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The Horometer instrument in Peter Apian's 1533 Instrument Buch is described and analyzed. This paper is illustrated by several examples of how to manipulate and set up the instrument using the Sun, the Moon and stars to determine time. The paper also contains an Appendix on the mathematics behind its construction. [ABSTRACT FROM AUTHOR]

A Silesian astronomer, Maria Cunitia (1610?-1664) became known as the author of Urania propitia (1650), i.e. astronomical tables based on Johannes Kepler's Rudolphine Tables (1627), which she adapted to facilitate their use. However, little has been said about Cunitia's observations of the sky with the use of advanced astronomical instruments. In this paper, we intend to use all extant printed and manuscript sources to draw a picture of Cunitia as an active astronomer engaged in astronomical observations. Considering the fact that in the years 1648-1654 Cunitia and her husband, Elias von Löwen (Crätschmair, 1602?-1661), exchanged a number of letters with Johannes Hevelius (1611-1687), we will argue that Cunitia could have been an inspiration of sorts to Hevelius who sought the assistance of his second wife, Elizabeth (née Koopman, 1647-1693) married in 1663, in his own astronomical endeavours. [ABSTRACT FROM AUTHOR]

We have determined the most probable date for the catalog of 34 stars that was used in the construction of a Latin astrolabe originally owned by the Dominican preacher friars and presently in the Musée des Arts Précieux Paul-Dupuy in Toulouse, France. To this end we digitized a photograph of the rete and the rule of the astrolabe, computed the equatorial coordinates of the ends of the 34 star pointers of the rete, and produced a list of 113 reference stars taken from several lists of stars on astrolabes. We then compared the coordinates of the ends of the pointers and those of the reference stars for dates between 1400 and 1700. The most probable date for this astrolabe is 1550. [ABSTRACT FROM AUTHOR]

In 1524, Petrus Apianus published two closely related works—one the Latin Cosmographicus liber, aimed at an educated audience of international readers, and the other, Ein kunstlich Instrument, a shorter, more practical book for those who could read German but had no Latin. Both books nevertheless make use of most of the same instruments, including Apianus' early volvelles. Most of these instruments also reappear in subsequent editions of Cosmographicus liber (or Cosmographia, a frequent alternative title). While the Cosmographicus liber has received much scholarly attention, Ein kunstlich Instrument has received very little. In this paper we (1) set the instruments of Ein kunstlich Instrument in the context of Apianus' earlier work, especially his lost Mappa mundi and the extant booklets (Declaratio and Isagoge) that explained it, (2) compare the German- and Latin-language books of 1524, (3) explain in detail those instruments that have not heretofore been adequately discussed, and (4) explore their later history. We also make available, in the on-line edition of the Journal, working virtual copies of Apianus' instruments from Ein kunstlich Instrument. [ABSTRACT FROM AUTHOR]

Copyright of Scientific Journal of the Military University of Land Forces is the property of Gen. Tadeusz Kosciuszko Military Academy of Land Forces and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Astrophotonics is a burgeoning field that lies at the interface of photonics and modern astronomical instrumentation. Here we provide a pedagogical review of basic photonic functions that enable modern instruments, and give an overview of recent and future applications. Traditionally, optical fibres have been used in innovative ways to vastly increase the multiplex advantage of an astronomical instrument, e.g. the ability to observe hundreds or thousands of stars simultaneously. But modern instruments are using many new photonic functions, some emerging from the telecom industry, and others specific to the demands of adaptive optics systems on modern telescopes. As telescopes continue to increase in size, we look to a future where instruments exploit the properties of individual photons. In particular, we envisage telescopes and interferometers that build on international developments in quantum networks, the so-called quantum internet. With the aid of entangled photons and quantum logic gates, the new infrastructures seek to preserve the photonic state and timing of individual photons over a coherent network. [ABSTRACT FROM AUTHOR]

