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This paper delves into the origin and significance of Copernicus’ tellurium. It will show that this astronomical model, which appeared in the Frontispiece of Galileo’s Dialogue and turned out to become Copernicus’ most representative symbol, resulted from Galileo’s analysis of the arguments supporting heliocentrism. A particular version of the tellurium, closely associated with the Galilean Florentine context, is also depicted in a painting of the Uffizi Gallery and a canvas owned by a well-known eighteenth-century astronomer. These two portraits of Copernicus, which have been largely overlooked, are now being considered to underscore the deep connection between the emergence and recognition of this iconographical model of Copernicus and Galileo’s work and legacy. [ABSTRACT FROM AUTHOR]

In his unfinished Ad harmonicon coeleste, François Viète (1540–1603) approaches astronomical models in a purely mathematical way, analyzing the equations involved in them and suggesting new geometrical approaches, usually equivalent but simpler. After dealing with the Copernican planetary models, he develops three different lunar models. The first one describes a model geometrically similar but not identical to the Ptolemaic lunar model. The second is identical to that of Copernicus, but Viète significantly simplifies the calculation methods, and the third one is inspired by Tycho's lunar model. In a previous paper, I analyzed the first model. In this paper, I describe and analyze the second one, leaving for a future work the third one. Extending the ellipse models used by Viète for the outer planets, I also show that every model of epicycle and deferent can be replaced by a planet revolving on a rotating ellipse. [ABSTRACT FROM AUTHOR]

The coal‐bearing series of the Eocene Pinghu Formation is one of the focused reservoir exploration in the Xihu Sag. This study conducted a cyclostratigraphy time series analysis using natural gamma‐ray (GR) logging data from four boreholes of the Xihu Sag. The spectral analysis shows a good match with the La2004 orbital solution. The sedimentation duration calculated by the astronomical age models spans at least 4.31–5.94 Myr, with an average sedimentation rate of 13.47–18.57 cm/kyr. The Pinghu Formation is subdivided into 1 second‐order, 3 third‐order and 14 fourth‐order sequences within seismic, well logging and 405 kyr‐long cycles constraints. Based on available age‐control data, the Pinghu Formation is corresponding to the middle‐late Eocene. The floating astronomical timescale of XH‐3 borehole now provides a new age constraint for the Pinghu Formation. There are four shorter‐term (<2 Myr) regional sea‐level cycles in the Pinghu Formation, which are similar to the calibrated global sea‐level fluctuations. Inconsistencies between reconstructed sea‐level curve by sedimentary noise modelling and true sea level inferred from lithology and sequence reveal various sources of noise in the sedimentary record. Variations in the distribution and thickness of coal seams in the Pinghu Formation appear to be a stratigraphic response to astronomical and non‐astronomical forcing such as regional tectonicssm and facies changes. [ABSTRACT FROM AUTHOR]

The control system for terrestrial two-axis devices for orientation to the Sun has been improved with a highspeed microcontroller operation algorithm. A geomagnetic sensor was introduced into the system to increase the reliability of monitoring the positioning of solar cells. The basis of the algorithm is a simplified astronomical and geographical model of the movement of the Sun in the celestial sphere. The control system automatically tracks the trajectory of the Sun and calculates its angular coordinates for the current moment of time on any day of the year and for any point on the globe. The derived equations of the simplified mathematical model are suitable for calculations of orientation angles to the Sun in real time on 8-bit microcontrollers with low computing power. The control system by AVR-328 microcontrollers was studied. It was established that the use of the algorithm when programming microcontrollers for two-axis orientation systems ensures high stability and reliability of the tracker`s functioning process. The technical parameters of the AVR-328 microcontrollers in the case of using the developed algorithm ensure that the control system performs one reorientation step in a time interval of less than 2 seconds, which ensures the minimum technical period of the reorientation process by the tracker drive mechanisms which is about 5 seconds. Deviations of the calculated orientation angle from the exact value do not exceed 3°, which corresponds to the relative accuracy of recording the solar radiation intensity, which is less than 0.3 %. The microcontroller program written according to the developed simplified algorithm occupies about 35 % of its memory. Therefore, the use of the developed algorithm frees up the resources of AVR-328 microcontrollers for performing additional data processing operations and automatic control over various additional devices related to the process of orientation to the Sun. In the case of solar energy, the algorithm ensures the use of about 98 % of the power of solar radiation. [ABSTRACT FROM AUTHOR]

At present, large-scale sky surveys have obtained a large volume of stellar spectra. An efficient classification algorithm is of great importance to the practice of astronomical research. In this paper, we propose a novel parallel optimization algorithm based on a lock-free and shared-memory environment to solve the model for astronomical spectra class. Firstly, the SMOTE-TOMEK and RobustScaler are introduced to use for class balancing and data normalization. Secondly, 1-Dimensional Convolutional Neural Networks (1-D CNN) with L2-norm loss function is utilized as a classifier. Finally, LFA-SGD, LFA-Adagrad, LFA-RMSprop and LFA-Adam algorithms are proposed and applied to the classifier solution. The Lock-Free and shared-memory parallel Asynchronous environment (LFA) relies on GPU multiprocessing, allowing the algorithm to fully utilize the multi-core resources of the computer. Due to its sparsity, the convergence speed is significantly faster. The experimental results show that LFA-SGD algorithm and its variants achieved state-of-the-art accuracy and efficiency for astronomical spectra class. [ABSTRACT FROM AUTHOR]

Rapid strides are currently being made in the field of artificial intelligence using transformer-based models like Large Language Models (LLMs). The potential of these methods for creating a single, large, versatile model in astronomy has not yet been explored. In this work, we propose a framework for data-driven astronomy that uses the same core techniques and architecture as used by LLMs. Using a variety of observations and labels of stars as an example, we build a transformer-based model and train it in a self-supervised manner with cross-survey data sets to perform a variety of inference tasks. In particular, we demonstrate that a single model can perform both discriminative and generative tasks even if the model was not trained or fine-tuned to do any specific task. For example, on the discriminative task of deriving stellar parameters from Gaia XP spectra, we achieve an accuracy of 47 K in T eff, 0.11 dex in log  g , and 0.07 dex in [M/H], outperforming an expert XGBoost model in the same setting. But the same model can also generate XP spectra from stellar parameters, inpaint unobserved spectral regions, extract empirical stellar loci, and even determine the interstellar extinction curve. Our framework demonstrates that building and training a single foundation model without fine-tuning using data and parameters from multiple surveys to predict unmeasured observations and parameters is well within reach. Such 'Large Astronomy Models' trained on large quantities of observational data will play a large role in the analysis of current and future large surveys. [ABSTRACT FROM AUTHOR]

