dataesr/scientific-paragraphs-categorization huggingface dataset:
DISCUSSION One of the main questions emerging from the data presented is the possible origin of the H features observed in NGC 895. Asymmetries are common in disc galaxies. They are often seen in the form of morphological, kinematical or integrated H spectral asymmetries    (Sancisi et al. 2008; Jog & Combes 2009; Espada et al. 2011; de Blok et al. 2014 ). Among the different mechanisms used to explain such asymmetries in galaxies are tidal interactions. Here, we discuss the implications of the above results by considering several possible interaction scenarios that may have caused the observed H and optical features detected in NGC 895.
This is also supported by the fact that the calculated tidal radius of each satellite is much larger than their H radius, meaning that it is unlikely that they are prone to disruption. For J022138, the tidal radius is of the order of the radius at which we observe a slight excess of light in the optical profile and it might well be that during an earlier phase of encounter, when the companion may have been closer to NGC 895, tidal effects did play some role. (vii) We find that the SFR of NGC 895 has not been enhanced. The galaxy has an active star-forming disk and lies on the main sequence with a SFR of SFR = 1. 75 ± 0. 09 [ /]. Based on previous studies, this does not rule out any possible interaction with its companion galaxies. Our work shows the high potential and synergy of using state-ofthe-art data in both H and optical to reveal a more complete picture of galaxy environments.
dation. KM is grateful for support from the Polish National Science Centre via grant UMO-2018/30/E/ST9/00082. NM acknowledges support of the LMU Faculty of Physics. MJJ, IH and AAP acknowledge support of the STFC consolidated grant [ST/S000488/1] and [ST/W000903/1] and MJJ and IH support from a UKRI Frontiers Research Grant [EP/X026639/1]. MJJ also acknowledges support from the Oxford Hintze Centre for Astrophysical Surveys which is funded through generous support from the Hintze Family Charitable Foundation. LVM acknowledges financial support from the grant SEV-2017-0709 funded by MCIN/AEI/ 10. 13039/501100011033, from the grants RTI2018-096228-B-C31 and PID2021-123930OB-C21 funded by MCIN/AEI/ 10. 13039/501100011033, by "ERDF A way of making Europe" and by the "European Union" and from the grant IAA4SKA (R18-RT-3082) funded by the Economic Transformation, Industry, Knowledge and Universities Council of the Regional Government of Andalusia and the European Regional Development Fund from the European Union.
ACKNOWLEDGEMENTS The MeerKAT telescope is operated by the  South African Radio Astronomy Observatory , which is a facility of the  National Research Foundation , an agency of the  Department of Science and Innovation. BN 's research is supported by the  South African Radio Astronomy Observatory (SARAO). We acknowledge the use of the ilifu cloud computing facilitywww. ilifu. ac. za, a partnership between the  University of Cape Town , the  University of the Western Cape , the  University of Stellenbosch, Sol Plaatje University , the  Cape Peninsula University of Technology  and the  South African Radio Astronomy Observatory. The Ilifu facility is supported by contributions from the  Inter-University Institute  for Data Intensive Astronomy (IDIA -a partnership between the  University of Cape Town , the  University of Pretoria , the  University of the Western Cape  and the  South African Radio astronomy Observatory) , the  Computational Biology division at UCT  and the  Data Intensive Research Initiative of South Africa (DIRISA).
BN acknowledges financial support from the  Women by Science programme of the Fundación Mujeres por África , from the  Gobierno de Canarias , and from the  Instituto de Astrofísica de Canarias (IAC). JR and JHK acknowledge support from the  Spanish Ministry of Science and Innovation  under the grant "The structure and evolution of galaxies and their central regions" with reference  PID2019-105602GB-I00/10. 13039/501100011033 , from the  ACI-ISI ,  Consejería de Economía ,  Conocimiento y Empleo del Gobierno de Canarias  and the  European Regional Development Fund (ERDF)  under grant with reference  PROID2021010044 , and from  IAC  project  P/300724 , financed by the  Ministry of Science and Innovation, through the State Budget  and by the  Canary Islands Department of Economy , Knowledge and Employment, through the  Regional Budget of the Autonomous Community.
