dataesr/scientific-paragraphs-categorization huggingface dataset:
J. G. F-T is supported by FONDECYT No. 3180210. D. M. is supported by the BASAL Center for Astrophysics and Associated Technologies (CATA) through grant AFB 170002, and by project FONDECYT Regular No. 1170121. D. G. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) BASAL grant AFB-170002. D. G. also acknowledges financial support from the Dirección de Investigación y Desarrollo de la Universidad de La Serena through the Programa de Incentivo a la Investigación de Académicos (PIA-DIDULS). T. C. B. acknowledges partial support for this work from grant PHY 14-30152: Physics Frontier Center / JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation. S. V. gratefully acknowledges the support provided by Fondecyt reg.
n. 1170518. J. A. -G. acknowledges support from Fondecyt Regular 1201490 and from ANID, Millennium Science Initiative ICN12_009, awarded to the Millennium Institute of Astrophysics (MAS). S. O. S acknowledges the FAPESP PhD fellowship 2018/22044-3. A. P-V acknowledges the FAPESP postdoctoral fellowship no. 2017/15893-1 and DGAPA-PAPIIT grant IG100319. B. B acknowledge partial financial support from FAPESP, CNPq, and CAPES -Finance Code 001. B. T. gratefully acknowledges support.
Acknowledgements. The authors thank the expert anonymous referee, who provided generous detailed feedback that substantially improved the paper. We gratefully acknowledge data from the  ESO   Public Survey program  ID 179. B-2002 taken with the VISTA telescope, and products from the  Cambridge Astronomical Survey Unit (CASU)  and from the  VISTA Science Archive (VSA). This publication makes use of data products from the WISE satellite, which is a joint project of the  University of California, Los Angeles , and the  Jet Propulsion Laboratory/California Institute of Technology , funded by the  National Aeronautics and Space Administration. This research has made use of NASAs Astrophysics Data System Bibliographic Services and the SIMBAD database operated at  CDS, Strasbourg, France.
The NNPDF30lo PDF set was used. The parton showers and hadronisation were modelled with P 8. 186 using the A14 tune. Theoretical cross-sections were used to normalise background contributions. The cross-sections of single-top-quark -and -channel production were calculated with the Hathor v2. 1 program  [57, 58] , while the -channel followed the prescriptions from Refs. [59, 60]. Cross-sections for diboson production were calculated at NLO  [55, 61]. The normalisations of  +jets and  t contributions were estimated from data using the control regions as described in Section 6. 1.
Categorisation of production processes For the three production processes shown in Figure  1 , the ggF and DY processes have the same final states while the VBF process possesses two additional jets, called VBF-tag jets. The kinematics of these jets differ from those from the -boson hadronic decays. They are typically well separated in pseudorapidity and usually have large dĳet invariant mass. These characteristics were used in previous searches  [22, 23]  to separate VBF production from ggF/DY production. In this search, a recurrent neural network (RNN)  [74, 75]  is used to classify the VBF and ggF/DY event topologies. It is built with the Keras  [76]  library using the Theano python library  [77]  as a back end for mathematical computations. The RNN has 2 hidden layers with 25 recurrent cells to exploit the hidden correlation of the input sequence.
Comparisons of the limits Table  5  summarises the observed and expected 95% CL lower limits on the masses of the resonances in the benchmark models studied in this paper. These mass limits and the cross-section upper limits presented above are significantly more stringent than those published previously from similar searches. The cross-section upper limits are a factor of three or more lower than those of the search using the same data set, but in the hadronic  →  final state  [16]. Compared to the searches with the 36. 1 fb -1 data set in the same leptonic final states  [22, 23] , an improvement of a factor of three or more in the cross-section upper limits is also obtained for most of the searches at the highest masses. The observed lower mass limits of this search for the HVT  and  as well as for the RS graviton are also similar to those from the combinations of searches in the fully-leptonic, semi-leptonic, and fully-hadronic final states from smaller datasets of ∼ 36 fb -1  [12, 15].
Summary Searches for the production of heavy diboson resonances are performed using the proton-proton collision data with an integrated luminosity of 139 fb -1 at √  = 13 TeV. The data were recorded by the ATLAS experiment between 2015 and 2018 at the LHC. The ,   and   decay modes of the heavy resonances in the 0-lepton, 1-lepton and 2-lepton final states are considered. The data are found to be in good agreement with background expectations. Upper limits on the production of heavy resonances in the mass range 300-5000 GeV through gluon-gluon fusion, Drell-Yan or vector-boson fusion processes are derived for Standard Model extensions with an additional neutral scalar, a heavy vector triplet, or warped extra dimensions. Combining the  and   decay modes, the observed 95% confidence-level upper limit on (   →  → ) for the ggF (VBF) process ranges from 1.
