dataesr/scientific-paragraphs-categorization huggingface dataset:
Since a H 2 O-layer has a much higher heat capacity than a H/He envelope, this evolutionary pathway could result in waterworlds. If K2-3 d is surrounded by a gaseous envelope, with the properties estimated here, this would likely result in surface pressure and temperature too high to support an habitable planet scenario. A better characterization of K2-3 c and K2-3 d is left to the next generation of high-precision, high-stability spectrographs and to new photometric transit observations. We have shown that an intensive observing sampling over one season with two of the best spectrographs now available would still not have detected a signal with K=1 m s -1 and a period P=44. 5 days. Assuming that our GP result is a good representation of the stellar activity contribution, this means that the true mass of K2-3 d is expected to remain unmeasurable even with a dataset of more than 500 RVs, which is currently not possible for a single target and without a collaboration among different teams.
Acknowledgements. MD acknowledges funding from  INAF through the Progetti Premiali funding scheme of the Italian Ministry of Education, University, and Research. We used high performance computing resources made available by  INAF  through the pilot programme CHIPP (through the proposal Precise planetary mass determination in radial velocity data collected with the HARPS and HARPS-N spectrographs: facing the challenges posed by the time sampling and the presence of stellar noise). We thank especially  F. Vitello  ( INAF-OACt ) for his assistance within the  CHIPP programme. This research has received funding from the  European Union Seventh Framework Programme  ( FP7/2007-2013)  under grant Agreement No. 313014  (ETAEARTH). Parts of this work have been supported by  NASA  under grants No. NNX15AC90G  and  NNX17AB59G  issued through the  Exoplanets Research Program.
AVa acknowledges support from the  California Institute of Technology (Caltech) / Jet Propulsion Laboratory (JPL)  funded by  NASA  through the  Sagan Fellowship Program  executed by the  NASA Exoplanet Science Institute. PF acknowledges support by  Fundação para a Ciência e a Tecnologia (FCT)  through Investigador FCT contract of reference  IF/01037/2013/CP1191/CT0001 , and  POPH/FSE (EC)  by  FEDER funding through the program  " Programa Operacional de Factores de Competi-tividade -COMPETE ". NCS acknowledges support by  Fundação para a Ciência e a Tecnologia (FCT, Portugal)  through the research grant through national funds and by  FEDER  through  COMPETE2020  by grants  UID/FIS/04434/2013 & POCI-01-0145-FEDER-007672  and  PTDC/FIS-AST/1526/2014 & POCI-01-0145-FEDER-016886 , as well as through Investigador FCT contract nr.
Acknowledgements. -C. S. thanks the  ERC  for support within the project  Unlimit2D. M. M. G. is grateful to the  Russian Science Foundation  (Grant No. 17-12-01265 ). T. K. gratefully acknowledges financial support by the  German science foundation (DFG)  via grants  KO3612/1-1  and  KO3612/3-1. S. H. is grateful for support within the  EPSRC Hybrid Polaritonics Grant  ( EP/M025330/1 ). B. U. thanks  ANR 2D-vdW-Spin  and  ERC  Grant No. 306719  for financial support.
ACKNOWLEDGEMENTS We acknowledge helpful discussions with  V. Vitelli  and  A. M. Turner. This work was supported by the  National Research Council of Argentina, CONICET ,  ANPCyT , and  Universidad Nacional del Sur. J. L acknowledges financial support by  Italian MIUR  under projects  PRIN-RIDEIRON-2012X3YFZ2 , and  Italian MAECI  under collaborative projects  SUPERTOP-PGR04879  and  AR17MO7.
The reconstruction of Ricci-flat spacetimes from Carrollian boundary data is conducted with a flat derivative expansion, resummed in a closed form in Eddington-Finkelstein gauge under further integrability conditions inherited from the ancestor anti-de Sitter set-up. These conditions are hinged on a duality relationship among fluid friction tensors and Cotton-like geometric data. We illustrate these results in the case of conformal Carrollian perfect fluids and Robinson-Trautman viscous hydrodynamics. The former are dual to the asymptotically flat Kerr-Taub-NUT family, while the latter leads to the homonymous class of algebraically special Ricci-flat spacetimes.