JR also acknowledges funding from  University of La Laguna  through the  Margarita Salas Program  from the  Spanish Ministry of Universities ref. UNI/551/2021-May 26 , and under the  EU Next Generation. JF-B acknowledges support through the  RAVET  project by the grant  PID2019-107427GB-C32  from the  Spanish Ministry of Science, Innovation and Universities (MCIU) , and through the  IAC  project  TRACES  which is partially supported through the state budget and the regional budget of the  Consejería de Economía, Industria, Comercio y Conocimiento of the Canary Islands Autonomous Community. RI acknowledges financial support from the grant  CEX2021-001131 -S funded by  MCIN/AEI/10. 13039/501100011033 ,from the grant  IAA4SKA (Ref. R18-RT-3082 ) from the  Economic Transformation, Industry, Knowledge and Universities Council of the Regional Government of Andalusia  and the  European Regional Development Fund  from the  European Union  and financial support from the grant  PID2021-123930OB-C21  funded by  MCIN/AEI/10.
13039/501100011033 ,by " ERDF A way of making Europe " and by the  "European Union " and the  Spanish Prototype of an SRC (SPSRC)  service and support funded by the  Spanish Ministry of Science and Innovation (MCIN) , by the  Regional Government of Andalusia  and by the  European Regional Development Fund (ERDF). EN and THJ acknowledge support from the  National Research Foundation  (South Africa). OS's research is supported by the  South African Research Chairs Initiative of the Department of Science and Technology and National Research Foundation  (grant number  81737 ). LM and MV acknowledge financial support from the  Inter-University Institute  for Data Intensive Astronomy (IDIA), a partnership of the  University of Cape Town , the  University of Pretoria , the  University of the Western Cape  and the  South African Radio Astronomy Observatory , and from the  South African Department of Science and Innovation's National Research Foundation  under the  ISARP RADIOSKY2020 Joint Research Scheme (DSI-NRF Grant Number   113121 ) and the  CSUR HIPPO Project (DSI-NRF  Grant Number  121291 ).
Petrographic, analytical and modelling methods The petrography, microstructure and composition of carbonated serpentinites and listvenites were determined and mapped using optical microscopy and a CamScan CrystalProbe X500FE Scanning Electron Microscope (SEM), equipped with UltimMax 100 EDS (energy-dispersive X-ray spectroscopy) detector at the Géosciences Montpellier SEM-EBSD facility. EDS data were processed with Oxford Instruments Aztec. Further back-scattered and secondary electron images were acquired using a Zeiss Gemini SUPRA 55 field-emission scanning electron microscope (FE-SEM) at the Institute of Tectonics and Geodynamics of RWTH Aachen University. Mineral compositions of carbonates, silicates (serpentine, fuchsite), oxides and sulphides were quantified, and mapped for a subset of 25 samples, using a Cameca SX100 (Géosciences Montpellier) and a JEOL JXA-8530F HyperProbe (ISTE, University of Lausanne) Electron Probe Micro-Analyzer (EPMA).
Elemental maps were quantified by coupling EDS semi-quantitative data and EPMA compositions using XMapTools 3. 4. 1 MatLab toolbox  (Lanari et al. , 2019). Trace element compositions of carbonates were measured for a subset of 12 samples by laser ablation inductively-coupled plasma mass spectrometry (LA-ICP-MS) on a ThermoScientific Element XR mass spectrometer (ISTE) and a ThermoScientific Element 2 mass spectrometer (Géosciences Montpellier). Data were processed using Glitter  (Griffin et al. , 2008). Sample preparation, operating conditions, analytical and data processing protocols are reported in Text S1. Analytical errors and measurements on reference materials are provided in Tables  S3  and S9. Thermodynamic calculations were performed using Perple_X 6. 9. 1  (Connolly, 2005 (Connolly, , 2009)) , in a H2O-CO2 saturated FeO-Fe2O3-MgO-SiO2 system to constrain the stability fields of metasomatic assemblages resulting from carbonation.
g. ,  Frost et al. , 1985; Frost and Beard, 2007). These implications have to be considered for mass transfers at a larger-scale, as listvenite formation is inferred to occur along basal sections of obducted ophiolites and in the shallow mantle wedge of subduction zones  (Kelemen and Manning, 2015) , with potential impact on the cycling of redoxsensitive elements and metals. description of the analytical techniques used to acquire the geochemical dataset presented in this article (Tables  S3-S11 ) is provided in Text S1-2. 1 Geological setting: field observations, mapping, and sampling along Wadi Mansah (OmanDP Hole BT1B, Site 1) and the Jebel Fanja (Site 2) In the Fanja region (23. 465760°N, 58. 108835°E), listvenites crop out along NW-SE direction, interlayering ophiolite mantle segments atop the metamorphic sole and autochthonous sediments of the Arabian margin on the flanks of the Jebel Akhdar and Saih Hatat domes (Fig.
