dataesr/scientific-paragraphs-categorization huggingface dataset:
Spectr-W 3 The Spectr-W 3 project 8 is a long-term collaboration between the Russian Federal Nuclear Centre -All-Russian Institute of Technical Physics (RFNC-VNIITF) and the Joint Institute for High Temperatures of the Russian Academy of Sciences (JIHT RAS)  [8]. At present, Spectr-W 3 is the largest available database providing information on spectral properties of multicharged ions. The database contains over 450,000 records of experimental, theoretical and compiled numerical data on ionisation potentials, energy levels, wavelengths, radiative and autoionisation widths, satellite-line intensity factors for free atoms and ions and also fitting parameters, and analytic formulae to represent electron-collisional cross sections and rates (optional). References to the original sources and comments on the methods of data acquisition, etc.
are also provided. Since 2016, a new section of Spectr-W 3 providing graphical data on X-ray emission spectra (densitograms) recorded from various plasma sources has been made available to users. Densitogram graphic images are characterised with a set of fields enabling one to perform queries specifying the shortest and longest wavelengths of interest, the identification of up to five chemical elements and ionic isosequences, emission from which contributes to the recorded spectra, the upper and lower principal quantum numbers of optical single-electron transitions corresponding to the spectral lines pictured and the reference to the relevant publication. Densitogram database records are also supplied with comments elucidating details of the experimental measurements. 2. 1. 5. CHIANTI CHIANTI  9  , first released in 1996  [55] , is a well-established atomic database and modelling code for optically thin plasmas.
For a recent overview of the status of the database and future plans, see  [9]. The database consists of a series of ASCII files with all the relevant atomic collisional and radiative rates (collisional excitation rates by electron and proton impact, transition probabilities, as well as theoretical/experimental wavelengths) required to calculate spectral line emissivities. The database 8 http://spectr-w3. snz. ru originally only included ions of astrophysical importance but in recent versions data for minor ions and some neutrals have also been added. Radiative transition rates and wavelengths from CHIANTI versions 6 and 7. 1 were included in VAMDC. The CHIANTI database also has ionisation/recombination rates and various other types of data that are specific for the modelling codes but these were not included in VAMDC.
CHIANTI version 8  [56]  included new atomic rates for ions in the Li, B and Ne isoelectronic sequences, plus atomic data for several iron ions participating in emission of light from the solar corona. Excitation rates among all states have been included (for modeling of high-density plasma), which has increased the size of the database significantly. Version 8 also changed the format of some of the main ASCII files. CHIANTI version 9  [57]  then introduced a significant change in the structure of the data for several ions to allow the calculation of the emissivities of satellite lines, with autoionising states and rates having been added to those of the bound levels. These changes mean that a straightforward update to include all the changes of CHIANTI version 8 onwards within VAMDC could not be carried out, so at present the VAMDC portal only accesses CHIANTI version 7.
TIPbase-TOPbase The Iron Project (IP) and The Opacity Project (OP) databases provide energy levels/terms, radiative transitions probabilities, photoionisation cross sections and collision strengths for a large selection of ions in the range H to Ni. The TOPbase contains the OP data for radiative processes  [11, 58, 59] , and the TIPbase the IP data for collisional and radiative processes  [10]. The data have been calculated using state-of-the-art computer programs developed and maintained by the IP-OP members including the R-matrix suite of codes  [60, 61]  and the AUTOSTRUCTURE code  [62]. These data are relevant for experiment analysis, theoretical comparisons and for various astrophysical or laboratory experimental applications. The OP radiative data are used to calculate monochromatic and mean opacities  [63]  required in stellar codes and for the analysis of experiments.
The TOPbase and TIPbase are hosted at the University of Strasbourg in France  10. Sets of new (there were no data of that type in the database before) and recalculated data (with a better methodology) for existing data are being implemented in TOPbase for Fe I (new), Fe II (new) and Fe XVII (recalculated) as well as all the Ni ions (new); other recalculated ions will follow. A new service for opacity table is available on the TIPTOP webserver  [64]  (but not yet accessible through VAMDC). It should be noted that the TIPbase-TOPbase databases are linked to the VAMDC Query Store (see Section 3. 2. 2).