In China, the precession of the equinoxes was conceptualized as an "annual difference" (suicha 歲差) between the tropical and sidereal year. The idea was introduced in the fourth century, it saw universal acceptance from the eighth century on, and it was in the four centuries in between that it was tried, debated, and spread whilst a Mediterranean-origin concept thereof arrived from India. Its four-century journey from fringe idea to universal truth is a well-studied point of interest in the history of astronomy. In this article, we will shift focus to the idea's polymathic protagonists and epistemic foundations to explore how a scientific idea was born, debated, transmitted, and taught in Confucian commentary and, no less important, how politics, geography, regional schools, foreign transmission, and the Buddhist and Daoist religions shaped how thinkers engaged with it as individuals and as communities. Inspired by the work of Chen Kanli and Randall Collins, the goal is to show that there is nothing simple or inexorable about how even an empirically useful tool of predictive astronomical modeling is received in the relevant expert community, as it is but one element in a complex network of people and ideas aligning and opposing in ever-evolving strategies to assert relevance. [ABSTRACT FROM AUTHOR]

There are few documentations of far‐field effects of coolhouse glaciation and its signature preserved within Middle Jurassic carbonate platforms. Through outcrop logging and time series analysis we document the cyclostratigraphy of the upper Bajocian‐Bathonian interval of the Adriatic Platform, Croatia. The 200 m thick, ∼3.3 Myr duration cyclic platform record consists of peritidal carbonate parasequences (n = 109) with high‐energy grainstone‐rudstone bases fining up into micritic carbonate caps. There is little evidence of long‐term exposure near purported sequence boundaries, indicating the succession is conformable above the parasequence scale. Time series were constructed using Dunham rank and stratigraphic position, and parasequence thickness and stratigraphic position. A statistical estimation of accumulation rates using average spectral misfit (ASM) and correlation coefficient (COCO) methods that compare spectral peaks with an astronomical model at various sedimentation rates suggests that these rates ranged from 4.5 to 6 cm/kyr, which is compatible with long‐term rates based on thickness divided by duration. The time series analysis of rank series and cycle thickness series indicates long‐term obliquity modulation (∼1 Myr), short obliquity modulation (173 kyr), strong obliquity, and weak precession. The 173 kyr cycle is particularly evident in the cycle thickness series. The similarity of the spectra to the obliquity‐dominated Cenozoic coolhouse supports moderate southern hemisphere glaciation driving glacioeustatic sea level changes during the Middle Jurassic. Plain Language Summary: Earth's climate has been paced by eccentricity of its orbit (periods of 405,000 and 100,000 years) which modulates precession (or wobble, ∼20,000 years), and the tilt (obliquity) of its axis (∼40,000 years), with tilt and wobble being slightly shorter as we go back in time. We examined the succession of carbonate rocks in a 166–169.5 million‐year‐old, Middle Jurassic carbonate platform in Croatia, deposited during a time when there is evidence of moderate glaciation at the poles. The results indicate that the rock record was dominated by the tilt signal with little evidence of eccentricity. This is very similar to the deep sea record from 2 million to 700,000 years ago, which also is dominated by obliquity associated with moderate glaciation at both poles. The results strongly support the contention of moderate glaciation during the Middle Jurassic. Key Points: Middle Jurassic Bajocian‐Bathonian dominated by obliquity forcing of climate/sea levelOrbital signal is dominated by ∼1 Myr long obliquity cycle, short (173 kyr) obliquity modulation cycle, obliquity, and minor precessionObliquity forcing supports the existence of moderate ice sheets at high latitudes in the Middle Jurassic [ABSTRACT FROM AUTHOR]

In his unfinished Ad harmonicon coeleste, François Viète (1540–1603) approaches astronomical models in a purely mathematical way, analyzing the equations involved in the geometrical models and suggesting new geometrical approaches, usually equivalent but simpler. After dealing with the Copernican planetary models, he develops three different lunar models. The first one describes a model geometrically similar but not identical to the Ptolemaic lunar model. The second is identical to that of Copernicus, but offers simpler calculation methods, and the third one is inspired by Tycho's lunar model in the Progymnasmata. In this paper, I describe and analyze the first (Ptolemaic) model, leaving the other two for future works. [ABSTRACT FROM AUTHOR]

A dedicated simulator, Poisson_CCD, has been constructed which models astronomical CCDs by solving Poisson's equation numerically and simulating charge transport within the CCD. The potentials and free carrier densities within the CCD are self-consistently solved for, giving realistic results for the charge distribution within the CCD storage wells. The simulator has been used to model the CCDs that are being used to construct the LSST digital camera. The simulator output has been validated by comparing its predictions with several different types of CCD measurements, including astrometric shifts, brighter-fatter induced pixel–pixel covariances, saturation effects, and diffusion spreading. The code is open source and freely available. [ABSTRACT FROM AUTHOR]

Tracking Planetary Motion in the Classroom by Using Video Analysis in Astronomical Model Experiments In this article, we show that with the use of video analysis software, in our case Tracker, the trajectories can be highlighted, and complex phenomena such as formation of planetary orbits or gravity-assisted maneuvers of spacecraft can be illustrated. Gravity-assisted maneuver (flyby maneuver) The gravity-assisted maneuver uses the gravity of an astronomical object to save propellant and reduce expense. Formation of planetary orbits The third experiment simulates a primordial solar system, indicating an answer to why the bodies in a solar system revolve in the same direction. [Extracted from the article]

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The 19th annual Sophia Centre Conference, titled "The Harmony of Heaven and Earth," took place at the University of Wales Trinity Saint David in June 2022. Scholars from various disciplines gathered to explore the concept of harmony in relation to cosmology, culture, and the environment. The conference covered a wide range of topics, including astrology, medieval Spain, astrological beliefs of Pope Leo X, Romanian folk stories and music, Pythagorean principles of harmony, Daoist cosmology, Tibetan Buddhist spirituality, Hindu conceptualizations of harmony, and the preservation of astronomical sites in Kenya. Presentations also addressed the social impacts of light pollution and the proliferation of artificial satellites. The conference aimed to provide a diverse and unified perspective on the theme of harmony. [Extracted from the article]

