory. The majority of the sources have CO envelope sizes that are consistent with a spherically symmetric, smooth outflow, at least on larger scales. For about a third of the sources, indications of strong asymmetries are detected. This is consistent with what was found in previous interferometric investigations of northern sources. Smaller scale asymmetries are found in a larger fraction of sources. Conclusions. These results for CO envelope radii and shapes can be used to constrain detailed radiative transfer modeling of the same stars so as to determine mass-loss rates that are independent of photodissociation models. For a large fraction of the sources, observations at higher spatial resolution will be necessary to deduce the nature and origin of the complex circumstellar dynamics revealed by our ACA observations., This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.2.00025.S and #2017.1.00595.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www. cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/ consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
Published: 2020

37. Lignans in knotwood of Norway spruce

Author: Mansikkala, Tuomas, Patanen, Minna, Kärkönen, Anna, Korpinen, Risto, Pranovich, Andrey, Ohigashi, Takuji, Swaraj, Sufal, Seitsonen, Jani, Ruokolainen, Janne, Huttula, Marko, Saranpää, Pekka, Piispanen, Riikka, University of Oulu, Luke Natural Resources Institute Finland, Åbo Akademi University, National Institutes of Natural Sciences, Institute for Molecular Science, CNRS, Department of Applied Physics, Aalto-yliopisto, and Aalto University
Subjects: Cryosectioning, Extractives, Picea abies, Knotwood, STEM-EDS, STXM, Hydroxymatairesinol, Lignin, Osmium tetroxide, Resin-embedding
Abstract: openaire: EC/H2020/730872/EU//CALIPSOplus Lignans are bioactive compounds that are especially abundant in the Norway spruce (Picea abies L. Karst.) knotwood. By combining a variety of chromatographic, spectroscopic and imaging techniques, we were able to quantify, qualify and localise the easily extractable lignans in the xylem tissue. The knotwood samples contained 15 different lignans according to the gas chromatography-mass spectrometry analysis. They comprised 16% of the knotwood dry weight and 82% of the acetone extract. The main lignans were found to be hydroxymatairesinols HMR1 and HMR2. Cryosectioned and resin-embedded ultrathin sections of the knotwood were analysed with scanning transmission X-ray microscopy (STXM). Cryosectioning was found to retain only lignan residues inside the cell lumina. In the resin-embedded samples, lignan was interpreted to be unevenly distributed inside the cell lumina, and partially confined in deposits which were either readily present in the lumina or formed when OsO4 used in staining reacted with the lignans.Furthermore, the multi-technique characterisation enabled us to obtain information on the chemical composition of the structural components of knotwood. A simple spectral analysis of the STXM data gave consistent results with the gas chromatographic methods about the relative amounts of cell wall components (lignin and polysaccharides). The STXM analysis also indicated that a torus of a bordered pit contained aromatic compounds, possibly lignin.
Published: 2020

38. On-sky verification of Fast and Furious focal-plane wavefront sensing: Moving forward toward controlling the island effect at Subaru/SCExAO