On the other hand, the stretched horizon in the membrane paradigm seems to be rather described in terms of Galilean hydrodynamics  [17, 18, 84]. Whether and how these two pictures could been related is certainly worth refining. Fundamental Physics (within the 6th International Conference on New Frontiers in Physics -ICNFP), Kolybari, Greece, August 2017, where many stimulating discussions on the topic of this work helped making progress. We thank each others home institutions for hospitality and financial support. This work was supported by the ANR-16-CE31-0004 contract Black-dS-String.
Acknowledgements We would like to thank  G. Barnich ,  G. Bossard ,  A. Campoleoni ,  S. Mahapatra ,  O. Miskovic ,  A. Mukhopadhyay ,  R. Olea  and  P. Tripathy  for valuable scientific exchanges. Marios Petropoulos  would like to thank  N. Banerjee  for the  Indian Strings Meeting, Pune, India , December 2016,  P. Sundell ,  O. Miskovic  and  R. Olea  for the  Primer Workshop de Geometría y Física, San Pedro de Atacama, Chile ,  May 2017 , and  A. Sagnotti  for the Workshop on Future of.
Results The numerical computations are carried out using the finite-element-based commercial package COMSOL v5. 2  [30]. Recent numerical work shows that the system (  9 )-(  11 ) subject to the boundary conditions (  13 ),  (14)  and either  (15)  or (  16 ) along with initial conditions (  18 )-  (20)  has multiple solutions, which can be interpreted as multiple steady-state solutions or locally stable states for the long-time dynamics. Hence, our numerical results are not exhaustive but serve to illustrate interesting solutions that can be attained under certain model situations, particularly with reference to flow-reversal solutions for the velocity profiles.
Acknowledgments: Sourav Mondal is grateful to  Engineering and Physical Sciences Research Council (EPSRC)  and the  Royal Society  for financial support. Ian M. Griffiths  gratefully acknowledges support from the  Royal Society  through a  University Research Fellowship. Florian Charlet is grateful to the  University of Oxford  for hosting him on a visiting scholarship supported by  ENSTA ParisTech. Apala Majumdar  acknowledges support from the  UK Fluids Network ,  MI-NET (Mathematics for Industry Network) , an  OCIAM Visiting Fellowship , the  Keble Advanced Studies Centre  and grants  EP/J001686/1  and  EP/J001686/2. The authors are grateful to  Oliver Whitehead  for identifying the possibility of multiple steady-state solutions.
2. D. 2 | Passive detector In order to find the beam center of the film and to place automatically a region of interest (ROI), a computer code was written on MATLAB software. The code search along the in-plane and cross plane directions was to find out the beam center from the full width at half-maximum (FWHM) of the profiles. The ROI size was 0. 6 mm for the 4 mm cone diameter and 1 mm for all the others. The film absolute dose was evaluated by taking the average of the voxels dose on the ROI. Films measurements were averaged over a series of thirteen irradiation times on different days. Monitor units (MU) number issued for each cone was calculated so as to obtain an absorbed dose in the film of about 4 Gy whatever the cone size is (Table  2 ). MU number was determined from diode SRS results.
2. G | Monte Carlo simulation The PENELOPE code  9  is one of the several general-purpose MC packages available intended for simulation of particle transport in radiation therapy. This code is reliable mostly due to the advanced physics and algorithms for their electron transport component. Here, the user-code PenEasy  13  was used. PenEasy is a modular, generalpurpose main program for the PENELOPE Monte Carlo system including various source models, tallies and variance-reduction techniques (VRT). The code includes a new geometry model for performing quadratic and voxelized geometries. The treatment heads of the Clinac 2100C were simulated according to manufacturer specifications. The geometry of the accelerator is composed of: target, primary collimator, beryllium plate, flattening filter, monitor chambers, mirror, jaws, Mylar plate, and collimator cone (see Fig.
Quantification was performed for nitrogen, oxygen and titanium elements, using the INCA Energy+software. Overlap between Ti L α and N K α lines was accounted for using a correction procedure described elsewhere  [43]. Reported atomic fraction values were an average of three measurements. The crystal structure was examined by X-ray diffraction (XRD) using a Bruker D8 diffractometer operating in Bragg-Brentano θ/2θ configuration using a Cu Kα wavelength (1. 5418 Å). XRD patterns were measured along two angular 2θ ranges, from 30°to 65°and 72°to 90°. These ranges cover the main diffraction lines of TiN, namely 111, 200, 220, 311 and 222, while avoiding the intense 400 Bragg reflection from the single-crystal Si substrate at 2θ = 69. 13°. XRD pole figure measurements were additionally carried out, using a four circle Seifert XRD 3000 diffractometer, to determine the texture of the TiN thin films.