The homologous collapse of a sphere of uniform density from a resting state under its self-gravity has been used to model the formation of astronomical objects. It is well known that the evolution of the radius with time cannot be obtained explicitly because of the need to solve a transcendental equation of cycloidal parameter with respect to time. By combining the Padé approximation and the Schröder formula, we construct an approximate analytical solution of radius as a function of time. Our method is a direct method rather than an iteration method and it requires only solving a cubic equation and evaluating three trigonometric functions. Compared with the existing methods, the accuracy and effectiveness of this method are clearly illustrated. [ABSTRACT FROM AUTHOR]

We combine data sets from the CGM2 and CASBaH surveys to model a transition point, R cross, between circumgalactic and intergalactic media (CGM and IGM, respectively). In total, our data consist of 7244 galaxies at z < 0.5 with precisely measured spectroscopic redshifts, all having impact parameters of 0.01–20 comoving Mpc from 28 QSO sightlines with high-resolution UV spectra that cover H i Ly α. Our best-fitting model is a two-component model that combines a 3D absorber–galaxy cross-correlation function with a simple Gaussian profile at inner radii to represent the CGM. By design, this model gives rise to a determination of R cross as a function of galaxy stellar mass, which can be interpreted as the boundary between the CGM and IGM. For galaxies with 108 ≤ M ⋆/ M ⊙ ≤ 1010.5, we find that R cross(M ⋆) ≈ 2.0 ± 0.6 R vir. Additionally, we find excellent agreement between R cross(M ⋆) and the theoretically determined splashback radius for galaxies in this mass range. Overall, our results favor models of galaxy evolution at z < 0.5 that distribute T ≈ 104K gas to distances beyond the virial radius. [ABSTRACT FROM AUTHOR]

The companion to PSR J1622-0315, one of the most compact known redback millisecond pulsars, shows extremely low irradiation despite its short orbital period. We model this system to determine the binary parameters, combining optical observations from the New Technology Telescope in 2017 and the Nordic Optical Telescope in 2022 with the binary modeling code ICARUS . We find a best-fit neutron star mass of 2.3 ± 0.4 M _⊙ , and a companion mass of 0.15 ± 0.02 M _⊙ . We detect for the first time low-level irradiation from asymmetry in the minima as well as a change in the asymmetry of the maxima of its light curves over five years. Using starspot models, we find better fits than those from symmetric direct heating models, with consistent orbital parameters. We discuss an alternative scenario where the changing asymmetry is produced by a variable intrabinary shock. In summary, we find that PSR J1622-0315 combines low irradiation with variable light-curve asymmetry and a relatively high neutron star mass.

Multiwavelength modeling of the synchrotron radiation from relativistic transients such as gamma-ray burst (GRB) afterglows is a powerful means of exploring the physics of relativistic shocks and of deriving properties of the explosion, such as the kinetic energy of the associated relativistic outflows. Capturing the location and evolution of the synchrotron cooling break is critical to break parameter degeneracies associated with such modeling. However, the shape of the spectrum above the cooling break, as well as the location and evolution of the break itself can be significantly altered by synchrotron self-Compton (SSC) cooling. We present an observer’s guide to applying SSC cooling with and without Klein–Nishina (KN) corrections to GRB afterglow modeling. We provide a publicly available Python code to calculate the Compton Y -parameter as a function of electron Lorentz factor, from which we compute changes to the electron distribution, along with KN-corrected afterglow spectra and light curves. In this framework, the canonical synchrotron spectral shapes split into multiple subregimes. We summarize each new spectral shape and describe its observational significance. We discuss how KN corrections can account for harder spectra and shallower decline rates observed in some GRB X-ray afterglows. Our overall aim is to provide an easy application of SSC+KN corrections into analytical multiwavelength modeling frameworks for relativistic transients.

We explore the galaxy-halo connection information that is available in low-redshift samples from the early data release of the Dark Energy Spectroscopic Instrument (DESI). We model the halo occupation distribution (HOD) from z = 0.1 to 0.3 using Survey Validation 3 (SV3; a.k.a., the One-Percent Survey) data of the DESI Bright Galaxy Survey. In addition to more commonly used metrics, we incorporate counts-in-cylinders (CiC) measurements, which drastically tighten HOD constraints. Our analysis is aided by the Python package, galtab , which enables the rapid, precise prediction of CiC for any HOD model available in halotools . This methodology allows our Markov chains to converge with much fewer trial points, and enables even more drastic speedups due to its GPU portability. Our HOD fits constrain characteristic halo masses tightly and provide statistical evidence for assembly bias, especially at lower luminosity thresholds: the HOD of central galaxies in z ∼ 0.15 samples with limiting absolute magnitude M _r < −20.0 and M _r < −20.5 samples is positively correlated with halo concentration with a significance of 99.9% and 99.5%, respectively. Our models also favor positive central assembly bias for the brighter M _r < −21.0 sample at z ∼ 0.25 (94.8% significance), but there is no significant evidence for assembly bias with the same luminosity threshold at z ∼ 0.15. We provide our constraints for each threshold sample’s characteristic halo masses, assembly bias, and other HOD parameters. These constraints are expected to be significantly tightened with future DESI data, which will span an area 100 times larger than that of SV3.

Chapter 5 turns to the first woodblock-printed Japanese Buddhist world map, which was produced in 1709 - the same year as the second of the two maps discussed in Chapter 4 - and created by a prominent monk of the era, Hotan (1659-1738). Moerman does allude, particularly in Chapter 2, to the specific concerns of Nara monks, but does not, in my view, sufficiently address the vast gulf between the very genres of these maps and their sources, respectively, in competing institutions. The earliest Buddhist maps created in Japan were often inscribed with the movement of the well-known traveler-monk Xuanzang (600-664), who was also historically influential both as an importer-cum-translator of vast quantities of sutras and as a progenitor of what came to be called the Faxiang (Jp. [Extracted from the article]

