Astronomy and Computing最新文献

{"title":"Confirmation of binary clustering in gamma-ray bursts through an integrated p-value from multiple nonparametric tests of hypotheses","authors":"S. Modak","doi":"10.1016/j.ascom.2025.100931","DOIUrl":"10.1016/j.ascom.2025.100931","url":null,"abstract":"<div><div>The paper applies a new, nonparametric, interpoint distance-based measure to confirm the inherent groups prevailing in the brightest source of light in the universe: gamma-ray bursts. Our effective metric, in association with clustering methods like Gaussian-mixture model-based and <span><math><mi>K</mi></math></span>-means algorithms, resolves the conflict regarding the possibility about existence of more than binary clusters in the gamma-ray burst population. Here we carry out multiple nonparametric statistical tests of hypotheses, as many as the number of bursts available from the ‘BATSE’ catalog. An integrated <span><math><mi>p</mi></math></span>-value achieved from the aforesaid dependent tests solves our concern confirming two groups of short and long bursts.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100931"},"PeriodicalIF":1.9,"publicationDate":"2025-01-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143268282","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":"Disentangling transients and their host galaxies with scarlet2: A framework to forward model multi-epoch imaging","authors":"C. Ward ,&nbsp;P. Melchior ,&nbsp;M.L. Sampson ,&nbsp;C.J. Burke ,&nbsp;J. Siegel ,&nbsp;B. Remy ,&nbsp;S. Birmingham ,&nbsp;E. Ramey ,&nbsp;S. van Velzen","doi":"10.1016/j.ascom.2025.100930","DOIUrl":"10.1016/j.ascom.2025.100930","url":null,"abstract":"<div><div>Many science cases for wide-field time-domain surveys rely on accurate identification and characterization of the galaxies hosting transient and variable objects. In the era of the Legacy Survey of Space and Time (LSST) at the Vera C. Rubin Observatory the number of known transient and variable sources will grow by orders of magnitude, and many of these sources will be blended with their host galaxies and neighboring galaxies. A diverse range of applications – including the classification of nuclear and non-nuclear sources, identification of potential host galaxies in deep fields, extraction of host galaxy spectral energy distributions without requiring a transient-free reference image, and combined analysis of photometry from multiple surveys – will benefit from a flexible framework to model time-domain imaging of transients. We describe a time-domain extension of the <span>scarlet2</span> scene modeling code for multi-epoch, multi-band, and multi-resolution imaging data to extract simultaneous transient and host galaxy models. <span>scarlet2</span> leverages the benefits of data-driven priors on galaxy morphology, is fully GPU compatible, and can jointly model multi-resolution data from ground and space-based surveys. We demonstrate the method on simulated LSST-like supernova imaging, low-resolution Zwicky Transient Facility imaging of tidal disruption events, and Hyper Suprime Cam imaging of variable AGN out to <span><math><mrow><mi>z</mi><mo>=</mo><mn>4</mn></mrow></math></span> in the COSMOS fields. We show that <span>scarlet2</span> models provide accurate transient and host galaxy models as well as accurate measurement of host–transient spatial offsets, and demonstrate future applications to the search for ‘wandering’ massive black holes.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100930"},"PeriodicalIF":1.9,"publicationDate":"2025-01-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143377213","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":"Data based investigation on galaxy formation and evolution theory through statistical techniques","authors":"Prasenjit Banerjee ,&nbsp;Tanuka Chattopadhyay ,&nbsp;Asis Kumar Chattopadhyay","doi":"10.1016/j.ascom.2025.100928","DOIUrl":"10.1016/j.ascom.2025.100928","url":null,"abstract":"<div><div>The present work deals with a large data set of star-forming as well as quiescent galaxies at red shifts ranging from 0 to 4 (0<span><math><mo>≤</mo></math></span>z<span><math><mo>≤</mo></math></span>4). The present selected catalogues of objects have been compiled from the NEWFIRM Medium-Band Survey (NMBS). We have concatenated both the catalogues AEGIS and COSMOS, present in NMBS, one after another to form a master catalog. Several derivable parameters were present in the catalog, but we have limited our choice to the observable as well as the physical parameters of the galaxies. In this paper, we have studied the evolutionary pattern of the galaxies by dividing them into various groups according to red shift, and observing the distributional pattern of those groups. Later, the evolutionary pattern of the galaxies is investigated by examining the size-mass relationship corresponding to these groups and comparing the level of dependence of the parameters under study.