Astronomy and Computing最新文献

{"title":"DarsakX: A Python package for designing and analyzing imaging performance of X-ray telescopes","authors":"N.K. Tiwari ,&nbsp;S.V. Vadawale ,&nbsp;N.P.S. Mithun ,&nbsp;C.S. Vaishnava ,&nbsp;B. Saiguhan","doi":"10.1016/j.ascom.2024.100829","DOIUrl":"https://doi.org/10.1016/j.ascom.2024.100829","url":null,"abstract":"<div><p>The imaging performance and sensitivity of an X-ray telescope when observing astrophysical sources are primarily governed by the optical design, geometrical uncertainties (figure errors, surface roughness, and mirror alignment inaccuracies), and the reflectivity properties of the X-ray reflecting mirror surface. To thoroughly evaluate the imaging performance of an X-ray telescope with an optical design similar to Wolter-1 optics, which comprises multiple shells with known geometrical uncertainties and mirror reflectivity properties, appropriate computational tools are essential. These tools are used to estimate the angular resolution and effective area for various source energies and locations and, more importantly, to assess the impact of figure errors on the telescope’s imaging performance. Additionally, they can also be used to optimize optics geometry by modifying it in reference to the Wolter-1 optics, aiming to minimize the optical aberration associated with the Wolter-1 configuration. In this paper, we introduce DarsakX, a Python-based ray tracing computational tool specifically designed to estimate the imaging performance of a multi-shell X-ray telescope. DarsakX has the capability to simulate the impact of figure errors present in the axial direction of a mirror shell. The geometrical shape of the mirror shells can be defined as a combination of figure error with the base optics, such as Wolter-1 or Conical optics. Additionally, DarsakX allows the exploration of new optical designs involving two reflections similar to Wolter-1 optics but with an improved angular resolution for wide-field telescopes. Developed through an analytical approach, DarsakX ensures computational efficiency, enabling fast processing.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100829"},"PeriodicalIF":2.5,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140842939","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":"Probing Weyl-type f(Q,T) gravity: Cosmological implications and constraints","authors":"A.H.A. Alfedeel ,&nbsp;M. Koussour ,&nbsp;N. Myrzakulov","doi":"10.1016/j.ascom.2024.100821","DOIUrl":"10.1016/j.ascom.2024.100821","url":null,"abstract":"&lt;div&gt;&lt;p&gt;In this paper, we investigate the cosmological implications and constraints of Weyl-type &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;f&lt;/mi&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; gravity. This theory introduces a coupling between the non-metricity &lt;span&gt;&lt;math&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt; and the trace &lt;span&gt;&lt;math&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt; of the energy–momentum tensor, using the principles of proper Weyl geometry. In this geometry, the scalar non-metricity &lt;span&gt;&lt;math&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;, which characterizes the deviations from Riemannian geometry, is expressed in its standard Weyl form &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mo&gt;∇&lt;/mo&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;μ&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;g&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;mi&gt;β&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;w&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;μ&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;g&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;mi&gt;β&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; and is determined by a vector field &lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;w&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;μ&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;. To study the implications of this theory, we propose a deceleration parameter with a single unknown parameter &lt;span&gt;&lt;math&gt;&lt;mi&gt;χ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;, which we constrain by using the latest cosmological data. By solving the field equations derived from Weyl-type &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;f&lt;/mi&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; gravity, we aim to understand the behavior of the energy conditions within this framework. In the present work, we consider two well-motivated forms of the function &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;f&lt;/mi&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;: (i) the linear model represented by &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;f&lt;/mi&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;+&lt;/mo&gt;&lt;mfrac&gt;&lt;mrow&gt;&lt;mi&gt;β&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;6&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;κ&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/mfrac&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, and (ii) the coupling model represented by &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;f&lt;/mi&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mo&gt;,&lt;/mo&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mfrac&gt;&lt;mrow&gt;&lt;mi&gt;γ&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;6&lt;/mn&gt;&lt;msubsup&gt;&lt;mrow&gt;&lt;mi&gt;H&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;κ&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/mfrac&gt;&lt;mi&gt;Q&lt;/mi&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, where &lt;span&gt;&lt;math&gt;&lt;mi&gt;α&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;, &lt;span&gt;&lt;math&gt;&lt;mi&gt;β&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;, and &lt;span&gt;&lt;math&gt;&lt;mi&gt;γ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt; are free parameters. Here, &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mi&gt;κ&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mfrac&gt;&lt;mrow&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;16&lt;/mn&gt;&lt;mi&gt;π&lt;/mi&gt;&lt;mi&gt;G&lt;/mi&gt;&lt;/mrow&gt;&lt;/mfrac&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; represents the gravitational coupling constant. In both of the models considered, the strong energy condition is violated, indicating consistency with the present accelerated expansion. However, the null, weak, and dominant ener","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100821"},"PeriodicalIF":2.5,"publicationDate":"2024-03-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140199472","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":"Orbit classification in a galaxy model with a biaxial dark matter halo","authors":"H.I. Alrebdi ,&nbsp;K.E. Papadakis ,&nbsp;F.L. Dubeibe ,&nbsp;E.E. Zotos","doi":"10.1016/j.ascom.2024.100820","DOIUrl":"https://doi.org/10.1016/j.ascom.2024.100820","url":null,"abstract":"<div><p>This paper presents an analysis of a galaxy model with axial symmetry that includes a spherical nucleus, a disk, and a biaxial halo composed of dark matter. The aim is to provide a complete overview of the orbital dynamics of the galactic system and determine the impact of the flattening parameter of the dark matter halo using various numerical methods. Additionally, a comprehensive presentation of the system’s network of symmetric periodic orbits is provided. The findings indicate that the flattening parameter has a reduced effect on the network of symmetric periodic orbits when an oblate halo component is considered, as compared to the case when the prolate halo is present. Finally, the study reveals that the convergence of the characteristic curves of the orbital families with multiplicities 2, 3, 4, and 5 strongly depends on the flattening parameter.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100820"},"PeriodicalIF":2.5,"publicationDate":"2024-03-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140141543","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":"Orbital dynamics of a binary system composed of a massive star and a black hole companion","authors":"E.M. Moneer ,&nbsp;F.L. Dubeibe ,&nbsp;E.E. Zotos","doi":"10.1016/j.ascom.2024.100819","DOIUrl":"https://doi.org/10.1016/j.ascom.2024.100819","url":null,"abstract":"<div><p>In this work, we consider a binary system composed of a massive star and a black hole companion. By monitoring the mass transfer from the star to the black hole, we perform a thorough and systematic orbit classification for determining the final states of a test particle moving inside the gravitational field of the binary system. For this purpose, we deploy the theory of the time-independent restricted three-body problem for modeling the motion of the test particle. Our analysis strongly suggests that escaping, collisional and bounded motion dominate in different phases of the mass transport, while the overall orbital dynamics of the test particle become very intricate for larger differences between the masses of the two primaries. Moreover, the bounded motion is further classified into regular, sticky, and chaotic by using the SALI chaos indicator.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100819"},"PeriodicalIF":2.5,"publicationDate":"2024-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140123230","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":"AstroSA: An astronomical observation scheduler assessment framework in python","authors":"H. Xie ,&nbsp;Z. Kang ,&nbsp;X. Jiang","doi":"10.1016/j.ascom.2024.100806","DOIUrl":"https://doi.org/10.1016/j.ascom.2024.100806","url":null,"abstract":"<div><p>Time-domain astronomy, as a leading aspect of astronomical research, demands a significant increase in telescope hours. An efficient scheduler is crucial to handle the large number of observational requests effectively. However, the commonly used schedulers in observatories have not yet fully utilized the advancements in mathematics and computer science. In order to establish a connection between astronomy and the latest achievements in these fields, we propose the Astronomical Observing Scheduler Assessment Framework (<span>AstroSA</span>), implemented as a Python package. The <span>AstroSA</span> offers a rapid and user-friendly quantitative evaluator of the scheduler with five built-in metrics: expected quality of observed data, overhead ratio, scientific value, schedule rate, and ratio to the best airmass. Additionally, <span>AstroSA</span> includes a default virtual telescope and a night of cloud coverage, so that users can start to use it with minimal settings.