dataesr/scientific-paragraphs-categorization huggingface dataset:
INTRODUCTION Neutron-induced reactions play a crucial role in various fields of fundamental and applied Nuclear Physics. In Stars, neutron capture reactions are at the basis of the production of elements heavier than Fe. On Earth, neutron-induced fission of U and Pu isotopes are responsible for energy production in nuclear reactors. Furthermore, neutron-induced reactions are a useful tool for studying fundamental properties of nuclear matter, and can be of help in various applied fields, like Nuclear Medicine, nondestructive analysis of archeological and art objects, detection of fissile material, etc… Neutron data are being collected at various facilities around the world. Since 2001, a new installation has joined the large family of neutron time-of-flight facilities: n_TOF at CERN, Geneva.
Based on a spallation neutron source, n_TOF was built with the aim of providing fresh new data on neutron cross sections for a variety of isotopes relevant mainly to Nuclear Astrophysics and advanced nuclear technologies for energy production and nuclear waste incineration. In the first ten years of operation, a large body of interesting results has been obtained at n_TOF by an International Collaboration of more than one hundred researchers from thirty Institutes. An extensive experimental program on capture reactions has been carried out with the aim of improving current knowledge of Stellar Nucleosynthesis of heavy elements, and gaining a better insight on stellar evolution  [1]. Furthermore, high accuracy and high resolution capture cross sections have been measured for some actinides, as requested for the design of advanced nuclear waste burners and/or Generation IV fast nuclear reactors.
At the beginning of the second experimental campaign, the experimental area was upgraded to a "Work Sector Type A", with a series of safety and monitoring systems, so to allow measurements of high-activity samples without certified sealing. This crucial modification was essential for exploiting the full strength of the facility. The convenient features of the neutron beam are complemented by state-of-the-art detection and data acquisition systems. The neutron flux in the experimental area is continuously monitored with a low-mass device, the SiMon detector, made of a thin foil with 6 Li deposit surrounded by an array of Silicon detectors outside the beam. Measurements of the energy-dependent neutron flux were performed in the commissioning phase of the new target with MicroMegas detectors equipped with 10 B and 235 U layers, as well as with a calibrated fission chamber.
An intense program on Nuclear Astrophysics has been carried out at n_TOF both in Phase I and II. In particular data have been collected with the C 6 D 6 detectors on isotopes with very small cross-sections. To this class belong 139 La and different Zr isotopes, that represent a bottle-neck in Stellar Nucleosynthesis, as well as some Mg and Pb isotopes. In all these cases, capture cross sections have been determined with better accuracy than in the past, thanks to the characteristics of the neutron beam and optimized neutron sensitivity of the apparatus. Recently, measurements of the capture cross-sections have also been completed for different isotopes of Fe and Ni, two elements at the beginning of the path of the s process nucleosynthesis. It should be mentioned that many of the above isotopes are also relevant to reactor technology, as part of structural material.
To this purpose, reference samples of 235 U (and 238 U) are always mounted in the same detector and measured simultaneously. The neutron-induced fission cross section of several isotopes, essentially all long-lived actinides, has been measured so far at n_TOF, in some cases up to 1 GeV. High accuracy results are now available for 232 Th, 233,234,236 U, 237 Np, 241,243 Am and 245 Cm, while a measurement of 240,242 Pu(n,f) cross section is currently under way. The use of the ratio method allows the determination of the energy dependence of the cross section with accuracy close to 3%. In most cases, cross sections are also determined in absolute value with 3-5% accuracy. As for capture reactions, n_TOF fission data are typically characterized by a higher accuracy and/or better resolution than past measurements.
The high quality of the data is also a consequence of the wide energy range, from thermal to hundreds of MeV, covered simultaneously in a single measurement, a feature that allows minimizing systematic uncertainties associated with the absolute normalization of the data. As an example, in the very difficult measurement of the 245 Cm fission cross section  [10] , normalization to recently determined thermal values allowed the determination of the absolute cross section with a 5% accuracy over more than seven decades in neutron energy. At low energy, where only two, largely discrepant data sets existed before, the high accuracy; high resolution n_TOF data will serve as basis for a more precise re-evaluation.