Electrical properties were assessed by standard four-point probe technique. The average value of the electrical resistivity was calculated from measurements taken along two orthogonal in-plane directions of the coating (longitudinal and perpendicular to the projected flux). The computer code SIMTRA  [44]  was used to simulate the transport of Ti particle flux from the Ti target towards the substrate. This code provides the angular (θ, Φ) and energy distribution of neutral particles (sputtered Ti atoms and backscattered Ar) reaching the substrate, where θ and Φ represent the incidence angle and azimuthal angle, respectively. The model assumes binary elastic collisions with neutral gas atoms (Ar) until deposition on a surface occurs. Depending on the Ar working pressure, particles experience a different number of collisional events in the gas phase, which affect both their kinetic energy as well as their trajectories.
Computational results The cross-section views of the TiN thin film morphologies computed at 0. 3 and 0. 5 Pa, but also at the fictitious 0. 0 Pa, are shown in Fig. 8  using the angular distributions of Fig. 2. For the MODENA code, these angular distributions were used for both N and Ti species. The Simul3D and MODENA simulation boxes are respectively 200 px * 5 nm and 200 unit cell * 0. 212 nm, so their lateral size cannot be directly compared. Note that for better visualization of columns, contrast has been enhanced for images obtained by MODENA (original images showing layer density projection can be found in Fig. S2  of Supplementary material). Both simulations clearly reproduce a columnar growth, in fairly good agreement with the SEM observations. The nature of the arriving species (individual Ti and N particles in MODENA code and TiN building blocks in Simul3D code) does not seem to significantly alter the results.
Acknowledgements This work has been performed within the M. ERA-NET  project  MC 2 "Multi-scale Computational-driven design of novel hard nanostructured Coatings " and funded by the  French ANR program  (Project No. ANR-13-MERA-0002-02 ). BB acknowledges the financial support from the  Algerian Ministry of Higher Education and Scientific Research  through the grant n°173 of the  PNE 2016-17 program.
X-ray diffraction data Data for the structures were collected on a Rigaku Oxford Diffraction Gemini-S S1 diffractometer with a Sapphire3 detector. Cu-Ka radiation was used with a graphite monochromator and a fiber-optics Mo-Enhance collimator for HC8. The data for S-HC8 and R-HC8 were collected with synchrotron radiation (l = 0. 78965 Å) at the CRYSTAL beamline of Soleil. Data were corrected for absorption with CrysAlisPRO  (41) , and the structures were solved by iterative charge-flipping methods with Superflip  (42). The structure refinements were carried out with CRYSTALS  (43) , and all nonhydrogen atoms were refined by full-matrix least squares on F using reflections with I > 2s(I) (table  S1 ). The crystals of HC8 were tiny and scattered only weakly as diffracting crystals. Despite ~60 hours of prolonged measurement, no observable data were observed beyond 1.
System preparation On the basis of the x-ray structures, we embedded ca. 3-nm-wide I-quartet channel patches in a mixed PC/PS/Chl lipid bilayer envi-ronment. We used the Mercury 3. 5. 1 software to fill the crystallographic unit cell with missing molecules, and then we replicated it keeping two, six, and eight slices in x-, y-, and z-axis directions, respectively, resulting in a 96-molecule patch. The three HC8, R-HC8, and S-HC8 systems include respectively two, six, and six water channels that we inserted in a pre-equilibrated triclinic membrane patch containing a 5:4:1 ratio of Chl/PC/PS molecules. We deleted overlapping water and lipid molecules and added a concentration of roughly 50 mM Na + Cl - to the solvent, as well as an excess of Na + ions to neutralize the system charge induced by the negatively charged PS lipids.
MD simulation conditions Simulations were performed using the CHARMM-36 force field  (46)  for lipid molecules and the TIP3P model  (47)  for water. To represent the HC8, R-HC8, and S-HC8 molecules and generate their topologies, we used the CHARMM General Force Field  (48)  together with the ParamChem web service  (49). The GROMACS 4. 6 software (50) was used to run the simulations with virtual interaction sites allowing a 5-fs integration time step. All bonds were constrained using the LINear Constraint Solver algorithm. Particle mesh Ewald electrostatics was used with a 10 Å cutoff with the Verlet buffer scheme for nonbonded interactions; the neighbor list was updated every 20 steps. Three baths (imidazoles, lipids, and water and ions) were coupled to a temperature of 310 K using the Bussy velocity rescaling thermostat with a time constant t = 0.
