dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgments We particularly thank  F. Holon  and  Androm ede Oc  eanologie for the logistics and for sharing their habitat maps and information on the meadows studied. We also thank  STARESO (Corsica, France)  and its programme STARECAPMED for field work support in Calvi. We thank  J. Decelle ,  M. Bolgan  and anonymous reviewers for constructive comments on previous drafts. Thanks to 'The Clash' for the song 'London calling' that inspired the title. XR was financially supported by an  'Erasmus +'  grant of the  European Commission. L. Di Iorio  and  X. Raick  equally contributed to the realization of this work.
Participants After being informed of the experimental procedures, its risks and benefits, the participants (20 young heathy male) signed an informed consent form. The study was approved by the local Ethics Committee of under the number CAAE 69724617. 7\. 0000. 5169. A priori sample size tests (G*Power 3. 0. 10) revealed that a total of 20 participants would be required to detect an effect size of 0. 8 with a statistical power of 0. 90 and a alfa of 0. 05. Therefore, 24 volunteers were recruited to prevent critical data loss due to attrition. The invitation was performed through fliers distributed over the university campus, by social media and by word-of-mouth. The inclusion criteria were being at least 18 years old, having no previous RT experience and being free of clinical problems that could be aggravated by the study procedures.
Information sources and search strategy We searched the following electronic bibliographic databases on December 19, 2017: Medline, Embase, and Evidence-Based Medicine Reviews (which includes the Cochrane Library). The search was repeated on May 22, 2018 to capture any articles published during the review process. We used a combination of various search terms for cardiac arrest and extracorporeal circulation. The bibliographies of included articles were reviewed for potential additional articles. To identify ongoing trials, we searched the International Clinical Trials Registry Platform (http://www. who. int/ictrp/en/) (which includes entries in ClinicalTrials. gov) on March 13, 2018. The search strategies for each database and the Clinical Trials Registry Platform are provided in eTables 1-2 in the Supplementary Contents.
Data synthesis and confidence in cumulative evidence Studies were assessed for clinical (i. e. participants, interventions, and outcomes), methodological (i. e. study design or risk of bias), and statistical heterogeneity  [14]. Separate meta-analyses were planned for adult IHCA, adult OHCA, pediatric IHCA, and pediatric OHCA as described in the protocol. The quality of the overall evidence was assessed using the Grading of Recommendations Assessment, Development and Evaluation (GRADE) methodology ranging from very low quality of evidence to high quality of evidence  [15]. Detailed assessment of overall risk of bias, inconsistency, indirectness, imprecision and potential other issues such as publication bias were tabulated. Review Manager (The Cochrane Collaboration, 2014) was used to generate forest plots.
Risk of bias for individual studies The risk of bias within individual studies was judged overall as critical for all studies, with confounding being the primary source. Risk of selection bias was judged to be low for the majority of studies. Few studies were at moderate risk of bias for missing data. The majority of studies did not report any missing data and were therefore classified as low risk of bias, but the risk of bias could also be considered "unknown". All studies were at moderate risk for selective reporting since none provided a pre-registered protocol. The remaining ROBINS-I domains were all judged to be at low risk of bias. A detailed list of risk of bias assessments is provided in eTable 3 in the Supplementary Contents.
Methods. Consenting participants were antiretroviral therapy (ART)-naïve and SPVL was taken as log 10 (HIV RNA) at study entry. Genotypic data were generated on a custom content Affymetrix Axiom SNP array covering 770,558 probes. The Ensembl Gene database, assembly GRCh37. p13, was used for annotation. Principal component analysis (PCA) was used to identify population structures, and analysis of variance (ANOVA) was performed to detect associations between SNPs and SPVL. SNPs with zero variance or minor allele frequency (MAF) ≤0. 05 were removed. Results. Among the 2,544 participants, PCA showed distinct population structures with strong separation between black (n = 578) and nonblack (n = 1,966) participants, Figure  1. ANOVA was performed independently on both subsets. Two SNPs located in the Major Histocompatibility Complex (MHC) class I region of chromosome six reached genome-wide significance (P < 5 × 10 -8 ) in the non-black population: rs4418214 (P = 1.