Author: Christoph U. Keller, Olivier Guyon, Nemanja Jovanovic, Sébastien Vievard, Julien Lozi, Frantz Martinache, Steven P. Bos, Frans Snik, Michael J. Wilby, Barnaby Norris, Jean-François Sauvage, Leiden University, Rapenburg 70, Leiden, 2311 EZ, Netherlands, National Astronomical Observatory of Japan, Subaru Telescope, 650 North Aohoku Place, Hilo, HI 96720, United States, Astrobiology center, National Institutes of Natural sciences, Tokyo, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Leiden Observatory, Leiden University, The Netherlands, National Astronomical Observatory of Japan, Subaru Telescope, 650 North A‘ohoku Place, Hilo, HI 96720, United States, Sydney Astrophotonic Instrumentation Labs, University of Sydney, Australia, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Observatoire de la Cte d’Azur, 96 Boulevard de l’Observatoire, Nice, 06300, France, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, and Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
Subjects: Point spread function, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, 010309 optics, [SPI]Engineering Sciences [physics], Optics, Distortion, 0103 physical sciences, Adaptive optics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Optical path length, instrumentation, [PHYS]Physics [physics], Physics, Wavefront, Earth and Planetary Astrophysics (astro-ph.EP), business.industry, Strehl ratio, Astronomy and Astrophysics, Wavefront sensor, adaptive optics -instrumentation, Space and Planetary Science, business, Astrophysics - Instrumentation and Methods for Astrophysics, high angular resolution, Astrophysics - Earth and Planetary Astrophysics
Abstract: High-contrast imaging (HCI) observations of exoplanets can be limited by the island effect (IE). On the current generation of telescopes, the IE becomes a severe problem when the ground wind speed is below a few meters per second. This is referred to as the low-wind effect (LWE). The LWE severely distorts the point spread function (PSF), significantly lowering the Strehl ratio and degrading the contrast. In this article, we aim to show that the focal-plane wavefront sensing (FPWFS) algorithm, Fast and Furious (F&F), can be used to measure and correct the IE/LWE. We deployed the algorithm on the SCExAO HCI instrument at the Subaru Telescope using the internal near-infrared camera in H-band. We tested F&F with the internal source, and it was deployed on-sky to test its performance with the full end-to-end system and atmospheric turbulence. The performance of the algorithm was evaluated by two metrics based on the PSF quality: 1) the Strehl ratio approximation ($SRA$), and 2) variance of the normalized first Airy ring ($VAR$). Random LWE phase screens with a peak-to-valley wavefront error between 0.4 $��$m and 2 $��$m were all corrected to a $SRA$ $>$90\% and an $VAR\lessapprox0.05$. Furthermore, the on-sky results show that F&F is able to improve the PSF quality during very challenging atmospheric conditions (1.3-1.4'' seeing at 500 nm). Closed-loop tests show that F&F is able to improve the $VAR$ from 0.27 to 0.03 and therefore significantly improve the symmetry of the PSF. Simultaneous observations of the PSF in the {optical} ($��= $ 750 nm, $��=$ 50 nm) show that during these tests we were correcting aberrations common to the optical and NIR paths within SCExAO. Going forward, the algorithm is suitable for incorporation into observing modes, which will enable PSFs of higher quality and stability during science observations., Accepted for publication in A&A. Abstract shortened for arXiv
Published: 2020
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39. ERGO: Breaking Down the Wall between Human Health and Environmental Testing of Endocrine Disrupters

