dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgments. The research was carried out at the  Jet Propulsion Laboratory, California Institute of Technology , under a contract with the  National Aeronautics and Space Administration. The Juno mission and the team members at JPL were supported by  NASA  grant  NNN12AA01C. TG acknowledges support from  CNES. We thank all Juno team members for the collaborative efforts and three anonymous reviewers for insightfull suggestions to improve the manuscript.
ACKNOWLEDGMENTS The work of BB was supported by the  French National Agency for Research  grant  ANR-17-CE31-0001-02. The work of LD was supported by the  US Department of Energy  under contract  DE-AC02-76SF00515  and by a  Humboldt Research Award. GP acknowledges support from the  Deutsche Forschungsgemeinschaft  under  Germany's Excellence Strategy EXC 2121 "Quantum Universe "  390833306. BB and LD thank the  Pauli Center of ETH Zürich  and the  University of Zürich  for hospitality. LD is also grateful to the  Laboratoire de physique de l'Ecole normale supérieure and Humboldt Universität zu Berlin  for hospitality.
Therefore, the enantioselective reaction was evaluated by varying The results revealed that a decrease of the catalyst loading led to an increase of the enantiomeric excess of the product (from 76% to 84% ee with ZnEt2, and from 16% to 49% ee with ZnMe2). Moreover, the shape of the two curves are identical with the one seen in our NLE investigations. Thus, it would seem possible to link the observed non-linear effects to the experiments from Figure  2. Indeed, if we assume that the heterochiral aggregate is fully precipitated, a catalytic system with e. g. 20 mol% catalyst loading of a ligand of 50% ee should be equivalent to a 10 mol% catalyst loading of enantiopure catalyst. Thus, we could correlate all data points from Figure  2  with a virtual enantiomeric excess if a scalemic ligand was used.
Preprocessing As previously described  (Jacini et al. , 2018; Rucco et al. , 2019) , the MEG signals, after an anti-aliasing filter, were acquired with a sampling frequency of 1,024 Hz. A fourth-order Butterworth IIR band-pass filter in the 0. 5-to 100-Hz band was subsequently applied to the acquired signals. Environmental noise, measured by reference magnetometers, was removed by using the principal component analysis. MEG data were cleaned of physiological artifacts, such as eye blinking and heart activity, by means of independent component analysis  (Sorriso et al. , 2019). Visual inspection was used for identification of noisy channels. For all the preprocessing steps, we used the FieldTrip toolbox  (Oostenveld et al. , 2011). corresponding to the cerebellum because of their low reliability in MEG  (Lardone et al.
Branching Parameter As previously described  (Beggs and Plenz, 2003; Shriki et al. , 2013) , an avalanche is defined as a sequence of contiguous time bins starting when at least one ROI is active and ending when all regions are inactive. The number of events in all ROIs in an avalanche corresponds to its size. For each subject and for each time bin size, the branching parameter σ was estimated by calculating, for each avalanche, the averaged (over all the time bins) ratio of the number of events between the subsequent time bin (descendants) and that in the current time bin (ancestors), and then averaging it over all the cascades  (Bak et al. , 1987). More specifically: σ = 1 N aval N aval i=1 σ i (1) where σ i is the branching parameter of the i-th avalanche in the dataset, N bin is the total amount of bins in the i-th avalanche, n events (j) is the total number of events active in the j-th bin, and N aval is the total number of avalanche in the dataset.
Goodness of Fit We performed the goodness of fit (GOF) via the evaluation of Hellinger distance (HD)  (Oosterhoff and van Zwet, 2012)  between the distribution of real data and the distribution of fitted data, in order to quantify the similarity between two probability distributions, as follows. HD (P, Q) = 1 √ 2 x m i=x 0 ( P i -Q i ) 2 ( 4 ) where P is the probability mass function of real data, and Q is the probability mass function of fitted data. The HD is in between 0 and 1; and the lower the HD, the better the fit to real data (ideally, HD = 0). Furthermore, to assess the GOF overall RTT patients and HS, we provided the empirical cumulative distribution function (ECDF) of HD.
Statistical Analysis We compared the distribution parameter α in patients and controls using permutation testing  (Nichols and Holmes, 2002) , for each frequency band. Specifically, at each iteration, each subject is randomly assigned to one of the two groups and then the difference between the averages of the two groups was computed. The group assignment is permuted 104 times, obtaining the null distribution of group differences, which was used to define the statistical significance of the observed difference between patients and controls. All the analyses were performed at a significance level of 0. 05, using Matlab R2017a (MathWorks R ) environment.