Acknowledgments Funding: This work was conducted within  DYNAFUN  ( ANR-15-CE29-0009 ) (M. B. ) and the  LabEx CheMISyst  ( ANR-10-LABX-05-01 ) (I. K. ). The study was further supported by the " Initiative d'Excellence" program  from the  French State  (grants " DYNAMO ,"  ANR-11-LABX-0011-01 , and  ANR-11-EQPX-0008 ). Computational work was performed using High Performance Computing (HPC) resources from  GENCI-CINES  (grant number  2016-072292 ) to  M. Baaden. Funding to G. B. was from his  Rensselaer Endowed Chair Fund  ( 140124 ) and from the  U. S. Department of Energy, Basic Energy Sciences  ( DE-FG02-09ER16005 ) for the QCM-D measurements and calculations. H. V. , S. E. S. , and P. B. P. were supported by The  Arnold  and.
Acknowledgments This work was supported by  Labex NUMEV  (contract numbers:  ANR-10-LABX-20  projects  2013-2-021  and  AAP 2014 026 ) and Agropolis fondation in the context of APLIM (Advanced Plant Life Imaging) project (contract  1504-005 ). The Authors would like to thank reviewers for their careful reading and their constructive remarks.
Acknowledgements EB work is partially supported by the  Abdus Salam International Centre for Theoretical Physics (ICTP, Trieste, Italy)  through the  Office of External Activities (OEA)-Prj-15. The ICMPA is in partnership with the  Daniel Iagolnitzer Foundation (DIF) ,  France. DOS research at  Max-Planck Institute  is supported by the  Alexander von Humboldt foundation.
Electron candidates are identified by the association of a charged-particle track from the PV, with energy deposits clusters (superclusters) in the ECAL. The association takes into account energy deposits both from the electron and from bremsstrahlung photons produced during its passage through the inner detector. The electron momentum is estimated by combining the energy measurement in the ECAL with the momentum measurement in the tracker. The experimental mass resolution for barrel-barrel (barrel-endcap) dielectron pairs with a mass of 1 TeV is 1. 0 (1. 5)%  [20]. To correct for observed discrepancies in energy scale and resolution between data and simulation, the measured electron energy is adjusted by a multiplicative factor that depends on η and R 9 , where R 9 is the ratio of the energy in a 3×3 matrix of ECAL crystals, centered on the crystal with the largest energy, to the full energy collected by a supercluster.
Results The strategy followed in this analysis is to search for deviations from the shape of the m jj distribution expected in the standard model. This distribution extends over a range of several TeV. While the LR symmetric models motivate the choice of the jj final state, we do not impose requirements on the signal shape specific to these models, in order to maintain sensitivity to other models. The strategy to search for an excess of events in a wide mass range is effective in analyzing the data without exploiting other characteristics of the benchmark signal model and reduces the effect of the uncertainties in the shapes of the backgrounds, especially in the highm jj region. The expected number of signal and background events is estimated by counting the events falling in a particular m jj window.
The LISA Pathfinder charge management device was responsible for neutralising the cosmic ray induced electric charge that inevitably accumulated on the free-falling test masses at the heart of the experiment. We present measurements made on ground and in-flight that quantify the performance of this contactless discharge system which was based on photo-emission under UV illumination. In addition, a two-part simulation is described that was developed alongside the hardware. Modelling of the absorbed UV light within the Pathfinder sensor was carried out with the GEANT4 software toolkit and a separate MATLAB charge transfer model calculated the net photocurrent between the test masses and surrounding housing in the presence of AC and DC electric fields. We confront the results of these models with observations and draw conclusions for the design of discharge systems for future experiments like LISA that will also employ free-falling test masses.
In addition, a significant net charge could also be transferred to the test masses during their initial release as well as after any subsequent re-grabbing maneuvers. Due to work function differences between surfaces in last direct mechanical contact as well as triboelectric processes, this was predicted to be of order 10 8 e. To mitigate the effects of test-mass charging, Pathfinder included a Charge Management System (CMS) as part of the LISA technology package (LTP) instrument. While other sensitive space-borne accelerometers, such as CHAMP  [11] , GRACE  [12] , GOCE  [13]  and MICROSCOPE  [14]  have relied on a physical electrical connection to control the charge of the test mass, in order to reach the desired force noise goals for LISA, a contactless method is essential. The Pathfinder CMS exploited the same principles of photo-emission under UV illumination as successfully demonstrated in the Gravity Probe B (GP-B) mission  [15].
