Astronomy and Computing最新文献

{"title":"Modified f(Q)-gravity string cosmological models with observational constraints","authors":"D.C. Maurya ,&nbsp;J. Singh","doi":"10.1016/j.ascom.2024.100789","DOIUrl":"10.1016/j.ascom.2024.100789","url":null,"abstract":"<div><p>In the current study, we have investigated a modified <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span>-gravity theory in an anisotropic, locally rotationally symmetric (LRS) Bianchi type-I spacetime universe model. The arbitrary function <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>Q</mi><mo>+</mo><mi>Λ</mi></mrow></math></span>, where <span><math><mi>Λ</mi></math></span> is the “cosmological constant,” and <span><math><mi>Q</mi></math></span> is the non-metricity scalar, has been taken into consideration. To obtain the exact solution of the modified field equations, we considered a dusty string fluid matter source and the shear scalar (<span><math><mi>σ</mi></math></span>) is proportional to the expansion scalar (<span><math><mi>θ</mi></math></span>). The resultant Hubble function has been fitted with observational datasets <span><math><mrow><mi>H</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow></mrow></math></span> and SNe Ia datasets of apparent magnitude <span><math><mrow><mi>m</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow></mrow></math></span> in order to obtain the best fit values for the cosmological parameters. And utilizing these best fit values throughout the investigation, the many cosmic phenomena are examined. We have investigated the cosmographic coefficients like <span><math><mrow><mi>H</mi><mo>,</mo><mi>q</mi><mo>,</mo><mi>j</mi><mo>,</mo><mi>s</mi></mrow></math></span> to see if an accelerated dual mode expanding dark energy (DE) model of the universe exists. Our Om diagnostic study shows that our universe model is a quintessence example of a dark energy model. We have also calculated the universe’s present age.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100789"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133724000040/pdfft?md5=507fc889cd13983580002639d34e34c6&pid=1-s2.0-S2213133724000040-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139459762","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":"Calibration and testing strategies to correct atmospheric effects on star tracking algorithms","authors":"L. Jannin ,&nbsp;L. Felicetti","doi":"10.1016/j.ascom.2024.100794","DOIUrl":"10.1016/j.ascom.2024.100794","url":null,"abstract":"<div><p>Star trackers are usually considered to be the most accurate sensors, able to achieve a sub-arcminute precision. Star tracker algorithms are often tested and validated with simulated space views. Testing the algorithms with real space images is expensive as it requires implementing them on existing in-space star trackers, or to launch new satellites. This study shows that those algorithms are usually performing poorly with ground-based sky pictures and that some adaptations are necessary to take into account the atmospheric effects. The adaptation of star tracking algorithms to ground pictures could ease the prototyping phase for new star trackers, or for ground-based and air-borne star trackers, without the need to buy specific testing simulators. In order to tackle this issue, this study will start by implementing and testing two published Lost-In-Space algorithms with a simulated sensor to compare their performance against various noise sources. After comparing the space-based generated views with ground-based images, an adaptation for the aforementioned algorithms is proposed. In order to counter the effect of atmospheric extinction, the number of stars visible in the image is increased by modifying the field-of-view of the camera, the exposure time and estimating the experimental inter-star angular distance error. The idea is to match the star density used in the state-of-the-art algorithms in the experimental pictures. The modified algorithms are tested with the experimental images, and the adaptation process is validated with a good success rate.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100794"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S221313372400009X/pdfft?md5=6bbe80144ed5d21cee2a6185ec1023e4&pid=1-s2.0-S221313372400009X-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139582005","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":"Deep Learning LSTM-based approaches for 10.7 cm solar radio flux forecasting up to 45-days","authors":"G. Jerse ,&nbsp;A. Marcucci","doi":"10.1016/j.ascom.2024.100786","DOIUrl":"10.1016/j.ascom.2024.100786","url":null,"abstract":"<div><p>Accurate forecasting of F10.7 index is important on short, medium and long-term timescales since F10.7 is an excellent proxy of solar activity and it plays an important role within the Space Weather framework. The analysis of the signatures of transient solar radio emission and its prediction are a challenging task as the underpinning physical processes are typically nonlinear, non-stationary and chaotic. In this paper we want to present three Deep Learning approaches for the daily forecasting of the adjusted F10.7 solar radio flux up to 45 days, using a family of Long Short Term Memory (LSTM) based models. We investigated two novel hybrid architectures: the LSTM model used in combination with Fast Iterative Filtering as decomposition algorithm (FIF-LSTM) and a