Interpreting and modelling astronomical catalogues requires an understanding of the catalogues' completeness or selection function: what properties determine an object's probability of being including in the catalogue? Here we set out to empirically quantify the completeness of the overall catalogue of Gaia's third data release (DR3). This task is not straightforward because Gaia is the all-sky optical survey with the highest angular resolution to date and no consistent ground truth exists to allow direct comparisons. However, well-characterised deeper imaging enables an empirical assessment of Gaia's G-band completeness across parts of the sky. On this basis, we devised a simple analytical completeness model of Gaia as a function of the observed G magnitude and position over the sky, which accounts for both the effects of crowding and the complex Gaia scanning law. Our model only depends on a single quantity: the median magnitude M10 in a patch of the sky of catalogued sources with astrometric_matched_transits ≤10. We note that M10 reflects elementary completeness decisions in the Gaia pipeline and is computable from the Gaia DR3 catalogue itself and therefore applicable across the whole sky. We calibrated our model using the Dark Energy Camera Plane Survey (DECaPS) and tested its predictions against Hubble Space Telescope observations of globular clusters. We found that our model predicts Gaia's completeness values to a few per cent (RMS) across the sky. We make the model available as a part of the gaiaunlimited Python package built and maintained by the GaiaUnlimited project. [ABSTRACT FROM AUTHOR]

Despite the fact that jets from black holes were first understood to exist over 40 years ago, we are still in ignorance about many primary aspects of these systems – including the radiation mechanism at high energies, the particle makeup of the jets, and how particles are accelerated, possibly to energies as high as 100 TeV and hundreds of kpc from the central engine. We focus in particular on the discovery (and mystery) of strong X-ray emission from radio jets on kpc-scales, enabled by the unequaled high resolution of the Chandra X-ray observatory. We review the main evidence for and against the viable models to explain this X-ray emission over the last 20 years. Finally, we present results of a recent study on the X-ray variability of kpc-scale jets, where we find evidence that between 30-100% of the X-ray jet population is variable at the tens-of-percent level. The short (∼years) variability timescale is incompatible with the IC/CMB model for the X-rays and implies extremely small structures embedded within the kpc-scale jet, and thus requires a reconsideration of many assumptions about jet structure and dynamics. [ABSTRACT FROM AUTHOR]

Studying blazar radio variability on timescales ranging from months to years provides information on the sub-parsec-scale structures of the jets, and the physics of the central active galactic nuclei. In this study, we focus on the radio variability of 1158 blazars observed at 15 GHz through the Owens Valley Radio Observatory Blazar Monitoring Program, where these sources have been observed about twice a week for over a decade. We investigate the dependence of the variability amplitudes and timescales, derived using a simple model fit to the structure function, on the milliarcsecond radio core sizes measured by Very Long Baseline Interferometry. The most compact sources exhibit larger variability amplitudes and shorter variability timescales than the more extended sources; this could be explained by light travel-time effects. [ABSTRACT FROM AUTHOR]

The astronomical cycle characteristics of Mesozoic lacustrine fine-grained sedimentary rocks play a crucial role in understanding the formation environment of such sediments. The fine-grained sedimentary rocks of the Middle Jurassic Lianggaoshan Formation in the Sichuan Basin, China, constitute a significant lacustrine deposit. Previous research has primarily focused on its reservoir characteristics, with limited understanding of the relationship between lithofacies changes and astronomical cycles. To fill this knowledge void, we provide a continuous lacustrine core record of approximately 260 m from the XY-4 well, spanning the Lianggaoshan Formation in the Eastern Sichuan Basin. Initially, we categorized it into eight lithofacies types and established a lithologic ranking sequence based on this classification. Through time-series analysis, we identified the 405 Kyr long eccentricity cyc lecycle, 125 Kyr short eccentricity cycle, obliquity, and precession cycle. We emphasize the significance of the 125 Kyr short eccentricity cycle as the primary controlling factor during the deposition of the Lianggaoshan Formation. Subsequently, based on the 405 Kyr long eccentricity cycle, we established an age model for astronomical tuning, creating an astronomical age scale. The calculated sedimentation interval for the Lianggaoshan Formation ranges from 170.00 Ma to 172.74 Ma, spanning a total duration of 2.74 Ma. Meanwhile, the sedimentation interval for the Lower Liang 2 Submember is determined to be from 171.54 Ma to 172.52 Ma, lasting 0.98 Ma. Further comparison of TOC content and mineral composition with the orbital cycles reveals that TOC content and clay mineral content exhibit in-phase variations with the 125 Kyr short eccentricity. This characteristic contradicts the features of Cenozoic continental basins but aligns consistently with the characteristics of the Middle Triassic in North China. In contrast, silica minerals and carbonate minerals display anti-phase variations with the 125 Kyr short eccentricity. Different lithofacies demonstrate distinct responses to orbital cycles. Lithofacies characterized by higher organic matter content generally develop during the half-period with the maximum eccentricity. In contrast, lithofacies with lower organic matter content tend to occur during the half-cycle associated with the minimum eccentricity. Finally, based on the integrated analysis of lithological characteristics and astronomical cycles, we established two sedimentary modes: "Seasonally Pronounced Type" corresponding to the maximum eccentricity and "Seasonally Obscure Type" corresponding to the minimum eccentricity. • The fine-grained sedimentary rocks of the Lianggaoshan Formation can be classified into eight distinct lithofacies. • The deposition of the Lianggaoshan formation was influenced by astronomical orbital cycles. • Astronomical cycles influenced the variations in mineral composition, organic matter, and lithofacies. • Different eccentricity cycles correspond to different sedimentation patterns. [ABSTRACT FROM AUTHOR]

Project risk is an uncertain situation or event that, if it occurs, may have a negative or positive effect on one or more project objectives, such as scope, schedule, cost, and quality. Major industrial projects are increasingly facing complexity and uncertainty. The scope of this paper is related to petrochemical projects, in which risks directly affect the approved time, cost, and quality of the project. In such projects, there are risks that neither the owner nor the contractor has the main role in the occurrence or prevention of, and it is not easy to determine who is responsible for them. In such projects, there are risks that neither the owner nor the contractor has the main role in the occurrence or prevention of, and for which it is not easy to determine responsibility. Therefore, predicting, identifying, analyzing, and determining of the optimal allocation of risk responsibility between contracting parties is one of the most important steps before the start of the project. Suppose it is not correctly allocated among project stakeholders, then, in that case, risk responsibility imposes costs on the project that must be paid by the owner, contractor, and partnership, causing, in general, many problems for project management. Therefore, this paper presents a model to calculate the optimal ratio of risk allocation between the project parties in the concluding contract stage, using the UTA-STAR technique to obtain the owner and contractor utility function to create as much of a win-win relationship between them as possible. [ABSTRACT FROM AUTHOR]

