dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgment We gratefully acknowledge the cooperation of the  Kamioka Mining and Smelting Company. The Super-Kamiokande experiment has been built and operated from funding by the  Japanese Ministry of Education, Culture, Sports, Science and Technology , the  U. S. Department of energy , and the  U. C. National Science Foundation. Some of us have been supported by funds from the  National Research Foundation of Korea   NRF-2009-0083526 (KNRC) funded by the  Ministry of Education  ( 2018R1D1A3B07050696 ,  2018R1D1A1B07049158 ), the  Japan Society for the Promotion of Science , the  National Natural Science Foundation of China  under Grants No. 11620101004 , the  Spanish Ministry of Science, Universities and Innovation  (grant  PGC2018-099388-B-I00 ), the  National Science and Engineering Research Council (NSERC) of Canada , the  Scinet and Westgrid consortia of Compute Canada , the  National Science Centre, Poland  ( 2015/18/E/ST2/00758 ), the  Science and Technology Facilities Council (STFC)  and  GridPPP, UK , the  European Union 's  H2020-MSCA-RISE-2018.
The 16 AC signals are mixed with a reference signal delivered by a frequency generator whose frequency is swept, and low pass filtered with a cutoff frequency of 10 kHz. The resulting signals are then acquired by a data acquisition card NI-PXIe 6361 from National Instrument with a sampling rate of 100 kSa/s. The demodulation stage is used to measure noises at higher frequencies than the 1 MHz bandwidth of the acquisition card but also to prevent the saturation of its dynamics. The laser being very noisy at low frequencies, acquiring The experiment is composed of three parts. a) Reference filtering, to generate the reference beam via a high finesse cavity on which the repetition rate of the laser is locked. The CEO is also locked thanks to a f-2f interferometer to ensure maximum transmission through the cavity.
Implementation of the modified waveform The joint measurement of source and beyond-GR constraints have been performed for a variety of new physics parameterizations, including modification of the GW generation and propagation  [4]. Following a similar methodology, we implement the modifications of the GW signals derived from the SME framework in the GW simulation package of LALSuite. Such deformations can be anisotropic, as can be infered from the appearance of n in Eq. (  42 ) via β and δ. Here we focus on the simplest coefficients that produce dispersion and birefringence via Lorentz and CPT violating effects,i. e. , those of mass dimension 5. These coefficients are contained within β in (42) and obey the complex conjugate relation k (d) * jm = (-1) m k (d) j(-m) , for j = 0, 1, 2, 3, -j ≤ m ≤ j.
There are a priori independent coefficients in this set of terms  [26]. We display the first terms within β in SI units: β (5) = ω 2 τ (5) 2 √ πc k (5) (V)00 -3 2 sin θ e iφ k (5) (V)11 + e -iφ k (5) * (V)11 + √ 3 cos θ k (5) (V)10 +. ( 48 ) where the sky location of the source (θ, φ) appears. The coefficients are taken as expressed in the SCF in this expression. The general form of the signal observed in the interferometer is: S A = F (+) h (+) + F (×) h (×) , (49) where h (+,×) are the expressions  (42) , and F (+,×) are the (standard) detector response functions. The expressions for F (+,×) include the rotation angles relating different frames, e. g. , the merger frame and the detectors frame as defined in the LALSuite software. The effective propagation time τ parameter of equation (  48 ) is defined in equation (  40 ) as an integral function of the redshift.
Bayesian analysis After implementing the modification of the strain, we include the SME coefficients in LALInference, the parameter estimation package of LALSuite  [88]. LALInference performs Bayesian inference of the posterior probability of the GW source parameters with the inclusion of the systematic uncertainties due to the detectors resolutions. The vector set of GR prior parameters, θ GR , includes intrinsic parameters describing the binary system (e. g. the black holes masses and spins) as well as extrinsic parameters placing it in the astrophysical environment (e. g. the sky location, distance, inclination). We add to the preexisting parameters the SME coefficients (k  (5)  (V)jm ) e f f described in Section 3. 1 for the mass dimension 5 case, contained within θ SME. In order to include the correlation between the GR parameters and the SME coefficients, we perform a simultaneous inference of all the parameters, obtaining the joint posterior probability: P( θ GR , θ SME |d, I) = P(d| θ GR , θ SME ,I) P( θ GR , θ SME |I) P(d|I) , ( 50 ) where P( θ GR , θ SME |d, I) is the posterior probability, P(d| θ GR , θ SME , I) the likelihood, P( θ GR , θ SME |I) the prior probability and P(d|I) the evidence, and any pertinent background information is included in I.
