dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgements This work was partially supported by the  FP7 Ideas: European Research Council  for the Advanced Grants COXINEL (340015, PI: M. -E. Couprie) and X-Five (339128, PI: V. Malka), the  EuPRAXIA design study  ( 653782 ), the  Fondation de la Coopération Scientifique  ( QUAPEVA-2012-058T ), the  Agence Nationale de la Recherche  ( ANR-10-LABX-0039-PALM, LABEX CEMPI ANR-11-LABX-0007 ),  Ministry of Higher Education and Research, Hauts de France council and European Regional Development Fund (Contrat de Projets Etat-Région CPER Photonics for Society   P4S ). The authors acknowledge J. Daillant,  A. Nadji ,  A. Taleb  and  A. Rousse  for their support. The authors thank  A. Thompson  and  S. Podgorny  for English check. The authors would like also to thank members of the Accelerator and Engineering Division and of the  Experimental Division of SOLEIL  for their help,  J.
Given the similarities of the search of continuum sources and emission lines, any advancement in the understanding of completeness and fidelity of line searches can be applied to source detection and number counts computation for both samples. Here we present the emission line and continuum detections in the band 3 (3 mm) data from the ASPECS Large Program (hereafter ASPECS-LP), an ALMA large program that expands the legacy of ASPECS-Pilot to over a 4. 6 region within the UDF, i. e. five times larger than the ASPECS-Pilot coverage (Fig. 1 ), using the same frequency setup and with similar sensitivity. A general presentation of the ASPECS-LP is given in a companion publication by  Decarli et al. (2019). ASPECS-LP offers the unique opportunity to test and compare line search algorithms by allowing the confirmation of line candidates with alternative methods.
We chose to work with both datasets separately because the combination injected artifacts in the data cubes while adding a modest increase in sensitivity in a small region of the map. The ASPECS-LP, which covers a five times larger area than ASPECS-Pilot (Fig. 1 ), was mapped with 17 Nyquist-spaced pointings in band 3 cover an area of 4. 6 arcmin 2 (within mosaic primary beam correction ≥ 0. 5, see details in  Decarli et al. (2019) ). A small portion of the ASPECS-Pilot coverage is not covered by the ASPECS-LP. The ASPECS-LP observations in band 3 were made in antenna configuration C40-3. This antenna configuration should return a synthesized beam similar in size to the one that will be obtained for the ASPECS-LP band 6 observations. In both cases, the beam size was chosen to be as sensitive as possible to any extended emission.
Data reduction, calibration and imaging The data was processed using both the CASA ALMA calibration pipeline  (v. 4. 7. 0; McMullin et al. 2007 ) and our own scripts (see, e. g. ,  Aravena et al. 2016a) , which follow a similar scheme to the ALMA manual calibration scripts. Our independent inspection for data to be flagged allowed us to improve the depth of our scan in one of the frequency settings by up to 20%. In all the other frequency settings, the final rms appears consistent with the one computed from the cube provided by the ALMA pipeline. As the cube created with our own procedures is at least as good (in terms of low noise) as the one from the pipeline, we will refer to the former in the remainder of the analysis. We imaged the 3 mm cube with natural weighting using the task tclean, resulting in synthesized beam sizes between 1.
ALMA#2016. 1. 00324. L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We have made available online LineSeeker, the code used to search for emission lines in this work. The code is available as a set of Python scripts that search for emission line candidates and returns the different fidelities estimates described above. The website for the download can be found in the software section below. The Geryon cluster at the Centro de Astro-Ingenieria UC was extensively used for the calculations performed in this paper.
BASAL CATA PFB-06, the Anillo ACT-86, FONDEQUIP AIC-57, and QUIMAL 130008 provided funding for several improvements to the Geryon cluster. "Este trabajo contó con el apoyo de CON-ICYT + Programa de Astronomía+ Fondo CHINA-CONICYT". JGL acknowledges partial support from ALMA-CONICYT project 31160033. D. R. and R. P. acknowledge support from the National Science Foundation under grant number AST-1614213. IRS acknowledges support from the ERC Advanced Grant DUSTY-GAL (321334) and STFC (ST/P000541/1). FEB acknowledges support from CONICYT grant Basal  AFB-170002, and    SExtractor  (Bertin & Arnouts 1996) , LineSeeker.
We then studied the number of possible SD detections using an ESA software called MASTER (Meteoroid and SD Terrestrial Environment Reference). With the Mini-EUSO Engineering Model (Mini-EUSO EM), we performed some measurements to estimate the reflectance of the most common SD materials and to demonstrate the ability of Mini-EUSO to detect SD events. We also performed some tests in open-sky conditions, identifying and tracking fast-moving objects. In particular, the detection of a rocket body allowed us to confirm the simulation outcomes predictions and the expected performance of the detector.