The article discusses an interview with Dr. Tobias Jogler, the director of a planetarium in Muenster, Germany, about their new live, interactive show called Universum-Live!. The show takes audiences on a tour of the universe, starting from Earth and exploring various celestial objects such as the Crab Nebula and black holes. Dr. Jogler explains that they chose to develop a new show instead of using pre-rendered content to incorporate new scientific discoveries and provide a more personal experience for the audience. The show utilizes volumetric 3D-models, which enhance the audience's experience and make it easier for astronomers to explain certain features. The article also addresses concerns about the computational resources required for volumetric models and the training required for presenters. Dr. Jogler hopes that audiences will gain an understanding of the universe and appreciate the scientific results presented in the show. [Extracted from the article]

The theory of relativistic plasmas is attracting interest as a model of high-energy astronomical objects. The topological constraints, built in the governing equations, play an essential role in characterizing the structures of plasmas. Among various invariants of ideal models, the circulation is one of the most fundamental quantities, being included in other invariants like the helicity. The conventional enstrophy, known to be constant in a two-dimensional flow, can be generalized, by invoking Clebsch variables, to the topological charge of a three-dimensional fluid element, which essentially measures circulations. Since the relativistic effect imparts space-time coupling into the metric, such invariants must be modified. The non-relativistic generalized enstrophy is no longer conserved in a relativistic plasma, implying that the conservation of circulation is violated. In this work, we extend the generalized enstrophy to a Lorentz covariant form. We formulate the Clebsch representation in relativity using the principle of least action and derive a relativistically modified generalized enstrophy that is conserved in the relativistic model. [ABSTRACT FROM AUTHOR]

Precise forecasting of renewable energy production is crucial for ensuring the reliable operation of the electricity grid. Developing more accurate predictive models and computational methodologies can enhance energy production and improve overall system stability. This paper introduces a novel computational approach utilizing quaternions to calculate expected solar irradiance on a given surface. The proposed method incorporates quaternion rotations and translation vectors to model the motion of astronomical objects, both independently and in relation to each other, a factor critical for accurate irradiance estimation. This approach has the potential to replace the commonly used equatorial coordinate system-based computations, offering significant improvements in adaptability, efficiency, and accuracy. The quaternion-based method provides a 9.9% improvement in average angle deviation and a 25.46% improvement in maximum angle deviation from the ground truth of the Sun's angle of incidence, compared to the equatorial coordinate system-based model. This improvement translates to a 6.5905 kWh/m 2 discrepancy in clear sky annual irradiation between the two models, which is highly significant for solar power plants. Additionally, the proposed quaternion-based calculation is adaptable for estimating irradiation on any surface following an orbital trajectory, as well as on other planets. Moreover, the model is easily extendable to include other motions, thanks to the composition property of quaternions. The article presents the calculation methodologies of both models, performs a comparative analysis of the computational results, and presents the differences in computational efficiency between the two approaches. • Correction Factors Not Required : No correction factors needed for each GPS coordinate. • Applicability to Various Orbital Trajectories : Works with any orbital path, unlike equatorial-based method. • Extensibility for Additional Motions : Extends to handle additional motions like obliquity, nutation, and precession. • Reduced Computational Complexity : Fewer trigonometric functions mean faster, more stable calculations. • Improved Accuracy : Provides more accurate solar irradiation estimates than equatorial-based method. [ABSTRACT FROM AUTHOR]

The current paper is concerned with new cosmological models of the existence of a perfect fluid source in f(R) and f(R,T)-gravity. A varying polynomial deceleration parameter is utilized. Previously, such models were obtained without any restrictions on the parameter of the field equation. The dynamical features of the model, including the behavior of the state parameter, are examined. The behavior of the energy, pressure, and jerk parameters for the model are also discussed. Additionally, this is happening with a wide range of other parameters. These suggested cosmological models correspond to astronomical observations to some extent as an expectation of what will happen after the Big Rip. The first model covers a linearly varying deceleration parameter model. Furthermore, it covers the law of Berman. The second model is represented as a Rip–Crunch model. A varying polynomial deceleration parameter produced multiple cosmological models. These models may be utilized in explaining the evolution of the Universe. [ABSTRACT FROM AUTHOR]

It is now widely accepted that astronomical factors trigger the emergence of glacial and interglacial periods. However, nearly two centuries ago, the overall situation was not as apparent as it is today. In this article, I briefly discuss the astronomical model of ice ages put forward in the 19th and early 20th centuries. This period was indeed anni mirabiles for scientists to understand the ice age phenomenon. Agassiz, Adhémar and Croll laid the foundation stones for understanding the dynamics of ice ages. But it was Milankovitch who combined empirical geology with mathematical astronomy. Specifically, he identified the shortcomings of the preceding ice age models and modified his model accordingly. In what follows, I review earlier approaches to the ice age problem and show how they failed to meet their objectives. Next, I show how Milankovitch's model managed to capture all sufficient astronomical elements. The final sections focus on Milutin Milankovitch's successful approach, including his accomplishment of tackling the problem mathematically. [ABSTRACT FROM AUTHOR]

Telescope arrays are receiving increasing attention due to their promise of higher resource utilization, greater sky survey area, and higher frequency of full space-time monitoring than single telescopes. Compared with the ordinary coordinated operation of several telescopes, the new astronomical observation mode has an order of magnitude difference in the number of telescopes. It requires efficient coordinated observation by large-domain telescopes distributed at different sites. Coherent modeling of various abstract environmental constraints is essential for responding to multiple complex science goals. Also, due to competing science priorities and field visibility, how the telescope arrays are scheduled for observations can significantly affect observation efficiency. This paper proposes a multilevel scheduling model oriented toward the problem of telescope-array scheduling for time-domain surveys. A flexible framework is developed with basic functionality encapsulated in software components implemented on hierarchical architectures. An optimization metric is proposed to self-consistently weight contributions from time-varying observation conditions to maintain uniform coverage and efficient time utilization from a global perspective. The performance of the scheduler is evaluated through simulated instances. The experimental results show that our scheduling framework performs correctly and provides acceptable solutions considering the percentage of time allocation efficiency and sky coverage uniformity in a feasible amount of time. Using a generic version of the telescope-array scheduling framework, we also demonstrate its scalability and its potential to be applied to other astronomical applications.