Scientific-grade cameras are frequently employed in industries such as spectral imaging technology, aircraft, medical detection, and astronomy, and are characterized by high precision, high quality, fast speed, and high sensitivity. Especially in the field of astronomy, obtaining information about faint light often requires long exposure with high-resolution cameras, which means that any external factors can cause the camera to become unstable and result in increased errors in the detection results. This paper aims to investigate the effect of displacement introduced by various vibration factors on the imaging of an astronomical camera during long exposure. The sources of vibration are divided into external vibration and internal vibration. External vibration mainly includes environmental vibration and resonance effects, while internal vibration mainly refers to the vibration caused by the force generated by the refrigeration module inside the camera during the working process of the camera. The cooling module is divided into water-cooled and air-cooled modes. Through the displacement and vibration experiments conducted on the camera, it is proven that the air-cooled mode will cause the camera to produce greater displacement changes relative to the water-cooled mode, leading to blurring of the imaging results and lowering the accuracy of astronomical detection. This paper compares the effects of displacement produced by two methods, fan cooling and water-circulation cooling, and proposes improvements to minimize the displacement variations in the camera and improve the imaging quality. This study provides a reference basis for the design of astronomical detection instruments and for determining the vibration source of cameras, which helps to promote the further development of astronomical detection. [ABSTRACT FROM AUTHOR]

The point-spread function (PSF) is a fundamental property of any astronomical instrument. In interferometers, differing array configurations combined with their uv coverage, and various weighting schemes can produce an irregular but deterministic PSF. As a result, the PSF is often deconvolved using CLEAN-style algorithms to improve image fidelity. In this paper, we revisit a significant effect that causes the flux densities measured with any interferometer to be systematically offset from the true values. Using a suite of carefully controlled simulations, we show that the systematic offset originates from a mismatch in the units of the image produced by these CLEAN-style algorithms. We illustrate that this systematic error can be significant, ranging from a few to tens of per cent. Accounting for this effect is important for current and future interferometric arrays, such as MeerKAT, LOFAR, and the SKA, whose core-dominated configuration naturally causes an irregular PSF. We show that this offset is independent of other systematics, and can worsen due to some factors such as the goodness of the fit to the PSF, the deconvolution depth, and the signal-to-noise ratio of the source. Finally, we present several methods that can reduce this effect to just a few per cent. [ABSTRACT FROM AUTHOR]

The article discusses a workshop titled "Tracking Astronomical Instruments Through Ottoman World and Beyond" that took place at Istanbul University. The workshop, organized by the Department of History of Science, aimed to explore the history of astronomy through hands-on activities with portable astronomical instruments. Led by distinguished scholars, the workshop included sessions on the history of astronomical instruments, the abjad number system, astrolabes, and paper instruments. Participants engaged actively and the workshop received support from various organizations. The article concludes that the workshop was a valuable and enriching experience that blended theoretical knowledge with practical engagement, contributing to participants' understanding of astronomical history and setting a precedent for future interdisciplinary workshops. [Extracted from the article]

Nongsugak, an observatory built by Hong Daeyong in the yard of his residence, provides a rare example in the history of astronomy in pre-modern Korea of a Confucian scholar engaging in a systematic program of astronomical observation outside the government bureaucracy. This paper examines Hong’s program of astronomy and its place in his broader pursuit of literati learning. Particular emphasis is placed on the ways in which Hong intertwined two kinds of endeavor: first, the material practice of building instruments and the observatory, and second, the socio-literary practice of exchanging letters, poems, and essays about his observatory with his fellow literati. This illustrates how he culturally legitimized a new concept of a literati mathematician, an emerging figure in mid-eighteenth-century Korea. It also shows how Hong’s scholarly program and the role of astronomy within it evolved in the 1760s and 70s to increasingly emphasize the importance of calculation and observation as essential means of reforming the metaphysically oriented Confucian scholarship of the time. [ABSTRACT FROM AUTHOR]