Author: Marieke Reuver, Lisa Baumann, Gerrit Schüürmann, Martin Hansen, Dries Knapen, Frédéric Flamant, Marc Léonard, Taisen Iguchi, Klára Hilscherová, Werner Kloas, Volker Strauss, Peter Matthiessen, Henrik Holbech, Juergen Arning, Laurent Sachs, Department of Biology, University of Southern Denmark (SDU), Old School House, Centre for Environmental Research, AquaTT, Partenaires INRAE, Inflammasome NLRP3 – NLRP3 Inflammasome, Centre International de Recherche en Infectiologie - UMR (CIRI), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Physiologie moléculaire et adaptation (PhyMA), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Department of Endocrinology, Humboldt-Universität zu Berlin, Research Centre for Toxic Compounds in the Environment [Brno] (RECETOX / MUNI), Faculty of Science [Brno] (SCI / MUNI), Masaryk University [Brno] (MUNI)-Masaryk University [Brno] (MUNI), L'Oréal Research, L'OREAL, Okazaki Institute for Integrative Bioscience, National Institute for Basic Biology, National Institutes of Natural Sciences, Matthiessen Consultancy, Aarhus University [Aarhus], Department Community Ecology [UFZ Leipzig], Helmholtz Zentrum für Umweltforschung = Helmholtz Centre for Environmental Research (UFZ), Technishe Universität Bergakademie Freiberg (TU Bergakademie Freiberg), University of Antwerp (UA), Institut de Génomique Fonctionnelle de Lyon (IGFL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Leibniz-Institut für Gewässerökologie und Binnenfischerei (IGB), Leibniz Association, Masaryk University [Brno] (MUNI), L'Oréal Recherche France (L'Oréal Recherche), German Federal Environmental Agency / Umweltbundesamt (UBA), BASF SE, Yokohama City University (YCU), and Heidelberg University
Subjects: 0301 basic medicine, Integrated approach to testing and assessment, Cross species extrapolation, Endocrine Disruptors, integrated approach to testing and assessment, 010501 environmental sciences, 01 natural sciences, test guideline, Workflow, lcsh:Chemistry, Human health, Adverse Outcome Pathway, Animal testing, [SDV.BDD]Life Sciences [q-bio]/Development Biology, lcsh:QH301-705.5, ComputingMilieux_MISCELLANEOUS, Spectroscopy, thyroid hormone disruption, General Medicine, endocrine disruption, Computer Science Applications, adverse outcome pathway, Chemistry, OECD, %22">Fish , Biological Assay, Health Impact Assessment, Thyroid hormone disruption, cross-species extrapolation, Environmental Monitoring, Project Report, Endocrine disruption, In silico, Endocrine System, Computational biology, Biology, Risk Assessment, Catalysis, Inorganic Chemistry, Economic cooperation, 03 medical and health sciences, Adverse outcome pathway, Species Specificity, Data Warehousing, Animals, Humans, Endocrine system, Physical and Theoretical Chemistry, Molecular Biology, AOP, 0105 earth and related environmental sciences, Test guideline, Organic Chemistry, Health Plan Implementation, biomarkers, 030104 developmental biology, lcsh:Biology (General), lcsh:QD1-999, IATA
Abstract: International audience; ERGO (EndocRine Guideline Optimization) is the acronym of a European Union-funded research and innovation action, that aims to break down the wall between mammalian and non-mammalian vertebrate regulatory testing of endocrine disruptors (EDs), by identifying, developing and aligning thyroid-related biomarkers and endpoints (B/E) for the linkage of effects between vertebrate classes. To achieve this, an adverse outcome pathway (AOP) network covering various modes of thyroid hormone disruption (THD) in multiple vertebrate classes will be developed. The AOP development will be based on existing and new data from in vitro and in vivo experiments with fish, amphibians and mammals, using a battery of different THDs. This will provide the scientifically plausible and evidence-based foundation for the selection of B/E and assays in lower vertebrates, predictive of human health outcomes. These assays will be prioritized for validation at OECD (Organization for Economic Cooperation and Development) level. ERGO will re-think ED testing strategies from in silico methods to in vivo testing and develop, optimize and validate existing in vivo and early life-stage OECD guidelines, as well as new in vitro protocols for THD. This strategy will reduce requirements for animal testing by preventing duplication of testing in mammals and non-mammalian vertebrates and increase the screening capacity to enable more chemicals to be tested for ED properties.
Published: 2020
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40. A Pivotal Genetic Program Controlled by Thyroid Hormone during the Maturation of GABAergic Neurons

Author: Le Maire, Albane, Bouhours-Nouet, Natacha, Soamalala, Jessica, Mirebeau-Prunier, Delphine, Paloni, Matteo, Guee, Laura, Héron, Delphine, Mignot, Cyril, Illouz, Frederic, Joubert, Florence, Briet, Claire, Rodien, Patrice, Bourguet, William, Holbech, Henrik, Matthiessen, Peter, Hansen, Martin, Schuurmann, Gerrit, Knapen, Dries, Reuver, Marieke, Sachs, Laurent, Kloas, Werner, Hilscherova, Klara, Léonard, Marc, Arning, Jürgen, Strauss, Volker, Iguchi, Taisen, Baumann, Lisa, Richard, Sabine, Guyot, Romain, Rey-Millet, Martin, Prieux, Margaux, Markossian, Suzy, Aubert, Denise, Flamant, Frédéric, Centre de Biochimie Structurale [Montpellier] (CBS), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de la Santé et de la Recherche Médicale (INSERM), Physiopathologie Cardiovasculaire et Mitochondriale (MITOVASC), Université d'Angers (UA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Groupe de recherche clinique 'déficience intellectuelle et autisme', Université Pierre et Marie Curie - Paris 6 (UPMC), CHU Trousseau [APHP], Service d'Endocrinologie, Diabétologie et Nutrition [CHU Angers], Centre Hospitalier Universitaire d'Angers (CHU Angers), PRES Université Nantes Angers Le Mans (UNAM)-PRES Université Nantes Angers Le Mans (UNAM), Université Grenoble Alpes - UFR Médecine [ ?-2019] (UGA UFRM [ ?-2019]), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), PRES Université Nantes Angers Le Mans (UNAM), Department of Biology, University of Southern Denmark (SDU), Old School House, Centre for Environmental Research, AquaTT, Partenaires INRAE, Evolution des régulations endocriniennes (ERE), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Department of Endocrinology, Humboldt-Universität zu Berlin, Research Centre for Toxic Compounds in the Environment (RECETOX), Masaryk University, L'Oréal Research, L'OREAL, Okazaki Institute for Integrative Bioscience, National Institute for Basic Biology, National Institutes of Natural Sciences, Unité de recherches Avicoles, Institut National de la Recherche Agronomique (INRA), Institut de Génomique Fonctionnelle de Lyon (IGFL), École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Unité mixte de recherche biologie moléculaire de la cellule, and École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDV.BDD]Life Sciences [q-bio]/Development Biology
Published: 2020
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41. Polarized emission by aligned grains in the Mie regime: Application to protoplanetary disks observed by ALMA