RESULTS As described in the Methods section, we discretized the ROI signals as a train of events, each of them representing the signal exceeding the threshold of ±3 SD. First, we checked the critical condition in both groups, in all frequency bands, for all time bins. We found, for both groups, a branching parameter σ ≈ 1, in delta band for bin t = 5, in theta and alpha band for bin t = 1, in beta-, gamma-, and broadband for bin t = 2, as reported in Table  1. Moreover, to demonstrate the robustness of the estimation of the branching parameter, we estimated the variance around sigma both when we split our dataset into two segments (Table  2 ) and when we divided it into three segments (Table  3 ). To demonstrate the strength of our data, we reported, for the chosen threshold SD = 3, the size distribution fitted with a power law (Figure  2 ), duration distributions (Figure  3 ), and average size versus duration distributions (Figure  4 ) for each subject, in all time bins, for both groups separately (for brevity, we reported only delta, alpha, and broadbands).
(2019) , which would have depleted N only, and not C nor Ar, from forming planetesimals or proto-Earth. The fact that the C-N-Ar signature of the BSE is within the field of CV-CO data does not imply that the building blocks of Earth were made of this material. Conversely we propose that Earth was made of an assemblage of precursors that condensed and evaporated at various temperatures, which are best represented from a volatile element perspective by the CV chondrites. This possibility is independently supported with the monotonous volatile depletion trend of the silicate Earth that parallels that of CVs  (Palme and O'Neill, 2013; Braukmüller et al. , 2019). 4  for terrestrial estimates, Supplementary Table  S1  for meteoritic data, and Supplementary Fig. S5  for discussion of meteoritic data.
Acknowledgements M. A, D. V. B, M. W. B, D. J. B  and B. M were supported by the  European Research Council  ( PHOTONIS  project, grant agreement No. 695618  to B. M. ). Samples were collected as part of Study # YELL-08056 -Xenon anomalies in the Yellowstone Hotspot. We would like to thank  Annie Carlson  and all of the rangers at the  Yellowstone National Park  for providing invaluable advice and help when collecting the samples. This work was partially supported by a grant ( G-2016-7206 ) from the  Alfred P. Sloan Foundation  and the  Deep Carbon Observatory  to P. H. B as well as  NSF  award  2015789  to  P. H. B. Sampling  at  Mt. Etna  and gas analysis was supported by  Instituto Nazionale di Geofisica e Vulcanologia Palermo. Fruitful discussions with  Marc Hirschmann  helped us to shape the ideas presented in this work.
The pinning force (F p = J c × µ 0 ⋅H appl ) was calculated. Fitting of the experimental data with the universal scaling law  37, 38  where f p = F p /F p,max with F p,max being the maximum pinning force, h = H appl /H irr , and A, p and q are fitting parameters, provides in the case of MgB 2  25  p and q values far away from the theoretical ones. From this reason we shall not present them here. Considering percolation aspects, Eisterer  39  defined the parameter k n = h 0 /h(f p /2). The values of h 0 = h(f p = 1) and k n provide information on the vortex pinning mechanisms  38. Theoretical values for Grain-Boundary Pinning (GBP) and Point Pinning (PP) are h 0 = 0. 2, k n = 0. 34 and h 0 = 0. 33, k n = 0. 47, respectively  38, 39. Trapped magnetic field experiments were performed by using a 5 T superconducting coil (Oxford Instruments) built in a low-loss cryostat.
Acknowledgements This work was supported by  UEFISCDI   Romania through Core Program   PN19-03  (contract no. 21N/08. 02. 2019 ), the projects POC 37_697 no. 28/01. 09. 2016REBMAT  and  PFE 12 , and it is part of the  SUPERFOAM international project  funded by  ANR  and  DFG  under the references  ANR-17-CE05-0030  and  DFG-ANR Ko2323-10 , respectively. D. B. acknowledges support from  University POLITEHNICA of Bucharest (UPB) , through the  "Excellence Research Grants" Program, UPB-GEX , No. 51/2016 , Code 300, NEWADD.
