dataesr/scientific-paragraphs-categorization huggingface dataset:
Validation of parameters with experimental work Before starting the analyses of the proposed structure, we have examined the different parameters present in the literature  (Mukhopadhyay et al. , 2019; Srivastava et al. , 2021; Oyedele et al. , 2017; Taskesen et al. , 2018)  using SCAPS-1D software in order to check and stabilize our approach with the experimental work reported by Teoman Taskesen et al  (Taskesen et al. , 2018). Teoman Taskesen got a maximum efficiency of 11. 4 % with an V oc of 0. 443 V, a J sc of 38. 1 mA/cm 2 , and FF = 68 % which is a poor efficiency compared to the available theoretical work  (Simya et al. , 2015; Yakushev et al. , 2017). In order to check the causes of the poor efficiency in CZTSe based solar cells, we fitted the experimental J-V curve of CZTSe improved by T.
SCAPS-1D program was used to simulate the behavior of (Cu 2 ZnSnSe 4 ), a quaternary semiconductor (Cu 2 -II-IV-VI 4 systems). Fig. 5  displays the J-V curves of the Al-ZnO/CdS (0. 04 µm)/CZTSe (0. 9 µm)/Mo thin layers S. C. structure. The equation (  8 ) can show these changes  (Mohammadnejad et al. , 2020; Arbouz et al. , 2017) : j(V) = ( j n + j p + j w ) -j s ( exp qV nkT -1 ) (8) where J n is the electron current density, J p stands for hole current density, J s is the saturation current, J w is the current density in the region of depletion, and "n" stands for the ideal factor. As exhibited in Fig. 5 , the solar cell in darkness is a wide flat diode. A simple J-V measurement in the dark generates an exponential curve characteristic of a diode. The p-side of the PN junction acts as a positive electrode and the n-face of the PN junction acts as a negative electrode  (Wang et al.
As a result, n-type doping material is impossible to get for this absorber film  (Simya et al. , 2016) , thus we varied the charge carrier concentration in the range of 2. 21*10 17 cm -3 -2. 21*10 18 cm -3 (Adhi  Wibowo et al. , 2007). Fig. 8  exhibits that at 2. 21*10 18 cm -3 , both yield and fill factor are at their maximum. The effects of thickness, free carrier concentrations and defects density on the CZTSe S. C. performances have been simulated using the software SCAPS-1D and are shown in Figs. 6  and 8 (a-b ). At thicknesses greater than 5 μm, the CZTSe characters stabilize, but as «N A » increases, the J SC decreases, which should be assigned to the increment of the recombination among the abundant carriers throughout the cell. An increase in doping will increase the recombination current and there is a possibility that it will increase the built-in potential and hence the V oc.
Impact of the NiO HTL It is known that using a back surface field in solar cells is very important to create a back potential barrier for the electrons while having an ohmic behavior with the holes for decreasing the probability of back contact recombination and achieving high efficiency. In this work, we suggested the insertion of a highly HTL doped p-type layer   (NiO HTL) at the CZTSe/Mo interface. We studied the impact of the incorporation of NiO HTL as B. S. F (Al-ZnO/CdS/CZTSe(0. 9 µm)/NiO HTL/Mo) on the optimized CZTSe S. C. heterostructure using SCAPS-1D software. Fig. 10  shows the behavior of the new solar cell characteristics as a function of the NiO HTL layer thickness. A huge increase in the solar cell efficiency was achieved, due to the good alignment of the NiO HTL band with the CZTSe absorber layer.
Conclusion This article presents a numerical study using SCAPS-1D simulation software. It was investigated on a S. C. based on a quaternary Cu 2 -II-IV-VI 4 compound especially the Cu 2 ZnSnSe 4 (CZTSe) compounds, which is a promising alternative material for photovoltaic applications owing to its lower cost and abundance in nature. We had started this work by exploring the structure (n-Al-ZnO/n-     et al. , 2020)  CdS/p-CZTSe/Mo), and we have analyzed the impact of CZTSe thickness, and its acceptor's density «N A ». We also studied the influence of CdS thickness buffer film, hence we moved to add NIO HTL as B. S. F. to get the structure of n-Al-ZnO/n-CdS/p-CZTSe/NiO HTL/Mo. The NiO HTL has a great impact on cell performance. We have detected a remarkable improvement in yield jumping from 22.
The concept of publishing freely accessible data (meaning: accessible to the scientific community) has been pursued in PUNCH sciences for a long time, e. g. by the Sloan Digital Sky Survey (SDSS)  [10]  pioneering the use of relational database technology in astronomy, and the Virtual Observatory (VO) showcasing a federated information infrastructure. 1 Another example are data (and their associated metadata) collected by astronomy satellite missions, which regularly are made publicly available, e. g. from the Gaia satellite  [11]. Open data and Open science were furthered by initiatives from our communities, and the publication of data collections have a long tradition, even the development of FAIR criteria partially build on these. But the realisation of the FAIR and Open Data principles depends strongly on the (sub-)communities, the abstraction-level of their data, the status of data curation, and are therefore realised to vastly varying degrees.