HR-LA-ICP-MS Compositions of carbonates in transition metals (Sc, Ti, V, Mn, Fe, Co, Ni, Cu, Zn) were determined by HR-LA-ICP-MS over 4 sessions of measurements. A first batch of analyses was performed at ISTE (University of Lausanne), using a ThermoScientific Element XR mass spectrometer interfaced to a New Wave ArF 193 nm laser. Spot diameter for analysis was 100 µm, with on-sample energy density of 7 J/cm 2 and a repetition rate of 12 Hz. Data were collected in time resolved acquisition mode, with 120 s dedicated to background signal measurement followed by 45 s of sample ablation. Instrument mass bias was calibrated by 16 measurements of NIST SRM 612 reference material (synthetic glass). Calibration was controlled by 6 measurements of BCR-2G reference material (basaltic glass). Other batches of analysis were carried out at Géosciences Montpellier (AETE-ISO, OSU OREME), using a ThermoScientific Element 2 mass spectrometer coupled to an Excimer G2 193 nm laser.
Spot diameter for analysis was 110 µm (pre-ablated at 130 µm), with on-sample energy density of 6 J/cm 2 and a repetition rate of 7 Hz, to avoid contamination of neighbouring crystal grains to the ablation spot. Data were collected in time resolved acquisition mode, with 120 s dedicated to background signal measurement followed by 40 s of sample ablation. Instrument mass bias was calibrated by 24 measurements of NIST SRM 612 reference material. Calibration was controlled by 17 measurements of BIR-1G reference material (basaltic glass). Raw data were processed using the data reduction software Glitter  (Griffin et al. , 2008) , using the linear fit to ratio method. CaO content obtained by EPMA analysis was used as internal standard for quantification. Table  S9Values  obtained for certified rock materials NIST SRM 612, BIR-1G and BCR-2G are given in.
Menzel et al. (2022)itions of sulphides determined by EPMA. Abbreviations: bdl: beyond detection limit; m. b. g. : metres below ground; GM: Géosciences Montpellier TableS9Trace element concentrations and preferred values of certified rock standards NIST-612, BIR-1G, BCR-2G determined by LA-ICP-MS. Preferred values from a compilation of literature values downloaded over the 2020-2022 period from the GeoReM database (http://georem. mpch-mainz. gwdg. de). Vein nomenclature was adopted fromMenzel et al. (2022).
669972 ; Jamtveit PI), the  Swiss National Science Foundation  (SNF: 20FI21_163073 ,  Früh-Green  PI),  JAMSTEC , the  TAMU-JR Science Operator , and contributions from the  Sultanate of Oman Ministry of Regional Municipalities and Water Resources , the  Oman Public Authority of Mining, Sultan Qaboos University ,  CNRS-Univ. Montpellier, Columbia University of New York , and the  University of Southampton. This study was funded by Project  ANR-18-CE01-0014-01 LISZT.
Observations All data used in this work were obtained as part of the ALMA Large Program MAPS. 23  For the observational setup and calibration process, we refer readers to  Öberg et al. (2021). The imaging process is described in  Czekala et al. (2021). As part of the MAPS data release, all images have been postprocessed using the  Jorsater & van Moorsel (1995; JvM)  correction. For all analysis in this work, we use the robust = 0. 5 weighted, JvM-corrected images. 24  The synthesized beam size is 134 mas × 100 mas for 12 CO J = 2-1 with a position angle (PA) of 90°. 83, 140 mas × 104 mas for 13 CO J = 2-1 with a PA of 90°. 44, and 141 mas × 105 mas for C 18 O J = 2-1 with a PA of 91°. 37. The rms noise measured in a line-free channel is 0. 562, 0. 471, and 0. 339 mJy beam -1 for each data cube, respectively.
The data were imaged with a channel spacing of 200 m s -1 , set by the MAPS Program. In the top panels of Figure  1 , we present peak brightness temperature maps for 12 CO, 13 CO, and C 18 O J = 2-1 lines calculated using bettermoments (Teague & Foreman-Mackey 2018a). The 12 CO J = 2-1 peak brightness temperature map clearly shows the annular gap at about 1 7 (;200 au), which is the main feature we focus on in this paper. Additionally, the AS 209 disk suffers from foreground cloud contamination on the western side of the disk, visible in the CO brightness temperature map. Teague et al. (2018b)  estimated that the cloud absorbs ∼30% of the 12 CO emission along the western side of the disk and showed that this level of perturbation does not impact the kinematic analyses (see their Appendix A.