9 (4. 3) TeV and a  boson with ( ) < 3. 5 (3. 9) TeV. France; SRNSFG, Georgia; BMBF, HGF and MPG, Germany; GSRT, Greece; RGC and Hong Kong SAR, China; ISF and Benoziyo Center, Israel; INFN, Italy; MEXT and JSPS, Japan; CNRST, Morocco; NWO, Netherlands; RCN, Norway; MNiSW and NCN, Poland; FCT, Portugal; MNE/IFA, Romania; MES of Russia and NRC KI, Russia Federation; JINR; MESTD, Serbia; MSSR, Slovakia; ARRS and MIZŠ, Slovenia; DST/NRF, South Africa; MICINN, Spain; SRC and Wallenberg Foundation, Sweden; SERI, SNSF and Cantons of Bern and Geneva, Switzerland; MOST, Taiwan; TAEK, Turkey; STFC, United Kingdom; DOE and NSF, United States of America. In addition, individual groups and members have received support from BCKDF, CANARIE, Compute Canada and CRC, Canada; ERC, ERDF, Horizon 2020, Marie Skłodowska-Curie Actions and COST, European Union; Investissements d'Avenir Labex, Investissements d'Avenir Idex and ANR, France; DFG and AvH Foundation, Germany; Herakleitos, Thales and Aristeia programmes co-financed by EU-ESF and the Greek NSRF, Greece; BSF-NSF and GIF, Israel; La Caixa Banking Foundation, CERCA Programme Generalitat de Catalunya and PROMETEO and GenT Programmes Generalitat Valenciana, Spain; Göran Gustafssons Stiftelse, Sweden; The Royal Society and Leverhulme Trust, United Kingdom.
Acknowledgements We thank  CERN  for the very successful operation of the LHC, as well as the support staff from our institutions without whom ATLAS could not be operated efficiently. We acknowledge the support of  ANPCyT , Argentina; YerPhI, Armenia;  ARC, Australia ;  BMWFW  and  FWF , Austria; ANAS, Azerbaĳan; SSTC, Belarus;  CNPq  and  FAPESP, Brazil ;  NSERC ,  NRC  and  CFI ,  Canada ; CERN;  ANID, Chile ;  CAS ,  MOST  and  NSFC, China ;  COLCIENCIAS, Colombia; MSMT CR, MPO CR  and  VSC CR, Czech Republic ;  DNRF  and  DNSRC, Denmark ;  IN2P3-CNRS  and  CEA-DRF/IRFU ,.
We generate two-photon mediated final states using DIAG36  [20]  and TREPS  [21]. The DIAG36 program is applied for the e + e -qq production as well as for the e + e -e + e -and e + e -µ + µ -processes. We use TREPS to generate the e + e -pp final state with its cross section tuned to the known measurements. Additionally, MC samples for suppressed decays  [22]  τ -→ π -e + e -ν τ and π -µ + µ -ν τ are used to study possible background contaminations. We follow a "blind" analysis technique in this search, where the signal region (defined below) in data remains hidden until all of our selection criteria and background estimation methods are finalized. Below we describe different stages of event reconstruction and selection. All kinematic observables are measured in the laboratory frame unless stated otherwise.
Clinical data Clinical data used for the purpose of this study consisted in SEEG signals collected in a patient with drug-resistant focal epilepsy that required invasive EEG exploration. Recordings were performed using intracranial multichannel electrodes (DIXI Medical, 5-18 contacts; length, 2 mm, diameter, 0. 8 mm; 1. 5 mm apart). Electrodes were implanted according to the stereotactic method of Talairach  [22]. SEEG signals were recorded on a Deltamed™ system on a maximum number of channels equal to 128, and were sampled at 256 Hz and recorded to hard disk (16 bits/sample) using no digital filter. The only filter present in the acquisition procedure was a hardware analog high-pass filter (cut-off frequency of 0. 16 Hz) used to remove very slow variations that sometimes contaminate the baseline.