Stark-B Stark-B  [12, [65] [66] [67]  is devoted to the modelling and spectroscopic diagnostics of various plasmas in astrophysics, laboratory experiments, laser equipment design, laser produced plasma analysis and inertial fusion research. It contains Stark widths and shifts of isolated lines of atoms and ions due to collisions with electrons, protons, ionised helium (the most important colliders for stellar atmospheres) and other ions. The data are calculated using the semi-classical perturbation  [68]  and modified semi-empirical methods  [69]. Stark-B is continuously updated by adding new data and by introducing new facilities for their use. Under the website option "Data history" there are "New datasets" and "Updated datasets", which make available a description of newly added data including the date of import and details of the modifications for revised data.
In order to enable inclusion of data from Stark-B in the computer codes used for stellar atmospheres modelling and other numerical calculations, it is possible to fit tabulated data with temperature. In particular, a fitting formula for interpolation of the displayed data for different temperatures has been derived  [70]. Thus, to each table of Stark widths and shifts, an additional table has been added with the coefficients needed for the fitting formula. The latest updates are further described in the current issue  [13]. It should be noted that the Stark-B database is linked to the VAMDC Query Store (see Section 3. 2. 2).
CDMS and JPL Spectral Line Catalog Both these databases 11 provide spectral data for molecular species, which are or may be observed in various astronomical sources (usually) by radio astronomical means or for use in remote sensing. The JPL catalog  [15, 71, 72]  and the CDMS  [14, [72] [73] [74]  have been previously described to some extent in the literature. Briefly, the database content is generally restricted to effective Hamiltonian predictions and associated assigned experimental data for quantum transitions with entry fields including line position with accuracy, intensity, lower state energy and quantum numbers. These restrictions facilitate transfer of high-precision laboratory data into comprehensive predictions within the associated range of quantum numbers, and reconciliation and/or extension of models from multiple laboratory studies.
Separate entries exist for different isotopic species and usually also for different vibrational states. Updates and new entries to the spectral data are performed aperiodically, with focus on detection in the interstellar medium as well as candidates for terrestrial remote sensing target molecules. The incorporation of these two databases in VAMDC, and thus the application of its standards (see Section 3. 1. 1), not only greatly simplified the interoperability between the databases and improved the readability of the content (e. g. quantum number format), but also provided additional features and information. A listing of energy levels as well as all files that have been used to generate the data are commonly provided. Partition functions are now tabulated for 110 temperatures up to 1000 K.
In the context of VAMDC, a Python library (vamdclib) has been developed that allows queries of data via VAMDC protocols with the information being stored in a local SQLITE3 database for use in third-party applications (e. g. XCLASS, see below in the section of use cases). Both databases are linked to the VAMDC Query Store (Section 3. 2. 2), and thus support VAMDC's generation of digital object identifiers (DOIs) for individual queries that can be used to cite this data in publications. Creating new entries or updating existing ones is an important part of the work for the CDMS. As of July 2020, there are 1020 entries in the CDMS, up from 808 four years ago. Recent activities have emphasised species that are or may be observable with the Atacama Large Millimeter/submillimeter Array (ALMA), the Northern Extended Millimeter Array (NOEMA) and similar facilities.
HITRAN The HITRAN molecular spectroscopic database  [16]  is a canonical compilation of molecular spectroscopic parameters that are required for the input into the radiative-transfer codes. HITRAN provides the best unique parameter values assimilated from both experimental and theoretical studies. Before adapting data to the database, the HITRAN group performs independent evaluations (controlled laboratory, atmospheric retrievals and theoretical analyses) wherever possible. While the target audience of HITRAN are scientists that study terrestrial and planetary atmospheres, the applications of HITRAN span a great many fields of science, engineering and medicine. The database was first established several decades ago  [75]  and has been under continuous development since then  [16, [76] [77] [78] [79] [80] [81] [82] [83].