Emission Surface and Disk Geometric Properties To begin the characterization of disk kinematics, we first constrain the emission surface for 12 CO, 13 CO, and C 18 O. For our base model, we adopt a power-law emission surface with an exponential taper, given by ⎜ ⎟ ⎛ ⎝ ⎞ ⎠ ⎛ ⎝ ⎡ ⎣ ⎢ ⎤ ⎦ ⎥ ⎞ ⎠ z r z r r r 1 exp , 1 q 0 t t =  - y ( ) ( ) where z(r) describes the height z at a given radius r, ψ is the power-law exponent, r t is the characteristic radius for the exponential taper, and q t is the exponent of the taper term, following  Law et al. (2021b Law et al. ( , 2022a)). We note that Law et al. (2021b) already inferred the 12 CO and 13 CO emission surfaces of the AS 209 disk using the same data set as the one we use in this paper. However,  Law et al. (2021b)  limited the outer bound of the fit to 1 98 for 12 CO, which does not cover the full radial extent of the 12 CO disk (;2 5), and to 1 35 for 13 CO, which does not cover the gap around the CPD at ;1 7.
Acknowledgments We thank  Xiao Hu ,  Geoffroy Lesur , and  Gaylor Wafflard-Fernandez  for helpful discussion. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2018. 1. 01055. L. ALMA is a partnership of  ESO  (representing its member states),  NSF (USA)  and  NINS (Japan) , together with  NRC (Canada) ,  MOST  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. V. V. G. gratefully acknowledges support from  FONDECYT Regular   1221352 ,  ANID BASAL  projects  ACE210002  and  FB210003 , and  ANID-Millennium Science Initiative Program -NCN19_171.
Support for J. H. was provided by  NASA  through the  NASA   Hubble Fellowship  grant No. HST-HF2-51460. 001- A awarded by the  Space Telescope Science Institute , which is operated by the  Association of Universities for Research in Astronomy, Inc. , for  NASA , under contract  NAS5-26555. R. L. G. acknowledges support from the  Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI)  of  CNRS/INSU  with  INC/INP  cofunded by  CEA  and  CNES. This project has received funding from the  European Research Council (ERC)  under the  European Unionʼs Horizon 2020 research and innovation program  ( PROTOPLANETS , grant agreement No. 101002188 ). C. W. acknowledges financial support from the  University of Leeds , the  Science and Technology Facilities Council , and  UK Research and Innovation  (grant Nos.
ST/T000287/1  and  MR/T040726/1 ). This work was supported by a grant from the  Simons Foundation  ( 686302 , KIÖ) and an  NSF   AAG grant  (No. 1907653 , KIÖ). Support for F. L. was provided by  NASA  through the  NASA   Hubble Fellowship  grant No. HST-HF2-51512. 001- A awarded by the  Space Telescope Science Institute , which is operated by the  Association of Universities for Research in Astronomy, Inc. , under  NASA  contract  NAS5-26555. Y. A. acknowledges support by  NAOJ ALMA  Scientific Research Grant code  2019-13B. Facility: ALMA. Software: bettermoments ( Teague & Foreman-Mackey   2018b ), CASA (McMullin et al. 2007), disksurf (Teague et al. 2021), eddy (Teague 2019),  Matplotlib  (Hunter 2007), NumPy (van der Walt et al. 2011), SciPy (Virtanen et al. 2020).
It should be used for more precise activities like training. One example is through games or digital games. Psychology-based games can increase children's curiosity about something. Games can also increase creativity and explore self-potential and solve problems  (Yao & Wang, 2020). Learning in the form of games is an effective way for child development. Hijaiyah Letter Recognizing Game is a type of Islamic educational game that focuses on teaching children with special needs how to recognize hijaiyah letters. This game was made using Construct 2 software. This game is equipped with interesting pictures so that students are more interested and excited to learn hijaiyah letters. (Rahmawati, 2020). Learning through play requires children to train their motor skills. The slightest achievement can be a valuable achievement for them.