2019) , TOI-270  (Günther et al. 2019) , LP 791-18  (Crossfield et al. 2019) , and LP 729-54  (Nowak et al. 2020 ) among others. GJ 273 was observed by TESS in sector 7 with CCD camera 1 from 2019-Jan-07 to 2019-Feb-02 (TIC 318686860). An alert was not issued by TESS for this object, due to the lack of clearly identified transits by both the QLP (Quick Look Pipeline) and the SPOC (Science Processing Operations Center). With this in mind, we performed our own search for threshold-crossing events that might not have been detected by the aforementioned automated pipelines. Our custom-made pipeline SHERLOCK 4  (Searching for Hints of Exoplanets fRom Lightcurves Of spaCe-based seeKers) made use of the lightkurve package (Lightkurve  Collaboration et al. 2018 ) to obtain the TESS data of GJ 273 from the NASA Mikulski Archive for Space Telescope (MAST).
g. ,  Jenkins et al. 2009; Hinse et al. 2015; Wood et al. 2017; Horner et al. 2019). We used the MEGNO implementation within the N-body integrator rebound  (Rein & Liu 2012) , which made use of the Wisdom-Holman WHfast code  (Rein & Tamayo 2015). This allowed us to explore the whole parameter space at a small computational cost. As a first approach we only considered the two planets already confirmed in the system, i. e. , GJ 273b and GJ 273c. We then explored the stability of the system for different planetary eccentricities and inclinations following  Jenkins et al. (2019). The natural trend of planetary systems is to reside in a nearly co-planar configuration, hence, we assumed planets b and c as being co-planar, and the initial longitude of the ascending node Ω for both planets was taken as zero.
e. , MAB and KB analogues. Each of these parameters has an important influence on the potential habitability of the planet located in the HZ, GJ 273b. We also reviewed the published observational data obtained via HARPS and TESS, where we explored the detectability of the known, candidates and extra planets in the system. More specifically, our studies revealed: 1. We analyzed the process of formation and evolution of the planetary system around GJ 273 making use of N-body simulations. Our research allowed us to derive three important results: (1) the gaseous component of the disk played a key role in determining the physical and orbital properties of the planets of the system; (2) GJ 273c is a planet with very low water content, while GJ 273b seems to be a water world evolving within the HZ; and (3) the planetary system around GJ 273 might host more planets (in addition to the two confirmed) with different physical and orbital properties.
2. From our review of the observational data sets we found that these other possible planets predicted by the N-body simulations could not have been detected with the precision and cadence of the HARPS RV data-set that confirmed GJ 273b and GJ 273c. From the TESS data, however, we found that a transit of the innermost planet GJ 273c can be ruled out. On the other hand, for the rest of the planets in the system, the TESS photometric data were insufficient to confidently rule out the presence of any transit signals. 3. We tested the stability of the system using the MEGNO criterion. We found that in the two-planet configuration we could not constrain the inclination of the system, and consequently the masses of the planets remain unknown. However, in the four-planet configuration, the system was stable only for near-circular orbits of the two outermost planets, GJ 273d and GJ 273e, and minimum inclinations of the whole system down to ∼72 •.
Acknowledgements. We thank the anonymous referee for the helpful comments. J. C. S. acknowledges funding support from  Spanish  public funds for research under projects  ESP2017-87676-2-2  and  RYC-2012-09913  ( Ramón y Cajal programme ) of the  Spanish Ministry of Science and Education. Z. M. B. acknowledges  CONICYT-FONDECYT/Chile Postdoctorado 3180405. M. G. and E. J. are FNRS Senior Research Associates. V. V. G. is a FNRS Research Associate. M. N. G. acknowledges support from  MIT's Kavli Institute  as a Torres postdoctoral fellow. We acknowledge the use of public data from pipelines at the  TESS Science Office and at the TESS Science Processing Operations Center.
PDOS components were shifted vertically for the sake of clarity. The PDOSs for Fe(3d) and Ni(3d) states show only the majority spin components on all panels (the minority spin components correspond to unoccupied states). to describe accurately the formation energies and energetics in general  [58] , and which thus are expected to be of crucial importance for calculations of XANES spectra. Therefore, further applications of the novel XANES method based on DFT+U +V are envisaged to clarify further the impact of inter-site interactions on XANES spectra of complex TM compounds. The data used to produce the results of this work are available on the Materials Cloud Archive  [85]. Figure  3  shows the PDOS for occupied states of LFO and LFNO computed at three levels of theory: DFT, DFT+U , and DFT+U +V.
ACKNOWLEDGMENTS This research was partially supported by the  European Commission   FP6 Marie Curie project  HiTempEchem No. 042095 , the  European Commission  ( EU FP6 MIRG 042095 ), the  Swiss-China  project  IP03-092008 , the  Swiss National Science Foundation (SNSF)  through Grants No. 116688  and No. 179138  and its  National Centre of Competence in Research (NCCR) MARVEL. X. Z. acknowledges funding from the  National Natural Science Foundation of China  under Grant No. 51002130. I. T. , M. C. , and N. M. acknowledge partial support from the  EU-H2020  research and innovation programme under Grant Agreement No. 654360  within the framework of the  NFFA Europe Transnational Access Activity. Computer time was provided by  CSCS  ( Piz Daint ) through Project No. s836. This research used resources of the  Advanced Light Source  ( Beamline 9.