Statistical analyses Data are presented as the mean ± SEM. For each group, means of body mass and age for both males and females were calculated. Additionally, mean testosterone levels per group, mean female parity and the total number of offspring produced by group were analysed. Statistical analyses included multi-way analysis of variance or analysis of covariance with body mass or age. Non-parametric tests for mean difference according to the normality of the data and linear correlations between parameters were also used. Between-group variation with respect to age, body mass in both males and females, testosterone value, dominance rank, and number and sex of offspring produced was analysed using a centred-scaled principal component analysis (N = 52 groups) computed in R using the 'FactorminR' 1.
By flow cytometry and using a consensual panel of antibodies (CD90, CD73, CD105 and CD45)  [14] , we did not find any human MSC in mice bone marrow (data not shown) at 6 months of engraftment suggesting that MSC were essentially involved at the beginning of the engraftment process. Secondary grafts were only performed for mice derived from patient 1 (RAEB2) and each mouse of the first generation gave rise to two mice for the second generation. These secondary grafts were performed by intra bone injection of 1x10 5 CD34 + cells without autologous MSC to assess the propagating capacity of the cells obtained after the first PDX. For the secondary graft, we hypothesized that the engraftment would be faster so we performed a tibia bone marrow aspiration to monitor the engraftment 3 months after injection and as human engraftment was already evidenced by this intermediate point, the mice were sacrificed at 3 months.
Sanger and next generation sequencing A selected panel of 39 genes recurrently mutated in MDS was designed and mutations were identified by nextgeneration sequencing (NGS) in BM mononuclear cells (MNCs) using a PGM system (ThermoFisher Scientific, Waltham, MA) and the 384-reaction Ion AmpliSeq library kit 2. 0 (Life Technologies, Chicago, IL) Base calls were generated by the Torrent Browser software (Life Technologies). The annotated. vcf files were also analyzed using NextGENe software (Softgenetics, State College, PA, USA). Abnormalities identified by both analyses were considered if referenced in UCSC and absent in 1000 genomes databases. For a given mutation, the proportion of mutated cells was twice the VAF of heterozygous mutations, or one-fold the VAF for homozygous mutations or hemizygous mutations of X chromosome genes in males)  [21].
EXPERIMENTAL DESIGN AND STATISTICAL ANALYSIS Statistical analysis of fly survival was performed with IBM SPSS Statistics 20 for Windows (IBM Corporation). Survival data were analyzed with the Kaplan-Meier method, and statistical comparisons were made with Log rank pair-wise comparisons. Additionally, Cox Regression analysis was performed to estimate hazard coefficient for each treatment. Statistical analysis of motor skills under various treatments was performed with Prism 7 for Mac (OriginLab). Statistical significance for locomotor effects was determined by nonparametric one-way ANOVA for multiple comparisons. Groups were compared in post hoc analysis with Holm-Sidak correction. All samples and animals were included in the analysis. The mean difference was considered to be statistically significant at 95% confidence interval.
Ten flies of each genotype or drug treatment were placed at the bottom of plastic vials in replicates and allowed to climb, and several locomotor paradigms were assessed: mean distance or mean length of trajectories, mean velocity, overall motion that represents percentage of flies being in movement, maximum velocity, mean length of trajectory, and total distance or the sum of all trajectory lengths. 10-second recordings were acquired in duplicates and analyzed with FlyTracker hardware and software, as described before  (Pokrzywa et al. , 2017). Overall, TTR-A flies presented better climbing measures when compared to V30M flies (Fig. 2  vs. Fig. 3 ). For both genotypes, the computational analysis of climbing traces revealed that TabFH2 treatment results in a significant relative motor improvement in several parameters, including traveled distance, climbing velocity, and overall time of flies in motion (Fig.
The effects of TabFH2 on locomotor abilities were apparent after one week of treatment. 2D drawings of climbing traces were generated by Flytracker software to better visualize the effect of the studied drugs on locomotor skills of diseased flies after 7 days of treatment. They show a prominent positive effect on both fly lines after treatment with TabFH2 (Fig. 4 ). This effect was more noticeable in TTR-A flies, whose behavior when treated with TabFH2 was comparable to healthy flies (Fig. 4A ). In contrast, diflunisal treatment exhibits a significant positive effect in TTR-A flies after 7 days of treatment, but not in V30M flies (Fig. 4 ). Consistent with our locomotor assessment, climbing traces show that TabFH1 has a limited effect on treated flies (Fig. 4 ).