When fitting N -body models to astronomical data – such as transit times, radial velocity, and astrometric positions at observed times – the derivatives of the model outputs with respect to the initial conditions can help with model optimization and posterior sampling. Here, we describe a general purpose symplectic integrator for arbitrary orbital architectures, including those with close encounters, which we have recast to maintain numerical stability and precision for small step sizes. We compute the derivatives of the N -body coordinates and velocities as a function of time with respect to the initial conditions and masses by propagating the Jacobian along with the N -body integration. For the first time, we obtain the derivatives of the transit times with respect to the initial conditions and masses using the chain rule, which is quicker and more accurate than using finite differences or automatic differentiation. We implement this algorithm in an open source package, NbodyGradient.jl , written in the Julia language, which has been used in the optimization and error analysis of transit-timing variations in the TRAPPIST-1 system. We present tests of the accuracy and precision of the code, and show that it compares favourably in speed to other integrators that are written in C. [ABSTRACT FROM AUTHOR]

Machine learning-based techniques are used widely for the classification of images into various categories. The advancement of Convolutional Neural Network (CNN) affects the field of computer vision on a large scale. It has been applied to classify and localize objects in images. Among the fields of applications of CNN, it has been applied to understand huge unstructured astronomical data being collected every second. Galaxies have diverse and complex shapes and their morphology carries fundamental information about the whole universe. Studying these galaxies has been a tremendous task for the researchers around the world. Researchers have already applied some basic CNN models to predict the morphological classes of the galaxies. In this paper, a residual network (ResNet) model is applied for this purpose. The proposed methodology classified the galaxies depending on their shape into 37 different classes. The performance of the methodology was evaluated using the data set provided by Kaggle. In this data set, 61,578 galaxy images are given, which are classified by human eye. The model achieved nearly 98% accuracy. [ABSTRACT FROM AUTHOR]

In the publication Troshichev et al. (2006) (https://doi.org/10.1029/2005JA011402) on the polar cap (PC) indices, PCN and PCS, an error was made by using components of the interplanetary magnetic field (IMF) in their geocentric solar ecliptic (GSE) representation instead of the prescribed geocentric solar magnetospheric (GSM) representation for calculations of index scaling parameters. The mistake has caused a trail of incorrect relations and wrong conclusions extending since 2006 up to now (2020) which should be discontinued, for instance, by issuing a corrigendum note from the authors. The present contribution explains the error and discusses in an extended example its consequences for one of the publications that have referred to the invalid scaling parameter set. Further investigations reported here of the PC index versions recommended by the International Association for Geomagnetism and Aeronomy (IAGA) indicate occurrences of similar problems in the present derivation of index scaling parameters. Plain Language Summary: The publication Troshichev et al. (2006) (https://doi.org/10.1029/2005JA011402) on the polar cap (PC) indices, PCN and PCS, has by mistake used components of the interplanetary magnetic field (IMF) in their geocentric solar ecliptic (GSE) representation instead of the prescribed geocentric solar magnetospheric (GSM) representation for calculations of index scaling parameters. The mistake has caused a trail of incorrect relations and wrong conclusions extending since 2006 up to now (2020) which should be discontinued. The examinations have been extended to the PCN version recently endorsed by the International Association for Geomagnetism and Aeronomy (IAGA). The analyses indicate that the scaling parameters for this PC index version are also questionable. Key Points: The use of invalid scaling parameters for Polar Cap (PC) index calculations is disclosedRelated adverse consequences for derived publications on PC indices are analyzedA summary of publications devaluated by their use of inconsistent PC index versions is provided [ABSTRACT FROM AUTHOR]

As social scientists become increasingly aware of the limits of dominant models of subjectivity to address contemporary social, cultural, and environmental problems, Felix Guattari's emphasis on the machinic and processual dimensions of subjective production offers crucial insights. This paper explores the potential of Guattari's evocation of the "cosmos" for the reconceptualisation of subjectivity. Among the various concepts of exteriority that Guattari employs throughout his work, the notion of the cosmos evokes the ungrounding effects of encounters with radically unfamiliar ontological universes. The paper invents the notion of cosmic subjectivity as a way of theorising a mode of subjective production that draws from a maximum of ontological universes. Open to the diverse existential rhythms and durations of the universe, cosmic subjectivity abandons the myth of an a priori subject and rejects the universal sense of time that provides its ground. To speak of cosmic subjectivity is to entertain the possibility of subjective processes that are not subjugated to the dominant order, but become compatible with immanent processes of mutation. To give flesh to these claims, the paper briefly explores three science fiction films released in recent years, which gesture, in significantly different ways, beyond the human: War for the Planet of the Apes, Blade Runner 2059 and Arrival. Our use of the films is not meant to provide an outline of a new model of subjectivity, but to give a sense of the complexities of keeping subjective production open to the indeterminate forces of other ontological universes. [ABSTRACT FROM AUTHOR]

Calibration precision is currently a limiting systematic in 21 cm cosmology experiments. While there are innumerable calibration approaches, most can be categorized as either 'sky-based,' relying on an extremely accurate model of astronomical foreground emission, or 'redundant,' requiring a precisely regular array with near-identical antenna response patterns. Both of these classes of calibration are inflexible to the realities of interferometric measurement. In practice, errors in the foreground model, antenna position offsets, and beam response inhomogeneities degrade calibration performance and contaminate the cosmological signal. Here, we show that sky-based and redundant calibration can be unified into a highly general and physically motivated calibration framework based on a Bayesian statistical formalism. Our new framework includes sky-based and redundant calibration as special cases but can additionally support relaxing the rigid assumptions implicit in those approaches. We present simulation results demonstrating that, in a simple case, working in an intermediate regime between sky-based and redundant calibration improves calibration performance. Our framework is highly general and encompasses novel calibration approaches including techniques for calibrating compact non-redundant arrays, calibrating to incomplete sky models, and constraining calibration solutions across frequency. [ABSTRACT FROM AUTHOR]