CONCLUSIONS In more than ten years of operation, the n_TOF facility at CERN as allowed the succesfull measurements of a large number of neutron cross sections, of interest for Nuclear Astrophysics and for advanced nuclear technologies. The features of the facility and high performance of experimental devices have generally led to high quality data, serving as the basis for advances in the understanding of stellar nucleosynthesis and for improving the accuracy of nuclear data libraries used in the field of nuclear energy. The construction of a second flight path at the shorter distance, foreseen for the near future, will open new measurement opportunities, in particular on shortlived isotopes, currently out of reach at n_TOF and other neutron facilities around the world. As in the past, the goal of the n_TOF Collaboration for the next years is to collect excellent quality neutron data of interest for basic and applied Nuclear Physics.
ACKNOWLEDGMENTS The n_TOF Collaboration has been benefitting from the support of the  European Commission  under contracts n_TOF-ND-ADS (5 th FP), IP-EUROTRANS (6 th FP) and ANDES (7 th FP), as well as from the financial support of all participating Institutions. I acknowledge that this manuscript is considered to be a representation that it has been neither copyrighted or published, nor submitted for publication elsewhere.
The same conclusion was reached concerning F83005-5 inserts downstream NT6019 based on the progenies of line 76-05-06. Furthermore, Mt-FTQTL6 interval could be delineated to a smaller region of 0. 4 cM between markers MTIC153 and NT6054 (Figure  1 -NT6001 -CR504418 -NT6048 -NT6061 -MTIC153 -NT6053bis -CR313272 -CR499994 -NT6066 -CR321866 -NT6100 -NT6054 -NT6067 -NT6051 -162O18T -CG975036 -CG974949 -NT6055 -NT6019 -NT6010 -NT6012 -NT6014 -NT6032 -NT6040 -NT6044 mean FDS of F7/F8 line mean FDS of F83005-5 mean FDS of DZA045-5   Mt-FTQTL6, inserts from BAC clones mth2-92O15, mte1-60A22 and mth2-221P20, were first fully-sequenced (GenBank accession numbers [GB acc] KF006382-84). Sequence information from these 3 clones (Figure  2   All positional candidate genes for Mt-FTQTL6 were found to have highly similar counterparts across a set of dicotyledonous species for which genome sequence information is available (Additional file 7).
They show a total of 402 single nucleotide polymorphism (SNP), 41 insertion-deletion (indel) and 9 simple sequence repeat (SSR) polymorphisms with 206 SNP, 8 indel and 3 SSR located in the coding sequences (Additional file 10). Contrary to A17 and F83005-5, DZA045-5 has an insertion of a 160-bp short interspersed nuclear element (SINE) in the coding  (1) Corresponding EST and cDNA were identified through BLAST searches against M. truncatula EST and nr/nt databases in GenBank  [36]  (January 2013), respectively. In case of alternate splicing, the sequence(s) corresponding to the less represented transcript isoform is(are) in italics; (2) similar to  [41] , the C-terminal domains of MtCBF2-3;5-11;14 were considered as the amino acid sequences that occur after the signature motif "DSAWR" and that up to the last amino acid of the protein; (a) a cDNA sequence corresponding to MtCBF8 was directly submitted to GenBank  [36]    genes carrying a single AP2/ERF domain  [48, 49].
truncatula CBF/DREB1 genes through the assembly of Mt-FTQTL6 region. Apart from MtCBF2 and MtCBF3 that were identified by Pennycooke et al. [32]  and DREB1A whose cDNA sequence was directly submitted to GenBank (GB acc DQ778006), the other CBF/ DREB1 genes associated with Mt-FTQTL6 were not previously annotated or described (Table  1 ). As the name "MtCBF4" has been recently assigned to a CBF/DREB1 gene located on M. truncatula chromosome 1  [35] , the novel genes including DREB1A were here given consecutive numbers from 5 to 14 starting from the most proximal to MtPERLD (Figure  2 ). MtCBF2-3;5-14 occur in tandem array and are in direct orientation (Figure  2 ) which suggests that they are most likely derived from an unequal crossing over mechanism  [64, 65]. However, the contribution of transposable elements to this duplication event cannot be totally excluded  [65] , especially with several transposon and retrotransposon insertions being evident between CBF/DREB1 genes (data not shown).