The CsCl (B2) Structure is diatomic with equal numbers of atoms of each type. The L1 0 structure is a tetragonal distortion of the fcc structure. In the Heusler (L2 1 ) Structure, all of the atoms are located on the sites of a body centered cubic lattice. The Mg atoms of the MgZn 2 hexagonal Laves Structure (C14) are located on the sites of the hexagonal diamond structure. [10, 13, 14]  Several theoretical and experimental studies are available for the determination of the elastic constants of metals and alloys. If the equation of interatomic potential is known, then the elastic constants can be predicted theoretically from the first principles (ab initio) using the density functional theory (DFT) implemented in a software like Quantum Espresso  [16]  (QE) in combination with Exciting code  [17].
This permitted the retrieval of the optimal values of the elastic moduli and Poisson ratio that were recovered by the second model that follows. The computations were done in three dimensions (3D) using an elastodynamic finite element method (FEM)  [36, 37]  implemented in the commercial software Abaqus (version 6. 14, Dassault Systèmes Simulia Corporation, Providence, RI, USA)  [38]. This constituted the first interaction model.
The eigenvalues of a disc sample made of a single crystal of one of the components of the metal alloys were computed. This provided an idea of where the first and second modes would be situated in the vibration spectrum. The elastic moduli of the single crystal components from ab initio computation for pure metals that make up the alloy, and also parameters such as density and Poisson ratio were employed. The values for the single crystal were from the literature; therefore, the computations were done to confirm them and evaluate the different first principal DFT method calculation tools. For titanium, the density functional theory using the projector augmented-wave (PAW) method in Quantum Espresso associated with the Exciting  [17, 41]  package was employed. The mechanical parameters were then injected into the 3D finite element model to calculate the eigen-frequencies and plot the mode shapes/deformation.
Identification and Classification of Vibration Modes in the Spectrum and Validation of the Interaction Model Used for Inversion The 3D FEM elastic model of the disc specimen, implemented using Abaqus software, was discretized using 6041, 20-node quadratic hexahedral elements of type C3D20R  [36, 38, 43]. The first flexural and longitudinal mode shapes are depicted in Figure  3. The mode shape deformations induce mechanical deformations in the polarized PZT sensor crystal bonded to the deforming vibrating surface of the disc. The resulting tension and twisting of the sensor leads to the generation of an electric charge. Likewise, when the PZT crystal is submitted to a modulated electrical solicitation, it vibrates and induces a stress wave. The mode shapes showed that the vibrational modes of the disc could be easily detected using the thin PZT disc sensor.
Acknowledgments: The authors would like to thank  Pierre-Yves Le Bas  ( Los Alamos National Laboratory ) and  Cedric Payan  for providing the software RITA used for data acquisition and hardware to conduct the first RUV experiment, the Algerian government for the grant that supported D. C. during his stay at  LMA, Marseilles, France, and finally Brigitte Mourot of LMA  for helping with the administrative paper work.
TWA 22 3. 1. 1. NaCo observations TWA 22 AB was observed in field-tracking mode on February 11, 2013 with the NAOS-CONICA (NaCo) adaptive-optics instrument mounted on the VLT/UT4  (Lenzen et al. 2003; Rousset et al. 2003)  as part of a program dedicated to the orbit monitoring of young binaries (PI Bonnefoy; program ID 090. C-0819). The S13 camera was associated to the H-band filter (λ c = 1. 66 µm, ∆λ = 0. 33 µm), yielding a square field of view of 13. 5 arcsec. The wavefront sensing was achieved in the near-infrared on the pair (seen as a whole). We acquired 32 frames (NEXPO) of the binaries consisting of 0. 345 s × 30 (DIT × NDIT ) averaged exposures each. Small (±3") dithers were applied every four frames to allow for an efficient sky and bias subtraction at the data processing step. We observed immediately after TWA 22 AB the M6 star GSC08612-01565 to calibrate the point-spread function (PSF) of the instrument using the same adaptive-optics setup and the same DIT, NDIT, and NEXPO as for TWA 22 AB.
96 -1. 64 μm). Only the IRDIS data were exploited because the low-resolution (R∼30) IFS observations are superseeded by the SINFONI spectra  (R∼ 1500-2000)  of the binary exploited in  Bonnefoy et al. (2009)  and  Bonnefoy et al. (2014a). We acquired 240×4s IRDIS frames of the binary. The IRDIS dataset was reduced at the SPHERE Data Center 1  (DC) using the SPHERE Data Reduction and Handling (DRH) automated pipeline  (Pavlov et al. 2008; Delorme et al. 2017). The DC carried out the basic corrections for bad pixels, dark current, and flat field. It also includes correction for the instrument distortion  (Maire et al. 2016a). The wavefront-sensing of the adaptive optics system SAXO  (Fusco et al. 2006; Petit et al. 2014 ) could operate on the target in spite of its faintness at optical wavelengths (V=13.