Machine learning has achieved an important role in the automatic classification of variable stars, and several classifiers have been proposed over the last decade. These classifiers have achieved impressive performance in several astronomical catalogues. However, some scientific articles have also shown that the training data therein contain multiple sources of bias. Hence, the performance of those classifiers on objects not belonging to the training data is uncertain, potentially resulting in the selection of incorrect models. Besides, it gives rise to the deployment of misleading classifiers. An example of the latter is the creation of open-source labelled catalogues with biased predictions. In this paper, we develop a method based on an informative marginal likelihood to evaluate variable star classifiers. We collect deterministic rules that are based on physical descriptors of RR Lyrae stars, and then, to mitigate the biases, we introduce those rules into the marginal likelihood estimation. We perform experiments with a set of Bayesian logistic regressions, which are trained to classify RR Lyraes, and we found that our method outperforms traditional non-informative cross-validation strategies, even when penalized models are assessed. Our methodology provides a more rigorous alternative to assess machine learning models using astronomical knowledge. From this approach, applications to other classes of variable stars and algorithmic improvements can be developed. [ABSTRACT FROM AUTHOR]

This paper describes and explains the synthesis of an astronomical clock mechanism which displays the mean position of the Sun, the Moon, the lunar node and zodiac circle as well as the Moon phases and their motion during the year as seen from the Earth. The clock face represents the stereographic projection of the celestial equator, celestial tropics, zodiac circle (ecliptic) and horizon for the latitude of Belgrade from the north celestial pole to the equator plane. The observed motions of celestial objects are realized by a set of clock gear trains with properly calculated gear ratios. The method of continued fraction is applied in the computation of proper and practically applicable gear ratios of the clock gear trains. The fully operational 3D model of the astronomical clock is created and the motion study of its operation is accomplished by using the SolidWorks 2016 application. The simulation results are compared with the ephemeris data and the detected differences are used to evaluate the long-term accuracy of the astronomical clock operation. The presented methods of the clock mechanism synthesis can be useful for the design, maintenance and conservation of large-scale city astronomical clocks since these clocks represent a precious historical and cultural heritage of European civilization. [ABSTRACT FROM AUTHOR]

The question of whether cosmic microwave background (CMB) temperature and polarization data from Planck favor a spatially closed universe with curvature parameter ΩK < 0 has been the subject of recent intense discussions. Attempts to break the geometrical degeneracy combining Planck data with external data sets such as baryon acoustic oscillation (BAO) measurements all point toward a spatially flat universe at the cost of significant tensions with Planck, which makes the resulting data set combination problematic. Settling this issue requires identifying a data set that can break the geometrical degeneracy while avoiding these tensions. We argue that cosmic chronometers (CCs), measurements of the expansion rate H(z) from the relative ages of massive early-type passively evolving galaxies, are the data set we are after. Furthermore, CCs come with the additional advantage of being virtually free of cosmological model assumptions. Combining Planck 2018 CMB temperature and polarization data with the latest CCs, we break the geometrical degeneracy and find ΩK = −0.0054 ± 0.0055, consistent with a spatially flat universe and competitive with the Planck+BAO constraint. Our results are stable against minimal parameter space extensions and CC systematics, and we find no substantial tension between Planck and CC data within a nonflat universe, making the resulting combination reliable. Our results allow us to assert with confidence that the universe is spatially flat to the level, a finding that might possibly settle the ongoing spatial curvature debate and lends even more support to the already very successful inflationary paradigm. [ABSTRACT FROM AUTHOR]

This paper evaluates Kepler's 1618–1621 Epitome of Copernican Astronomy in light of two contextual events: the 1616 Decree of the Index banning Copernican books (including Volume 1 of Kepler's Epitome in 1619) and the start of the Thirty Years' War in 1618. Kepler's Epitome seems to defy traditional genre expectations: it takes the form of a textbook, and yet (especially in later volumes) it is more complicated than a traditional university primer, and seems targeted toward more expert readers. I argue that Kepler deliberately reframed the Epitome and modified its focus and approach in the years between the publication of its first volume in 1618 and its later volumes in 1620 and 1621. These changes were related to Kepler's attempt to circumvent the ban on the first volume and help the book reach readers in Italy. To Kepler, a lifelong advocate for the Copernican cause, it was imperative that his book reach as many readers as possible. The spread of his work would both help educate potential future Copernicans and aid in overturning the ban on Copernican publication itself. Further, Kepler believed that princely readers might use the book's arguments as a model for peace in a time of war. [ABSTRACT FROM AUTHOR]

The study of artificial light at night (ALAN) by satellite is very important for the analysis of new astronomical sites and for the long-term temporal evolution observation of the emission from the ground. The analysis of satellite data presents many advantages but also some critical points because of fluctuations in measurements. The main result of this paper is the discovery of a correlation between these fluctuations and the aerosol concentration combined with cloud cover and lunar cycles. In this work, we also present a mathematical empirical model for the light pollution propagation study in relation to the aerosol concentration detected by satellite. We apply this model to the astronomical site of Asiago (Ekar Observatory) providing a possible explanation for the temporal ALAN fluctuations detected by satellite. Finally, we validate the results with the ground collected data. [ABSTRACT FROM AUTHOR]

Context. Characterising the large-scale structure in the Universe from present times to the high redshift epoch of reionisation is essential to constraining the cosmology, the history of star formation, and reionisation, to measuring the gas content of the Universe, and to obtaining a better understanding of the physical processes that drive galaxy formation and evolution. Using the integrated emission from unresolved galaxies or gas clouds, line intensity mapping (LIM) provides a new observational window to measure the larger properties of structures. This very promising technique motivates the community to plan for LIM experiments. Aims. We describe the development of a large field-of-view instrument, named CONCERTO (for CarbON CII line in post-rEionisation and ReionisaTiOn epoch), operating in the range 130–310 GHz from the APEX 12-m telescope (5100 m above sea level). CONCERTO is a low-resolution spectrometer based on the lumped element kinetic inductance detectors (LEKID) technology. Spectra are obtained using a fast Fourier transform spectrometer (FTS), coupled to a dilution cryostat with a base temperature of 0.1 K. Two two kilo-pixel arrays of LEKID are mounted inside the cryostat that also contains the cold optics and the front-end electronics. Methods. We present, in detail, the technological choices leading to the instrumental concept, together with the design and fabrication of the instrument and preliminary laboratory tests on the detectors. We also give our best estimates for CONCERTO sensitivity and give predictions for two of the main scientific goals of CONCERTO, that is, a [CII]-intensity mapping survey and observations of galaxy clusters. Results. We provide a detailed description of the instrument design. Based on realistic comparisons with existing instruments developed by our group (NIKA, NIKA2, and KISS), and on the laboratory characterisation of our detectors, we provide an estimate for CONCERTO sensitivity on the sky. Finally, we describe, in detail, two of the main scientific goals offered by CONCERTO at APEX. [ABSTRACT FROM AUTHOR]