MtCBF11 has most likely arisen from an inframe fusion of the 5′ portion of the coding region from a first CBF/DREB1 gene with the 3′ portion of the coding sequence from a second gene. Alternative splicing events can diverge between duplicates, including organ-and stress-specific differences, and result in functional variation  [79]. Based on genomic sequence alignment with EST and cDNA data, MtCBF6 and MtCBF8 have two transcript variants each, generated by intron retention/splicing events (Table  1 ). MtCBF5 and MtCBF7 contain each an intron at the same position as for MtCBF6 and MtCBF8 intronspliced isoforms but no evidence yet suggests that MtCBF5 and MtCBF7 may have intron-retaining transcript forms similar to MtCBF6 and MtCBF8. As EST databases can be incomplete with regard to alternative splicing transcript variants, reverse transcription PCR or transcription analysis using second generation sequencing would allow determining alternative splicing patterns with more precision.
de novo assembly of the cleaned reads was performed using Newbler (version 2. 3; 454 Life Sciences, Roche Diagnostics). The resulting contigs were, when possible, ordered and oriented based on marker sequences located therein. End sequences from overlapping BAC clones (Additional file 5) were used for the same purpose. Complementarily, end sequences of the different contigs were submitted to blastn/blastx  [91]  search against M. truncatula nr/nt, high-throughput genomic sequence, EST, genome survey sequence and protein databases in GenBank  [36]  at the National Center for Biotechnology Information. End sequences sharing more than 99% identity with the same target sequence(s) were considered as indicative of adjacent contigs. Sequencing of CBF/DREB1 genes from F83005-5 and DZA045-5 The isolation and sequencing of MtCBF2-3;5-14 from F83005-5 and DZA045-5 was undertaken in order to determine if all genes composing the CBF/DREB1 cluster in A17 are similarly present in these accessions and to identify the polymorphism in the coding and immediate flanking sequences of these genes.
Primers and amplification conditions that were used in the sequencing step are provided in Additional file 10. For 9 out of the 12 CBF/DREB1 genes, one or two internal primers were needed to ensure full sequence coverage and/or overcome sequencing difficulties caused by simple sequence repeats [(A) n or (T) n ] present in 5′-or 3′-non-coding flanking regions (Additional file 10). Base calling was performed with Sequencing Analysis Software (version 5. 4; Applied Biosystems). Electropherograms were manually trimmed of poor sequence data.
Availability of supporting data The data sets supporting the results of this article are included within the article and its additional files. All sequences were submitted to GenBank  [36]. Insert sequences of BAC clones mth2-92O15, mte1-60A22 and mth2-221P20 were deposited in the "high throughput genomic sequences" division under accession numbers KF006382-84. BAC-end sequences were submitted to the "genome survey sequences" division and have been assigned the accession numbers JY974377-472. CBF/DREB1 gene sequences from A17, F83005-5 and DZA045-5 were deposited in the "plant, fungal, and algal sequences" division with accession numbers KC997199-225.
Acknowledgments The authors wish to thank  Dr. Jean-Marie Prosperi  for providing F 6 plants from which F 7 and F 8 recombinant lines were obtained,  Rosemonde Devaux  for plant care in the greenhouse and  Frédéric Depta  and  Jean-François Hû  for assistance in the conduct of freezing tolerance experiments. They acknowledge  Dr. Hélène Bergès  for helpful discussions concerning BAC clone isolation and sequencing. The authors would also like to thank the reviewers and the editor for their helpful comments which improved the manuscript. This work was partially financially supported by the  Région Nord Pas-de-Calais -France  ( FEDER ARCIR PLANTEQ3 program ) and by the  Union Nationale Interprofessionnelle des plantes riches en Protéines  ( UNIP -SAMPOIS program ). NT was the recipient of a Ph.
Radiation belt forecasting One of the most important elements of the SPACECAST project is to forecast the electron flux in the outer electron radiation belt. Since it takes approximately 40-60 min for the solar wind to flow from the ACE spacecraft to the magnetosphere, the ACE data provides some measure of advanced warning. The concept is therefore to take data derived from the ACE satellite and use it to drive the radiation belt models. The ACE satellite measures the polarity of the interplanetary magnetic field which controls the efficiency of energy transfer into the magnetosphere and subsequently into the radiation belts. Since the polarity of the interplanetary magnetic field cannot be measured remotely by other means, the ACE measurements are crucial and the speed of the solar wind flow is a key factor which limits the timescale of reliable forecasting to less than 1 h.