</div><div>In order to perform a proper analysis of the data for the above-mentioned objectives, we have used statistical techniques like multiple testing, the Shapiro–Wilk test, independent component analysis, multivariate outlier detection, multivariate kernel density estimation, and kernel regularized least squares method. Two noble findings that have been observed in this work are (a) The galaxy parameters with high red shifts (z <span><math><mo>&gt;</mo></math></span> 3.5) follow a multivariate Gaussian distribution, helping us to infer that high red shift (z <span><math><mo>&gt;</mo></math></span> 3.5) galaxy parameters show more randomness compared to other galaxies with z<span><math><mo>&lt;</mo></math></span>3.5. (b) There is a deviation from the linearity of the covariates in very high-redshift galaxies (z <span><math><mo>&gt;</mo></math></span> 3.5) for modeling log mass as a response variable. The same is also observed with the half-life radius as the response variable, although there exists a linear relationship between the mass and the effective radius of the galaxy. These observations may be treated as new findings of the present study.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100928"},"PeriodicalIF":1.9,"publicationDate":"2025-01-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143144126","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":"FRELLED Reloaded: Multiple techniques for astronomical data visualisation in Blender","authors":"R. Taylor","doi":"10.1016/j.ascom.2024.100927","DOIUrl":"10.1016/j.ascom.2024.100927","url":null,"abstract":"<div><div>I present version 5.0 of FRELLED, the FITS Realtime Explorer of Low Latency in Every Dimension. This is a 3D data visualisation package for the popular Blender art software, designed to allow inspection of astronomical volumetric data sets (primarily, but not exclusively, radio wavelength data cubes) in real time using a variety of visualisation techniques. The suite of Python scripts that comprise FRELLED have been almost completely recoded and many new ones added, bringing FRELLED’s operating environment from Blender version 2.49 to 2.79. Principle new features include: an enormously simplified installation procedure, a more modular graphical appearance that takes advantage of Blender 2.79’s improved interface, much faster loading of FITS data, support for larger data sets, options to show the data as height maps in 2D mode or isosurfaces in 3D mode, utilisation of standard <em>astropy</em> and other Python modules to support a greater range of FITS files (with a particular emphasis on higher-frequency radio data such as from ALMA, the Atacama Large Millimetre Array), and the capability of exporting the data to Blender 2.9+ which supports stereoscopic 3D displays in virtual reality headsets. In addition, in-built help files are accessible from each menu panel, as well as direct links to a complete wiki and set of video tutorials. Finally, the code itself is much more modular, allowing easier maintainability and, over the longer term, a far easier prospect of migrating to more recent versions of Blender.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100927"},"PeriodicalIF":1.9,"publicationDate":"2025-01-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143144124","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":"DCAPPSO: A novel approach for inverting asteroid rotational properties with applications to DAMIT and Tianwen-2 target asteroid","authors":"Yong-Xiong Zhang ,&nbsp;Wen-Xiu Guo ,&nbsp;Hua Zheng ,&nbsp;Wei-Lin Wang","doi":"10.1016/j.ascom.2024.100925","DOIUrl":"10.1016/j.ascom.2024.100925","url":null,"abstract":"<div><div>This paper introduces the Dynamic Coefficient Adjustment in Parallel Particle Swarm Optimization (DCAPPSO) algorithm for inverting asteroid rotational properties from lightcurve data. DCAPPSO integrates a Cellinoid shape model with Particle Swarm Optimization (PSO), dynamic coefficient adjustment, and parallel computing, offering improved efficiency and accuracy in asteroid parameter determination. The algorithm’s performance was evaluated using simulated asteroid lightcurves and applied to 24 real asteroids from the DAMIT database, including a detailed case study of asteroid (44)Nysa and an additional discussion of asteroid (433)Eros. Results show excellent consistency with established rotational periods, with uncertainties typically ranging from ± 0.000018 to ± 0.009981 h. Pole orientation determinations demonstrate good agreement, particularly for latitude components. The algorithm’s parallel implementation achieves a speedup of 48.617x with 100 workers on multicore CPUs. DCAPPSO was also applied to asteroid (469219) Kamo’oalewa, the Tianwen-2 mission target, providing new insights into its shape and rotational properties. For Kamo’oalewa, the algorithm derived a rotational period of <span><math><mrow><mn>0</mn><mo>.