method based on Multi-Head-Attention architecture (FIF-LSTM-MHA). FIF is a robust decomposition signal method very suitable for analyzing non-linear and non-stationary time series and it is used to separate the original time series into different oscillation components according to frequency, derived without leaving the time domain before to be fed into the neural network. The Attention mechanism is able to keep track of long-term dependencies in data sequences and improve the computational efficiency of the prediction model by reducing the effect of irrelevant information, mimicking human attention and selecting the most critical input. Our comparative analysis evaluated the models’ performance for different time lags and solar activity levels. The results indicated that the hybrid models achieve better performance than the LSTM model for mid-range F10.7 predictions while the LSTM achieves better performance within the first few time lags. FIF-LSTM-MHA gives more promising output for longer forecasts since it tends to smooth the prediction curve due to the peculiarity of the Attention module to discard less relevant features of the time series and highlight the global trend.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100786"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133724000015/pdfft?md5=702c624fbdced03b7eb08d858ec2dc15&pid=1-s2.0-S2213133724000015-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139101956","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":"Planetary orbital mapping and mosaicking (POMM) integrated open source software environment","authors":"Thomas L. Logan,&nbsp;Michael M. Smyth,&nbsp;Fred J. Calef III","doi":"10.1016/j.ascom.2024.100788","DOIUrl":"10.1016/j.ascom.2024.100788","url":null,"abstract":"<div><p>Several Open Source planetary orbital mapping and utility image processing software packages, including, VICAR, AFIDS, ISIS, GDAL, and GeoTIFF, have been integrated into a single software environment (POMM), where package programs can be run independently from a Linux command line, or combined in synergistic scripts that facilitate advanced trans-package applications. Several integrated scripts have been prepared to simplify some of the more difficult database building tasks such as (1) image co-registration (for stacking and time series analysis), (2) mosaicking (for regional analysis), and (3) map-projection of raw Planetary Data System (PDS) images for selected Mars and Luna sensor systems. A user interface/GUI is provided for the three planetary applications, but the underlying scripts can also be modified by an advanced user and run at the command-line. POMM is Open Source software available in “docker” container and “Yum-Install” versions that support cross-platform installation on Windows, Apple, and Linux products using available desktop applications and/or virtual containers. However, installation on systems requiring emulation can be slow, and the installation process can be challenging.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100788"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133724000039/pdfft?md5=5ff0b788994dbfd640979f734d497dba&pid=1-s2.0-S2213133724000039-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139412452","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":"Using GMM in open cluster membership: An insight","authors":"M. Mahmudunnobe ,&nbsp;P. Hasan ,&nbsp;M. Raja ,&nbsp;M. Saifuddin ,&nbsp;S.N. Hasan","doi":"10.1016/j.ascom.2024.100792","DOIUrl":"10.1016/j.ascom.2024.100792","url":null,"abstract":"<div><p>The unprecedented precision of Gaia has led to a paradigm shift in membership determination of open clusters where a variety of machine learning (ML) models can be employed. In this paper, we apply the unsupervised Gaussian Mixture Model (GMM) to a sample of thirteen clusters with varying ages (<span><math><mrow><mi>l</mi><mi>o</mi><mi>g</mi><mspace></mspace><mi>t</mi><mo>≈</mo></mrow></math></span> 6.38-9.64) and distances (441-5183 pc) from Gaia DR3 data to determine membership. We use ASteca to determine parameters for the clusters from our revised membership data. We define a quantifiable metric Modified Silhouette Score (MSS) to evaluate its performance. We study the dependence of MSS on age, distance, extinction, galactic latitude and longitude, and other parameters to find the particular cases when GMM seems to be more efficient than other methods. We compared GMM for nine clusters with varying ages but we did not find any significant differences between GMM performance for younger and older clusters. But we found a moderate correlation between GMM performance and the cluster distance, where GMM works better for closer clusters. We find that GMM does not work very well for clusters at distances larger than 3 kpc.