Astronomy and Computing最新文献

{"title":"Charge reconstruction of HERD silicon charge detectors based on MLP","authors":"Longkun Yu ,&nbsp;Jing Wang ,&nbsp;Rui Qiao ,&nbsp;Ke Gong ,&nbsp;Wenxi Peng ,&nbsp;Jiaju Wei ,&nbsp;Bing Lu ,&nbsp;Dongya Guo ,&nbsp;Yaqing Liu ,&nbsp;Xuan Liu ,&nbsp;Chenxing Zhang ,&nbsp;Ming Xu ,&nbsp;Zhigang Wang ,&nbsp;Ruijie Wang ,&nbsp;Tianwei Bao ,&nbsp;Yongwei Dong ,&nbsp;Oscar Adriani ,&nbsp;Eugenio Berti ,&nbsp;Pietro Betti ,&nbsp;Jorge Casaus ,&nbsp;Nicola Zampa","doi":"10.1016/j.ascom.2025.100986","DOIUrl":"10.1016/j.ascom.2025.100986","url":null,"abstract":"<div><div>The High Energy Cosmic-Radiation Detection (HERD) is an experimental facility designed for the study of space astronomy and particle astrophysics. The Silicon Charge Detector (SCD), as the outermost detector of HERD, has the primary objective of precisely measuring cosmic rays ranging from hydrogen to nickel. To enhance the charge resolution of the silicon charge detector by fully utilizing multi-channel information, this study employed Support Vector Machines (SVM) and Multi-Layer Perceptron (MLP) for charge reconstruction. Given the challenge of low statistics in high-<span><math><mi>Z</mi></math></span> data, we also introduced transfer learning to improve charge reconstruction for high-<span><math><mi>Z</mi></math></span> samples. Compared to our previous results (Zhanget al., 2024), the machine learning algorithm achieved an average improvement of approximately 9.8% in charge resolution for heavy nuclei with <span><math><mi>Z</mi></math></span> = 10 to <span><math><mi>Z</mi></math></span> = 28.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100986"},"PeriodicalIF":1.9,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144614636","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A cosmological probe in a theory of higher-order gravity","authors":"Shaily ,&nbsp;A. Srivastava ,&nbsp;H.V. Chauhan ,&nbsp;A. Pratap ,&nbsp;J.K. Singh","doi":"10.1016/j.ascom.2025.100988","DOIUrl":"10.1016/j.ascom.2025.100988","url":null,"abstract":"<div><div>In this work, we study a cosmological model in a modified gravity containing the Ricci scalar <span><math><mi>R</mi></math></span> and the Gauss–Bonnet invariant <span><math><mi>G</mi></math></span> in a linear combination. We establish the model by using a model’s unconventional technique by parameterizing the scale factor, in which the model begins with a finite spatial volume at the time of the early evolution of the Universe and exhibits an accelerating expansion at later times. The expansion of the Universe transitions from an early decelerating state to a late-time accelerating state. We use the various diagnostic techniques to examine the stability of the model. The prime goal of studying the model is to obtain precise cosmological constraints for <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>, <span><math><mi>α</mi></math></span>, and <span><math><msub><mrow><mi>t</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>, and discuss the various physical features of the model according to constrained model parameters. Finally, we find that our model is a stable expanding and accelerating quintessence dark energy model in late times.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100988"},"PeriodicalIF":1.9,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144606100","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Intrinsic dimensionality estimation for the galaxy’s distribution structure analysis","authors":"A. Chilingarian","doi":"10.1016/j.ascom.2025.100989","DOIUrl":"10.1016/j.ascom.2025.100989","url":null,"abstract":"<div><div>The proposed local intrinsic dimensionality method (TIDIM algorithm) demonstrates significant potential in detecting specific filament-like and globular cluster-like structures. It provides a non-parametric, reproducible, and resolution-flexible framework for identifying complex structures within three-dimensional distributions. This approach offers a complementary perspective to traditional statistical tools by focusing on local features such as voids, filaments, and globular clusters. Additionally, it allows for the reconstruction of discrete tracers using the same flexible framework. Its capacity to localize anisotropies and apply TIDIM on a spatial grid makes it particularly useful for comparisons with simulations. The Sobol grid-based TIDIM analysis complements galaxy-based assessments by enabling the detection of structures in sparsely populated regions.