Gwansanggam Jejo (觀象監提調) were in charge of Gwansanggam (The office for Observation of Natural Phenomenon) along with Yeongsa (領事). King Jeongjo appointed Gwansanggam Jejo in the hodae (互對) manner during the first half of his rule, but in the second half, he appointed them in the sanghwan (相換) method of changing the positions of ministers or in the teukji (特旨) method of appointment, specifically considering their expertise. At this time, Jejo were appointed when more than half were senior rank two (正二品) officials, and more than 90% were from Hanseong (漢城) and its suburbs, and were from the former Yeongsa and Jejo families. In the field of astronomy, Gwansanggam Jejo led the publication of various calendars, such as Cheonseryeok (千歲歷) and Imja year (壬子年, 1792) Supplementary Calendar, which also increased the supply of calendars. Gwansanggam Jejo Seo Ho-su (徐浩修) selected Kim Yeong (金泳), and instructed him to build astronomical instruments to calculate the accurate time, to write related books, and publish Gukjoyeoksanggo (國朝曆象考). In the fields of Geumlu (禁漏) and Myeonggwahak (命課學), talented Gwansanggam Jejo also participated in systematizing the two organizations. In particular, they placed Myeonggwahak on the level of an astronomical organization. In addition, some Gwansanggam Jejo displayed excellent ability in Gwansanggam’s regulatory enactment and financial management. [ABSTRACT FROM AUTHOR]

Ancient Chinese astronomical instruments, exemplifying classical Chinese traditional artefact design, represent a perfect amalgamation of ancient China's advanced scientific and technological prowess with the aesthetic philosophy underlying traditional Chinese artefact creation. Their scientific and artistic values are considerable and should not be underestimated. This research introduces these instruments' concepts, design characteristics, and innovative application cases, mainly focusing on the armillary sphere from an artistic design perspective. This research employs a mixed-methods approach, including surveys, literature reviews, and systematic analysis; the research examines the instruments' design features and cultural significance. The objective of the study is to highlight the armillary sphere's potential as a source of inspiration across various modern design domains, such as sculpture and installation, fashion accessory design and stage performance. The study concludes that reinterpreting these ancient astronomical instruments in modern design not only preserves cultural heritage but also encourages cross-border innovation. This fusion approach offers new perspectives for designers, blending traditional Chinese culture with contemporary design practice. Future research is suggested to explore the integration and wider application of ancient Chinese astronomical instruments in modern design. [ABSTRACT FROM AUTHOR]

Geometric optical distortion is a significant contributor to the astrometric error budget in large telescopes using adaptive optics. To increase astrometric precision, optical distortion calibration is necessary. We investigate using smartphone Organic Light-Emitting Diode (OLED) screens as astrometric calibrators. Smartphones are low-cost, have stable illumination, and can be quickly reconfigured to probe different spatial frequencies of an optical system's geometric distortion. In this work, we characterize the astrometric accuracy of a Samsung S20 smartphone, with a view towards providing large format, flexible astrometric calibrators for the next generation of astronomical instruments. We find the placement error of the pixels to be 189 nm ± 15 nm Root Mean Square (RMS). At this level of error, milliarcsecond astrometric accuracy can be obtained on modern astronomical instruments. [ABSTRACT FROM AUTHOR]

Characterizing the properties (e.g., effective dielectric constant εeff, attenuation constant α, and characteristic impedance Z0) of terahertz (THz) superconducting transmission lines is of particular interest in designing on-chip integrated THz bandpass filters, which are a critical component for THz astronomical instruments, such as multi-color camera and broadband imaging spectrometers. Here, we propose a novel method for the characterization of three parameters (εeff, α, and Z0) of THz superconducting transmission lines. This method measures the ratio of the THz signal powers through two different-length branches of the superconducting transmission line to be measured. In addition, only one measurement is required for an all-in-one device chip, including an antenna, a half-power divider, the superconducting transmission line to be measured, and two detectors. The key point is that the superconducting transmission line to be measured is impedance-mismatched with the two integrated detectors. The method is validated through simulation and measurement for superconducting coplanar waveguide transmission lines around 400 GHz. [ABSTRACT FROM AUTHOR]