Periods of fast solar wind, and rapid changes in the solar wind can lead to changes on timescales as short as 30 min or so. However, for periods where the solar wind does not change significantly (persistence) it is possible to forecast further ahead as studies show that it can take 4 h for information at the magnetospause to be transferred to geostationary orbit  (Borovsky et al. 1998 ). In the SPACECAST project we use a forecast of the K p index to drive the forecast models. Since K p is a 3 h index, the models can provide a forecast of up to 3 h. In reality we make a forecast for 3 h, updated every hour. The Swedish Institute of space Physics, Lund, uses ACE data to make a forecast of the K p index. This data is accessed by the SPACECAST system and downloaded to a central server. We also access an estimate of K p from the British Geological Survey which is derived from ground-based magnetometers.
These two data sources provide resilience. Modelling centres at the British Antarctic Survey and the French Aerospace Research Laboratory use these data to drive two independent forecasting models. The models forecast the differential and integral high-energy electron flux for the whole outer radiation belt. These forecasts are collected by a central data system and displayed on the web, together with other supporting data from the ACE satellite, GOES satellite and geomagnetic indices such as D st. The forecasts are also used to calculate the 24 h electron fluence >2 MeV and provide a risk index of internal satellite charging. Data from GOES 13 at geosynchronous orbit are not used to provide the forecast but are displayed to test how well the forecasting performs. In effect the system uses data from Europe, the USA and Japan and is truly international.
Wave database Wave-particle interactions can accelerate electrons to MeV energies leading to an increase in the electron flux  (Horne et al. 2005a,b)  and diffuse electrons into the loss cone leading to a reduction in the electron flux  (Lorentzen et al. 2001; O'Brien et al. 2004; Thorne et al. 2005). The conditions under which there is a net increase or decrease in the electron flux depends on the wave properties, such as the wave mode, power, frequency spectrum, latitude and magnetic local time distribution of the waves, and the plasma density and magnetic field. All these wave properties vary with geomagnetic activity driven by the solar wind, and thus realistic wave-particle interaction models are essential. To build an improved model of the relevant plasma waves for SPACECAST, we have developed a wave database using plasma wave data from Dynamics Explorer 1, CRRES, Cluster 1, Double Star TC1 and THEMIS.
We first performed quality checks on all the wave data to ensure that poor quality data and outliers were excluded from the analysis. For each satellite measurement we then determined the position in magnetic coordinates (L*, MLT, MLAT) with the ONERA DESP library V4. 2  (Boscher et al. 2008 ) using the IGRF field at the middle of the appropriate year and the Olson-Pfitzer quiet time model  (Olson & Pfitzer 1977). We also determined the position with respect to the plasmapause, essential for discriminating between the wave modes, using, where possible, signatures in the satellite data. We used a criterion based on the ECH wave amplitude for CRRES  (Meredith et al. 2004 ) and the number density for THE-MIS  (Li et al. 2010 (Li et al. , 2011)). For Dynamics Explorer 1, Cluster 1 and Double Star TC1 we used a model of the plasmapause location  (Carpenter & Anderson 1992).
Along the particle trajectory the Earth's magnetic field can be separated into a symmetric and an asymmetric part. Early work  (Falthammar 1965) , and more recent work  (Lejosne et al. 2012) , shows that radial diffusion can be related to perturbations in the asymmetric part of the magnetic field. Thus by using observations of these magnetic field components from the GOES satellites, at locations where two GOES satellites lie on approximately the same electron drift path, it is possible to calculate diffusion coefficients. Between September 1998 and May 2003 GOES 8 and 10 were at fixed longitudes of 75°W and 135°W separated by around 4 h in magnetic local time. When the two satellites were on the dawn side, and on dusk side, it was possible to select data corresponding to the same electron drift orbit but at different MLT, and calculate the asymmetries of the magnetic field with a time resolution of 5 mn.
Taking the variations of the asymmetric terms and sorting them as a function of K p , the average of the radial diffusion coefficient was calculated for the whole database as a function of K p. The results are shown in Figure  5  together with the model of  Brautigam & Albert (2000)  for magnetic radial diffusion for reference. The Brautigam and Albert model, which is valid for 1 K p 6, was extrapolated to K p = 9 for comparison. Figure  5  shows that the radial diffusion coefficients determined for the dawn and dusk sides are very similar for a wide range of K p up to about K p = 7. They deviate from each other for K p > 7 partly because there are only a few data points at large K p (13 points on the dawn side and 20 on the dusk side) but the deviation may also suggest a difference in ULF wave activity with MLT.