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100989"},"PeriodicalIF":1.9,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144588747","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cosmological implications and stability of f(Q,T) gravity with pilgrim dark energy model","authors":"M. Sharif ,&nbsp;Iqra Ibrar","doi":"10.1016/j.ascom.2025.100967","DOIUrl":"10.1016/j.ascom.2025.100967","url":null,"abstract":"<div><div>This manuscript endeavors to construct a pilgrim dark energy framework within the <span><math><mrow><mi>f</mi><mi>(Q,T)</mi></mrow></math></span> gravity theory, employing a correspondence approach aligned with a non-interacting model that incorporates pressureless matter alongside a power-law scale factor. Here <span><math><mi>Q</mi></math></span> and <span><math><mi>T</mi></math></span> represent the non-metricity and trace of the energy–momentum tensor, respectively. This extended modified gravity framework accurately replicates various epochs in the cosmological history. The <span><math><mrow><mi>f</mi><mi>(Q,T)</mi></mrow></math></span> gravity models are utilized to derive the equation of state parameter, phase planes and squared speed of sound. The analysis reveals that the reconstructed model exhibits an increasing or decreasing trend with the pilgrim dark energy parameter. The equation of state parameter characterizes the phantom regime, while the squared speed of sound parameter provides a stable framework for examining the ongoing cosmic evolution. The <span><math><mrow><msub><mrow><mi>ω</mi></mrow><mrow><mi>D</mi><mi>E</mi></mrow></msub><mo>−</mo><msubsup><mrow><mi>ω</mi></mrow><mrow><mi>D</mi><mi>E</mi></mrow><mrow><mo>′</mo></mrow></msubsup></mrow></math></span> plane trajectories reveal the freezing region, while the <span><math><mrow><mi>r</mi><mo>−</mo><mi>s</mi></mrow></math></span> phase plane shows the Chaplygin gas model. It is important to highlight that our findings align with the most recent observational data.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100967"},"PeriodicalIF":1.9,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144212679","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"OntoPortal-Astro, a semantic artefact catalogue for astronomy","authors":"Baptiste Cecconi ,&nbsp;Laura Debisschop ,&nbsp;Sébastien Derrière ,&nbsp;Mireille Louys ,&nbsp;Carmen Corre ,&nbsp;Nina Grau ,&nbsp;Clévent Jonquet","doi":"10.1016/j.ascom.2025.100991","DOIUrl":"10.1016/j.ascom.2025.100991","url":null,"abstract":"<div><div>The astronomy communities are widely recognised as mature communities for their open science practices. However, while their data ecosystems are rather advanced and permit efficient data interoperability, there are still gaps between these ecosystems. Semantic artefacts (SAs) – e.g., ontologies, thesauri, vocabularies or metadata schemas – are a means to bridge that gap as they allow to semantically described the data and map the underlying concepts. The increasing use of SAs in astronomy presents challenges in description, selection, evaluation, trust, and mappings. The landscape remains fragmented, with SAs scattered across various registries in diverse formats and structures – not yet fully developed or encoded with rich semantic web standards like OWL or SKOS – and often with overlapping scopes. Enhancing data semantic interoperability requires common platforms to catalogue, align, and facilitate the sharing of FAIR (Findable, Accessible, Interoperable and Reusable) SAs. In the frame of the FAIR-IMPACT project, we prototyped a SA catalogue for astronomy, heliophysics and planetary sciences. This exercise resulted in improved vocabulary and ontology management in the communities, and is now paving the way for better interdisciplinary data discovery and reuse. This article presents current practices in our discipline, reviews candidate SAs for such a catalogue, presents driving use cases and the perspective of a real production service for the astronomy community based on the OntoPortal technology, that will be called OntoPortal-Astro.