SPHERE observations The binary was observed as part of the SHINE survey on February 2015 and February 2017 in field and pupil tracking mode, respectively. For both nights, the IRDIFS_EXT mode was used. The reduction of the IFS data was performed following the procedure described in  Mesa et al. (2015)  and  Zurlo et al. (2014). The calibrated spectral datacubes are made of 39 narrow band images. We rotated the datacubes corresponding to each exposures to align them to the North and averaged them. We extracted from the resulting cube the flux ratio between each component of the binary for both epochs (74 mas wide circular aperture). We made use of the IRDIS data for the astrometric monitoring. We followed the procedure described in Section 3. 1. 2 to reduce those data. We used the True North and platescale values reported in Section 3.
AstraLux observations Three of the AstraLux data points presented here are previously unpublished. These were obtained as a continuation of the As-traLux orbital monitoring campaign for young M-dwarf binaries, with a particular focus on young moving group members  (Janson et al. 2014 (Janson et al. , 2017)). The new data were acquired in March and December of 2015 with the lucky imaging camera AstraLux Sur  (Hippler et al. 2009 ) at the ESO NTT telescope (programs 094. D-0609(A) and 096. C-0243(B)). They were reduced in an identical way as previously in the survey (e. g. ,  Janson et al. 2014). For the March run, the cluster NGC 3603 was used as astrometric calibrator, giving a pixel scale of 15. 23 mas/pixel and a true North angle of 2. 9 •. In the December run, the Trapezium cluster was used for astrometric calibration, yielding a pixel scale of 15.
We used the version 3. 0. 0 of the ESO data handling pipeline  (Abuter et al. 2006 ) through the workflow engine Reflex  (Freudling et al. 2013 ) which allowed for an end-to-end automatized reduction. Reflex performed the usual cosmetic steps on the bi-dimensional raw frames (flat field removal, bad-pixel flagging and interpolation). Those steps rely on calibration frames taken the days following our observations. The distortion and wavelength scale were calibrated on the entire detector. The positions of the slitlets on the detector were measured and used to build the datacubes containing the spatial (X,Y) and spectral dimensions (Z). In the final step, the cubes corresponding to individual exposures were merged into a master cube. GJ 2060 is well resolved into the J and H+K mastercubes but the sources contaminate each other.
We computed 2MASS J, H and K-band contrasts as well as the K1 and K2 SPHERE contrasts from GJ 2060 A and B spectra prior to the telluric line correction (Table  5 ). The H, K1 and K2 synthetic contrasts match those derived from the SPHERE and NaCo data within error bars. We therefore used the synthetic 2MASS H and K-band contrasts and the 2MASS magnitude of the system  (Cutri et al. 2003)  to retrieve the individual magni-  tudes of GJ 2060 A and B. J-band contrasts could be extracted from the SPHERE IFS data. They agree with the one derived with SINFONI. We used the contrast value of the 2015 SPHERE data to derive the J-band magnitude of the system components. The 2MASS J magnitudes could then be used to fluxcalibrate the J-band spectra using the 2MASS filter response curves and tabulated zero points 2.
(2001) , and the bisector velocity spans (BVS), R0HK indexes, etc. For a detailed description of SAFIR, see  Galland et al. (2005). The values obtained in October 2016 show a very strong dispersion, probably due to the high magnetic activity of the star. Indeed, the orbit of the binary is ∼ 8 years long, so that we do not expect the radial velocities to vary more than ∼ 0. 01 km/s within a few consecutive days, very different from the 0. 40 km/s variation we observed. Moreover, we note a strong correlation between the star bisector and the radial velocity measurements. We will therefore add this noise to the instrument uncertainty. 2 https://www. ipac. caltech. edu/2mass/releases/allsky/doc/sec6_4a. html The jitter evidenced in the HARPS data (section 3. 2. 6) must be taken into account in the FEROS set.