Simulation We performed simulations to estimate the range of distances and SD dimensions detectable by a Mini-EUSO-like telescope. The Focal Surface (FS) of such a telescope consist of a Photo-Detector-Module (PDM), which consists of 36 Hamamatsu 64-ch Multi-Anode PhotoMultiplier Tubes (MAPMTs), resulting in a readout of 2304 pixels. For SD detection, we used a time resolution of 40. 96 ms (= 1 Level 3 Gate Time Unit, 1 L3_GTU), which corresponds to the time resolution of the Mini-EUSO level 3 (L3) data. In this time resolution, Mini-EUSO records and store a continuous "movie" data through the entire observation time. We simulated the light track of a SD with ESAF (EUSO Simulation and Analysis Framework), an end-to-end simulation of the phenomenon from the light emission at the source, the propagation through the environment, to the simulation of the detector response and its reconstruction algorithms (see another contribution in this conference  [6]  for the details).
Acknowledgments The support received by the  Astronomical Observatory of Turin  is deeply acknowledged. The authors acknowledge support from  Compagnia di San Paolo  with the project " New techniques for the detection of space debris "; Id Project:  CSTO164394. This work was partially supported by  Basic Science Interdisciplinary Research Projects of RIKEN  and  JSPS KAKENHI  Grant ( 22340063 ,  23340081 , and  24244042 ), by the  Italian Ministry of Foreign Affairs and International Cooperation , by the  Italian Space Agency  through the  ASI INFN  agreement n. 2017-8-H. 0,by  NASA  award  11-APRA-0058  in the USA, by the  French space agency CNES , by the  Deutsches Zentrum für Luft-und Raumfahrt , the  Helmholtz Alliance for Astroparticle Physics  funded by the  Initiative and Networking Fund of the Helmholtz Association (Germany) , by  Slovak Academy of Sciences  MVTS JEM-EUSO, by  National Science Centre in Poland  grant ( 2015/19/N/ST9/03708 ), by Mexican funding agencies  PAPIIT-UNAM ,  CONACyT  and the  Mexican Space Agency (AEM) , as well as  VEGA  grant agency project  2/0132/17 , and by  State Space Corporation ROSCOSMOS and Russian Foundation for Basic Research  (grant  16-29-13065 ).
The SCET G calculation and the CoLBT-hydro model successfully capture the key features of the γ-tagged jet FF data in the region z < 0. 5. In the right panel, the inclusive and γ-tagged FF ratios in data are compared with those in SCET G. The γ-tagged FF ratio is larger than the inclusive-jet one in the region z < 0. 1 in both data and theory. In summary, this Letter presents a measurement of the charged-particle fragmentation functions for jets azimuthally balanced by a high-p T prompt and isolated photon. The measurement is performed using 25 pb -1 of pp and 0. 49 nb -1 of Pb+Pb collision data at 5. 02 TeV, with the ATLAS detector at the LHC. The kinematic selections result in events with a single leading jet, a large fraction of which are quark jets. In pp collisions, the γ-tagged jet fragmentation functions are systematically harder than those for inclusive jets at similar p jet T , consistent with the larger expected fraction of quark jets in γ-tagged events.
Acknowledgments 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; CONICYT, Chile; CAS,  MOST  and  NSFC, China ;  COLCIENCIAS, Colombia; MSMT CR, MPO CR  and  VSC CR, Czech Republic ;  DNRF  and  DNSRC, Denmark ;  IN2P3-CNRS ,.
Experimental Polycrystalline ingots with nominal compositions U(Al 1-x Ge x ) 3 , with x = 0, 0. 25, 0. 5, 0. 75 and 1, were prepared by arc melting stoichiometric amounts of elemental components (all purities ≥ 99. 5 %). The sample were turned upside down and remelted twice to ensure homogenisation. A subsequent annealing was performed at 973 K for two weeks after enclosing the samples in evacuated silica tubes. Resulting samples have been investigated by X-ray diffraction (XRD) using a Bruker D8 Advance diffractometer (θ -2θ Bragg-Brentano geometry, monochromatized Cu Kα 1 , λ = 1. 5406 Å) on powders obtained by manually grinding the ingots in an agate mortar. XRD data were modelled with the help of the FullProf code  [16]. Scanning electron microscopy was performed using a JEOL JSM 7100 F microscope while electron diffraction and elemental analysis (Energy dispersive spectroscopy,EDS) were performed by transmission electron microscopy on a JEOL 2100 LaB 6 instrument operating at 200kV.