B. Photoelectron Flow Model Written in MATLAB, the photoelectron flow model uses the output of the ray trace to estimate the apparent yield of the system, given the photoelectric properties of individual surfaces as well as any applied AC or DC electric fields. The model simplifies the problem by splitting the sensor up into pairs of adjacent surfaces on the test mass and electrode housing and treating them like parallel plates with a uniform electric field between them. The model calculates the net photoelectron flow between each surface pair while taking into account any instantaneous electrical potential difference as well as the energy distribution of the emitted photoelectrons. The system is then stepped in time, applied AC voltages recalculated and the test mass potential updated due to any charge transfer in the previous step.
During a weekly spacecraft station keeping period the CMS was used to discharge the test masses to a set level, for example -80 mV, taking around 30 minutes. Incident cosmic rays then gradually charged the test masses positively until the next station keeping; at which point the CMS reset the test masses' charge to the desired level. At the start of the mission this was performed weekly but was later reduced to every two or three weeks allowing longer uninterrupted science runs. Initially these fast discharges were done open-loop by bringing the test mass to an equilibrium potential that had been shifted by applying appropriate DC voltages during the discharge. While this method was both simple and reliable it was also fairly inefficient when it came to lamp usage. Once confidence in the system's performance had increased these routine fast discharges were instead handled by the automated closed-loop CMS software.
A. Long Term Stability As explained previously, the apparent yield for a particular lamp is dependent on the state of the system at the time of the measurement. To make a clean assessment of the stability of the photoelectric properties over course of the mission a sub-set of measurements need to be chosen that were made with the system in a reproducible state. The automated discharges carried out during the regular station keeping periods offer an ideal dataset for this. Functionally, the automated CMS software performed a discharge in the same way each time. After first measuring the test mass charge by applying a dither voltage it then calculated the appropriate lamp setting and duration to reach the requested level of final test mass charge. Following illumination it would remeasure the test mass charge and determine if it was within a predefined range of success.
ACKNOWLEDGEMENTS This work has been made possible by the  LISA Pathfinder mission , which is part of the  space-science program  of the  European Space Agency. The French contribution has been supported by  CNES  ( Accord Specific de  Projet No. CNES 1316634/CNRS 103747 ), the  CNRS , the  Observatoire de Paris  and the  University Paris-Diderot. E. Plagnol  and  H. Inchauspé  would also like to acknowledge the financial support of the  Uni-vEarthS Labex program  at  Sorbonne Paris Cit  (Grants No. ANR-10-LABX-0023  and No. ANR-11-IDEX-0005-02 ). The Albert-Einstein-Institut acknowledges the support of the  German Space Agency, DLR. The work is supported by the  Federal Ministry for Economic Affairs and Energy  based on a resolution of the  German Bundestag  (Grants No. FKZ 50OQ0501  and No.
(2010 Roseboom et al. ( , 2012)) , whilst those selected from the HerMES Large Mode Survey (HeLMS) are amongst the 477 red galaxies presented by 21 These targets were initially chosen for follow-up observations as their preliminary, albeit shallow, data at ∼ 850-µm suggested that they were robust detections. Asboth et al. (2016). All HerMES images and catalogs were accessed through the Herschel Database in Marseille  (HeDaM -Roehlly et al. 2011)   22.
6 hr was spent integrating on each target. Maps with longer integration times (t int 10 hr) provide deeper data sensitive to less luminous DSFGs in the vicinity of our signposts. Our shallower maps (t int 1 hr) help constrain the abundances of the brightest DSFGs, thus reducing the Poisson noise associated with these rare galaxies. These deep/shallow 870-µm data are necessary to constrain the photometric redshifts of the brighter/fainter DSFGs within the vicinities of our signposts, therefore allowing us to identify members of any candidate proto-cluster found. During our observations, we recorded typical precipitable water vapor (PWV) values between 0. 4-1. 3 mm, corresponding to a zenith atmospheric opacity of τ = 0. 2-0. 4. Finally, the flux density scale was determined to an r. m. s. accuracy of σ calib ≈ 7% using observations of primary calibrators, Uranus and Neptune, whilst pointing was checked every hour using nearby quasars and found to be stable to σ point ≈ 3 ′′ (r.