Author: Felipe O. Alves, Josep M. Girart, Anaëlle Maury, Vincent Guillet, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Max-Planck-Institut für Extraterrestrische Physik (MPE), Programme National PCMI of CNRS/INSU, European Project: 679937,H2020,ERC-2015-STG,MagneticYSOs(2016), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Smithsonian Institution-Harvard University [Cambridge], Ministerio de Ciencia, Innovación y Universidades (España), Max Planck Society, European Commission, National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, National Science Council (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), and Harvard University [Cambridge]-Smithsonian Institution
Subjects: FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, planetary systems [Submillimeter], Polarization, 0103 physical sciences, Rayleigh scattering, 010303 astronomy & astrophysics, Spinning, Astrophysics::Galaxy Astrophysics, Physics, polarization, 010308 nuclear & particles physics, extinction, magnetic fields [ISM], Astrophysics::Instrumentation and Methods for Astrophysics, Dust, Astronomy and Astrophysics, submillimeter: planetary systems, Extinction, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Grain size, Magnetic field, Azimuth, Wavelength, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, Millimeter, Astrophysics::Earth and Planetary Astrophysics, dust, ISM: magnetic fields, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: [Context] The azimuthal polarization patterns observed in some protoplanetary disks by the Atacama Large Millimetre Array (ALMA) at millimeter wavelengths have raised doubts about whether they are truly produced by dust grains that are aligned with the magnetic field lines. These conclusions were based on the calculations of dust polarized emission in the Rayleigh regime, that is, for grain sizes that are much smaller than the wavelength. However, the grain size in such disks is typically estimated to be in the range of 0.1-1 mm from independent observations., [Methods] By using the T-MATRIX and DustEM codes, we computed the spectral dependence of the polarization fraction in emission for grains in perfect spinning alignment for various grain size distributions. We restricted our study to weakly-elongated oblate and prolate grains of astrosilicate composition that have a mean size ranging from 10 μm to 1 mm., [Results] In the submillimeter and millimeter wavelength range, the polarization by B-field aligned grains becomes negative for grains larger than ∼250 μm, meaning that the polarization vector becomes parallel to the B-field. The transition from the positive to the negative polarization occurs at a wavelength of λ ∼ 1 mm. The regime of negative polarization does not exist for grains that are smaller than ∼100 μm., [Conclusions] When using realistic grain size distributions for disks with grains up to the submillimeter sizes, the polarization direction of thermal emission by aligned grains is shown to be parallel to the direction of the magnetic field over a significant fraction of the wavelengths typically used to observe young protoplanetary disks. This property may explain the peculiar azimuthal orientation of the polarization vectors in some of the disks observed with ALMA and attest to the conserved ability of dust polarized emission to trace the magnetic field in disks., J.M.G. is supported by the Spanish grant AYA2017-84390-C2-R (AEI/FEDER, UE). F.O.A. acknowledges financial support from the Max Planck Society. This work was funded by the European Research Council (ERC) under the European Union Horizon 2020 research and innovation programme (MagneticYSOs project grant agreement N.679937), and supported by the Programme National PCMI of CNRS/INSU. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.000291.S and #2016.1.01186.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.
Published: 2020
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42. ZNRF3 functions in mammalian sex determination by inhibiting canonical WNT signaling