2 mrad were used instead. Extended X-ray Absorption Fine Structure (EXAFS) data have been collected at Ge K edge (11403 eV) and at U L 3 edge (17166 eV) in transmission mode using specific intensity monitors with silicon diodes. Energy calibration has been monitored by measuring simultaneously the absorption of reference sample with residual photons (Y and Ge foils for U L 3 and Ge K edge, respectively). High Energy Resolution Fluorescence Detection (HERFD) X-ray absorption has been also collected on Ge K edge and at U L 3 edge using a spectrometer equipped with a Si(660) or Ge(777) secondary monochomator crystal selecting Ge K-L 3 (9886 eV) and U L 3 -M 5 (13615 eV) signals, respectively. For every compositions U(Al 1-x Ge x ) 3 (x= 0, 0. 25, 0. 5, 0. 75 and 1) fine structures µ(E) after the U L 3 and Ge K edges were measured and converted into χ(R) by Fourier transform using 1, 2 and 3 k-weight and Hanning window with dk = 1.
Results Samples of composition U(Al 1-x Ge x ) 3 with x=0, 0. 25, 0. 5, 0. 75 and 1 were synthesized and analyzed by powder diffraction (PD). The patterns of all the compositions are indexed with the cubic CuAu 3 structure-type (Pm 3m) and only a small amount of UC impurity (Fm 3m) could be detected on the pattern of UAl 3 (Figure  1b ). Le Bail refinements of the UAl 3 and UGe 3 patterns converges to lattice parameters of 4. 2676(1) Å and 4. 2078(2) Å, respectively, in good agreement with literature data  [19, 20]. By assuming the solid-solution to follow the Vegard's law, compounds with intermediate composition are expected to have a lattice parameter following the linear relation: a = -0. 0199 • x + 4. 2676 Å. (1) However, experimental lattice parameters found for x = 0. 25, 0. 5 and 0.
Acknowledgements We acknowledge with great pleasure important and illuminating discussions with our colleagues and close friends,  Mario Trigiante ,  Massimo Bianchi ,  Francisco Morales  and  Francesco Fucito. U. B. likes to thank  CEMPI  ( Centre Européen pour les Mathématiques, la Physique et leur Interactions ) for supporting his visit to  Université de Lille in February-March 2019 (Labex CEMPI   ANR-11-LABX-0007-01 ). U. B. 's research is also supported by  GNSAGA-INdAM  and by the  PRIN  project " Geometria delle Varietà Algebriche. ".
Third, the highest APXS Cl measurement in Gale is the bedrock target Stephen with 3. 3 wt. % Cl, where ChemCam observes a small Cl peak (average Cl peak area 0. 5 × 10 -4 ) indicating a threshold <3. 3 wt. % Cl in rock. This performance on Mars is similar to laboratory studies that estimate a detection threshold of 3-6 wt. % Cl  (Anderson, Ehlmann, et al. , 2017)  and >3 wt. % Cl  (Gaft et al. , 2014). Through mission Sol 2127, we examined all APXS data and all ChemCam spectra to identify targets containing Cl using the normalized Cl peak area. Then, using visual analysis of Remote Micro-Imager and Mastcam images, we classified the targets as rock, soil, or diagenetic (veins or nodules) and localized them along the traverse and within Mt. Sharp geologic units (Figure  1 ). To estimate the grain size of ChemCam bedrock targets, we used the Gini index mean score, a composition-based grain-size proxy that uses point-to-point chemical variabilities in ChemCam data  (Rivera-Hernández et al.
The reactor antineutrino anomaly The reactor antineutrino anomaly was discovered in 2011 (8) as a consequence of the new calculation of Mueller et al. of the fluxes of νe's produced in a reactor by the decay chains of the four fissionable nuclides 235 U, 238 U, 239 Pu, and 241 Pu  (7). The new calculation predicted fluxes that are about 5% larger than the previous calculation  (42) (43) (44). The resulting expected detection rate turned out to be larger than that observed in several short-baseline reactor neutrino experiments with detectors placed at distances between about 10 and 100 m from the respective reactor, generating the "reactor antineutrino anomaly". In Ref. (7) , the 238 U antineutrino flux was calculated with the "ab initio" method, using the nuclear databases, whereas the 235 U, 239 Pu, and 241 Pu antineutrino fluxes have been calculated inverting the spectra of the electrons measured at ILL in the 80's  (43) (44) (45).
