dataesr/scientific-paragraphs-categorization huggingface dataset:
Italian Medieval Epigraphy in the Vernacular Some Editorial Problems Discussed 180 14. 1 The Corpus 180 14. 2 The Background 181 14. 3 History, Geography, Forms and Functions 182 14. 4 How are the Data Organized 185 14. 5 Conclusion 189 Bibliography 190 Mark Depauw 15 Trismegistos: Optimizing Interoperability for Texts from the Ancient World 193 15. 1 The Development of Trismegistos (Texts) 193 15. 2 New Techniques & Other Trismegistos Databases 196 15. 3 The Raison d'Être of Trismegistos 198 Bibliography 200 Adam Rabinowitz, Ryan Shaw and Patrick Golden.
Acknowledgments: The corresponding author is sincerely grateful to thank the  Australian Academy of Science  and the  Japan Society  for the  Promotion of Sciences for his Invitation Research Fellowship (Long-term ), Grant No. JSPS-L15701  at the  Railway Technical Research Institute  and the  University of Tokyo, Japan. The authors are also wishes to thank to the  European Commission  for the financial sponsorship of the H2020- RISE  Project No. 691135  " RISEN: Rail Infrastructure Systems Engineering Network ", which enables a global research network that tackles the grand challenge of railway infrastructure resilience and advanced sensing in extreme environments (www. risen2rail. eu)[1].
Anyway, the mean discrepancy dM estimated with a single ionospheric measurement is coherent with the error of 1. 5 magnitude-units generally observed using a single seismometer  24. We additionally explored the possible link between the ionospheric magnitude estimation and the ionospheric weather conditions (daily time, month, solar flux; S1-S6), as well as the seismic event characteristics (depth, epicentral distance; S7-S12) without any evidence of dependence. Additionally, no-relation between the mean discrepancy dM and the reflection altitude (see S7-S12) strongly support the hypothesis of one-to-one coupling between the neutral and plasma. This surprising result opens terrific perspective in seismology: first of all, the ionospheric measurement by Doppler sounder and OTH radar could be included in the seismic database as GPS has been included in the last decade  [25] [26] [27] [28]  performing a better coverage of the planet.
Acknowledgements This project is supported by the  Programme National de Télédétection Spatiale (PNTS) , grant n  PNTS-2014-07 , by the  CNES grants GISnet&back and SI-EuroTomo , and by the  Institut Universitaire de France (IUF). G. O. thanks  H. Kanamori  ( Caltech ) for friendly and constructive suggestions. Authors thank anonymous reviewers for constructive remarks. This is IPGP contribution 3877.
The obtained results are then combined with results from searches in the same dataset in the single-lepton and all-jet final states  [19, 20]. Finally, we consider for the first time the T8bb νν model (Fig. 1 , lower left), where both top squarks decay via charginos to sleptons and, subsequently, to neutralinos leading to a final state with the same particle content as in the T2tt model. Here, sleptons are the SUSY partners of leptons, and the branching fraction of the chargino is taken to be identical for all three flavors. In this way, and contrary to the T2tt and T2bW models, the branching fraction to a pair of oppositely charged leptons is 100% when decays to τ leptons are included. Searches based on T2tt and T2bW models using 8 and 13 TeV pp collision data recorded before 2016 were published by the CMS  [21] [22] [23]  and the ATLAS  [24] [25] [26] [27] [28]  experiments, with a t 1 mass excluded up to 700 GeV in the T2tt model.
Event samples During data taking, events are selected for offline analysis by different trigger algorithms that require the presence of one or two leptons (electrons or muons). For the dilepton triggers, which accept the majority of events with two leptons, the thresholds are 23 GeV on the leading lepton p T and 12 GeV (electron) or 8 GeV (muon) on the subleading lepton p T. Efficiencies of the dilepton triggers are measured in data events that are selected independently of the leptons, based on the presence of jets and requirements on the transverse momentum imbalance (p miss T ). Typical values range from 95 to 99%, depending on the momenta and pseudorapidities (η) of the two leptons and are applied as scale factors to simulated events. The top quark antiquark pair production (tt) and t-channel single top quark background samples are simulated using the POWHEG v2  [42, 43]  event generator, and are normalized to next-tonext-to-leading order (NNLO) cross sections  [44] [45] [46] [47] [48] [49] [50].