In particle physics, some aspects of the FAIR and open data principles are well realised. The raw data that are gathered by the scientific instruments, the lower level-derived data, and the corresponding simulations are typically only available within the producing collaborations. Within a collaboration, the data and analysis software are freely available for all researchers. Nevertheless, there are efforts ongoing to gradually release more and more (older) data together with the required software to allow re-analyses by non-collaborators. There is also a long-standing tradition to release higher abstractions of the data and relevant simulations (distributions, histograms, likelihoods) digitally in searchable public archives, e. g. hepdata. net [12]. These archives are connected with databases of research results such as inspire.
Lower data levels and the associated software packages are findable and accessible only for researchers inside the corresponding collaborations. Notable exceptions are, e. g. the open portal KCDC (see below) providing public access to raw data and software tools. Final data products in reusable data formats (e. g. FITS) are often connected to the publication through the ADS service  [13]  and accessible through the collaboration's websites. The gamma-ray community is in the process of moving towards the usage of open community software (e. g. Gammapy  [14] ) and data format standards on the reconstructed gamma-like event level ("open gamma-ray data format"), which enables one to publish these data and combine multi-messenger data sets from different observatories in a consistent manner. Observatories under construction (e.
g. CTA) will follow FAIR and Open data principles in their research data management. In astronomy, the requirement of sharing and using data collections from archives and sites across the world began long ago and has accelerated in the digital age. For sharing (initially satellite) data, the FITS format with a limited and controlled metadata vocabulary has been established as a ubiquitous data storage format in all astronomy. Its development started in 1979, first standard was released in 1981, and "evolved out of the recognition that a standard format was needed for transferring astronomical data from one installation to another. " [15]. The growing size of astronomical data collections, the need for online selection of subsets on the one hand side (using databases and SQL) and the notion of a "multiwavelength view of the universe", requiring combination of data sets from distributed data collections on the other hand started the Virtual Observatory initiative  (2002).
In addition, we made available educational examples how to use the data, more than 100 cosmic ray energy spectra from various experiments, and recently attached a public server with access to Jupyter notebooks. Within PUNCH4NFDI, KCDC aims for an integration into the PUNCH Science Data Platform. Doing so, KCDC will benefit from the community overarching synergetic developments for a coherent data and metadata description. In addition, KCDC can be the test base for a coherent concept for data storage and access as well as for a widely used Authentication and Authorisation Infrastructure (AAI) in order to enable a PUNCH-wide multi-experimental and multi-messenger analysis platform.
Data and Analysis Reinterpretation at CERN The data collected by the LHC experiments represent a unique tool to probe theories Beyond the Standard Model (BSM). While open data are useful to probe so-far untested theories outside of the original collaborations, the process is very resource-intensive. An alternative route to openly test new theories is through reinterpretations of existing analyses. Here, existing phase-space definitions and background estimates can be reused and only a new signal contribution must be estimated using an alternative physics model and processing it through the analysis pipeline. Building on recent progress in analysis preservation utilizing software packaging using Linux Containers and the implementation of data analysis pipelines using workflow languages such as yadage  [37]  or Common Workflow Language, a new reinterpretation portal RECAST  [38]  is intended to be established at CERN, which allows external researchers to request new theories to be tested.
The procedure has been tested within the ATLAS collaboration for a number of initial analyses and is ready to be extended to a public interface. Besides the analysis pipeline the existing background estimates, including systematic and statistical uncertainty estimation, must be archived, ideally in the form of an existing likelihood model. This has been achieved for a large class of models at the LHC through the pyhf  [39, 40]  package and an associated JSON format, which is used to publish full-fidelity statistical models to the common and open HEP data repository hepdata. net [12, 41].
Smaller Hadron and Nuclear Physics Communities The smaller communities of hadron and nuclear physics cover a diverse range of topics and produce data of very heterogeneous types. Although the size of research data from experiment and theory is considerably smaller than in bigger communities, their volume is expected to increase significantly. Raw data remain usually at individual institutes and are only partly maintained for long times. The data management relies on available equipment, tools and limited financial/human resources. In particular, there is lack of data specialists. Processed data are stored locally, published in journals or contribute to specific repositories operated by individuals, universities or special institutions. However, they often do not follow FAIR principles, have very specific modes of public access, if at all, and are often not accompanied by formalized metadata.