</mo><mn>460510</mn><mspace></mspace><mi>h</mi></mrow></math></span> (27.63 min) and a pole orientation of <span><math><mrow><mo>(</mo><mn>134</mn><mo>.</mo><mn>67</mn><mo>°</mo><mo>,</mo><mo>−</mo><mn>11</mn><mo>.</mo><mn>39</mn><mo>°</mo><mo>)</mo></mrow></math></span>. Uncertainty analysis yielded estimates of <span><math><mrow><mn>133</mn><mo>.</mo><mn>52</mn><mo>°</mo><mo>±</mo><mn>0</mn><mo>.</mo><mn>01</mn><mo>°</mo></mrow></math></span> for pole longitude, <span><math><mrow><mo>−</mo><mn>10</mn><mo>.</mo><mn>67</mn><mo>°</mo><mo>±</mo><mn>0</mn><mo>.</mo><mn>05</mn><mo>°</mo></mrow></math></span> for pole latitude, and 0.466017 ± 0.006090 h for the rotational period. Shape analysis indicates a moderately elongated form with axis ratios <span><math><mrow><mi>b</mi><mo>/</mo><mi>a</mi><mo>≈</mo><mn>0</mn><mo>.</mo><mn>67</mn></mrow></math></span> and <span><math><mrow><mi>c</mi><mo>/</mo><mi>a</mi><mo>≈</mo><mn>0</mn><mo>.</mo><mn>56</mn></mrow></math></span>. This research advances asteroid inversion techniques, offering an efficient tool to address increasing observational data volumes in planetary science.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100925"},"PeriodicalIF":1.9,"publicationDate":"2025-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143144127","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 behavior of a hyperbolic solution in f(Q) gravity","authors":"K. Haloi,&nbsp;R. Roy Baruah","doi":"10.1016/j.ascom.2024.100926","DOIUrl":"10.1016/j.ascom.2024.100926","url":null,"abstract":"<div><div>In this work, we study the universe’s dynamics in the context of f(Q) gravity by use of a flat FLRW model. Two particular forms are considered: <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><mi>Q</mi></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>λ</mi><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span>, where Q and <span><math><mi>λ</mi></math></span> represent the nonmetricity and arbitrary constant, respectively. We take a special form for the scale factor, <span><math><mrow><mi>a</mi><mo>=</mo><mi>s</mi><mi>i</mi><mi>n</mi><mi>h</mi><msup><mrow><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow></mrow><mrow><mfrac><mrow><mn>1</mn></mrow><mrow><mi>α</mi></mrow></mfrac></mrow></msup></mrow></math></span>, to solve the Friedmann field equations within the f(Q) formalism. The scale factor’s behavior is here determined by the model parameter <span><math><mi>α</mi></math></span>. In our model, we primarily analyze the behavior of the equation of state parameter <span><math><mi>ω</mi></math></span>. We examine the scalar field and examine the resultant solution’s energy conditions. We use a number of diagnostic techniques, including the Jerk, Om, and statefinder diagnostic tools, to validate our model. We also include the observational constraints from the BAO and Hubble databases. A thorough explanation of the outcomes and the model is given.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100926"},"PeriodicalIF":1.9,"publicationDate":"2025-01-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143144125","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":"Observational constraints on quark and strange quark matters in f(R,T) theory of gravity","authors":"D.D. Pawar ,&nbsp;N.G. Ghungarwar ,&nbsp;Shah Muhammad ,&nbsp;E. Zotos","doi":"10.1016/j.ascom.2024.100924","DOIUrl":"10.1016/j.ascom.2024.100924","url":null,"abstract":"<div><div>We have examined a plane symmetric cosmological model in the presence of quark and strange quark matter with the help of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> theory of gravity. To find solutions for this type of space–time, we applied a power-law relationship between the scale factor and the deceleration parameter. We used a variable deceleration parameter. We applied constraints on the parameters using the <span><math><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup></math></span> test and obtained the best-fit values for the Hubble parameter <span><math><mrow><mi>H</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow></mrow></math></span> using 57 observed data points, achieving an <span><math><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup></math></span> value of 0.9321 and an RMSE of 11.0716. The best-fit parameters were <span><math><mrow><mi>α</mi><mo>=</mo><mn>0</mn><mo>.