Drell-Yan and multiboson backgrounds Drell-Yan events constitute only a small background component after the analysis selection. In order to measure the residual contribution, we select dilepton events where we invert the Z boson veto, the b jet requirements, and the angular separation requirements on jets and p miss T. From simulation, this selection is expected to retain about 85% Drell-Yan events, while the subleading contribution comes from multiboson events. For each same-flavor signal region, we define a corresponding control region with the selections above and the signal region requirements on M T2 ( ), M T2 (b b ), and p miss T. Including systematic uncertainties, we perform a likelihood fit of the predicted yields in these control regions and extract simulation-to-data scale factors that amount to 1.
We can also begin to illustrate the urban landscape with people in their homes and shops and markets, side by side with the more and less prominent religious institutions that have dotted the Jerusalem landscape. Combining the two censuses, we can track the changing urban landscape over a thirty-year period (between 1299 and 1321) as families moved from intra to extra muros neighborhoods, as households began to shrink and reconstitute themselves, as sons received modern educations or took apprenticeships that paved paths for them different from those of their fathers. We can carefully construct kinship ties within the city, tracing the strategies behind marriages. Beyond this critical "thickening" of Jerusalem from the bottom up, the real promise of the census perhaps lies in its power as a database to be used in conjunction with other primary sources.
The IPA was established in 1974 to create a microfilm (and later a digitized) database of Greek-language manuscripts and historical archives that are kept in major libraries and archives in Greece and elsewhere. It also aims to provide consultation and information about the study of Greek manuscripts in collaboration with archivists, philologists, and historians. Since the foundation of the IPA, more than 200 missions have been completed, during which almost 9,500 manuscripts have been digitized, as well as 20 full archival fonds (including the archives of the Catholic bishops of the Cycladic islands, the Greek Orthodox patriarchates of Alexandria and Jerusalem, the archdiocese of Cyprus, several monasteries of Mount Athos and Chalki Theological School), 150 codices and dozens of books from the eighteenth and nineteenth centuries.
It is a time-consuming process, especially when it comes to registers. In these cases, handling the material necessitates the establishment and development of databases. The language issue often creates additional difficulties. For instance, the names of people of the two subcommunities (Arab and Greek) are often given in the two respective languages. Discrepancies in the transcription of names from one language to another often make it difficult to match them. This is an old challenge, for the language problem surfaces in various Jerusalem archives due to the continuous transliterations of names and places when traversing language and community frontiers. How, then, can such material be organized and prepared for future research? Practical difficulties may hinder the creation of a historical archive, but the Open Jerusalem database will mobilize all possible means to open the patriarchal archives and put them in dialogue with other Jerusalem records.
Instead, citizens appear as objects of socioeconomic developments than as subjects of historical processes. They remain historically unimportant or become simple, "silent masses. " In order to establish a bottom-up approach and to hear the voices of ordinary people, historians have started to give much more importance to historical sources such as private journals, autobiographies, and diaries; so-called "ego-documents. "2 Some archival materials in state archives are also valuable sources, presenting data that enable historians to overcome the methodological challenges of a state-centric approach and concentrate on the questions and theoretical issues of social history. Petitions are one of these sources. Although studying petitions is a well-accepted way of assessing the political trends of a society, it would be naive to consider petitions as transparent mirrors of directly accessible public opinion.
" 20  From the beginning to the end of the empire, original petitions and related correspondences are fragmentary and dispersed among many classifications in the BOA. In order to trace the individual and collective petitions of the nineteenth century, we may use the BOA's ever-growing and improving computerized system. As all Ottoman historians know, almost every file after the nineteenth century has a summary in the database. Our research in these archives showed that it is not easy to trace petitions by searching file summaries. When we carry out a catalogue search in the summaries using related keywords such as ʿarż-ı ḥāl (individual petition), istidāʿ (petition), or ʿarż-ı maḥżār (collective petition), with the word "Jerusalem," few documents are found. We have been able to isolate the set of two hundred collective petitions used in this study by searching through the digital images of almost seven thousand files from various collections collected for the Open Jerusalem project from the BOA.