Author: Silvia Corrochano, Abigail Harris, Hans Clevers, Caroline Eozenou, Isabelle Stévant, Joelle Bignon-Topalovic, Nick Warr, Neila Belguith, Sara Wells, Bochra Ben Rhouma, Pam Siggers, Serge Nef, Daniel T. Grimes, Ken McElreavey, Rebecca D. Burdine, Feng Cong, Makoto Suzuki, Andy Greenfield, Danielle Sagar, Anu Bashamboo, Bon-Kyoung Koo, Raja Brauner, Medical Research Coucil Harwell [Oxford, UK] (MRC Harwell), MRC Harwell, Department of Molecular Biology [Princeton], Princeton University, Novartis Institutes for BioMedical Research (NIBR), Hubrecht Institute [Utrecht, Netherlands], University Medical Center [Utrecht]-Royal Netherlands Academy of Arts and Sciences (KNAW), Université de Genève = University of Geneva (UNIGE), Fondation Ophtalmologique Adolphe de Rothschild [Paris], Université Paris Descartes - Paris 5 (UPD5), Faculté de médecine - Faculty of Medicine [Sfax, Tunisie] (FMS), Université de Sfax - University of Sfax, Génétique du Développement humain - Human developmental genetics, Institut Pasteur [Paris] (IP), This work was supported by the Medical Research Council by core funding Grant MC_U142684167 (to A.G.) at the Harwell Institute, and the Agence Nationale de la Recherche Grant ANR-10-LABX-73 (to K.M.). S.N. acknowledges support from Swiss National Science Foundation Grant 31003A_173070. M.S. was a visiting scientist supported by the Strategic International Research Exchange Program between Princeton University and National Institutes of Natural Sciences, Japan. D.T.G. was supported by National Institute of Arthritis and Mucoskeletal and Skin Diseases Pathway to Independence Award 1K99AR070905. Work in the R.D.B. laboratory is supported by the National Institute of Child Health and Development Grant 2R01HD048584., We thank the husbandry team in Ward 5 of the Mary Lyon Centre at Harwell and the Frozen Embryo and Sperm Archive (FESA) and histology teams. We thank Dagmar Wilhelm for the kind gift of anti-FOXL2 antibody. We thank Phil Johnson for zebrafish husbandry. We acknowledge European Cooperation in Science & Technology (COST) Action BM1303 (DSDnet)., ANR-10-LABX-0073,REVIVE,Stem Cells in Regenerative Biology and Medicine(2010), Université de Genève (UNIGE), Génétique du développement humain, Institut Pasteur [Paris], and Hubrecht Institute for Developmental Biology and Stem Cell Research
Subjects: 0301 basic medicine, Male, Embryo, Nonmammalian, Sex Differentiation, Organogenesis, Wnt Proteins/antagonists & inhibitors, Disorders of Sex Development, DSD, MESH: Wnt Proteins / metabolism, MESH: Testis / metabolism, MESH: Disorders of Sex Development / genetics, MESH: Testis / pathology, MESH: Embryo, Nonmammalian / cytology, Mice, Embryo, Nonmammalian/cytology, MESH: Gene Expression Regulation, Developmental, Testis, Missense mutation, MESH: Animals, ddc:576.5, Developmental, Disorders of sex development, 10. No inequality, MESH: Ubiquitin-Protein Ligases / genetics, Exome sequencing, Cells, Cultured, beta Catenin, Zebrafish, Multidisciplinary, Cultured, MESH: Thrombospondins / genetics, MESH: SOX9 Transcription Factor / metabolism, Wnt signaling pathway, Gene Expression Regulation, Developmental, SOX9 Transcription Factor, beta Catenin/antagonists & inhibitors, MESH: beta Catenin / metabolism, Sex reversal, MESH: Gonads / pathology, Cell biology, MESH: Young Adult, Embryo, MESH: Gonads / metabolism, Female, MESH: Cells, Cultured, Adult, Adolescent, Ubiquitin-Protein Ligases, Cells, Thrombospondins/genetics, Mutation, Missense, MESH: beta Catenin / antagonists & inhibitors, SOX9, Biology, Gonads/metabolism, MESH: Embryo, Nonmammalian / metabolism, 03 medical and health sciences, Young Adult, MESH: Wnt Proteins / genetics, WNT signaling, medicine, Animals, Humans, Ubiquitin-Protein Ligases/genetics, MESH: SOX9 Transcription Factor / genetics, MESH: Zebrafish, RSPO1, Gonads, General, MESH: Mice, Nonmammalian/cytology, MESH: Disorders of Sex Development / pathology, MESH: Adolescent, MESH: Wnt Proteins / antagonists & inhibitors, MESH: Mutation, Missense, MESH: Humans, MESH: beta Catenin / genetics, ZNRF3, MESH: Adult, Sex determination, medicine.disease, MESH: Male, MESH: Ubiquitin-Protein Ligases / physiology, SOX9 Transcription Factor/genetics, Wnt Proteins, 030104 developmental biology, MESH: Thrombospondins / metabolism, [SDV.GEN.GH]Life Sciences [q-bio]/Genetics/Human genetics, Gene Expression Regulation, Mutation, Testis/metabolism, Missense, Thrombospondins, MESH: Female, Function (biology), Disorders of Sex Development/genetics, MESH: Sex Differentiation
Abstract: International audience; Mammalian sex determination is controlled by the antagonistic interactions of two genetic pathways: The SRY-SOX9-FGF9 network promotes testis determination partly by opposing proovarian pathways, while RSPO1/WNT-β-catenin/FOXL2 signals control ovary development by inhibiting SRY-SOX9-FGF9. The molecular basis of this mutual antagonism is unclear. Here we show that ZNRF3, a WNT signaling antagonist and direct target of RSPO1-mediated inhibition, is required for sex determination in mice. XY mice lacking ZNRF3 exhibit complete or partial gonadal sex reversal, or related defects. These abnormalities are associated with ectopic WNT/β-catenin activity and reduced Sox9 expression during fetal sex determination. Using exome sequencing of individuals with 46,XY disorders of sex development, we identified three human ZNRF3 variants in very rare cases of XY female presentation. We tested two missense variants and show that these disrupt ZNRF3 activity in both human cell lines and zebrafish embryo assays. Our data identify a testis-determining function for ZNRF3 and indicate a mechanism of direct molecular interaction between two mutually antagonistic organogenetic pathways.
Published: 2018
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43. Cryo-EM structure of a Marseilleviridae virus particle reveals a large internal microassembly