</mo><mn>54</mn><msubsup><mrow><mn>2</mn></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>022</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>019</mn></mrow></msubsup></mrow></math></span>, <span><math><mrow><mi>β</mi><mo>=</mo><mn>52</mn><mo>.</mo><msubsup><mrow><mn>9</mn></mrow><mrow><mo>−</mo><mn>2</mn><mo>.</mo><mn>7</mn></mrow><mrow><mo>+</mo><mn>2</mn><mo>.</mo><mn>3</mn></mrow></msubsup></mrow></math></span>, and <span><math><mrow><msub><mrow><mi>c</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mo>−</mo><mn>0</mn><mo>.</mo><mn>87</mn><msubsup><mrow><mn>7</mn></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>058</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>055</mn></mrow></msubsup></mrow></math></span>, resulting in <span><math><mrow><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>64</mn><mo>.</mo><mn>3</mn><msubsup><mrow><mn>9</mn></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>47</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>04</mn></mrow></msubsup><mspace></mspace><mtext>km/s/Mpc</mtext></mrow></math></span>. These results show that our model closely matches the <span><math><mi>Λ</mi></math></span>CDM model, demonstrating its accuracy in describing the universe’s expansion history across the given redshift range. We also discussed cosmological parameters such as spatial volume, the mean anisotropic parameter, the shear scalar, deceleration parameter, energy density and pressure for quark matter and strange quark matter for plane symmetric spacetime.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100924"},"PeriodicalIF":1.9,"publicationDate":"2025-01-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143144118","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":"More than a void? The detection and characterization of cavities in a simulated galaxy’s interstellar medium","authors":"Abolfazl Taghribi ,&nbsp;Marco Canducci ,&nbsp;Michele Mastropietro ,&nbsp;Sven De Rijcke ,&nbsp;Reynier Frans Peletier ,&nbsp;Peter Tino ,&nbsp;Kerstin Bunte","doi":"10.1016/j.ascom.2024.100923","DOIUrl":"10.1016/j.ascom.2024.100923","url":null,"abstract":"<div><div>The interstellar medium of galaxies is filled with holes, bubbles, and shells, typically interpreted as remnants of stellar evolution. There is growing interest in the study of their properties to investigate stellar and supernova feedback. So far, the detection of cavities in observational and numerical data is mostly done visually and, hence, is prone to biases. Therefore, we present an automated, objective method for discovering cavities in particle simulations, with demonstrations using hydrodynamical simulations of a dwarf galaxy. The suggested technique extracts holes based on the persistent homology of particle positions and identifies tight boundary points around each. With a synthetic ground-truth analysis, we investigate the relationship between data density and the detection radius, demonstrating that higher data density also allows for the robust detection of smaller cavities. By tracking the boundary points, we can measure the shape and physical properties of the cavity, such as its temperature. In this contribution, we detect 808 holes in 21 simulation snapshots. We classified the holes into supernova-blown bubbles and cavities unrelated to stellar feedback activity based on their temperature profile and expansion behaviour during the 100 million years covered by the simulation snapshots analysed for this work. Surprisingly, less than 40% of the detected cavities can unequivocally be linked to stellar evolution. Moreover, about 36% of the cavities are contracting, while 59% are expanding. The rest do not change for a few million years. Clearly, it is erroneous to interpret observational data based on the premise that all cavities are supernova-related and expanding. This study reveals that supernova-driven bubbles typically exhibit smaller diameters, larger expansion velocities, and lower kinetic ages (with a maximum of 220 million years) compared to other cavities.