The resulting dependence is demonstrated in the curve shown in Fig. 3. The first step in this calculation is to run TRANSP simulations  [18]  for a set of pure D reference plasmas in similar conditions as the mixed isotope experiments. This is necessary to quantify the discrepancy between measured and calculated neutron rates, which is typically found on JET  [19] , for this set of plasmas. A key assumption in the method is that any discrepancy in the neutron rate is consistent for the relevant plasma parameters over a range of H/D ratio. Pure D reference plasmas were taken from both the 2013 and 2014 JET campaigns, 3 pulses from each campaign  [12]. The plasma current, toroidal field, NBI power, Z ef f , average density and temperature were similar to the plasmas used in this experiment. TRANSP simulations were performed with fitted profile data from high resolution Thomson scattering (HRTS) and core Thomson scatting (LIDAR) for electron density and temperature, charge exchange recombination spectroscopy (CXRS) for toroidal rotation and ion temperature, horizontal visible bremsstrahlung for Z ef f , assuming beryllium as the sole impurity, and using the TRANSP internal equilibrium solver.
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 and 2019-2020 under grant agreement No 633053 and from the RCUK Energy Programme [grant number EP/I501045]. The views and opinions expressed herein do not necessarily reflect those of the European Commission. The support from the H2020 Marie-Sklodowska Curie programme (Grant No. 708257) and the Spanish Ministry of Economy and Competitiveness (Grant No. FJCI-201422139) is gratefully acknowledged.
We clearly observe that the nucleus shape evolves over an 8 µm propagation range, as seen Fig. 5  where the nuclear size varies from 8 to 11 µm. Using a 3D slicing package from the Image J software suite, we have compiled the displayed slices to achieve a 3D representation of the sample, which is available in the supplementary material (movie). The 3D rendering is satisfying but we notice that the depth resolution (theoretically of 700 nm) limits the quality of the Z perception.
Acknowledgement We acknowledge support from the  CEA/DRF   Impulsion program  with the grant " NanoBiom", Défi "IMAG'IN"CNRS grant program  " Nano-bio-4D. We acknowledge support from  Région Ile de France  through the  DIM ELICIT program , grant IMAChip and the  Action de Soutien à la Technologie et à la Recherche en Essonne  ( ASTRE) program  through the  "NanoLight " project. We acknowledge financial support from the  European Union  through the  Future and Emerging Technologies (FET) Open H2020: VOXEL (grant   665207 ) and  PETACom  (grant  829153 ) and the integrated initiative of European laser research infrastructure ( LASERLAB-EUROPE)  (grant agreement no. 654148 ). Support from the  French ministry of research  through the 2013  Agence Nationale de Recherche (ANR)  grants "NanoImagine", 2014 "ultrafast lensless.
* This research was supported by the  ONR  Contracts  N00014-11-1-0712 ,  N00014-12-1-0561 , and  N00014-15-1-2181 ; the  NSF  Grants  DMS 1222715 ,  DMS 1720297 ,  DMS 1222390 , and  DMS 1521067 ; the  Institut Universitaire de France ; The  European Research Council  under grant  ERC  AdG  338977  BREAD; and by the  SmartState and Williams-Hedberg Foundation.
ACKNOWLEDGMENTS We thank  Masha Baryakhtar ,  Saptarshi Chaudhuri ,  Aaron Chou ,  Peter Graham ,  Anson Hook ,  Junwu Huang ,  Yonatan Kahn ,  Robert Lasenby ,  Steve Ritz , and  Jesse Thaler  for valuable discussions. AB is supported by the  James Arthur Fellowship. SE, PS, and NT are supported by the  U. S. Department of Energy  under Contract No. DE-AC02-76SF00515. SE is also supported by the  Swiss National Science Foundation ,  SNF  project number  P400P2 186678. KZ is supported by the  NSF GRFP  under grant  DGE-1656518. RTD thanks MIAPP and KITP for their hospitality and support. SE.
Global Asteroseismic Parameters To perform asteroseismic analysis on TOI-257 we produced a custom light curve using the TESS Asteroseismic Science Operations Center (TASOC,  Lund et al. 2017 ) photometry pipeline 5   (Handberg et al. , in prep. ) , which is based on software originally developed to generate light curves for data collected by the K2 Mission  (Lund et al. 2015). The TASOC pipeline implements a series of corrections to optimize light curves for an asteroseismic analysis  (Handberg & Lund 2014) , including the removal of instrumental artefacts and of the transit events using a combination of filters utilizing the estimated planetary period. The photometric performance of the TASOC light curve was comparable to the light curve produced by the SPOC pipeline. Solar-like oscillations are broadly described by a frequency of maximum oscillation power ( max ) and a large frequency separation (Δ), which approximately scale with log  and the mean stellar density, respectively (see,  García & Ballot 2019).