Acknowledgments: The authors gratefully acknowledge the support of the  NSF  for the construction and operation of the  LIGO Laboratory  and  Advanced LIGO  as well as the  Science and Technology Facilities Council (STFC)  of the United Kingdom, the  Max-Planck-Society (MPS) , and the  State of Niedersachsen/Germany  for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the  Australian Research Council , and further support from the  Italian Istituto Nazionale di Fisica Nucleare (INFN) , the  French Centre National de la Recherche Scientifique (CNRS)  and the  Netherlands Organization for Scientific Research  for the construction and operation of the Virgo detector and the creation and support of the EGO consortium.
The XXL Survey  (Pierre et al. 2016, hereafter XXL paper I)  is the largest survey carried out with XMM-Newton, covering some 50 deg 2. One of the two XXL Survey fields, XXL-N, overlaps the field G02 of the Galaxy And Mass Assembly (GAMA) survey  (Driver et al. 2011; Liske et al. 2015; Baldry et al. 2018 ) that has nearcomplete spectroscopic coverage of galaxies (including AGNs) in a total of five fields down to a magnitude limit of r = 19. 8. In this paper, we combine the two surveys. Specifically, we utilize the matched data for XXL point sources that have GAMA counterparts. We are therefore able to explore a sample of the lowest optical luminosity (hence mass) galaxies that are able to host Xray detectable AGNs, or other potential point sources such as X-ray binaries (XRBs). Section 2 describes the data used and details our sample selection from matching XXL and GAMA [originally Sloan Digital Sky Survey (SDSS)] objects.
2016b, XXL paper VI). (The AGN luminosity function from XXL has been discussed by  Koulouridis et al. 2018 , XXL paper XIX. ) However, relatively few of the AGN are expected to be at the low redshifts required in order to study any low-luminosity hosts (see e. g. Fotopoulou et al. 2016a ). G02 and XXL-N additionally overlap with the CFHT Legacy Survey field CFHTLS-W1 (Gwyn 2012;  Heymans et al. 2012). Links to other multiwavelength and spectroscopic data for objects in the XXL-N field are provided at the XXL website. 2  The point sources in the northern field have been spatially linked to GAMA G02 galaxies by the GAMA/XXL Matching Group. The maximum allowable position difference between the X-ray and optical centroids was 10 arcsec, as in the construction of the 3XLSS source catalogue (XXL paper XXVII).
To follow up Roman's objects at z > 5, after JWST's lifetime, we need an instrument like MISC on Origins. The ELT might bring some information, though, but mainly below 2. 5 µm. Using Origins/MISC to study the Fig. 7  Left: Black hole shadow diameter versus redshift for SMBHs. Right: Flux density as a function of interferometer baseline length. In both plots the parameters for the L2-Earth baseline is shaded in purple galaxies detected at 5 < z < 10 in Roman-Deep and Roman-Wide surveys will enable critical measurements of the star formation rate (SFR), stellar mass (M), and dust attenuation. Two surveys using Origins/MISC WFI photometric and spectroscopic capabilities will provide unique data that broaden our understanding of the evolution of the mass function (cosmic mass assembly), star formation rate density, and average dust attenuation for a representative sample of galaxies at 5 < z < 10.
Acknowledgements The study was largely funded by  National Aeronautics and Space Administration (NASA) , which allowed us to hire engineering staff, subcontract parts of the study to industry and to pay for travel and meetings. The non-American team members are grateful for funding from their respective space agency and/or their research institute, in particular  Centre National de Recherche Scientifiques (CNES) ,  Swedish National Space Agency, Netherlands Institute for Space Research (SRON), Japan Aerospace Exploration Agency (JAXA). A large team of people carried out the  Origins Space Telescope study. The  Science and Technology Definitions Team  (consisting of 25 American voting members, and 14 international non-voting members) defined the satellite in open meetings with additional interested scientists joining in the discussions, and the  NASA/GSFC  Study Center Engineering Design team carried out a preliminary design.
Then, when the jet has zero or one net flavour, the jet is tagged as a gluon or quark jet, respectively. Otherwise, whenever the jet is multi-flavored, i. e. it contains two (anti)-quarks of different flavor, it pertains to what we call the 'else' category. The LO k t,g differential cross-section for these multi-flavored jets goes to zero at small k t,g and contributes to the full match result via the Σ LO else (k t,g ) term in Eq. (2. 56). Finally, as for the resummation part, we would like to comment on how to further extend the matching procedure to higher accuracy. In this case, the equivalent of the multiplicative matching formula Eq. (  2. 56) at NLO can be found in Ref. [43]  and it involves the NLO k t,g differential cross-section. The latter can be obtained by generating 3-jet events at NLO with MadGraph, or any other code dedicated to matrix element calculations.