MOONS is a multi‐object spectrograph that will be installed at the Nasmyth focus of the VLT ESO Telescopes in Chile. The instrument has the capacity to deploy approximately 1000 fibers over a field of view of 500 square arcminutes, with a total wavelength coverage of from 0.6 to 1.8 μ$$ \mu $$m, offering both low‐ and medium‐resolution modes. The high demand for fast and large optics in all spectral channels prompted the use of similar f/0.95$$ f/0.95 $$ Schmidt cameras. As a result, the Detector Unit (DU) must be located within the optical beam and its footprint must be minimized to reduce vignetting. The instrument consists of four H4RG‐15um pixel detectors and two fully depleted LBNL CCDs. This article provides a comprehensive description of the detector systems, focusing particularly on the H4RG‐15, including a brief overview of the newly developed cryogenic pre‐amplifier for 64‐output operation, and a detailed discussion of the woven cable technology used for signal routing. Some results of the characterization of three H4RG detectors are presented, with a focus on crosstalk and buffer output performance. The use of the buffer output for the H4RG results in a glow‐per‐read observed at the bottom of the detectors. This article also describes the trade‐offs and alternatives used to optimize detector performance in this situation. [ABSTRACT FROM AUTHOR]

The paper describes an improved spectrograph of the Cassegrain focus of the 2-meter ShAO reflector using a CCD camera. The classic Universal Astro Grid Spectrograph (UAGS) was adapted to use the Andor CCD camera to obtain spectra of objects with low brightness in the range of 3600–8000 Å. A spectrograph with a diffraction grating of 651 lines/mm makes it possible to obtain the spectra of stars on the 2‑m ShAO telescope up to 18 mag with the resolution R = 1200, with a signal-to-noise ratio of about 50 for half an hour of exposure. The maximum allowable resolution is R = 3400 with binning 1 × 1. The complex can be used for observations of various types of transient objects, variable stars, and extragalactic objects. [ABSTRACT FROM AUTHOR]

The first photographs taken at the Cape of Good Hope (and therefore South Africa) date from 1843 and were due to Charles Piazzi Smyth, Chief Assistant at the Royal Observatory, Cape. His surviving positives and negatives are gathered here with descriptions of their subjects. They are mainly of the Royal Observatory, Cape of Good Hope, of a Magnetic Observatory on the same site that no longer exists, and of various buildings in Cape Town. However, they also include the first photographic portraits made at the Cape and images of two astronomical instruments. [ABSTRACT FROM AUTHOR]

This paper presents a new instrument setup at the Bucharest Observatory of the Astronomical Institute of the Romanian Academy, as well as preliminary results using this setup. It consists of records of VLF (very low frequency) perturbations using a superSID instrument. During March and December 2022 various mounts and settings tests have been performed. Starting October we obtained satisfactory data. We report on detecting the signature of moderate to intense solar flares (M and X-class). In this configuration, the C-class solar flares are less distinguishable from the background noise. [ABSTRACT FROM AUTHOR]

In this article we describe the developement of an insulated box with a thermostat controller to protect the sensitive Baader Solar Spectrum H alpha filter in the low temperatures of winter. Our goal is to facilitate daily solar synoptic observations in all seasons. [ABSTRACT FROM AUTHOR]

The article informs about repair in astronomical instrumentation, focusing on the challenges faced in building telescope instrumentation and the definition of damage in this field. Topics include the identification of damage in astronomical instruments, the definition of repair, and the methods supporting diagnosis and repair processes in telescope instrumentation.

We present an estimation and analysis of Near Infrared (NIR) background for the astronomical site at Mount Abu. Mount Abu Observatory is situated at Gurushikhar, Rajasthan, India, operated by the Physical Research Laboratory. Data obtained from the NIR observations of various sources using the Near Infrared Camera/Spectrograph (NICS) on the 1.2-m telescope are used to derive the NIR background estimates. We notice seasonal variations in these values, with the summer months showing brighter background compared to the winter. We also present a comparison of synthetic atmospheric transmission at Mount Abu with other Indian observatories at various altitudes. We identify the plausible contributors to the NIR background in our observations and discuss the potential ones that can contribute to the noticed seasonal variations. Overall, we found that the NIR background does not show any systematic variation over the period of observations from 2010 to 2019. The results reported here are specific to the NICS instrument on the 1.2-m telescope. [ABSTRACT FROM AUTHOR]