The latest edition of the database is HITRAN2016  [16]  and is distributed through HITRANonline  [84]  that is accessible through the VAMDC portal. The VAMDC portal provides access to a traditional line-by-line high-resolution section of HITRAN, which contains spectral parameters for 49 molecules along with their significant isotopologues appropriate for terrestrial and planetary atmospheric applications. HITRAN provides references to the original sources for the majority of the parameters for every transition. The details of how such referencing was incorporated is described by Skinner et al. [85]  in this special issue. It is worth pointing out that with an exception of some diatomic molecules (including hydrogen halides) for which the line lists can be used at temperatures up to 5000 K or higher, the majority of the HITRAN line lists are intended to be used at the lower temperatures encountered in the terrestrial atmosphere.
For higher temperature applications, it is recommended to use the HITEMP database  [86] , which mimics the format of HITRAN but contains a substantially larger amount of lines. However, at the present time, the HITEMP database provides data for only eight molecules  [86] [87] [88] [89] , and is not currently accessible through VAMDC due to the large number of transitions it contains. HITRAN also provides a section that contains high-resolution experimental cross sections for molecules with very dense spectra that are not amenable to a full quantum-mechanical description. A recent update  [90]  provided spectra of almost 300 molecules at various pressures and temperatures. There is also a section of the compilation that provides collision-induced absorption cross sections, which has been updated recently  [91].
These data are not accessible through VAMDC yet but can be accessed through HITRANonline  12  or through the HITRAN Application Programming Interface (HAPI)  [92]. A very extensive effort is currently underway to release the new HITRAN2020 edition of the database. 2. 1. 10. S&MPO S&MPO (Spectroscopy and Molecular Properties of Ozone) is an information system  [17]  jointly developed by Reims University (France), Institute of Atmospheric Optics (Russia) and Tomsk State University (Russia). The line-by-line list of vibration-rotation transitions, energy levels, transition moments and other related information can be requested from S&MPO via the VAMDC portal. Since the previous edition of VAMDC  [3] , considerable new spectroscopic information has been included using experimental data and extended analysis of ozone bands in the infrared  [93]  and isotopic spectra enriched by 17 O and 18 O oxygen  [94, 95].
Supplementary information concerning theoretical spectra simulation, comparisons with experimental records, dipole moment functions  [96]  and ab initio intensities for strong lines  [97]  can be accessed via the Reims  13  and Tomsk 14  sites. The S&MPO interactive software was completely rewritten to make it relevant to current trends in internet application development. A new version 3. 0 of the S&MPO relational database and information system is now operational and provides supplementary functionalities for the fully updated graphical interface. More information about the version 3. 0 S&MPO information system can be found on its public website  15. Applications of the S&MPO may include education/training in molecular and atmospheric physics, studies of radiative processes and spectroscopic analysis.
2. 1. 11. MeCaSDa, ECaSDa, TFMeCaSDa, SHeCaSDa, GeCaSDa, RuCaSDa, TFSiCaSDa, UHeCaSDa These databases contain calculated rovibrational transitions (mostly infrared absorption and also some Raman scattering lines) for highly symmetrical molecules. They result from the analysis and fit of effective Hamiltonian and transition moments using experimental spectra recorded at high resolution. The calculation uses a model  [98]  and programs  [99]  developed by the group at the Laboratoire Interdisciplinaire Carnot de Bourgogne, Dijon, France, and based on group theory and tensorial formalism  [100]. The MeCaSDa database  [101]  contains methane (CH 4 ) lines, which constitutes the main research subject of the Dijon group. It is Dijon's biggest database and is of importance for atmospheric and planetary applications.
Its contents have recently been updated, and it now has more than 16 million lines  [18]. Other databases for several molecules of either atmospheric, planetological or industrial applications have been significantly updated recently  [18] : ECaSDa (C 2 H 4 found in Earth's and planetary atmospheres  [101] ), TFMeCaSDa (CF 4 found in Earth's atmosphere), SHeCaSDa (SF 6 found in Earth's atmosphere), GeCaSDa (GeD 4 found in giant planets' atmospheres) and RuCaSDa (RuO 4 important for the nuclear industry). Two new databases have been added recently: TFSiCaSDa  [19]  concerning the SiF 4 molecule with applications to volcanic gases and UHeCaSDa (UF 6 ) for applications for the nuclear industry. This latter database is an exception: no experimental data are publicly available for this peculiar radioactive molecule and calculations are only based on literature data  [102, 103].