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100923"},"PeriodicalIF":1.9,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143144117","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":"Virtual realities: Is there only one advanced image display that astronomers need?","authors":"C.J. Fluke,&nbsp;H.K. Walsh,&nbsp;L. de Zoete Grundy,&nbsp;B. Brady","doi":"10.1016/j.ascom.2024.100896","DOIUrl":"10.1016/j.ascom.2024.100896","url":null,"abstract":"<div><div>Data visualisation is an essential ingredient of scientific analysis, discovery, and communication. Along with a human (to do the looking) and the data (something to look at), an image display device is a key component of any data visualisation workflow. For the purpose of this work, standard displays include combinations of laptop displays, peripheral monitors, tablet and smartphone screens, while the main categories of advanced displays are stereoscopic displays, tiled display walls, digital domes, virtual/mixed reality (VR/MR) head-mounted displays, and CAVE/CAVE2-style immersive rooms. We present the results of the second Advanced Image Displays for Astronomy (AIDA) survey, advertised to the membership of the Astronomical Society of Australia (ASA) during June–August 2021. The goal of this survey was to gather background information on the level of awareness and usage of advanced displays in astronomy and astrophysics research. From 17 complete survey responses, sampled from a population of <span><math><mrow><mo>∼</mo><mn>750</mn></mrow></math></span> ASA members, we infer that: (1) a high proportion of ASA members use standard displays but do not use advanced displays; (2) a moderate proportion have seen a VR/MR HMD, and may also have used one — but not for research activities; and (3) there is a need for improved knowledge in general about advanced displays, along with relevant software or applications that can target specific science needs. We expect that this is compatible with the experiences of much of the international astronomy and astrophysics research community. We suggest that VR/MR head-mounted displays have now reached a level of technical maturity such that they could be used to replicate or replace the functionality of most other advanced displays.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"50 ","pages":"Article 100896"},"PeriodicalIF":1.9,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143137147","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":"A high performance multi-band data fusion approach for CSST based on column-oriented database","authors":"Zhipeng Huang (黄智鹏) ,&nbsp;Wei Du (杜薇) ,&nbsp;Feng Wang (王锋) ,&nbsp;Shoulin Wei (卫守林) ,&nbsp;Hui Deng (邓辉) ,&nbsp;Ying Mei (梅盈) ,&nbsp;Tianmeng Zhang (张天萌)","doi":"10.1016/j.ascom.2024.100922","DOIUrl":"10.1016/j.ascom.2024.100922","url":null,"abstract":"<div><div>High-performance multi-catalog fusion or cross-matching has always been an essential issue in astronomical data processing. In this study, we focus on the fusion of multi-band catalog data in a wide-area survey for the China Space Station Telescope (CSST). We implemented a simple and efficient data fusion method based on column-oriented database technology to produce a more consistent and accurate catalog, and this method can carry out the fusion of millions of source records in a few dozen seconds. We analyze and discuss several significant issues related to data fusion, such as the spatial partitioning and indexing of the target sky regions, the efficient implementation of fusion based on joining in the database, and the segmented processing method to address the issue of missing sources at different declinations. The performance profiling results show that by employing the MergeTree table engine within ClickHouse, establishing high-speed indexes based on the spatial partition index number, adopting an appropriate partitioning strategy, and maintaining orderly storage of records in the database according to the spatial partition index number, the efficient fusion of astronomical catalogs can be accomplished through SQL statements. Performance tests show that the proposed method can fulfill CSST data processing requirements, and it is also of reference value for future work related to massive astronomical data fusion. Compared with data fusion systems such as Large Survey DataBase (LSDB), our method can achieve similar performance results with consistent results.</div></div>","PeriodicalId":48757,"journal":{"name":"Astronomy and Computing","volume":"51 ","pages":"Article 100922"},"PeriodicalIF":1.9,"publicationDate":"2024-12-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143144128","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}