Acknowledgements We thank  Leticia Cunqueiro ,  Raymond Ehlers  and  James Mulligan  for clarifications on the experimental aspects of the measurements reported in [31,32]. Further, we acknowledge  Keith Hamilton ,  Silvia Ferrario-Ravasio ,  Yacine Mehtar-Tani ,  Gavin Salam ,  Gregory Soyez  and  Konrad Tywoniuk  for many insightful discussions on different aspects of this calculation and their feedback on the manuscript. A. S. O. 's work was supported by the  European Research Council (ERC)  under the European Union's  Horizon 2020 research and innovation programme  (grant agreement No. 788223 , PanScales). A. T. is supported by a Starting Grant from  Trond Mohn Foundation  ( BFS2018REK01 ), the  MCnetITN3 H2020 Marie Curie Initial Training Network , contract  722104 , and wishes to thank the  Institut de Physique Théorique (IPhT)  and  Gregory Soyez  for the hospitality.
Inelastic neutron scattering (INS) experiments. We carried out INS experiments on the single crystal h-YMn1-xAlxO3 using two time-of-flight (ToF) spectrometers: the MAPS spectrometer at ISIS, UK  39  for h-YMnO3, and the 4SEASONS spectrometer at J-PARC, Japan  40  for h-YMn0. 9Al0. 1O3 and h-YMn0. 85Al0. 15O3. In the case of h-YMnO3, the data were collected at 4 K with the incident neutron energy (Ei) of 30 meV. The chopper frequency was set to 350 Hz, which yields a resolution of 0. 50 ~ 0. 80 meV depending on the energy transfer, as shown in Fig. S4. For h-YMn1-xAlxO3 with x = 0. 1 and 0. 15, the data were collected at 5 K with multiple Ei (6. 8, 10, 16, 30, and 75 meV) and the Fermi chopper frequency of 250 Hz (see Fig. S4  for the instrumental resolution), thanks to the repetition-rate-multiplication (RRM) method implemented in 4SEASONS  41.
In all experiments, the samples were mounted in the geometry of (HHL) plane horizontal and were rotated during the measurement. For the data analysis, we used the Utsusemi  42  and Horace software  43. Considering the crystal and magnetic symmetry of h-YMnO3, the data were symmetrized into the irreducible Brillouin zone, which reduced the data's statistical error. Also, as the magnon modes' dispersion along the c * -axis is negligible in h-YMn1-xAlxO3, the data were integrated over the c * -axis direction in a range of L= [-3, 3]. To acquire further information, we also carried out INS experiments in the Taipan triple-axis spectrometer at ANSTO, Australia, for h-YMnO3 and h-YMn0. 95Al0. 05O3. The data were collected at 5 K with the scattered neutron energy of 14. 86 meV.
Acknowledgments We thank  Collin Broholm  and  Daniel I. Khomskii  for fruitful discussions. This work was supported by the  Leading Researcher Program of the National Research Foundation of Korea  (Grant No. 2020R1A3B2079375 ) and the  Institute for Basic Science in Korea  ( IBS-R009-G1 ). The inelastic neutron scattering experiments at the  Japan Proton Accelerator Research Complex  (J-PARC) was performed under the user program (Proposal and No. 2016A0171  No. 2017B0005 ). M. E. Z. acknowledges financial support from  ANR, France  (Grant No. ANR-18-CE05-0023 ). The work of A. L. C. was supported by the  U. S. DOE, Office of Science, Basic Energy Sciences  under Awards  DE-FG02-04ER46174  and  DE-SC0021221.
Galaxy J1233+4959 J1349+5631 J1355+1457 J1455+6107 𝑇 e ([O ]), K 12600±1490 14860±2420 16940±1090 15030±1060 𝑇 e ([O ]), K 12340±1380 13920±2120 14920±900 14020±920 𝑁 e ([S ]), cm -3 10±10 77±130 76±59 1151±305 O + /H + ×10 The SDSS, GALEX and WISE apparent magnitudes of the selected galaxies are shown in Table  2 , indicating that these SFGs are among the faintest low-redshift LyC leaker candidates selected for HST observations. In fact, only four out of nine galaxies have been detected in the FUV range and only two galaxies are present in the AllWISE catalogue. To derive absolute magnitudes and other integrated parameters we adopted luminosity and angular size distances (NASA Extragalactic Database (NED) 1  , Wright 2006) with the cosmological parameters  0 =67. 1 km s -1 Mpc -1 , Ω Λ =0.