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100991"},"PeriodicalIF":1.8,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144894967","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Morphological classification of eclipsing binary stars using computer vision methods","authors":"Š. Parimucha ,&nbsp;M. Gabdeev ,&nbsp;Y. Markus ,&nbsp;M. Vaňko ,&nbsp;P. Gajdoš","doi":"10.1016/j.ascom.2025.100998","DOIUrl":"10.1016/j.ascom.2025.100998","url":null,"abstract":"<div><div>We present an application of computer vision methods to classify the light curves of eclipsing binaries (EB). We have used pre-trained models based on convolutional neural networks (<em>ResNet50</em>) and vision transformers (<em>vit_base_patch16_224</em>), which were fine-tuned on images created from synthetic datasets. To improve model generalisation and reduce overfitting, we developed a novel image representation by transforming phase-folded light curves into polar coordinates combined with hexbin visualisation. Our hierarchical approach in the first stage classifies systems into detached and overcontact types, and in the second stage identifies the presence or absence of spots. The binary classification models achieved high accuracy (<span><math><mrow><mo>&gt;</mo><mn>96</mn><mtext>%</mtext></mrow></math></span>) on validation data across multiple passbands (Gaia <span><math><mi>G</mi></math></span>, <span><math><mi>I</mi></math></span>, and <span><math><mrow><mi>T</mi><mi>E</mi><mi>S</mi><mi>S</mi></mrow></math></span>) and demonstrated strong performance (<span><math><mrow><mo>&gt;</mo><mn>94</mn><mtext>%</mtext></mrow></math></span>, up to 100% for <span><math><mrow><mi>T</mi><mi>E</mi><mi>S</mi><mi>S</mi></mrow></math></span>) when tested on extensive observational data from the OGLE, DEBCat, and WUMaCat catalogues. While the primary binary classification was highly successful, the secondary task of automated spot detection performed poorly, revealing a significant limitation of our models for identifying subtle photometric features. This study highlights the potential of computer vision for EB morphological classification in large-scale surveys, but underscores the need for further research into robust, automated spot detection.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100998"},"PeriodicalIF":1.8,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144903854","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"AutoKnots: Adaptive knot allocation for spline interpolation","authors":"Sandro D.P. Vitenti ,&nbsp;Fernando de Simoni ,&nbsp;Mariana Penna-Lima ,&nbsp;Eduardo J. Barroso","doi":"10.1016/j.ascom.2025.100970","DOIUrl":"10.1016/j.ascom.2025.100970","url":null,"abstract":"<div><div>In astrophysical and cosmological analyses, the increasing quality and volume of astronomical data demand efficient and precise computational tools. Interpolation methods, particularly spline-based approaches, play a critical role in this context. This work introduces a novel adaptive algorithm for automatic knots (AutoKnots) allocation in spline interpolation, designed to meet user-defined precision requirements. Unlike traditional methods relying on manually configured knot distributions, the proposed technique automatically determines the optimal number and placement of knots based on interpolation error criteria, often requiring only a single parameter. The algorithm progressively improves interpolation by adaptively sampling the function-to-be-approximated, <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>x</mi><mo>)</mo></mrow></mrow></math></span>, in regions where the interpolation error exceeds the desired threshold. All function evaluations contribute to the final approximation, ensuring efficiency. Although each resampling step involves recomputing the interpolation table, this process is highly optimized and computationally negligible compared to the cost of evaluating <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>x</mi><mo>)</mo></mrow></mrow></math></span>. For inherently fast functions, interpolation may not offer significant benefits. Precision tests on