Summary and conclusions In this paper we present some recent results from the SPACE-CAST project to forecast the high-energy electron radiation belts, and to model solar energetic particle events. The results of our studies can be summarized as follows: 1. We have developed the first system to forecast the highenergy electron radiation belt flux that uses physical models which include wave-particle interactions. The system uses data and models from Europe, the USA and Japan, and is truly international. The forecasts are made for a period of 3 h, updated every hour, using data derived from the ACE spacecraft and ground-based magnetometers which provides a measure of resilience. The models were able to reproduce the >2 MeV electron flux measured by GOES 13 to within a factor of 5 for a period of several hours during the moderate storm of the 7-8 October 2012, and the quiet period following a fast solar wind stream on 25-26 October 2012.
3. We have developed a new database of plasma waves from five different satellites which show that during active conditions, when K p ! 3, enhanced equatorial lower band chorus extends from 4 < L* < 9 between 23:00 and 12:00 MLT. Since the wave power for L* > 6 is comparable to or higher than that observed at L* by previous satellite missions, the results suggest that waveparticle interactions are likely to be very important outside geostationary orbit, and that they can now be incorporated into global models. 4. Using data from the GOES satellites we constructed a model for radial diffusion coefficients at geosynchronous orbit based on a separation of the symmetric and antisymmetric components of the magnetic field. The results obtained for the dawn and dusk sides of the magnetosphere agree with that obtained by  Brautigam & Albert (2000)  over approximately four orders of magnitude for different levels of K p , but are consistently lower by a factor of 5 or so.
Acknowledgements. The SPACECAST forecasting system uses data from several sources to produce the radiation belt forecasts. In particular we thank the  ACE SWEPAM  and MAG instrument teams and the  ACE Science Center  for providing plasma and magnetic field data on the solar wind, the  National Oceanic and Atmosphere Administration (NOAA) , for real time data from the GOES and POES satellites, the  Swedish Institute of Space Physics, Lund , for providing forecasts of the K p and D st indices, the  British Geological Survey , for providing an estimated K p magnetic index in near realtime, the  Regional Warning Centre, Kyoto , for the preliminary and quick look D st index, the  World Data Center for Geomagnetism, Kyoto  for providing AE and AL, the  Helmholdz Centre, Potsdam , for providing an archive of the K p index, the  National Geophysical Data Centre  for providing an archive of the D st index, the  European Space Agency  for use of their open data interface.
We thank  Roger Anderson  and  Keith Yearby  for provision of the CRRES and  Double Star  plasma wave data, respectively. We also acknowledge the  CDAWeb and CLUSTER Active Archive Web  sites for the provision of the wave data from DE 1 and CLUSTER, respectively. We thank  LPCEE laboratory (Orleans, France)  for their help in the analysis of DE1 and CLUSTER wave data. We acknowledge  NASA  contract  NAS5-02099 ,  V. Angelopoulos  and  Wen Li  for data from the THEMIS mission and its analysis. The research leading to these results has received funding from the  European Union Seventh Framework Programme  ( FP7/2007-2013 ) under Grant Agreement No. 262468. We also acknowledge financial support from the  UK Natural Environment Research Council (NERC)  and the  French Aerospace Research Laboratory (ONERA) , and the  Spanish MINECO  project  AYA2010-17286.
We searched the Spitzer Space Telescope data archive for Galactic planetary nebulae (PNe), that show the characteristic 17. 4 and 18. 9 µm features due to C 60 , also known as buckminsterfullerene. Out of 338 objects with Spitzer/IRS data, we found eleven C 60 -containing PNe, six of which (Hen2-68, IC2501, K3-62, M1-6, M1-9, and SaSt2-3) are new detections, not known to contain C 60 prior to this work. The strongest 17. 4 and 18. 9 µm C 60 features are seen in Tc 1 and SaSt 2-3, and these two sources also prominently show the C 60 resonances at 7. 0 and 8. 5 µm. In the other nine sources, the 7. 0 and 8. 5 µm features due to C 60 are much weaker. We analyzed the spectra, along with ancillary data, using the photo-ionization code CLOUDY to establish the atomic line fluxes, and determine the properties of the radiation field, as set by the effective temperature of the central star.