High-Energy Astroparticle Physics Data providers in high-energy astrophysics range from observatories operated by international organisations like CTAO, ESO, or NASA, international collaborations (e. g. , HESS, MAGIC, or VERITAS) operating high-energy experiments, to small-scale instruments operated by institutional groups. The Fermi gamma-ray data and software are publicly accessible  [42]. The CTA (Cherenkov Telescope Array) observatories will provide show-cases for FAIR and open data management: high-level data products are available in less then a day (respectively after a proprietary period for CTAO) to the community; software and guest observer support are provided as a service. Access to the large data archives of currently operating gamma-ray observatories is more difficult, as data, data model, and software are mostly behind closed doors.
However, an ongoing community effort aims for the definition of common high-level data formats  [43]  and public software tools, providing a realistic scenario for accessible and open archives for the future. Demonstrator projects  [44]  show that this allows additionally to perform multi-instruments and multi-wavelength type of analysis in clearly outlined and reproducible workflows. This interoperability is essential for the exchange of transient alerts, which are by definition public. Transient factories provide alert rates, which increasingly require transparent and complex real-time decision making workflows for optimal usage of both the observatories and the archival data. Challenges outlined above are shared in many cases with other members of the PUNCH4NFDI community; the NFDI activities are expected to provide a significant push towards the FAIR treatment of data, workflows and software products from high-energy observatories.
The International Lattice Data Grid The international lattice data grid (ILDG) represents a grid of inter-operable data-grids for community-wide sharing of so-called gauge field configurations  [45] [46] [47] [48] [49] [50]. These are the raw data objects in Lattice QCD and are generated by Markov Chain Monte Carlo simulations utilising significant fractions of the most powerful HPC systems. The Lattice QCD workflow is based on these configurations, and includes further measurement and analysis steps which are not yet covered by the ILDG. The ILDG consists of a virtual organisation, working groups and a governance board. They define standards for (meta-)data formats and the services, like a file and a metadata catalogue, operated by each regional grid and publicly accessible. The ILDG architecture and metadata schema already implement FAIR principles.
LOFAR and MeerKAT The world leading instruments of radio astronomy are interferometers, networks of hundreds of antennas or antenna stations, optimised for different frequency bands covering the radio window of Earth's ionosphere and atmosphere (10 MHz to 1 THz). The science questions addressed by radio astronomy range across the history of the Universe from the very first stars and black holes to the cradle of life, across size scales from exoplanets to the largest cosmic structures, across duration scales from fast radio burst to nHz gravitational waves, and from the the laws of gravity to cosmic magnetism and many more. There are several aspects to take into account when talking about open data in the context of radio astronomy: (i) resource allocation; (ii) data policy; (iii) dissemination.
Below we give a brief description of the status quo of open data aspects for LOFAR and MeerKAT, two projects that are supported by the BMBF via ErUM-Pro. At the lowest radio frequencies the International LOFAR Telescope (ILT), carried by 9 national consortia with its base in the Netherlands and a strong German contribution, operates since a decade and has generated over 50 PB of archived data (as of early 2021), which are accessible via the LOFAR Long Term Archive (lta. lofar. eu). The LTA is a federated archive with sites at SurfSARA, FZ Jülich, and Poznan. Most of LOFAR data are kept on tapes and the processing demands of raw LOFAR data require close access to HPC. LOFAR resources are allocated via cycle proposals (programmes that run within a single semester) and long term proposals (over four cycles), open to everybody in the world.
National consortia have a reserved share of access, depending on their financial contribution to LOFAR. Proposals include requests for observing time, computing time, data volume, and user support. The LOFAR Programme Committee (PC) ranks proposals and allocates resources together with the observatory, taking into account the reserved shares of the national consortia. The ILT board endorses the PC decisions. This procedure is the first element to guarantee open access to LOFAR data. The ILT knows two categories of data, ILT data and station owner data. All ILT data become public eventually, all ILT observing and standard pipeline processing data remain ILT property. Station owner data (at least 10% of the available observing time) remain at discretion of station owners. Derived data are property of scientists, e.
g. LOFAR survey catalogues are released by Key Science Projects. There is a proprietary data period for the proposer, which is 1 year. The PC can change data rights and scope for each ILT project. All ILT data are stored in the LOFAR Long Term Archive. So far LOFAR gave rise to about 1800 publications that mention LOFAR in the abstract (according to ADS in February 2021). Most of them are on extragalactic astrophysics or pulsars and transients, but solar physics, cosmic ray physics and galactic physics as well as instrumentation and methods are important topics. Besides dissemination via the classic channel of scientific publications, LOFAR surveys are used for citizen science projects like e. g. Radio Galaxy Zoo (LOFAR)  [51]. At mid-frequencies, MeerKAT, owned by the South African Radio Observatory and enhanced with contributions from the MPG, is operating in a rather different way.