Author: Filipe R. N. C. Maia, Hemanth K. N. Reddy, Naoyuki Miyazaki, Daniel S. D. Larsson, Janos Hajdu, Kazuyoshi Murata, Kenta Okamoto, Martin Svenda, Max F. Hantke, Chantal Abergel, Jean-Michel Claverie, National Institutes of Natural Sciences, Information génomique et structurale (IGS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Department of Cell and Molecular Biology [Uppsala], and Uppsala University
Subjects: 0301 basic medicine, Melbournevirus, Marseilleviridae, Cryo-electron microscopy, Genome, Viral, Nucleocytoplasmic large DNA viruses, Genome, Virus, Viral Proteins, 03 medical and health sciences, Capsid, Virology, Amoeba, Lipid bilayer, Tomography, biology, Virus Assembly, Cryoelectron Microscopy, Capsomere, DNA Viruses, Virion, Structure, Protein complex, biology.organism_classification, 030112 virology, [SDV.MP.VIR]Life Sciences [q-bio]/Microbiology and Parasitology/Virology, Biophysics, NCLDV
Abstract: International audience; Nucleocytoplasmic large DNA viruses (NCLDVs) blur the line between viruses and cells. Melbournevirus (MelV, family Marseilleviridae) belongs to a new family of NCLDVs. Here we present an electron cryo-microscopy structure of the MelV particle, with the large triangulation number T = 309 constructed by 3080 pseudo-hexagonal capsomers. The most distinct feature of the particle is a large and dense body (LDB) consistently found inside all particles. Electron cryo-tomography of 147 particles shows that the LDB is preferentially located in proximity to the probable lipid bilayer. The LDB is 30 nm in size and its density matches that of a genome/protein complex. The observed LDB reinforces the structural complexity of MelV, setting it apart from other NCLDVs.
Published: 2018
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44. Decoding the state distribution in a nonadiabatic rotational excitation by a nonresonant intense laser field

Author: Ohshima, Yasuhiro [Institute for Molecular Science, National Institutes of Natural Sciences, Myodaiji, Okazaki 444-8585 (Japan) and SOKENDAI - Graduate University for Advanced Studies, Okazaki 444-8585 (Japan)]
Published: 2006
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45. Electronic and Nuclear Responses of Fixed-in-Space H{sub 2}S to Ultrashort Intense Laser Fields