Relaxing the T -matrix parameters, reasonably good fits become possible and we actually found two distinct minimums of the total χ 2 combining the πη and the K S K S data, χ 2 | tot = (119 + 76)| πη + 233| K S K S (fit I) = (93 + 117)| πη + 229| K S K S (fit II). (88) In the case of πη the first number corresponds to the region E < 1. 1 GeV. In this region fit II is better than fit I while the overall χ 2 is slightly smaller in fit I (χ 2 = 428) than in fit II (χ 2 = 439). The χ 2 is defined in a simple and naive way: the correlation matrix is assumed to be diagonal and the statistical and systematic errors provided by the Belle collaboration are added in quadrature. The searches for minimums were performed with the help of the computer code MINUIT  [49]. The numerical values of the set of T -matrix parameters resulting from these two fits are shown in table 2.
Acknowledgements We would like to thank prof. S. Uehara  for many clarifying explanations about the Belle experiments. JXL thanks  Prof. Lisheng Geng  for useful discussions. JXL is partly supported by the  National Natural Science Foundation of China  under Grant Nos. 11735003 ,  11975041 ,  11961141004  and by the  Fundamental Research Funds for the Central Universities. He also gratefully acknowledges the financial support from the  China Scholarship Council. This.
In this contribution, we re-evaluate the Ni isotope composition of the BSE through high-precision isotope measurements of four carefully selected suites of mantle peridotites. These samples cover a wide range in degrees of melt depletion and are minimally affected by metasomatic overprint. For five of these unmetasomatised peridotites, we have also measured the Ni isotope composition of pristine olivine separates. In addition, five peridotite samples with evidence for modal or cryptic metasomatism were included to specifically investigate the effects of melt-rock reactions in the mantle. We complement the peridotite dataset with measurements of chondritic meteorites to compare mantle-and chondrite Ni isotope compositions obtained using the same methodology.
Mass spectrometry and data reduction Nickel isotope measurements were carried out using a Thermo Scientific Neptune multi-collector inductivelycoupled plasma mass spectrometer (MC-ICP-MS; s/n 1020). Samples were introduced in 0. 3 M HNO3 with a 50 µL/min capillary, PFA nebuliser and CETAC Aridus desolvating nebuliser (typical gas flows are ~5. 5 L/min Ar and ~5 mL/min N2). The Neptune was operated in medium resolution (m/Δm ≥6000, 5-95 % peak height definition) in order to resolve isobaric interferences, notably 40 Ar 18 O on 58 Ni and minor oxide and argide complexes on other Ni isotopes (see online supplementary material). Interference of 58 Fe on 58 Ni could not be resolved but was corrected by monitoring 56 Fe and 57 Fe. This correction was found to be robust at least up to 56 Fe/ 60 Ni = 0.
A blank subtraction was not applied as it was found to have a detrimental effect on the precision; blank corrected and uncorrected data proved identical within uncertainty with the latter being more precise. The double spike inversion yielded the 60 Ni/ 58 Ni of the sample that was expressed relative to the two adjacent SRM 986 measurements as δ 60/58 NiSRM 986 (hereafter written as δ ] -1 Each sample was measured at least six times. We report the average δ 60/58 Ni and quote a 2sx̄ precision that is the standard error of the mean for the repeat measurements assuming homoscedasticity for each measurement session. No measurements were excluded at this stage. The reproducibility of the analytical protocol was evaluated through the repeated measurement of reference materials. Our in-house Bristol Isotope Group Ni solution (BIG-Ni) was measured both directly and after processing through the ion-exchange separation procedure, which yield indistinguishable means and an intermediate precision of δ 60/58 Ni = 0.