Missing mass: existence of GJ 2060 Ab or Bb Hidden mass close to the primary could explain the strong disagreement between models and data for GJ 2060. Indeed, a 0. 1 to 0. 2 M (depending on the system age) additional companion could account for the mass underestimation (see table  12 ) and could have been missed in the SPHERE datasets if close enough from one of the two components. Quick dynamical simulations with a symplectic integrator (SWIFT_ HJS Beust2003, see appendix) evidenced that a additional companion should orbit closer than 0. 1 au (6 mas) from either of the companion to remain bound for the system's lifetime. The PSFs of GJ 2060 A and B are not elongated, even in the SPHERE images (FWHM∼30 mas). In the latter, we injected models of putative companions with different fluxes and separations and checked whether they would induce a PSF lengthening that could be noticed by eye.
Acknowledgements. We thank  Carine Babusiaux ,  Benjamin Montet  and  Thierry Forveille  for fruitful discussions, as well as the anonymous referee for reviewing our work and for insightful and constructive comments which improved the manuscript. The project is supported by  CNRS , by the  Agence Nationale de la Recherche  ( ANR-14-CE33-0018 , GIPSE), the OSUG@2020 labex and the  Programme National de Planétologie (PNP, INSU)  and  Programme National de Physique Stellaire (PNPS, INSU). Most of the computations presented in this paper were performed using the Froggy platform of the CIMENT infrastructure (https://ciment. ujf-grenoble. fr), which is supported by the  Rhône-Alpes region  ( GRANT CPER07_13 CIRA ), the OSUG@2020 labex (reference  ANR10 LABX56 ) and the  Equip@Meso project  (reference  ANR-10-EQPX-29-01 ) of the  programme Investissements d'Avenir , supervised by the  Agence Nationale pour la Recherche.
This research has made use of the SIMBAD database operated at the  CDS (Strasbourg, France). Research on moving groups by  Thomas Henning  is supported by the  DFG-SFB 881  " The Milky Way System ". SPHERE is an instrument designed and built by a consortium consisting of  IPAG (Grenoble, France ),  MPIA (Heidelberg, Germany) ,  LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France) ,  INAF-Osservatorio di Padova (Italy) ,  Observatoire de Genève (Switzerland) ,  ETH Zurich (Switzerland) ,  NOVA (Netherlands) ,  ONERA (France)  and  ASTRON (Netherlands)  in collaboration with  ESO. SPHERE was funded by  ESO , with additional contributions from  CNRS (France) ,  MPIA (Germany) ,  INAF (Italy) ,  FINES (Switzerland)  and  NOVA (Netherlands). SPHERE also received funding from the  European Commission Sixth and Seventh Framework Programmes  as part of the  Opti-cal Infrared Coordination Network for Astronomy (OPTICON)  under grant number  RII3-Ct-2004-001566  for  FP6  ( 2004-2008 ), grant number  226604  for FP7 (2009)(2010)(2011)(2012) and grant number  312430  for FP7 (2013)(2014)(2015)(2016).
We also acknowledge financial support from the  Programme National de Planétologie (PNP)  and the  Programme National de Physique Stellaire (PNPS)  of  CNRS-INSU in France. This work has also been supported by a grant from the  French Labex OSUG@2020  (Investissements d'avenir - ANR10 LABX56 ). The project is supported by  CNRS , by the  Agence Nationale de la Recherche  ( ANR-14-CE33-0018 ). It has also been carried out within the frame of the  National Centre for Competence in Research PlanetS  supported by the  Swiss National Science Foundation  (SNSF). MRM, HMS, and SD are pleased to acknowledge this financial support of the  SNSF. Finally , this work has made use of the the SPHERE Data Centre, jointly operated by  OSUG/IPAG (Grenoble), PYTHEAS/LAM/CESAM (Marseille) ,  OCA/Lagrange (Nice)  and  Observatoire de Paris/LESIA (Paris).
The measurements were performed as described elsewhere  (Cébron et al. , 2013). Briefly, 3 mL of the bottle atmosphere was sampled with a plastic syringe through a rubber stopper and CO 2 quantified by and infrared gas analyzer (Binos 1004; Rosemount). After the measurements, the bottles were opened and brought to equilibrium with the external atmosphere in a laminar flow hood. Mineralization curves (CO 2 emission vs. time) were fitted using the "grofit" package  (Kahm et al. , 2010)  present in the R software (R Development Core Team, 2010) to determine quantitative parameters of CO 2 production such as the maximum mineralization (max value at plateau) and mineralization rate (the initial slope of the CO 2 evolution vs. time curve). To better understand the dynamics of the C-source in the presence of the different SPs, the soluble fractions of phenanthrene and glucose (i.