Author: Matsuda, Akitaka [Institute for Molecular Science, National Institutes of Natural Sciences, Myodaiji, Okazaki, Aichi 444-8585 (Japan)]
Published: 2006
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46. Hypo-osmotic shock induces nuclear export and proteasome-dependent decrease of UBL5

Author: Setou, Mitsutoshi [Mitsubishi Kagaku Institute of Life Sciences (MITILS), Machida, Tokyo 194-8511 (Japan) and National Institutes of Natural Sciences, National Institute for Physiological Sciences, 5-1 Higashiyama, Myodaiji-cho, Okazaki, Aichi 444-8787 (Japan)]
Published: 2006
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47. A boundary for histone acetylation allows distinct expression patterns of the Ad4BP/SF-1 and GCNF loci in adrenal cortex cells

Author: Morohashi, Ken-ichirou [Division for Sex Differentiation, National Institute for Basic Biology, National Institutes of Natural Sciences, Higashiyama 5-1, Myoudaiji-cho, Okazaki 444-8787 (Japan)]
Published: 2005
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48. Structural variability and complexity of the giant Pithovirus sibericum particle revealed by high-voltage electron cryo-tomography and energy-filtered electron cryo-microscopy

Author: Okamoto, Kenta, Miyazaki, Naoyuki, Song, Chihong, Maia, Filipe, Reddy, Hemanth K.N., Abergel, Chantal, Claverie, Jean-Michel, Hajdu, Janos, Svenda, Martin, Murata, Kazuyoshi, National Institutes of Natural Sciences, Information génomique et structurale (IGS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Department of Cell and Molecular Biology [Uppsala], and Uppsala University
Subjects: Electron Microscope Tomography, viruses, Cryoelectron Microscopy, lcsh:R, Virion, Biophysics, lcsh:Medicine, Article, Biofysik, Imaging, Three-Dimensional, [SDV.MP.VIR]Life Sciences [q-bio]/Microbiology and Parasitology/Virology, Viruses, lcsh:Q, lcsh:Science
Abstract: International audience; The Pithoviridae giant virus family exhibits the largest viral particle known so far, a prolate spheroid up to 2.5 μm in length and 0.9 μm in diameter. These particles show significant variations in size. Little is known about the structure of the intact virion due to technical limitations with conventional electron cryo-microscopy (cryo-EM) when imaging thick specimens. Here we present the intact structure of the giant Pithovirus sibericum particle at near native conditions using high-voltage electron cryo-tomography (cryo-ET) and energy-filtered cryo-EM. We detected a previously undescribed low-density outer layer covering the tegument and a periodical structuring of the fibres in the striated apical cork. Energy-filtered Zernike phase-contrast cryo-EM images show distinct substructures inside the particles, implicating an internal compartmentalisation. The density of the interior volume of Pithovirus particles is three quarters lower than that of the Mimivirus. However, it is remarkably high given that the 600 kbp Pithovirus genome is only half the size of the Mimivirus genome and is packaged in a volume up to 100 times larger. These observations suggest that the interior is densely packed with macromolecules in addition to the genomic nucleic acid.
Published: 2017
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49. Magnetic Fields in the Early Stages of Massive Star Formation as Revealed by ALMA