different functions demonstrate the algorithm’s efficacy, while a heuristic enhancement improves accuracy in flat regions. Integrated into the Numerical Cosmology library (NumCosmo), this algorithm has been extensively used and tested. NumCosmo includes rigorous unit tests that underscore its robustness and reliability. As a practical application, we compute the surface mass density <span><math><mrow><mi>Σ</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow></mrow></math></span> and average surface mass density <span><math><mrow><mover><mrow><mi>Σ</mi></mrow><mo>¯</mo></mover><mrow><mo>(</mo><mo>&lt;</mo><mi>R</mi><mo>)</mo></mrow></mrow></math></span> for Navarro–Frenk–White and Hernquist halo density profiles, offering analytical benchmarks. This adaptive algorithm provides a mature, user-friendly tool for interpolation challenges in computational astrophysics and cosmology.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100970"},"PeriodicalIF":1.9,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144254205","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"SAS in ESA Datalabs: A new platform for XMM-Newton analysis","authors":"Esin G. Gülbahar ,&nbsp;Camille M. Diez ,&nbsp;Aitor Ibarra ,&nbsp;Ivan Valtchanov ,&nbsp;Richard Saxton ,&nbsp;Ignacio de la Calle Pérez ,&nbsp;Jose Lopez-Miralles ,&nbsp;Alejandro González Ganzábal ,&nbsp;Peter Kretschmar","doi":"10.1016/j.ascom.2025.100969","DOIUrl":"10.1016/j.ascom.2025.100969","url":null,"abstract":"<div><div>XMM-Newton is a cornerstone mission of the European Space Agency (ESA) for X-ray astronomy, providing high-quality X-ray data for astrophysical research since the start of the century. Its Science Analysis System (SAS) has been a reliable data reduction and analysis software, evolving throughout the years to meet changing user needs, while incorporating new methods. This paper presents the XMM-SAS Datalab, a tool within the cloud-based ESA Datalabs platform, designed to enhance the interactivity and collaborative potential of SAS. By integrating SAS with a modern, Python-based JupyterLab interface, it enables shared analysis workspaces, removes the need for local software setup, and provides faster access through containerised environments and preconfigured libraries. Moving SAS to the cloud preserves a consistent software setup while eliminating installation complexities, saving time and effort. A case study of the X-ray binary Vela X-1 demonstrates that the Datalabs platform reliably replicates local SAS outputs, with minimal deviations attributed to calibration file versions. The XMM-SAS Datalab allows straightforward X-ray data analysis with collaborative process, setting the way for future adaptations in e-science platforms and multi-wavelength astronomy, while offering traceability and reproducibility of scientific results.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100969"},"PeriodicalIF":1.9,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144262710","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"PWV and coherence time for Tassemit by ERA5","authors":"Tarik Mouhtafid,&nbsp;M. Sabil,&nbsp;Z. Ihsane,&nbsp;S. Oujaoura,&nbsp;E.A. Siher","doi":"10.1016/j.ascom.2025.100981","DOIUrl":"10.1016/j.ascom.2025.100981","url":null,"abstract":"<div><div>In this publication, we follow up our work in the High Atlas, in particular at of Tassemit in the Beni Mellal mountains. Our database is drawn from reanalyses ERA5 by the European Centre for Weather Forecasting, covering a period of 10 years, evaluating new parameters: precipitation water vapor (PWV), cloud cover, wind speed, geopotential, total precipitation, evaporation, coherence time <span><math><msub><mrow><mi>τ</mi></mrow><mrow><mi>O</mi><mi>A</mi></mrow></msub></math></span>, and scintillation rate <span><math><msubsup><mrow><mi>σ</mi></mrow><mrow><mi>I</mi></mrow><mrow><mn>2</mn></mrow></msubsup></math></span>. The latter are key astroclimatic parameters for qualifying of new astronomical sites.