When the Numbers Speak for Themselves: Statistical Data Describing the Collective Petitions of Jerusalemites Petitions are scattered throughout many different collections in the BOA. As figure  8. 1 shows, many of the collective petitions submitted by the inhabitants of Jerusalem come from the collection of the Bāb-ı ʿĀlī Evrāḳ Odası (Sublime Porte Record Office -BEO). This bureau, established in 1851, coordinated all the correspondence between the imperial center and the provinces, the ministries, and all other state offices in Istanbul. The circulation of all official correspondence at the level of the imperial center was under its control. 36  After the petitions were registered, the Ministry of Interior generally handled them. The ministry sent copies of petitions to the appropriate offices and requested the investigation of the issues raised in the petitions.
For instance, in France, Paris-Est Marne-la-Vallée University historians led a collective academic research project from 2007 to 2012. Its aim was to build a database of all petitions submitted to the National Assembly and to the Senate from 1815 to 1940, and to analyze the results by matching them with geographic, gender, and social data. 7 Response: An Epigraphic Study of Petitions to Roman Emperors, 181-249 (Bergen: Norwegian Institute at Athens, 1998); William Mark Ormrod, Gwilym Dodd, and Anthony Musson, eds. , Medieval Petitions: Grace and Grievance (Rochester: York Medieval Press, 2009); Ronald J. Krotoszynski, Reclaiming the Petition Clause: Seditious Libel, Offensive, Protest, and the Right to Petition the Government for a Redress of Grievances (New Haven: Yale University Press, 2012).
Because iron is absent from these plots, the comparisons are independent of the modeling of the iron production and in particular the time-delay function used for the SNIa. To conclude, main features of the MDF, [α/Fe]-DF and [α/H]-DF are reproduced by our model with the exception of the offset at the metal-poor end as previously discussed. We emphasize that the aim here is not to fine-tune the comparisons and to design a best fit model, but to check how, in first approximation, a CBM fitted on inner disk stars found in the solar vicinity, is capable of representing the main observed features of chemical abundances. Reproducing the details of observed distributions is also less meaningful given that the APOGEE data has its own uncertainties (contamination by outer disk solar vicinity stars and the distances, among others), while the MDF as a function of R is likely to improve significantly in the near future, with Gaia DR2 in particular.
7 dex. The dip is not visible in the MDF of the APOGEE data (Fig. 6 , top plot), but the overall distribution is nonetheless well reproduced by the model at [Fe/H]>-0. 5 dex. A reason for the absence of the dip may be due to the distance distribution of APOGEE stars in the Galactic bulge, which is biased towards the near side of the bulge (see, for example, Fig 2 in  Ness et al 2016) , and against the lower metallicity stars. A discussion of this distance bias and its impact on the bulge MDF is discussed in  Fragkoudi et al, submitted. In several other datasets, the bimodality of the bulge MDF is apparent. Gonzalez et al. (2015)  found two components centred on [Fe/H]=-0. 31 and +0. 26 dex. Uttenthaler et al. (2012)  found a transition at [Fe/H]∼0 dex (their Fig. 8 ), and two peaks at [Fe/H]=-0.
0 -1. 5 -1. 0 -0. 5 0. 0 0. 5 Age  [Gyr]  [Fe/H] q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q Fig. 7 : The age-metallicity distribution of the bulge from  Bensby et al. (2013)  compared to our models. Overall, we consider the match between the model and the data to be satisfactory given that (1) the model is entirely designed by fitting chemical abundances of stars of the inner disk sequence observed at the solar vicinity, and no tuning has been introduced to fit the inner regions. (2) the uncertainties that still exist in the metallicity scales, and the apparent variability between fields at the same latitude  (Zoccali et al. 2017)  (3) the difference in sampling between the four different datasets considered here.