Global fits The global fits of short-baseline oscillation data addressing the anomalies discussed in Section 3 in terms of active-sterile neutrino oscillations are combined analyses of a wide variety of experimental data. The adjective "global" is only indicative, because there is no established consensus on the exact set of data that must be taken into account. In particular, there is some variation in the global analyses performed by different groups on the inclusion of old experimental data, as those of old reactor experiments, and controversial data, as the low-energy MiniBooNE data. Moreover, the method of analysis of the data of old experiments (as LSND and old reactor experiments) is not unique, because the only available information is that in the published articles, which is not complete.
The current status of the spectral ratio measurements is that the NEOS/Daya Bay and DANSS data are in agreement on the indication of active-sterile neutrino oscillations generated by ∆m 2 41 1. 3 eV 2 and |Ue4| 2 0. 01  (84, 85). The old Bugey-3 spectral ratio measurement and the initial PROSPECT and STEREO measurements exclude large mixing, without affecting mixing as small as |Ue4| 2 0. 01. On the other hand, the Neutrino-4 collaboration reported an unexpected evidence of activesterile neutrino oscillations generated by ∆m 2 41 7 eV 2 and |Ue4| 2 0. 1, which is in conflict with the NEOS/Daya Bay and DANSS results, with the exclusion limit of PROSPECT  (73) , and with the solar neutrino upper bound for |Ue4| 2 in the following item 4. Therefore, the Neutrino-4 data are typically not considered in global fits.
The overall conclusions obtained from the analyses of SBL  (-)  νe disappearance data is that there is an indication in favor of oscillations into sterile neutrinos at the 3σ level, which is independent of the theoretical reactor flux calculations. This is an improvement with respect to the original reactor antineutrino anomaly that was based on the theoretical reactor   νe appearance experiments: LSND (4), MiniBooNE (6), BNL-E776 (96), KARMEN  (5) , NOMAD (97), ICARUS  (98)  and OPERA  (99). Of all the experiments only LSND and MiniBooNE found indications in favor of SBL |U e4 | 2 (-) νµ → (-) νe transitions and in Fig. 4a  they have closed contours in the plane of the oscillation parameters sin 2 2ϑeµ and ∆m 2 41. The other experiments provide exclusion curves that constitute upper limits on sin 2 2ϑeµ for each value of ∆m 2 41.
2σ (see also Ref. (85) ). Therefore, the current status of the global fit of appearance and disappearance data indicates that the interpretation of the results of some experiment or group of experiments in terms of neutrino oscillations is not correct. We can envisage the following scenarios: (A) The LSND excess of νe-like events is not due to oscillations and the coincidence of oscillations in NEOS/Daya Bay and DANSS is a fluke. In this case the remaining indications in favor of neutrino oscillations (MiniBooNE, total reactor event rates versus theoretical predictions, and the Gallium anomaly) are rather weak and could also have other explanations, leading to the demise of the eV-scale sterile neutrinos. (B) The LSND excess is not due to oscillations, but the coincidence of oscillations in NEOS/Daya Bay and DANSS is real.
Because Daya Bay being is on a different site, this procedure may lack of robustness and lead to uncontrolled systematic uncertainties. NEOS took data from August 2015 to May 2016 and reported sizable limits on the sterile neutrino parameters. In addition they reported a hint for an oscillation pattern in the ratio of the NEOS and Day Bay spectra (see Subsections 3. 3 and 4. 1), but this shall be considered with a grain of salt. The NEOS detector resumed data taking since September 2018  (115).
Solid SoLid  (86, 117)  is an experiment in preparation using 12800 cells made of cubes of polyvinyltoluene (PVT) of (5×5×5) cm 3 in dimension, partially coated with thin sheets of 6 LiF:ZnS(Ag) to capture and detect neutrons. The detector is installed at the surface level, about 6 m away from the 60 MW SCK•CEN BR2 research reactor in Belgium. A 288 kg prototype detector was deployed in 2015 and collected data during the operational period of the reactor and during reactor shut-down. The detector energy resolution is modest, σE/E ∼ 14% at E = 1 MeV. Moreover, because of the high number of cells, the electronics, data acquisition, and the calibration are real challenges. This extremely high segmentation allows 3D reconstruction and background-tagging, however. The full SoLid detector was commissioned at the beginning of 2018 at the BR2 nuclear plant.