The δ 60/58 Ni data for peridotites and chondritic meteorites are listed in Tables  1  and 2 , respectively, and shown in Figure  3. Terrestrial peridotites display a range in δ 60/58 Ni from 0. 041 to 0. 147 ‰ where the lower end of this distribution is formed by three peridotites with δ 60/58 Ni between 0. 041 and 0. 075 ‰. The 22 fertile to refractory peridotites yield a mean of 0. 115 ± 0. 011 ‰ (2sx   2017 ) did not consider the potential effects of post-melting events. Yet, their Tanzanian xenolith samples cannot be simple melting residues and show clear evidence for cryptic and modal metasomatism (Figure  1  and supplementary Figure  S1 ;  Dawson and Smith, 1973; Gibson et al. , 2013). Our peridotite dataset covers a wider range from fertile to variably melt-depleted peridotites that are largely free from metasomatic overprints, complemented with five samples with different types of metasomatic overprint (Figure  1 ), which allows us to re-assess the influence of melt depletion and melt-rock reactions on Ni isotope systematics.
, 2013). We have measured four Tariat xenoliths and one Zabargad sample with clear evidence for metasomatic enrichment to investigate its effect on Ni isotope systematics. The metasomatised Tariat xenoliths have LREE-enriched compositions, in combination with the introduction of phlogopite in sample Mo4230-16, that results from silicate-and carbonatite melt metasomatism  (Kang et al. , 2017; Carlson and Ionov, 2019). The hand specimen of Zabargad lherzolite BZ-230 is enriched in clinopyroxene, which occurs in clusters that contain up to 30 % clinopyroxene, and has an unusually heavy Li isotope signature, but no obvious LREE enrichment  (Brooker et al. , 2004). Three out of four metasomatised Tariat samples in our dataset have marginally higher δ 60/58 Ni than the pristine peridotites (Figure  3 ) but only the clinopyroxene-enriched Zabargad lherzolite has a composition (0.
Conclusions We present a high-precision Ni isotope dataset for terrestrial peridotites and chondritic meteorites. The main findings of this work can be summarised as follows: 1) Mantle peridotites have a limited range in δ 60/58 Ni and do not exhibit systematic variation with degree of melt depletion. This is consistent with olivine and orthopyroxene dominating the Ni budget of residual peridotite, thus buffering the isotope composition. The composition of the BSE is constrained at δ 60/58 Ni = 0. 115 ± 0. 011 ‰. 2) Melt-metasomatised peridotites may show isotopically heavier compositions. Disequilibrium processes are required to increase δ 60/58 Ni, which is otherwise buffered by olivine and orthopyroxene. The introduction of isotopically heavy clinopyroxene can drive an increase in δ 60/58 Ni, but the exact nature of this process remains obscure.
Acknowledgements We would like to thank  Richard Brooker  for providing the Zabargad samples,  Pieter Vroon  for donating an aliquot of reference material PCC-1 and  Rick Carlson  who participated in collection and characterisation of Tariat xenoliths. Chris Coath  is acknowledged for keeping the mass spectrometers in perfect working order whilst Roel van Elsas was of great help with mineral separation. Tu-Han Luu  is thanked for providing the microdrilled meteorite samples. Stimulating discussions with  Daan Hos ,  Edgar Steenstra  and  Remco Hin  helped with interpretations of the data. The comments by associate editor  Munir Humayun ,  Frank Poitrasson  and two anonymous reviewers significantly helped to improve the manuscript. This work was funded by  STFC  through grant no. ST/M007715/1  and  ERC AdG 321209 ISONEB.
Acknowledgements. We thank  Steve Tobias  for the original motivation to perform this study. We thank  Karl-Ludwig Klein  and  Sophie Masson  for useful discussions. This work was supported by a  CEA 'Thèse Phare ' grant, by  CNRS  and  INSU/PNST program , by  CNES SHM  funds and by the  ERC Synergy  grant WholeSun. Computations were carried out using CEA CCRT and CNRS IDRIS facilities within the  GENCI  20410133 allocation, and a local meso-computer founded by DIM ACAV+. We thank  Eric Buchlin  and the  MEDOC facility  for hosting the simulation outputs.
Initial conditions The main parameters for the simulated galaxies and their host DM haloes are presented in Table  1. Similar simulation settings were used in  Rosdahl et al. (2015 Rosdahl et al. ( , 2017)). The initial conditions are generated with the makedisc code  (Springel et al. 2005). We focus most of our analysis on the higher mass galaxy that we name G9. The rotating isolated galaxy of G9 has a baryonic mass of M bar = M disc + M bulge = 3. 8 × 10 9 M , with an initial gas fraction of f gas = 0. 5, and is hosted by a DM halo of mass M halo = 10 11 M. We also compare, at the same spatial resolution, a less detailed set of results for feedback models in a ten times less massive galaxy, that we name G8, with a baryonic mass M bar = 3. 8 × 10 8 M , f gas = 0. 5 and M halo = 10 10 M. Each simulation is run for 250 Myr that is 2.