Conclusion To conclude, our fiducial model provides a good representation of a large range of observational constraints of the bulge: MDF, alpha-DF, [Fe/H]-[Si/Fe] distribution, age-[Si/Fe] and age-metallicity distribution with the same model as the inner disk, which we find remarkable given that the model (for both the inner disk and bulge) was built only from the comparison with inner disk stars sampled at the solar vicinity. The model so far has no free parameters (apart from the initial assumption of a CBM), while in standard chemical evolution models of the bulge (e. g. Tsujimoto & Bekki 2012;  Grieco et al. 2012) , the datasets are fitted allowing for several additional (and unconstrained) parameters such as the gas accretion timescale, the IMF, which usually differ from those of the disk, while in our case the model is the same.
The other crucial point are the systematics. To assess if the differences between the thick disk and bulge stars are real, we must understand what are the level of the systematics that are expected between different samples. For instance, if the systematics measured on two samples of bulge stars are of the order of the differences measured between the bulge and the local thick disk, then we may infer that these differences are not significant. Both aspects are explored in detail in Appendix A. We show that when these caveats are taken into account, either the match for several elements abundances is remarkable (alpha elements, Ni, Zn, Cr, Ba, Eu, La), or the differences, when they exist, are likely to remain within the level of systematics (Mg). Differences are not explained for some elements (Cu), but the usually small number of existing datasets prevents any strong conclusions.
This is higher than the percentage we estimated in the SWEEPS field (35%,  Haywood et al. 2016b ), but a significant fraction of the stars in the  Bensby et al. (2017)  dataset is observed closer to the plane, favoring the young population  Ness et al. (2014). 5. 2. Three hints that the formation of the thick disk was not inside-out That the whole inner disk and bulge can be described by a simple CBM as shown by the good match obtained on the MDF, alpha-metallicity distributions, age-metallicity relation and age-[α/Fe] relation, implies that no significant differentiation of the chemical evolution as a function of radius occurs within the limit of the system taken in consideration. This is at variance with the assumptions of the inside-out formation of the disk, which is commonly implemented in GCE models by parametrizing the infall timescale of gas accretion as a function of the distance to the Galactic center (see e.
Acknowledgements. The  Agence Nationale de la Recherche (ANR)  is acknowledged for its financial support through the  MOD4Gaia  project ( ANR-15-CE31-0007 , P. I. :  P. Di Matteo ), also providing the postdoctoral grant for  Sergey Khoperskov. Francesca Fragkoudi  is supported by a postdoctoral grant from the  Centre National d'Etudes Spatiales (CNES). MH and PDM acknowledge the hospitality of  Valerie de Lapparent and the 'Galaxies' team at the Institut d'Astrophysique de Paris , where this work has been partially developed.
BDTSR definition The BDTSR is defined by all events passing the preselection requirements (Section 5. 1), but vetoing events contained in the RECOSR. It contains events with less than three large-R jets and thus it is not possible to reconstruct the full B B system from the reconstructed objects alone. As a result, a BDT as implemented in the toolkit for multivariate data analysis with ROOT (TMVA)  [74]  is used to discriminate between potential signal and background events. For training and testing, a set of signal simulation samples assuming B(B → Wt) = 1 is used, combining signal masses ranging from 1050 GeV to 1600 GeV. Simulated t t events are used as background in the training, as they are the dominant background contribution in this region. Starting from a list of 75 variables describing the kinematics of the event, individual variables are removed through an iterative process and the performance of the BDT is evaluated, until a final set of 20 variables is selected.
Multi-jet background estimation The multi-jet background originates from either the misidentification of a jet or photon as a lepton candidate (fake lepton) or from the presence of a non-prompt lepton (e. g. from a semileptonic bor c-hadron decay) that passes the isolation requirement. The multi-jet shape, normalisation, and related systematic uncertainties are estimated from data using the matrix method (MM)  [76]. The MM exploits the difference in efficiency for prompt leptons to pass loose and tight quality requirements, obtained from W and Z boson decays, and non-prompt or fake lepton candidates, from the misidentification of photons or jets. The efficiencies, measured in dedicated control regions, are parameterised as functions of the lepton candidate p T and η, ∆φ between the lepton and jets, and the b-tagged jet multiplicity.