HST/COS OBSERVATIONS AND DATA REDUCTION HST/COS spectroscopy of the nine LyC leaker candidates was obtained in program GO 15639 (PI: Y. I. Izotov) during the period September 2019 -May 2020. The observational details are presented in Table  6. As in our previous programs  (Izotov et al. 2016a (Izotov et al. ,b, 2018a,b),b) , the galaxies were directly acquired by COS near ultraviolet (NUV) imaging. The NUV-brightest region of each target was centered in the ∼ 2. 5 arcsec diameter spectroscopic aperture (Fig. 2 ). Although the galaxies show generally a compact star-forming region superimposed upon an extended low-surface-brightness (LSB) component and, in the case of J0232-0426, several star-forming knots, their sizes are smaller than the central unvignetted 0. 8 arcsec diameter region of the spectroscopic aperture  (Fisher et al.
The 800Å setup was used for the G140L grating (COS Lifetime Position 4: wavelength range 770-1950 Å, resolving power  1050 at 1150 Å) to include the redshifted LyC emission for all targets. We obtained resolved spectra of the galaxies' Ly emission lines with the G160M grating ( ∼ 16000 at 1600 Å), varying the G160M central wavelength with galaxy redshift to cover the emission line and the nearby continuum on a single detector segment. The G140L observations of J1046+5827 and J1121+3806 were partially executed due to technical problems (Table  6 ). The individual exposures were reduced with the pipeline v3. 2. 1, followed by accurate background subtraction and co-addition with custom software  (Worseck et al. 2016). We used the same methods and extraction aperture sizes as in  Izotov et al.
ACKNOWLEDGEMENTS Based on observations made with the  NASA/ESA Hubble Space Telescope , obtained from the data archive at the  Space Telescope Science Institute. STScI is operated by the  Association of Universities for Research in Astronomy, Inc. under  NASA  contract  NAS 5-26555. Support for this work was provided by  NASA  through grant number  HST-GO-15639. 002 -Afrom the  Space Telescope Science Institute , which is operated by  AURA, Inc. , under  NASA  contract  NAS 5-26555. Y. I. and N. G. acknowledge support from the  National Academy of Sciences of Ukraine  by its priority project No. 0120U100935  "Fundamental properties of the matter in the relativistic collisions of nuclei and in the early Universe". Funding for SDSS-III has been provided by the  Alfred P. Sloan Foundation , the Participating Institutions, the  National Science Foundation , and the  U.
S. Department of Energy Office of Science. The  SDSS-III  web site is http://www. sdss3. org/. SDSS-III is managed by the  Astrophysical Research Consortium  for the Participating Institutions of the  SDSS-III Collaboration. GALEX is a NASA mission managed by the  Jet Propulsion Laboratory. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the  Jet Propulsion Laboratory, California Institute of Technology , under contract with the  National Aeronautics and Space Administration.
Results and discussion The composition of the Al x Ga 1-x As/Al y Ga 1-y As heterostructure was sim- ulated in 2D with RSoft-LaserMOD software to obtain red emission. The Al composition of the barriers, cladding layer and quantum wells were calculated to be 45% and 30% respectively. The Al compositions were calculated to be 45% for the barriers and cladding layers and 30% for the quantum wells. The thickness and composition of the bottom cladding layer is estimated to be 400 nm to avoid the optical losses in the underlying GaAs buer and silicon substrate as well. The ideal structure is presented in Figure  1. The growth of this structure by SEG-ART has been studied. To reduce the structural defects density  [21]  in the active part of the device, a 400 nm GaAs buer layer is grown inside the SiO 2 cavity before the growth of the AlGaAs cladding layer and multiple quantum wells out of the cavity.
Acknowledgments This work was supported by the  French Recherches Technologiques de Base (Basis Technological Research)  and RENATECH programs and by the  French government  managed by  ANR  under the Investissements d'avenir economic stimulus package, with reference  IRT  Nanoelec  ANR-10-IRT-05  and  ANR-15-IDEX-02. The authors want to thank  Franck Bassani  for the helpful suggestions, the  CEA-Leti clean  room sta and  Frederic Charlot  from the  CMTC platform in Grenoble.