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100806"},"PeriodicalIF":2.5,"publicationDate":"2024-03-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140069551","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":"Single star SCIDAR: Atmospheric parameters profiling using the power spectrum of scintillation","authors":"Y. Errazzouki ,&nbsp;A. Habib ,&nbsp;A. Jabiri ,&nbsp;M. Sabil ,&nbsp;Z. Benkhaldoun ,&nbsp;Y. El Azhari ,&nbsp;O. Azagrouze ,&nbsp;J. Chafi","doi":"10.1016/j.ascom.2024.100817","DOIUrl":"https://doi.org/10.1016/j.ascom.2024.100817","url":null,"abstract":"<div><p>Optical parameters of atmospheric turbulence have a significant impact on high angular resolution, adaptive optics, and site testing. The single star SCIDAR technique provides vertical profiles of these parameters, including the refractive index structure constant <span><math><mrow><msubsup><mrow><mi>C</mi></mrow><mrow><mi>n</mi></mrow><mrow><mn>2</mn></mrow></msubsup><mrow><mo>(</mo><mi>h</mi><mo>)</mo></mrow></mrow></math></span>. Its is based on the analysis of single stars scintillation. This study introduces a new approach for real-time measurement of atmospheric parameters using the Single Star SCIDAR. The key element of this approach is the utilization of a modified power spectrum of atmospheric speckles, that have more significant variation with altitude. By using that modified power spectrum, an objective function is computed, and the minimization process is performed using the Active-Set algorithm. With this approach, we successfully obtained real-time vertical profiles of <span><math><mrow><msubsup><mrow><mi>C</mi></mrow><mrow><mi>n</mi></mrow><mrow><mn>2</mn></mrow></msubsup><mrow><mo>(</mo><mi>h</mi><mo>)</mo></mrow></mrow></math></span> with good accuracy. The processing takes approximately 3 s per profile, and the recovery rate (i.e. sum of <span><math><mrow><msubsup><mrow><mi>C</mi></mrow><mrow><mi>n</mi></mrow><mrow><mn>2</mn></mrow></msubsup><mrow><mo>(</mo><mi>h</mi><mo>)</mo></mrow></mrow></math></span>) is about 95%. The reliability of this approach is validated through simulation results and a comparison with data obtained from sounding balloons. These validations confirm the accuracy and credibility of this method, which can be useful in many practical applications.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100817"},"PeriodicalIF":2.5,"publicationDate":"2024-03-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140113258","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":"Irregular longitudinal data analysis with statistical and machine learning methods for hazardous asteroids","authors":"I. Tanriverdi ,&nbsp;O. Ilk ,&nbsp;M.A. Gürkan","doi":"10.1016/j.ascom.2024.100818","DOIUrl":"10.1016/j.ascom.2024.100818","url":null,"abstract":"<div><p>Observations of the asteroids have been performed as long as it has been feasible by the available observational equipment. Recorded data, going back to 18<span><math><mtext>th</mtext></math></span> century, allowed a classification of these celestial objects’ hazardous status. Unfortunately, previous studies used methods that ignore subject dependency in Near-Earth Asteroids (NEA) data. This study aims to perform hazard classification of asteroids by proposing various statistical and machine learning methods on NEA data to overcome these shortcomings. We analyze data from 751 asteroids observed at irregular time intervals through the NASA. We compare algorithms suitable for longitudinal data structure, such as the Generalized Linear Mixed Models (GLMM), marginal model, GLMM-Tree, Historical Random Forest, GPBoost, and Spline. To the best of our knowledge and based on a comprehensive review of the existing literature, our study stands as the pioneering in the utilization of these advanced methodologies for the in-depth analysis of Near-Earth Asteroid (NEA) data. According to the findings, the accuracies of the models range from 0.89 to 0.99. The GPBoost model has the highest performance, while the marginal model has the poorest one.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100818"},"PeriodicalIF":2.5,"publicationDate":"2024-03-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140056247","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":"Synthetic light curves of exoplanet transit using nanosatellite data","authors":"A. Fuentes ,&nbsp;M. Solar","doi":"10.1016/j.ascom.2024.100816","DOIUrl":"https://doi.org/10.1016/j.ascom.2024.100816","url":null,"abstract":"<div><p>In this article, we present a dataset of light curves with synthetic signals. BRITE light curves (a constellation of five nanosatellites) are the main source of this dataset. We create the synthetic light curves of exoplanet transit by applying a pre-processing to the BRITE data and an injection of transit according to the Mandel and Agol model with a constraint of stellar radius <span><math><mrow><mo>&lt;</mo><mn>3</mn><mo>.