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100792"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133724000076/pdfft?md5=181a3f6ba38a1f4c62fc1ed559a32440&pid=1-s2.0-S2213133724000076-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139581902","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":"The constrained accelerating universe in f(R,T) gravity","authors":"J.K. Singh,&nbsp;H. Balhara,&nbsp;Shaily,&nbsp;P. Singh","doi":"10.1016/j.ascom.2024.100795","DOIUrl":"10.1016/j.ascom.2024.100795","url":null,"abstract":"<div><p>In this paper, we study an alternative phenomenological model in <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity, where <span><math><mi>R</mi></math></span> indicates Ricci scalar curvature and <span><math><mi>T</mi></math></span> is the trace of the stress–energy–momentum tensor consisting of a modification in General Relativity, to explain the dynamics of a dark energy model at cosmological scales employed in a flat universe. Our basic concept is to create a model to analyze the behavior of the Universe right from early evolution up to its ultimate fate, which is an accelerated expansion in late times. Using the parametrization of the Hubble parameter <span><math><mi>H</mi></math></span>, we find a model, that begins with infinite energy density and infinite pressure and shows accelerating expansion in late times. We concentrate on contrasting this model with the most recent cosmological observations of the Hubble parameter (77 data points) and Pantheon measurements (1048 data points). Our joint analysis yields the present values of the free model parameter <span><math><mrow><mn>0</mn><mo>.</mo><mn>77</mn><msubsup><mrow><mn>6</mn></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>014</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>014</mn></mrow></msubsup></mrow></math></span> and Hubble parameter <span><math><mrow><mn>71</mn><mo>.</mo><mn>3</mn><msubsup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>25</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>66</mn></mrow></msubsup></mrow></math></span> for a flat universe. Finally, we conclude that our model behaves like a quintessence dark energy model in late times and is in good agreement with the recent observations.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100795"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133724000106/pdfft?md5=b2c85d12862e5b2f4900684a67eb6639&pid=1-s2.0-S2213133724000106-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139581741","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":"Quintessence behaviour dark energy models in f(Q,B)-gravity theory with observational constraints","authors":"D.C. Maurya","doi":"10.1016/j.ascom.2024.100798","DOIUrl":"https://doi.org/10.1016/j.ascom.2024.100798","url":null,"abstract":"<div><p>The present paper is an investigation of dark energy scenarios of cosmological models in recently proposed modified non-metricity gravity theory with boundary term in a flat FLRW spacetime universe. We have considered an arbitrary function <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>B</mi><mo>)</mo></mrow><mo>=</mo><mi>α</mi><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>+</mo><mi>β</mi><msup><mrow><mi>B</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span>, where <span><math><mi>Q</mi></math></span> is the non-metricity scalar, <span><math><mi>B</mi></math></span> is the boundary term given by <span><math><mrow><mi>B</mi><mo>=</mo><mover><mrow><mi>R</mi></mrow><mrow><mo>̊</mo></mrow></mover><mo>−</mo><mi>Q</mi></mrow></math></span>, and <span><math><mrow><mi>α</mi><mo>,</mo><mi>β</mi></mrow></math></span> are the model parameters, which is quadratic in both <span><math><mi>Q</mi></math></span> and <span><math><mi>B</mi></math></span>, for the action. We have investigated the dark energy features of the model with observational constraints on an specific Hubble function <span><math><mrow><mi>H</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow><mo>=</mo><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><msup><mrow><mrow><mo>[</mo><mi>λ</mi><msup><mrow><mrow><mo>(</mo><mn>1</mn><mo>+</mo><mi>z</mi><mo>)</mo></mrow></mrow><mrow><mi>n</mi></mrow></msup><mo>+</mo><mi>k</mi><mo>]</mo></mrow></mrow><mrow><mfrac><mrow><mn>1</mn></mrow><mrow><mn>2</mn></mrow></mfrac></mrow></msup></mrow></math></span>, where <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> is present value of Hubble constant, <span><math><mrow><mi>n</mi><mo>,</mo><mi>k</mi><mo>,</mo><mi>λ</mi></mrow></math></span> are arbitrary parameters with <span><math><mrow><mi>λ</mi><mo>+</mo><mi>k</mi><mo>=</mo><mn>1</mn></mrow></math></span>. We have found a transit phase (decelerated in past and accelerated at present) expanding universe model and have found the behaviour of dark energy equation of state (EoS) <span><math><msup><mrow><mi>ω</mi></mrow><mrow><mrow><mo>(</mo><mi>d</mi><mi>e</mi><mo>)</mo></mrow></mrow></msup></math></span> as <span><math><mrow><mo>(</mo><mo>−</mo><mn>1</mn><mo>.</mo><mn>007</mn><mo>≤</mo><msup><mrow><mi>ω</mi></mrow><mrow><mrow><mo>(</mo><mi>d</mi><mi>e</mi><mo>)</mo></mrow></mrow></msup><mo>≤</mo><mo>−</mo><mfrac><mrow><mn>1</mn></mrow><mrow><mn>3</mn></mrow></mfrac><mo>)</mo></mrow></math></span> and Om diagnostic analysis of the model shows the quintessence behaviour at present and cosmological constant scenario at late-time universe. We have also, analysed the statefinder parameters for the classification of dark energy models during expansion and also, we have estimated the present age of the universe that are found very closed to the recent observations.