From the joint analysis, we find that TOI-257 hosts a sub-Saturn sized planet with a radius of   = 0. 639 ± 0. 013 R J (7. 16 ± 0. 15  ⊕ ) and mass of   = 0. 138 ± 0. 023 M J (43. 9 ± 7. 3  ⊕ ), on a circular ∼ 18. 4 day orbit. To ensure that our results are not potentially biased from the use of the  Claret & Bloemen (2011)   in EXOFASTv2, we ran two additional transit only circular models, one with and one without the Claret and Bloemen tables (setting the NOCLARET flag in EXOFASTv2 such that  1 and  2 are completely free parameters). Both transit only models provided consistent results confirming the stellar and planetary parameters are not being biased by the EXOFASTv2 Claret and Bloemen interpolation tables. Whilst we do find that the circular model provides a somewhat better fit to the TESS light curve and radial velocity data than compared with the eccentric model, the planet could still be on an eccentric orbit given the ∼ 3.
Complementary Analysis, and Limits on Additional Planets We further analyze the radial velocity data set in Table  2  with RadVel  (Fulton et al. 2018 ) to provide both an independent analy-Table  4. Median values and 68% confidence interval for TOI-257 from the MCMC EXOFASTv2 analysis of both eccentric and circular orbital models. Notes. -M-A T3, M-A T4, and M-A T6 are M -Australis Telescope3, Telescope4, and Telescope6, respectively. * The time of conjunction that is closest to the starting value supplied as a prior and is typically a good approximation for the mid transit time. ∧ The equilibrium temperature of the planet assumes no albedo and perfect heat redistribution. ★ The tidal circularization timescale is calculated using Equation 3 from  Adams & Laughlin (2006)  and assuming a  = 10 6.
† TESS LC1 is the TESS light curve from PDC and TESS LC2 is the TESS light curve produced using the  Vanderburg et al. (2019)   13. 9 +1. 7 -1. 4 14. 0 +1. 7 -1. 4 13. 9  The radial velocity measurements from each instrument have been binned by day for clarity, however, the analysis was performed using the unbinned data. M -Australis radial velocities are represented by the purple filled-in circles. Radial velocities from FEROS and HARPS are the lime green and gold filled-in circles, respectively. The best-fit model is plotted as the dashed grey line and the center-of-mass velocity has been subtracted. The bottom panel shows the residuals between the data and the best-fit model. sis for checking consistency in the mass and eccentricity of planet b, and to search for any additional planets.
The search for additional planets is motivated by two reasons. First, moderately eccentric Keplerian signals can sometimes resolve into two near-circular resonant signals with additional radial velocity data (e. g. Wittenmyer et al. 2013; Trifonov et al. 2017; Boisvert et al. 2018; Wittenmyer et al. 2019). Second, we wish to evaluate the multiplicity of systems like TOI-257 with warm sub-Saturns. The combined analysis of the HARPS, M -Australis, and FEROS data sets are consistent with a planet at the known transiting period and   from Table  4. The circular orbital solution is marginally favored over an eccentric model (in agreement with -Australis radial velocities. There is no significant correlation between the bisector velocity span and the radial velocities. the ExoFASTv2 analysis), according to the relative small-sample Akaike Information Criterion (ΔAICc = 3.
DISCUSSION Here we have presented the discovery of TOI-257b, the first M -Australis led confirmation of a TESS transiting planet candidate. TOI-257b is a warm sub-Saturn planet with a radius ∼ 24% smaller than Saturn (  = 7. 16 ± 0. 15  ⊕ ) and a mass ∼ 54% less than Saturn (  = 43. 9 ± 7. 3  ⊕ ) on an orbit of  = 18. 38818 +0. 00085 -0. 00084 days. The measured mass and radius give a mean density of 0. 65 +0. 12  -0. 11 g cm -3 , consistent with the density of Saturn (0. 687 g cm -3 ) and less dense than Jupiter (1. 326 g cm -3 ). Therefore, based on the mass, radius, and bulk density of this planet, it lies within the regime of planets classified as 'Neptunian worlds' by  Chen & Kipping (2017). Further analysis of the radial velocity data also reveals hints for a second sub-Saturn mass planet (  = 70 ± 14  ⊕ ) in the system with an orbit of ∼ 71 days.