</mo><mn>08</mn><mrow><mo>[</mo><msub><mrow><mi>R</mi></mrow><mrow><mi>s</mi><mi>u</mi><mi>n</mi></mrow></msub><mo>]</mo></mrow></mrow></math></span> and planetary radius between 0.95 and 2.1 <span><math><mrow><mo>[</mo><msub><mrow><mi>R</mi></mrow><mrow><mi>j</mi><mi>u</mi><mi>p</mi></mrow></msub><mo>]</mo></mrow></math></span>. We apply a quality criterion, obtaining 597 Planet Candidate (PC) examples and 3126 Not Planet Candidate examples as a dataset. PCs are injected simulated planets and are not around unique stars. We design a Deep Learning (DL) model to be trained with the created dataset. The DL model is a modified AstroNet Convolutional Neural Network (CNN) from literature to detect possible exoplanets. After evaluation over the testing set we obtain an accuracy of 99.46%, precision of 100% (<span><math><mrow><mi>P</mi><mi>C</mi><mi>p</mi><mi>r</mi><mi>e</mi><mi>c</mi><mi>i</mi><mi>s</mi><mi>i</mi><mi>o</mi><mi>n</mi></mrow></math></span>) and a recall of 96.72% for the PC class (<span><math><mrow><mi>P</mi><mi>C</mi><mi>r</mi><mi>e</mi><mi>c</mi><mi>a</mi><mi>l</mi><mi>l</mi></mrow></math></span>), and an area under the curve receiver operating characteristics (<span><math><mrow><mi>A</mi><mi>U</mi><mi>C</mi><mo>−</mo><mi>R</mi><mi>O</mi><mi>C</mi></mrow></math></span>) of 100%, overcoming the results of existing networks tested on BRITE data. We ultimately search for potential exoplanets using the pre-processed data from BRITE, finding signals similar to exoplanetary transits in the targets HD 039060, HD 022049, HD 036861 and HD 218396.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100816"},"PeriodicalIF":2.5,"publicationDate":"2024-02-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140062316","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":"SDHDF: A new file format for spectral-domain radio astronomy data","authors":"L.J. Toomey ,&nbsp;G. Hobbs ,&nbsp;D.C. Price ,&nbsp;J.R. Dawson ,&nbsp;T. Wenger ,&nbsp;D. Lagoy ,&nbsp;L. Staveley-Smith ,&nbsp;J.A. Green ,&nbsp;E. Carretti ,&nbsp;A. Hafner ,&nbsp;M. Huynh ,&nbsp;J. Kaczmarek ,&nbsp;S. Mader ,&nbsp;V. McIntyre ,&nbsp;J. Reynolds ,&nbsp;T. Robishaw ,&nbsp;J. Sarkissian ,&nbsp;A. Thompson ,&nbsp;C. Tremblay ,&nbsp;A. Zic","doi":"10.1016/j.ascom.2024.100804","DOIUrl":"10.1016/j.ascom.2024.100804","url":null,"abstract":"<div><p>Radio astronomy file formats are now required to store wide frequency bandwidths and multiple simultaneous receiver beams and must be able to account for versatile observing modes and numerous calibration strategies. The need to capture and archive high-time and high frequency-resolution data, along with the comprehensive metadata that fully describe the data, implies that a new data format and new processing software are required. This requirement is suited to a well-defined, hierarchically-structured and flexible file format. In this paper we present the Spectral-Domain Hierarchical Data Format (‘SDHDF’) — a new file format for radio astronomy data, in particular for single dish or beam-formed data streams. Since 2018, SDHDF has been the primary format for data products from the spectral-line and continuum observing modes at Murriyang, the CSIRO Parkes 64-metre radio telescope, and we demonstrate that this data format can also be used to store observations of pulsars and fast radio bursts.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100804"},"PeriodicalIF":2.5,"publicationDate":"2024-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133724000192/pdfft?md5=a8940702da8fbe932e90a581cd25609a&pid=1-s2.0-S2213133724000192-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139953156","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Scenario of FLRW Dark Energy Universe and f(Q) Gravity","authors":"K. Haloi,&nbsp;R. Roy Baruah","doi":"10.1016/j.ascom.2024.100805","DOIUrl":"10.1016/j.ascom.2024.100805","url":null,"abstract":"<div><p>In this paper, we discuss the accelerated expansion of the Universe in the context of f(Q) gravity theory, where Q is the non-metricity scalar. We consider a well-established parametrization of the Hubble parameter in order to determine the solution of the field equations in the FLRW universe. To obtain the best-fit value for the model parameters we use the combined Hubble, BAO, and Pantheon datasets. In order to analyze the cosmological parameters, we take two different f(Q) models into consideration, Specifically, <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>λ</mi><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span> and <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>Q</mi><mo>+</mo><mi>m</mi><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span>, where <span><math><mi>λ</mi></math></span> is a constant and <span><math><mi>m</mi></math></span> is the free parameter. Additionally, we examine how statefinder analysis, the jerk parameter, and the Om diagnostic parameter behave. Finally, we came to the conclusion that the parameters of both f(Q) models show quintessential behavior and that the cosmos is in an accelerating phase.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"47 ","pages":"Article 100805"},"PeriodicalIF":2.5,"publicationDate":"2024-02-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139952962","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}