More databases of such highly symmetrical molecules maybe developed in the near future. The databases SHeCaSDa, MeCaSDa, GeCaSDa, TFMeCaSDa and RuCaSDa are linked with the Query Store service (Section 3. 2. 2), while the databases ECaSDa, TFSiCaSDa and UHeCaSDa are currently being connected to the Query Store. 2. 1. 12. CDSD-296, CDSD-1000, CDSD-4000, ASD-1000, NOSD-1000 and NDSD-1000 Six molecular databanks in VAMDC of atmospheric and astrophysical interest have been provided by the Laboratory of Theoretical Spectroscopy, V. E. Zuev Institute of Atmospheric Optics, Siberian Branch, Russian Academy of Sciences, Russia. These include three versions of the Carbon Dioxide Spectroscopic Databank (CDSD-296, CDSD-1000, CDSD-4000), the Acetylene Spectroscopic Databank (ASD-1000), the Nitrous Oxide Spectroscopic Databank (NOSD-1000) and the Nitrogen Dioxide Spectroscopic Databank (NDSD-1000).
These databanks provide positions, intensities, air-and self-broadened half-widths, coefficients of temperature dependence of the half-widths and quantum numbers associated with the transitions. The line positions and intensities are calculated within the framework of the method of effective operators. The line shape parameters are calculated using different theoretical approaches or empirical equations in terms of the rotational quantum numbers. CDSD-296 and CDSD-1000 have been described in our previous paper  [3]. CDSD-296 has been updated recently  [20]  to improve the line parameters accuracy. CDSD-4000 contains more than 628 million lines of the four most abundant isotopologues of carbon dioxide and covers the 226-8310 cm -1 wavenumber range  [21]. The reference temperature is T ref = 296 K and the intensity cutoff is 10 -27 cm -1 /(molecule cm -2 ) at 4000 K.
ASD-1000 has more than 30 million lines of the principal isotopologue of acetylene in the 3-10000 cm -1 spectral range  [24]. The database is adopted for the temperatures up to 1000 K with an intensity cutoff 10 -27 cm -1 /(molecule cm -2 ). The line intensities and pressure broadening coefficients are given for T ref = 296 K. NOSD-1000 contains more than 1. 4 million lines of the principal isotopologue of nitrous oxide and covers the 260-8310 cm -1 region  [22]. The intensity cutoff is at 10 -25 cm -1 /(molecule cm -2 ) at T ref = 1000 K. Finally, the NDSD-1000 has more than 1 million lines in the 466-4776 cm -1 wavenumber range  [23]. The intensity cutoff is at Currently, the above mentioned databanks are presented in VAMDC as separate nodes with a similar basic set of "restrictables" 16 parameters (wavenumber, wavelength, line strength, InChIKey and state energies).
The common set of returnable entities includes radiative transitions, sources, isotopic species, environment signatures and function descriptions for the temperature and pressure dependencies of line shape parameters. The parametric content of these returnables however, depends on the original structure of the particular databank. Unification of these databanks, which is a step necessary for their merging into a single VAMDC node, is subject of future work. Besides being available through VAMDC, the databanks can be downloaded from the IAO ftp server  17  where they are presented in the original tabular format. 2. 1. 13. SESAM SESAM  18  is restricted to the electronic spectra of molecular hydrogen and its deuterated substitutes, as well as CO. The hydrogen spectra includes the Lyman and Werner band systems as well as B'-X, D-X electronic bands.