(L. Zahrotun: 2015). Children can learn hijaiyah letters through interactive tutorials. This interactive learning application can also help users learn the shape and pronunciation of hijaiyah letters as a basis for learning or reading the Qur'an. There is also a practice quiz to measure how well application users understand hijaiyah letters (W. Gunawan, 2019). Construct 2 is an HTML 5-based game creation tool specifically for 2D platforms developed by Scirra. Construct2 does not use a special programming language, so to develop games with Construct 2 users do not need to understand programming languages which are relatively more complicated and difficult (E. Pujiono, 2018). The end result of the game built by Construct 2 can be run in various browsers such as Chrome, Firefox, Internet Explorer and Opera.
The fourth stage is Implementation, in implementing the use of gamification-based learning media, there are some minimum software and hardware requirements for gamification-based learning media. The last stage is Evaluation, the process of ensuring the success of the learning media built in accordance with the initial development expectations. In fact, the evaluation phase can occur at the end of one of the four phases or stages above. The assessment that takes place at each of the four phases above is called formative assessment and aims to improve as quickly as possible. The evaluation phase is the final step in the ADDIE learning system design model. Evaluation is a process conducted to add value to a learning program  (Trisiana and Wartoyo, 2016). Only formative assessment is used in this phase and aims to collect data on the effectiveness and efficiency of the learning media to achieve the set objectives.
The data is intended to improve and complement the learning media in question to make it more effective and efficient. Formative assessment consists of expert assessment, individual assessment, small group assessment, and field test. After a product is declared feasible by an expert, individual testing, small group testing, and field testing are carried out. If the research still finds shortcomings, then the learning media developed must be re-evaluated. Evaluation activities in this phase are not only limited to product design, development and implementation, but are carried out in all phases of the ADDIE model development. The types of data used in this research are qualitative and quantitative. This data was obtained from surveys of material and media experts. Responses from teachers as learning practitioners and answers obtained from experiments with first grade students.
Investigations of the in-plane positioning capabilities of microscopes using commercially available nanoGPS OxyO scales are presented. The scales have patterns that contain absolute position information, and nanoGPS software accurately determines the in-plane position from the scale images captured by the microscope camera. This makes in-plane positioning experiments simple and fast. We investigated different microscopy systems and found that positioning performance is a system issue that is not determined solely by the stage performance. In some cases, our experiments revealed software or hardware glitches that limited the positioning performance, which we easily xed. We have also shown that it is possible to investigate vibrations using this approach and quantify their impact on image blurring.
This approach can also be used to determine the repositioning reproducibility at one position. Interferometers can be used to investigate stage performance with excellent precision, but their implementation on a microscope can be challenging. An additional limitation is that they provide the position in a referential external to the microscope, while the camera is the relevant referential. Another family of position sensing technique is based on imaging a scale with engineered patterns and retrieving the position and orientation from the image  [17] [18] [19] [20] [21] [22]. It has been used to perform in-plane position determination in various contexts, including robotics  17  , machine vision  23  , and microscopy  13, 24. Our group has developed a particular family of position-encoding patterns and reading software, termed nanoGPS.
Methods Two commercially available nanoGPS OxyO kits from HORIBA were used (Fig. 1a ): one OxyO evaluation kit containing a scale with the same format as a microscopy slide 26 ; and one 5-inch OxyO kit for 10x vision system, Ultra High Accuracy 27. Each kit includes OxyO software. The evaluation kit can be used with a wide variety of magni cations because it contains nanoGPS patterns at different scales (Fig. 1b ). It can also be used with home-built micro or macro vision systems. The patterns are pseudoperiodic, and each pseudoperiod (Fig. 1c ) contains an orientation pattern (A), chess patterns (B), and patterns in which position and scale references are encoded (C,D). The patterns are metallic and can be observed using a microscope either in re ection or transmission. The scale images have excellent contrast (Fig.
1d ). The OxyO software can be applied to a folder of images to determine the corresponding trajectories. We have previously reported a precision of approximately 1nm and 10µrad of the nanoGPS technology when used with a 10x objective  19  , both for glass and quartz scales. In this study, we carried out stability and bidirectional reproducibility experiments indifferently with both scales, and 1nm precision is more than enough for both conventional and super-resolution microscopes. The positioning accuracy in X,Y depends on both the registration accuracy of the patterns on the scale and the thermal expansion of the scale between ambient and manufacturing temperatures. Registration accuracy is related to the fabrication technology, and thermal expansion is related to the scale material. In the case where the ambient temperature is in the [19,6°C, 23,6°C] range, the accuracy of the glass discovery kit slide for a 25mm travel is estimated to be within ± 0,7µm.