Regarding the detection of the bands and sub-bands of carbon dust in its many forms, which can be weak on a strong continuum, the combination of high spatial and spectral resolution, and sensitivity is essential. The forthcoming MATISSE/VLT and JWST observations will provide data that will allow us to further analyses and interpretations. the disk. The average FHWM of the 8. 6 and 11. 3 µm is of 0. 232" or 67 AU and 0. 280" or 81 AU. Based on spatial and spectroscopic considerations as well as on qualitative comparison with IRS 48 and HD 97048, they favor a scenario in which PAHs extend out to large radii across the flared disk surface and are at the same time predominantly in an ionized charge state due to the strong UV radiation field of the central star. The 3. 3 µm aromatic feature is detected from 0.
Acknowledgements. We thank our referee,  A. Candian , for the care and quality of her comments and suggestions which greatly improved the clarity of this paper. This work was based on observations collected at the  European Southern Observatory, Chile  (ESO proposal number:  075. C-0624(A) ) and was supported by  P2IO LabEx  ( ANR-10-LABX-0038 )» in the framework " Investissements d'Avenir"  ( ANR-11-IDEX-0003-01 ) managed by the  Agence Nationale de la Recherche  ( ANR, France) ,  Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI)  of  CNRS/INSU  with  INC/INP  co-funded by  CEA  and  CNES. We also acknowledge  Paolo Pilleri  for sharing his observations of the PDR NGC7023 (Pilleri et al. 2015).
Acknowledgments. -We thank  A. Andronic ,  J. Berges ,  N. Borghini ,  M. Heller ,  C. Klein-Bösing ,  A. Kurkela ,  T. Lappi ,  M. Martinez ,  J. Y. Ollitrault ,  K. Reygers ,  C. Schmidt ,  D. Teaney , and  R. Venugopalan  for stimulating discussions and  P. Romatschke  for also providing the AdS/CFT attractor curve. This work was supported in part by the  German Research Foundation (DFG)  through the  Collaborative Research Centres "CRC-TR 211: Strong-interaction matter under extreme conditions " (S. S. ) and " SFB 1225: Isolated quantum systems and universality in extreme conditions (ISOQUANT) " (A. M. ). We thank the  Institute for Nuclear Theory at the University of Washington  for its kind hospitality and stimulating research environment.
Acknowledgements: We would like to thank  Ali Chamseddine ,  Paolo Aschieri ,  Thanassis Chatzistavrakidis ,  Evgeny Ivanov ,  Larisa Jonke ,  Danijel Jurman ,  Alexander Kehagias ,  Dieter Lüst ,  Denjoe O'Connor ,  Emmanuel Saridakis ,  Harold Steinacker ,  Kelly Stelle ,  Patrizia Vitale  and  Christof Wetterich  for useful discussions. The work of two of us (GM and GZ) was partially supported by the  COST Action   MP1405 , while both would like to thank  ESI -Vienna  for the hospitality during their participation in the Workshop " Matrix Models for Noncommutative Geometry and String Theory ", Jul  09 -13 , 2018. One of us (GZ) has been supported within the  Excellence Initiative  funded by the  German  and  States Governments , at the  Institute for Theoretical Physics, Heidelberg University  and from the  Excellent Grant Enigmass of LAPTh.
A first catalogue of periodic giants based on the LINEAR experiment was published by  Palaversa et al. (2013). It covers 10000 square degrees and reaches r SDSS =18. A second catalogue is the one by  Drake et al. (2009; 2014) , from the Catalina experiment, covering over 20000 square degrees down to V ∼ 19. In addition to yielding a number of new results on variable objects in general, these databases dramatically increase the number of known MSRa out of the Milky Way plane. From their Catalina sample of ∼ 500 MSRa,  Drake et al. (2014)  show that some of these trace the Sgr stream. We decided to reanalyse their data for several reasons. First, we intend to build a catalogue of M stars in the halo, as a complement to the HG2015 compilation of C stars. Secondly, in order to determine distances and since periods are provided, we shall use the K-band period-luminosity relation instead of an absolute magnitude M v ∼ -3 adopted by  Drake et al.
Building the sample To build a preliminary list of MSRas, we consider first the catalogue of  Drake et al. (2014). Note that this catalogue is based on the Data Release 1 (DR1) of Catalina, and that supplementary monitoring data are provided in the DR2, which is usable on the Catalina web site. We add the MSRa stars contained in the catalogue of  Palaversa et al. (2013). We also add the C stars, periodic or irregular, compiled by HG2015, as well as other C stars that are warmer, but may have been missed as pulsators in previous studies. Finally, we examined stars that had been found as contaminants in our survey for C stars. After checking their light curves on the Catalina DR2 database, those which were periodic were included. Because the LINEAR or Catalina coordinates have an accuracy of ∼3 ′′ , we cross-correlated our list with the 2MASS catalogue with a search radius of 5 ′′.