Author: Ke Wang, Josep M. Girart, Keping Qiu, Junhao Liu, Thushara Pillai, Hauyu Baobab Liu, Qizhou Zhang, Zhi-Yun Li, National Natural Science Foundation of China, China Scholarship Council, Ministerio de Economía y Competitividad (España), National Science Foundation (US), National Institutes of Natural Sciences (Japan), National Research Council of Canada, Ministry of Science and Technology (Taiwan), Academia Sinica (Taiwan), Korea Astronomy and Space Science Institute, and Ministerio de Ciencia e Innovación (España)
Subjects: 010504 meteorology & atmospheric sciences, Stars: formation, Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Observatory, Polarization, 0103 physical sciences, ISM: individual objects (IRDC G28.34+0.06), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, formation [Stars], 0105 earth and related environmental sciences, computer.programming_language, Physics, Member states, Astronomy and Astrophysics, Python (programming language), Radio astronomy observatory, Astrophysics - Astrophysics of Galaxies, individual objects (IRDC G28.34+0.06) [ISM], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Magnetic fields, computer
Abstract: We present 1.3 mm ALMA dust polarization observations at a resolution of $\sim$0.02 pc of three massive molecular clumps, MM1, MM4, and MM9, in the infrared dark cloud G28.34+0.06. With the sensitive and high-resolution continuum data, MM1 is resolved into a cluster of condensations. The magnetic field structure in each clump is revealed by the polarized emission. We found a trend of decreasing polarized emission fraction with increasing Stokes $I$ intensities in MM1 and MM4. Using the angular dispersion function method (a modified Davis-Chandrasekhar-Fermi method), the plane-of-sky magnetic field strength in two massive dense cores, MM1-Core1 and MM4-Core4, are estimated to be $\sim$1.6 mG and $\sim$0.32 mG, respectively. \textbf{The ordered magnetic energy is found to be smaller than the turbulent energy in the two cores, while the total magnetic energy is found to be comparable to the turbulent energy.} The total virial parameters in MM1-Core1 and MM4-Core4 are calculated to be $\sim$0.76 and $\sim$0.37, respectively, suggesting that massive star formation does not start in equilibrium. Using the polarization-intensity gradient-local gravity method, we found that the local gravity is closely aligned with intensity gradient in the three clumps, and the magnetic field tends to be aligned with the local gravity in MM1 and MM4 except for regions near the emission peak, which suggests that the gravity plays a dominant role in regulating the gas collapse. Half of the outflows in MM4 and MM9 are found to be aligned within 10$^{\circ}$ of the condensation-scale ($, Comment: 28 pages, 17 figures (Published in ApJ)
Published: 2020

50. SUNRISE Chromospheric Infrared spectroPolarimeter (SCIP) for SUNRISE III: Scan mirror mechanism

Author: Fumihiro Uraguchi, Kazuhide Kodeki, T. Oba, Masahito Kubo, Yukio Katsukawa, Kazuya Shinoda, Tomonori Tamura, Jose Carlos del Toro Iniesta, Kazuhiko Fukushima, Achim Gandorfer, Toshifumi Shimizu, Toshihiro Tsuzuki, Japan Society for the Promotion of Science, National Astronomical Observatory of Japan, and National Institutes of Natural Sciences (Japan)
Subjects: Physics, Balloons, Infrared, business.industry, media_common.quotation_subject, Sun, Tip-tilt mirror, SUNRISE III, Spectro-polarimeter, Optical path, Tilt (optics), Optics, Sky, Thermal, Astrophysics::Solar and Stellar Astrophysics, Sunrise, SCIP, business, Spectrograph, Image resolution, media_common
Abstract: Ground-Based and Airborne Telescopes VIII 2020; Virtual, Online; United States; 14 December 2020 through 22 December 2020; Code 166573.--Proceedings of SPIE - The International Society for Optical Engineering Volume 11445, 2020, Article number 114454F, The SUNRISE Chromospheric Infrared spectroPolarimeter (SCIP) is a balloon-borne long-slit spectrograph for SUNRISE III to precisely measure magnetic fields in the solar atmosphere. The scan mirror mechanism (SMM) is installed in the optical path to the entrance slit of the SCIP to move solar images focused on the slit for 2-dimensional mapping. The SMM is required to have (1) the tilt stability better than 0.035″ (3σ) on the sky angle for the diffraction-limited spatial resolution of 0.2″, (2) step response shorter than 32 msec for rapid scanning observations, and (3) good linearity (i.e. step uniformity) over the entire field-of-view (60″x60″). To achieve these performances, we have developed a flight-model mechanism and its electronics, in which the mirror tilt is controlled by electromagnetic actuators with a closed-loop feedback logic with tilt angles from gap-based capacitance sensors. Several optical measurements on the optical bench verified that the mechanism meets the requirements. In particular, the tilt stability achives better than 0.012″ (3σ). Thermal cycling and thermal vacuum tests have been completed to demonstrate the performance in the vacuum and the operational temperature range expected in the balloon flight. We found a small temperature dependence in the step uniformity and this dependence will be corrected to have 2-demensional maps with the sub-arcsec spatial accuracy in the data post-processing. © COPYRIGHT SPIE., The SUNRISE III project is funded in Japan by the ISAS/JAXA Small Mission-of-Opportunity program for novel solar observations, JSPS KAKENHI Grant Number 18H05234 (PI:Y.Katsukawa), and NAOJ Research Coordination Committee, NINS. We would also thank significant technical support from the Advanced Technology Center (ATC), NAOJ.
Published: 2020

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