Thus no significant excess above the background expectation is found. Individual uncertainties are generally not significantly constrained by data, except for the uncertainty associated with the single top modelling, which is constrained to be within 50% of its initial size. A comparison of the post-fit agreement between data and prediction for both regions is shown in Figure  3. The RECOSR shows a slight deficit of data for the m had B distribution above 800 GeV. Hence, the observed upper limits on the B B production cross-section are slightly stronger than the expected sensitivity. The post-fit t t normalisation in these regions is found to be 0. 92 ± 0. 30 times the Monte Carlo prediction, normalised to the NNLO+NNLL cross-section.
Acknowledgments All authors would like to thank  Gerd Leuchs ,  Markus Grassl  and  Imran Khan  for helpful discussions. F. B. acknowledges the financial support of the Vanier graduate scholarship of the  NSERC. R. F. acknowledges the financial support of the Banting postdoctoral fellowship of the  NSERC. This work was supported by  Canada Research Chairs ;  Canada Foundation for Innovation (CFI) ;  Canada Excellence Research Chairs, Government of Canada (CERC) ;  Canada First Research Excellence Fund (CFREF) ;  Natural Sciences and Engineering Research Council of Canada (NSERC) ;  Singapore Ministry of Education  (partly through the  Academic Research Fund Tier   3 MOE2012-T3-1-009 ) and the  National Research Foundation of Singapore ; and  Spanish Ministerio de Economia y Competitividad (MINECO).
Introduction Pulsar Wind Nebulae (PWNe) are magnetized clouds of relativistic particles thought to be accelerated by a pulsar, that may be found in the inner regions of a supernova remnant (SNR). The composite SNR MSH 15-52 and the central compact object that has been identified as the pulsar PSR B1509-58 have been observed in X-rays and also in radio wavelengths. In 2005, VHE γ-ray emission was discovered by the High Energy Stereoscopic System (H. E. S. S. ), using 22. 1h of data, and the emission morphology was described as an elliptical Gaussian  [1]. We use a larger dataset of H. E. S. S. observations, from 2004 until 2014, consisting of the H. E. S. S. phase I era where events are reconstructed from an array of four 12-m sized Cherenkov telescopes. We have more than twice the statistics of the discovery paper, and we attempt to disentangle the morphology of MSH 15-52.
Model v1R+G : X-ray template × R α + Gaussian component As seen in Fig. 2  (middle column), the positive residuals between the v1R model and the dataset indicate strongly that one needs to take into account another component in the model, hinting that it should be located around the southern part of the PWN in MSH 15-52. Therefore, we added a geometrical component to our previous model: a symmetrical Gaussian component. We also explored the possibility to add other types of components such as a shell or a disc. The results of the fitting procedures indicate that the Gaussian component better suits our data. This model will be mentioned as the "v1R+G" model for the rest of the discussion. The portion of the total flux is computed as the fraction of the Gaussian integral over the total model flux.
The model was also evaluated for possible redundancy of elements and for elements missing from the model. The questionnaire was drafted following an initial workshop of the Global Pricing and Market Access (GPMA) team. The draft was piloted with the United Kingdom country affiliate, and the questionnaire revised in line with affiliate feedback. The final questionnaire was shared with country affiliate teams who completed one online questionnaire per team. All country affiliate staff participating in the survey were directly involved in evidence development, reimbursement submissions or payer negotiations for pharmaceuticals, to reflect experiences and needs associated with production and use of HTA within Roche. Data from completed questionnaires were analyzed using descriptive statistics and collated results were returned to country affiliates for preparation of workshops.
Acknowledgements This work was supported by  NuPNET  and the  German BMBF  by contracts no. 05P12PKNUF  and  05P12DRNUP , the  Spanish MINECO  via projects no. FPA2010-17142 ,  CPAN  ( CSD 2007-00042 ), and  PRI-PIMNUP-2011-1338  within the  ERA-NET NuPNET call  for translational joint activities, the  UK STFC  and the  UK National Measurement Office. The EXILL and FATIMA campaign would not have been possible without the support of several services at the ILL and the LPSC. We are grateful to the  EXOGAM collaboration  for the loan of the detectors, to GANIL for assistance during installation and dismantling, and to the FATIMA collaboration for the provision of LaBr 3 (Ce) detectors and analogue electronics.