</div><div>The results highlight favorable atmospheric conditions, with a mean and median PWV of 3.68 and 3.35 mm, respectively. The site also features low cloud cover, moderate wind speeds, and low total precipitation, ensuring climatic stability suitable for advanced astronomical projects. We compared the measurements made by MASS-DIMM and calculated by ERA5 for coherence time <span><math><msub><mrow><mi>τ</mi></mrow><mrow><mi>O</mi><mi>A</mi></mrow></msub></math></span> and scintillation rate <span><math><msubsup><mrow><mi>σ</mi></mrow><mrow><mi>I</mi></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> at the Observatorio del Roque de Los Muchachos ORM: The results were encouraging, as the recalculated values of <span><math><msub><mrow><mi>τ</mi></mrow><mrow><mi>O</mi><mi>A</mi></mrow></msub></math></span> and <span><math><msubsup><mrow><mi>σ</mi></mrow><mrow><mi>I</mi></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> for the Tassemit site showed improved precision and consistency with expected atmospheric conditions. We have also recalculated <span><math><msub><mrow><mi>τ</mi></mrow><mrow><mi>O</mi><mi>A</mi></mrow></msub></math></span> and <span><math><msubsup><mrow><mi>σ</mi></mrow><mrow><mi>I</mi></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> for the Tassemit site, and we have the medians of the values of <span><math><msub><mrow><mi>τ</mi></mrow><mrow><mi>O</mi><mi>A</mi></mrow></msub></math></span> and <span><math><msubsup><mrow><mi>σ</mi></mrow><mrow><mi>I</mi></mrow><mrow><mn>2</mn></mrow></msubsup></math></span> which are 5.93 ms and 0.00307 arcsec, respectively. This is used as a reference in astronomy.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100981"},"PeriodicalIF":1.8,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144932222","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cosmological implications and constraints in Hoyle–Narlikar gravity theory","authors":"Dinesh Chandra Maurya ,&nbsp;Y. Aditya","doi":"10.1016/j.ascom.2025.100993","DOIUrl":"10.1016/j.ascom.2025.100993","url":null,"abstract":"<div><div>We discuss some cosmological implications and constraints in Hoyle–Narlikar’s creation field theory to explain the cosmic evolution of the expanding universe. To obtain an analytical solution of the modified field equations, we use the specific choices of the creation field <span><math><mrow><mi>C</mi><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow><mo>=</mo><mi>t</mi><mo>+</mo><mo>∫</mo><mfrac><mrow><mn>1</mn></mrow><mrow><msup><mrow><mi>a</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></mfrac><mo>+</mo><msub><mrow><mi>c</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>,</mo><mi>t</mi><mo>+</mo><mo>∫</mo><mfrac><mrow><mn>1</mn></mrow><mrow><mi>a</mi></mrow></mfrac><mo>+</mo><msub><mrow><mi>c</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>,</mo><mi>t</mi><mo>+</mo><mo>∫</mo><mfrac><mrow><mn>1</mn></mrow><mrow><msqrt><mrow><mi>a</mi></mrow></msqrt></mrow></mfrac><mo>+</mo><msub><mrow><mi>c</mi></mrow><mrow><mn>3</mn></mrow></msub></mrow></math></span> and get three alternatives as Model I, II, and III. For the background source of dust fluid, we find the Hubble function for each model and subsequently obtain values for the model parameters <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> and <span><math><msub><mrow><mi>Ω</mi></mrow><mrow><mi>m</mi><mn>0</mn></mrow></msub></math></span> by combining the examination of the CC and Pantheon datasets with <span><math><mrow><mn>1</mn><mi>σ</mi></mrow></math></span> and <span><math><mrow><mn>2</mn><mi>σ</mi></mrow></math></span> confidence levels. Using these values of model parameters, we measure the values of derived parameters and discuss the results by presenting the geometrical behavior of cosmological parameters. We talk about three models side by side and compare them using the effective equation of state parameter <span><math><msub><mrow><mi>ω</mi></mrow><mrow><mi>e</mi><mi>f</mi><mi>f</mi></mrow></msub></math></span>, the deceleration parameter <span><math><mrow><mi>q</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow></mrow></math></span>, and Om diagnostic analysis to group the models into stages of evolution. We also discuss the present age of the universe.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"53 ","pages":"Article 100993"},"PeriodicalIF":1.8,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144813962","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}