The SESAM database allows queries, within a specific wavelength range, of the properties of available transitions of a selected molecule. The transitions are in the Vacuum Ultra Violet (VUV) range. It is also possible to download the full range of data for a particular goal. Different additions are considered, e. g. the query of these molecular transitions at any redshift, which can be interesting for extragalactic observations where the spectrum is shifted in the visible. Since 2016 the CO molecule has been added. Further information and the latest updates are described in this Special Issue  [13]. It should be noted that the SESAM database is linked to the VAMDC Query Store (Section 3. 2. 2).
W@DIS The W@DIS databases are part of the information system  [25]  designed to provide access to both tabular and graphical data, as well as information  [104]   19  and ontologies  [105]  for quantitative molecular spectroscopy necessary for solving fundamental and applied problems in a number of subject areas: atmospheric spectroscopy of planets and exoplanets, astronomy, etc. The semantic information system W@DIS is the next-generation molecular spectroscopy information system, based on application of Semantic Web technologies to its tabular and graphical information resources  [106, 107]. The W@DIS information system is available and hosted at the V. E. Zuev Institute of Atmospheric Optics in Tomsk, Russia  20. This system can be a prototype for semantic information systems in the atomic, ionic and solid-state spectroscopy to be used by the VAMDC consortium.
KIDA The KInetic Database for Astrochemistry (KIDA 21  )  [26, 27]  is a compilation of kinetic data (chemical reactions and associated rate coefficients) used to model chemistry in astrophysical environments (interstellar medium, protoplanetary disks, planetary atmospheres, etc. ). In addition to detailed information on each reaction (e. g. temperature range of validity of the rate coefficients, reference and uncertainty), particular attention is given to the quality of the data, which is evaluated by a group of experts in the field. Since 2016, KIDA also compiles data used to compute chemical reactions occurring on the surface of interstellar dust grains (branching ratios, activation energies and barrier width) and desorption/diffusion of species on these surfaces (desorption and diffusion energies).
UDfA The UMIST Database for Astrochemistry (UDfA), first released to the public in 1991  [108] , contains basic chemical kinetic data and associated software codes and documentation for modelling the chemical evolution of interstellar clouds and the circumstellar envelopes of evolved AGB stars. The core of the data, which can be accessed via its website  22  in addition to VAMDC, consists of reaction rate coefficients of several thousand gas-phase reactions and is supplemented by more restricted data sets concerning the chemistry of deuterium fractionation. The database does not contain any surface chemistry but a file of surface binding energies, which allows processes such as reaction and desorption to be taken into account, is supplied. Where possible, and in line with VAMDC policy, a great deal of effort has been made to identify the precise source of each datum entry through the application of its DOI, in particular for those rate coefficients measured experimentally.
BASECOL The BASECOL database collects, from the refereed literature, the rate coefficients for the excitation of rotational, vibrational and rovibrational levels of molecules by atoms, molecules and electrons. The processes are described in the temperature ranges relevant to the interstellar medium, to circumstellar atmospheres and to cometary atmospheres. The BASECOL database is currently the sole VAMDC connected database that implements the Java version of the node software  26. It can be displayed from the VAMDC portal with the "Collisional data XSAMS to HTML" processor and is accessible from the SPECTCOL tool  [109, 110]. Since its last review paper in 2013  [29]  the scientific content of the database is updated with published data. Since the last VAMDC review paper in 2016  [3] , the technical components of the database have been entirely replaced  [30]  with the internal structure of the database, and the data ingestion files have been made compliant with the metadata necessary for VAMDC interoperability.
BeamDB BeamDB (the Belgrade electron-atom/molecule DataBase) is a collisional database, in which electrons are projectiles while targets are considered to be atoms and molecules  [33]. Interactions of electrons with atoms and molecules are presented as both differential and integral cross sections for processes such as elastic scattering, excitation and ionisation  [114]. Since the previous review of VAMDC  [3]  a considerable volume of new collisional data on metal atom targets have been included from the published sources (e. g. for bismuth  [115]  or zinc  [116] ) and selected molecules (e. g. for methane  [113]  or nitrous oxide  [32] ). Curation and maintenance of electron collisional data is relevant in many research areas such as astrophysics  [117] , plasma  [118] , radiation damage  [119]  or in lighting applications  [120].