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100798"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133724000131/pdfft?md5=8478375a05e0a08e11bb7e548e1181d9&pid=1-s2.0-S2213133724000131-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139714047","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":"The HERMES calibration pipeline: mescal","authors":"G. Dilillo ,&nbsp;E.J. Marchesini ,&nbsp;G. Della Casa ,&nbsp;G. Baroni ,&nbsp;R. Campana ,&nbsp;E. Borciani ,&nbsp;S. Srivastava ,&nbsp;S. Trevisan ,&nbsp;F. Ceraudo ,&nbsp;M. Citossi ,&nbsp;Y. Evangelista ,&nbsp;A. Guzmán ,&nbsp;P. Hedderman ,&nbsp;C. Labanti ,&nbsp;E. Virgilli ,&nbsp;F. Fiore","doi":"10.1016/j.ascom.2024.100797","DOIUrl":"10.1016/j.ascom.2024.100797","url":null,"abstract":"<div><p>The HERMES Technologic and Scientific Pathfinder project is a constellation of six CubeSats aiming to observe transient high-energy events such as the Gamma Ray Bursts (GRBs). HERMES will be the first space telescope to include a <em>siswich</em> detector, able to perform spectroscopy in the 2 keV to 2 MeV energy band. The particular siswich architecture, which combines a solid-state Silicon Drift Detector and a scintillator crystal, requires specific calibration procedures that have not been yet standardized in a pipeline. We present in this paper the HERMES calibration pipeline, <span>mescal</span>, intended for raw HERMES data energy calibration and formatting. The software is designed to deal with the particularities of the siswich architecture and to minimize user interaction, including also an automated calibration line identification procedure, and an independent calibration of each detector pixel, in its two different operating modes. The <span>mescal</span> pipeline can set the basis for similar applications in future siswich telescopes.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100797"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S221313372400012X/pdfft?md5=f0527f7cc0e2a4311fcea397ff5032af&pid=1-s2.0-S221313372400012X-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139657925","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":"The effect of baseline on the uncertainties of range determination performed by two-site astrometric observations","authors":"H.G. Gökay ,&nbsp;S. Özdemi̇r ,&nbsp;M.N. Bağıran ,&nbsp;S. Aydın","doi":"10.1016/j.ascom.2024.100787","DOIUrl":"10.1016/j.ascom.2024.100787","url":null,"abstract":"<div><p>The uncertainties in range determination depending on two-site locations for GEO satellites were calculated and shown that the uncertainty in the range depends not only on linear baseline distance between the locations but also both latitude and longitude of geographic coordinates of the sites. By taking the first observing site as fixed and changing the location of the second site, the triangulated range calculations were performed by using SGP4 orbital model and published Two-Line Elements (TLE). Additionally, as a sample of triangulated observation, the results of nearly synchronous two-site astrometric measurements of two GEO satellites, TURKSAT 3A and TURKSAT 4A, were presented. These astrometric observations were carried out in TÜBITAK National Observatory (TUG), Antalya and TURKSAT Company’s site, Ankara. Although the baseline between the observatory sites corresponds to a relatively short distance of about 400 km, measured range determinations well stays under the error level expected by Choi et al. (2010).</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100787"},"PeriodicalIF":2.5,"publicationDate":"2024-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133724000027/pdfft?md5=6cfd1d122d56dbdf2ffa095e9b9f5360&pid=1-s2.0-S2213133724000027-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139412330","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":"Harnessing edge-enhanced attention mechanisms for supernova detection in deep learning frameworks","authors":"K. Yin ,&nbsp;J. Jia ,&nbsp;F. Li ,&nbsp;X. Gao ,&nbsp;T. Sun","doi":"10.1016/j.ascom.2023.100784","DOIUrl":"10.1016/j.ascom.2023.100784","url":null,"abstract":"<div><p>Recent studies have shown the advantages of convolutional neural networks in the classification and detection of supernovae. In our prior work, we employed one-stage object detection frameworks to address the challenges of presupposed location and varying image sizes in supernova detection. Notably, the backbone of the object detectors naturally emphasized the edges of candidate regions in the visualized heatmap, reflecting the strategies adopted by human observers. Capitalizing on this similarity, we introduce an innovative edge attention module, tailored to prioritize the edges of candidate regions, and improved the performance of supernova detectors. In parallel, we have developed a three-channel supernova detection dataset by integrating science (current), template (reference), and difference images into a three-channel configuration. The candidates in the new dataset are more conspicuous. To assess the efficacy of our edge attention module, we conducted a series of experiments on the proposed dataset. The experimental results establish the superiority of the proposed method in detecting supernovae. Additionally, visualizations of the feature maps shows the proposed edge attention is able to reallocate weights around the candidate edges, corroborating its effectiveness.</p></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"46 ","pages":"Article 100784"},"PeriodicalIF":2.5,"publicationDate":"2023-12-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S2213133723000999/pdfft?md5=ac31d2323a16f279ff700e51a1002074&pid=1-s2.0-S2213133723000999-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138689870","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}