This study presents subdaily resolved chemical records through fossil mollusk shell calcite. Trace element profiles resolve periodic variability across ~40‐μm‐thin daily growth laminae in a Campanian Torreites sanchezi rudist bivalve. These high‐resolution records are combined with seasonally resolved stable isotope and trace element records that allow shell‐chemical variability to be discussed on both seasonal and daily scale. A combination of layer counting, spectral analysis of chemical cyclicity and chemical layer counting shows that the rudist precipitated 372 daily laminae per year, demonstrating that length of day has increased since the Late Cretaceous, as predicted by astronomical models. This new approach to determine the length of a solar day in geologic history through multiproxy chemical records at subdaily resolution yields considerably more control on the uncertainty of this estimate. Daily chemical variability exceeds seasonal variability in our records, and cannot be explained by diurnal temperature changes. Instead, we postulate that rudist shell chemistry is driven on a daily scale by changes in light intensity. These results together with those of stable isotope analyses provide strong evidence that Torreites rudists had photosymbionts. Bivalve shell calcite generally preserves well. Therefore, this study paves the way for daily‐scale reconstructions of paleoenvironment and sunlight intensity on geologic time scales from bivalve shells, potentially allowing researchers to bridge the gap between climate and weather reconstructions. Such reconstructions improve shell chronologies, document environmental change in warm ecosystems, and widen our understanding of the magnitude of short‐term changes during greenhouse climates. Key Points: High‐resolution LA‐ICP‐MS profiles reveal strong diurnal cyclicity in rudist shellDominance of day‐night cycle suggests photosymbiosis in the rudist species Torreites sancheziLength of annual and daily cycle is used to constrain Campanian Earth‐Moon distance [ABSTRACT FROM AUTHOR]

A millenary description of the world as conceived by Chinese culture, appears in the Zhou bi Suanjing or "The book of the Gnomon and the Circular Paths of the Heaven", according Needham. Situated at Zhou (a legendary city) the dimensions of the earth and heaven, including the size of the Sun are presented in this book. The Chinese Gaì Ti'an astronomical model of a flat earth and a flat heaven, is measured with the aid of a gnomon (biao) and the application of the Pythagorean Theorem. Now, after making an adjustment to the scale of the data, the elements to locate the legendary Zhou City have been found making feasible the correspondence between the dimensions of the Zhoubi's given world and those of the actual Earth. Here I show that Zhou, centre of the world from which the measures are done, corresponds to the city Jining located in the province of Shandong, China; also, I confirm that the distance between Jining and the Pole of Zhoubi is 4,285 km as could be found with a geographical tool such as the Google-Earth program. With these results I am confident to say that: The city of Zhou appearing in the Zhoubi exists; and, that the Zhoubi was an accurate description of the Earth at the time of Zhou Dynasty (1045 - 256 BC). Moreover, the location of cities as important as Beijing (at 498 km to the north of Jining) would be related with projection of the heaven on Earth: it is about one diameter of Sun from Jining. Also, it important to know that this city is recognized as the birth place of the great philosopher Confucius, giving to my findings a relevance that goes beyond the field of Astronomy or Mathematics, in which frame the Zhoubi has been analysed through the years. These findings put new perspectives for the search in other non-mathematical or non-astronomical documents elements for these disciplines. [ABSTRACT FROM AUTHOR]

A typhoon struck the Pearl River Estuary in September 1874 ("Typhoon 1874"), causing extensive damage and claiming thousands of lives in the region during its passage. Like many other historical typhoons, the deadliest impact of the typhoon was its associated storm surge. In this paper, a possible track of the typhoon was reconstructed through an analysis of the historical qualitative and quantitative weather observations in the Philippines, the northern part of the South China Sea, Hong Kong, Macao, and Guangdong recorded in various historical documents. The magnitudes of the associated storm surges and storm tides in Hong Kong and Macao were also quantitatively estimated using storm surge model and analogue astronomical tides based on the reconstructed track. The results indicated that the typhoon could have crossed the Luzon Strait from the western North Pacific and moved across the northeastern part of the South China Sea to strike the Pearl River Estuary more or less as a super typhoon in the early morning on 23 September 1874. The typhoon passed about 60 km south–southwest of Hong Kong and made landfall in Macao, bringing maximum storm tides of around 4.9 m above the Hong Kong Chart Datum (http://www.geodetic.gov.hk/smo/gsi/Data/pdf/explanatorynotes.pdf , last access: 3 January 2020) at the Victoria Harbour in Hong Kong and around 5.4 m above the Macao Chart Datum (https://mosref.dscc.gov.mo/Help/ref/Macaucoord%5f2009%5fweb%5fEN%5fv201702.pdf , last access: 3 January 2020) at Porto Interior (inner harbour) in Macao. Both the maximum storm tide (4.88 m above the Hong Kong Chart Datum) and maximum storm surge (2.83 m) brought by Typhoon 1874 at the Victoria Harbour estimated in this study are higher than all the existing records since the establishment of the Hong Kong Observatory in 1883, including the recent records set by super typhoon Mangkhut on 16 September 2018. [ABSTRACT FROM AUTHOR]

This study documents the detailed palynology of the Bridge Creek Member, Greenhorn Limestone Formation, at the Rock Canyon anticline outcrop, west of Pueblo, Colorado, USA. The section is the formally ratified Global Boundary Stratotype Section and Point (GSSP) for the base of Turonian Stage and corresponding Lower Turonian Substage, and the only proposed GSSP for the base of the Middle Turonian Substage. The authors' previously published palynological data from the underlying Cenomanian strata in the nearby US Geological Survey (USGS) Portland-1 core, and from cores and an outcrop of Cenomanian, Turonian and earliest Coniacian age in SW Texas, are reviewed for biostratigraphy. Dinoflagellate cyst ranges and events in both areas are calibrated against other published bio- and chemostratigraphical (carbon isotope) data and an astronomical age model. A regional dinoflagellate cyst zonation is proposed, adapted from a Central and Northern European scheme, comprising three zones and four subzones. Comparison with vintage published palynological data from other states, including Arizona, Kansas, Utah, Wyoming and Montana, indicates that the zonation is probably applicable to marine sections throughout the Cretaceous Western Interior Seaway of the USA. The new palynological data from around the Lower–Middle Turonian boundary at Pueblo support its proposal as a GSSP. [ABSTRACT FROM AUTHOR]