MeerKAT is the mid-frequency precursor of the Square Kilometre Array, which will have its core on the same site in South Africa. Most of MeerKAT access is reserved for Large Scale Projects (LSP). Neither access nor data are open (limited resources). It is the duty of the LSPs to make data products eventually open. For some science programs performed at MeerKAT, i. e. the search for pulsars and transients (TRAPUM and MeerTRAP) the data rates are so high (approx. 2 PB/day) that storing or shipping of the raw data is impossible. Instead, the data are analysed (quasi-) online and only the reduction products (candidates with snippets of data) are stored and transferred for further processing. MeerKAT offers a small fraction of open time, which is open to the world-wide community (so far two calls).
Also it does not have an archive like the LOFAR LTA, access to limited archival data can be requested. Data are moved to a compute centre in Cape Town, from where the projects have to retrieve it within a certain time frame. The date volumes are huge, especially if low-level data are required, shipping discs is often still the best option for this purpose. The recently founded Square Kilometre Array (SKA) Observatory will pose new technical challenges that have their own implications on how we can or have to think about open data. There will be the issue of data irreversibility (online reduction in near-real time) since raw data are of the order of 1 Pb/s and the amount of archived data will reach 300 PB/a. Individual data cubes will be of the order of up to a PB. The access of users to the data is currently under investigation by the SKA Regional Centre Steering Committee.
Structure of Data Publication Methods and Stages of Access A number of questions and parts of the discussion focused on the different structures of data publication methods (archives, providers, sites) in the various PUNCH fields of research-questions of archival structure, storage sites, etc. As examples of data providers in high energy physics, CERN and KCDC were discussed and contrasted with the approach in astrophysics. The KCDC "data shop" is an example of an infrastructure offering astroparticle data in the low Terabyte regime to users, with monitored access; the data are free for download after certain selection cuts have been specified by the user, to reduce the necessary download volume. The CERN open data portal offers data from CERN experiments on a much larger scale, in the Petabyte range, including both data and the relevant Monte Carlo samples.
Also here, a simple selection is possible (e. g. data set, experiment,. ). In general, at least in high-energy physics, more and more data sets are maintained (and partly made openly available) in what might be called "archive mode"-the collaboration-specific state after operation and funding of the experiment has stopped, but in which data and software are still made available for analysis, either only for the collaboration or also beyond. It was noted in the discussion that archival and publication of data come with a price tag, and that it would be interesting to learn, for various activities, which fraction of the data taking cost is spent for archiving and publication, and how many results are derived from long-term archived data, especially if these are open data. For example, the ZEUS experiment at the HERA electron-proton collider stopped operation in 2007.
Since then, considerable effort has been invested to make data and software usable for the long term, and currently about 10% of the ZEUS collaboration publications are done with these long-term archive data formats after the official funding for the experiment stopped in 2015. More experience needs to be collected. A part of the discussion centered on the availability of astrophysics/astroparticle physics data like those from Fermi-LAT or CTA. The PUNCH science data platform aims at providing means to work on combined data from these data collections. This cannot be achieved by import of the data into the platform or its storage elements. Alternative paths are either implementing the access to the data via virtual organisations 4 or via Virtual Observatory protocols. In all the open data initiatives, the long-term focus is clearly on providing openly accessible (and interoperable) data for the general public.
However, it is also noted that for the time being, the main beneficiaries of open data efforts might be collaborators or other scientists from the same community. It is also clear that changing data access policies across the various PUNCH disciplines towards more open and publicly usable data collections is to a large extent a task for years to come. There is often a justified embargo period involved, and implementing transitions between closed and public access is a technical challenge as well (e. g. the SKA embargo policy for new data and its technical implementation  [52] ).
Curation Procedures, Provenance, Raw and Pipelined Data An important point is to define which data are still in the stage of being pre-processed and what data can be released, e. g. in repositories or in the context of publications. In astronomy, data can be released after the instrument signatures have been removed-the pictures need to be clean of instrument artefacts. These data is often referred to as "level-1" data. A question is also how observation proposals and data results should or can be connected, since FAIR data put also a strong demand on provenance information. ESO facilities, for example, run surveys as well as PI mode observations, where observation time is awarded in a highly formalised way based on proposals  5. In high-energy physics, data are in general confronted with theoretical predictions, e.
Currently, about 50 data centres are connected to the VO, but still many data sets and data sources are not connected. For the quality control of published data, the current refereeing process of the respective journals is not sufficient. Although most public data collections used by astronomers are already attached to published papers, the curation of the data sets is not yet handled sufficiently strict. To a large extent, quality control and data curation are also the responsibility of the observatory, for example, in the case of ESO, the rationale being that the use of expensive infrastructures with low-quality data is a waste of resources. The processes for quality control and data curation is still evolving.