Introduction: A plethora of geophysical, geo-chemical, and geodynamical observations indicate that the terrestrial planets have differentiated into silicate crusts and mantles that surround a dense core. The latter consists primarily of Fe and some lighter alloying elements (e. g. , S, Si, C, O, and H). There is strong evidence from measurements of the tidal deformation of the planet that the core of Mars is presently liquid. The InSight mission aims at constraining these numbers via the RISE radio tracking experiment, and the SEIS seismic package. We used data recorded by SEIS for high SNR marsquakes between March 2019 and July 2020. The InSight Marsquake Service located these events in the distance range 27-40 degrees, based on identification of P-and S-body waves. Later studies identified a number of secondary, surface-reflected phases, which were used to constrain the upper mantle.
Clinical data The patient pool consisted of 18 male patients and 1 female patient, with a mean age of 72 years, that were treated with  90    scans were resized using linear and bicubic interpolation, respectively. Overall, our dataset consisted of 76 3D volumes (i. e. , 19 patients with 4 sequences each) for a total of 9,728 2D images (Figure  2 ). For the present study, we used data only from the University Hospital of Patras departmental database. Our Institutional Review Board approved the study, and written informed consent was given by all patients to use their data.
e. , during catheterization slight differences in catheter position and angle can result in differences in the microsphere distribution. These procedural limitations can result in significant variations in dose predictions. 4, 13, 36 Based on the findings of this study, DL approaches in such an application can provide high accuracy in the prediction of the Y 90 microspheres distribution, compared to other methods (e. g. , DVK, MC, partition model). In general, the main difference in the accuracy of the result lies in the different approaches used. The DVK approach lies on the distribution of the 99m Tc-MAA (SPECT) image, while the DL is a prediction of the Y 90 (PET) distribution, using a dataset that has been trained, on real PET data. The guided mechanisms that were applied in our model not only successfully provided highly accurate dose predictions in the areas of interest but also precisely depicted the heterogeneous 90 Y biodistribution in both healthy and tumorous tissues, which could improve pretreatment decision making.
To our knowledge, ours is the only model that can depict the exact spatial biodistribution of 90 Y in the liver area, making our model especially useful for centers where PET/CT is not available. These centers must rely on post-treatment SPECT/CT imaging, which has been shown to be inaccurate. 11, 48, 51 egarding the specific training and validated data input profile of our study, three important aspects and limitations should be noted. First, we used only data from the University Hospital of Patras database, so that protocol consistency would enable stable training for our model. Several studies, for instance, have shown that parameters such as the catheter position can result in significant variations in dose predictions. 4, 13, 52 Therefore, to reduce the effect of such deviations to the maximum extent possible, we used data from a single source.
The use of this dataset, which was similar in size to those used in several other DL studies in nuclear medicine,  53  did not negatively affect our dosimetric results. However, our method was less accurate at predicting (and thus at depicting) heterogeneity in the tumorous area than in the healthy liver area. Second, to establish the model architecture of the applied hyperparameters,such as volume depths,our model architecture was adapted to the limited memory capacity of the GPU hardware used. Third, no registration between SPECT scans with the other images used for the training of our model was performed. We relied on the ability of convolutional layers within deep neural networks (such as GANs) with millions of parameters, to identify patterns in a 3D image irrespective of their position within the image.
We anticipate that registration of all our image data per patient would further optimize and improve our model's ability to predict. Finally,our study did not include patients with extended lung shunt function because predicting lung dose was outside of our current aims. Το resolve these limitations, our future goals are to: (i) augment our dataset with cases from other hospitals so that our model can be generalized, (ii) use GPUs with larger memory capacity that can perform more complicated calculations with higher-resolution images, (iii) perform image registration on all images that will be used for training, and (iv) incorporate cases with extended lung shunt function to estimate dose to the lungs as well. ] [56] [57]  However, pretreatment planning remains a challenge in nuclear medicine, mostly owing to the difficulty of accurately predicting the radionuclide biodistribution.
ACKNOWLEDGMENTS. C. M. wishes to thank  S. Cristofari  for stimulating discussions and  Laboratoire Collisions Agrégats Réactivité  and  Laboratoire de Physique Théorique  ( IRSAMC, Toulouse ) for their kind hospitality. This study has been supported through the  EUR grant NanoX  No. ANR-17-EURE-0009  in the framework of the " Programme des Investissements d'Avenir ", and research funding Grants No. ANR-17-CE30-0024 ,  ANR-18-CE30-0017  and  ANR-19-CE30-0013. We thank  Calcul en Midi-Pyrénées  ( CALMIP ) for computational resources and assistance.