However, additional high-precision radial velocity data is required to confirm the planet c candidate. To understand the planet formation process, we must determine the bulk compositions of warm sub-Saturns such as TOI-257b, a class of planet which is absent from the Solar System. Such objects provide important data for astronomers studying planetary interiors   5  (width is ±1), and harmonics 2/ rot , 3/ rot. The orange line includes a Gaussian Process (GP) to model stellar-activity with a quasiperiodic kernel with priors listed in Table  5 , while the black line models remaining jitter as per-instrument Gaussian noise. The dashed line represents the window function (arbitrary scaling). Top: A 1-planet circular model tested at a wide range in fixed periods, fitting for  ,   and the relative instrument dependent offsets and noise terms (or single GP).
CONCLUSIONS We report the discovery of TOI-257b, a   = 0. 639 ± 0. 013 R J (  = 7. 16  ⊕ ) and   = 0. 138 ± 0. 023 M J (  = 43. 9  ⊕ ) transiting planet found by TESS and confirmed using radial velocity data from M -Australis, FEROS, and HARPS as well as direct imaging from SOAR and Zorro. We also find hints for an additional non-transiting long-period (∼ 71 day) sub-Saturn mass planet candidate orbiting TOI-257 from analysis of the radial velocity data. TOI-257b belongs to a population of exoplanets between the sizes of Neptune and Saturn that appears to be rare. Furthermore, TOI-257b transits a very bright star ( = 7. 612 mag) on a relatively long-period orbit of 18. 423 days making it a great candidate for future follow-up observations to measure its spin-orbit alignment and transmission spectrum.
ACKNOWLEDGEMENTS We thank the anonymous referee for their careful review of the manuscript that has led to significant improvements. M -Australis is supported by  Australian Research Council LIEF  Grant  LE160100001 ,  Discovery Grant   DP180100972 ,  Mount Cuba Astronomical Foundation , and institutional partners  University of Southern Queensland ,  UNSW Australia, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida , and  The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognise their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the M -Australis facility at Mt Kent is situated.
The purpose of this work is to finally complete the set of scalar self-energy diagrams in the gauge coupling for general renormalisable theories, and provide the tadpole diagrams at the same time. This completes the set that was promised in Ref. [112]. In this paper we present the analytic expressions and the technical machinery that we have used, specialising to the Feynman gauge. However, since the final results (and therefore this paper) are rather long, we have created a new package TLDR where they are available in computer-readable form. Readers wishing to skip the details and apply the results are invited to download the code from: http://tldr. hepforge. org While some of the evaluation of spinor/Lorentz traces and tensor reduction for specific models could be accomplished using TwoCalc  [120]  and TARCER  [121]  (of which we have made use) we derived some reduction rules not available there with the help of the general relations of Refs.
However, such an approach does not respect the order of perturbation theory or gauge invariance. † Hence, we shall simplify the expressions where all couplings and masses are expressed in terms of tree-level parameters, so that the reader may use any of the other approaches. In this way, we are also able to make extensive use of relationships amongst the couplings in general theories, and so reduce the number of topologies to 16 for tadpoles and to 58 for self-energies for non-Goldstone boson scalars. To apply the results in practice for all but the simplest of models is a task for a computer. Even for the Standard Model it would be far too tedious to implement by hand. Hence, we have provided our results in electronic form as part of TLDR. All reduction rules are included so that the renormalised expressions can be applied for any physically relevant configurations of masses and momenta, in the form of Mathematica modules and notebooks, with code to link from Mathematica to TSIL.
A user manual is provided online. In the future we also intend to include c++ code to link to TSIL for use with packages such as SARAH, the (currently private) results for Landau and general R ξ gauges, and extensions to vector/mixed scalar-vector/fermion self-energies. † Moreover, theories with genuine Goldstone bosons would still suffer the GBC. Hence, in our integral reductions, we must still deal with infra-red singularities. In this work, we do so by means of dimensional regularisation: all infrared divergent diagrams acquire poles in the dimensional regulator. This actually provides yet another solution to the GBC; we shall elaborate on the connection more clearly elsewhere.