This paper explores the use of new scientific techniques to examine collections of historic scientific apparatus and other technological artefacts. One project under discussion uses interferometry to examine the history of lens development, while another uses X-ray fluorescence to discover the kinds of materials used to make early mathematical and astronomical instruments. These methods lead to surprising findings: instruments turn out to be fake, and lens makers turn out to have been adept at solving the riddle of aperture. Although exciting, in some ways this is neither novel nor particularly unusual. After all, lab techniques have been used in art and archaeological collections for a very long time. In fact, scientific instruments themselves have been examined in this way since at least the 1950s. What, then, is special about the use of new instruments to examine old instruments? We argue that the answer has less to do with measuring historical innovation or establishing priority, and more to do with networks of craft know-how that, typically, have left no other historical traces than those embodied in surviving instruments themselves. We show, in particular, how collections of objects can be mobilised within wider histories of knowledge, placing instruments within a dynamic interplay of craft knowledge, expertise, labour, commerce, and material exchange, over the longue durée. Finally, we suggest that these kinds of lab analyses can be given an extra dimension through the use of computational modelling, and we introduce the "Tools of Knowledge" project, which is designed to bring together XRF with techniques from the digital humanities, in order to tell a new story about the development of scientific instruments from the 16th to the 20th century. [ABSTRACT FROM AUTHOR]

Gravitational lensing is a topic of great application value in the field of astronomy. The properties and research methods of gravitational lensing are closely related to the geometric and relativistic characteristics of the background universe. This review focuses on the theoretical research and application of strong lenses and weak lenses. We first introduce the basic principles of gravitational lensing, focusing on the geometric basis of geometric lensing, the representation of deflection angles, and the curvature relationship in different geometric spaces. In addition, we summarize the wide range of applications of gravitational lensing, including the application of strong gravitational lensing in Schwarzschild black holes, time delay, the cosmic shearing based on weak lensing, the applications in signal extraction, dark matter, and dark energy. In astronomy, through the use of advanced astronomical instruments and computers, analyzing gravitational lensing effects to understand the structure of galaxies in the universe is an important topic at present. It is foreseeable that gravitational lensing will continue to play an important role in the study of cosmology and will enrich our understanding of the universe. [ABSTRACT FROM AUTHOR]

The eighth-century Latin manuscript Milan, Veneranda Biblioteca Ambrosiana, L 99 Sup. contains fifteen palimpsest leaves previously used for three Greek scientific texts: a text of unknown authorship on mathematical mechanics and catoptrics, known as the Fragmentum Mathematicum Bobiense (three leaves), Ptolemy's Analemma (six leaves), and an astronomical text that has hitherto remained unidentified and almost entirely unread (six leaves). We report here on the current state of our research on this last text, based on multispectral images. The text, incompletely preserved, is a treatise on the construction and uses of a nine-ringed armillary instrument, identifiable as the "meteoroscope" invented by Ptolemy and known to us from passages in Ptolemy's Geography and in writings of Pappus and Proclus. We further argue that the author of our text was Ptolemy himself. [ABSTRACT FROM AUTHOR]

In this article, we report the discovery of a new type of astronomical almanac by Joseph Ibn Waqār (Córdoba, fourteenth century) that begins at second station for each of the planets and may have been intended to serve as a template for planetary positions beginning at any dated second station. For background, we discuss the Ptolemaic tradition of treating stations and retrograde motions as well as two tables in Arabic zijes for the anomalistic cycles of the planets in which the planets stay at first and second stations for a period of time (in contrast to the Ptolemaic tradition). Finally, we consider some medieval astrological texts where stations or retrograde motions are invoked. [ABSTRACT FROM AUTHOR]

Prehistoric astronomical observatories include a specific type of rock-cut monuments from the Mountainous Thrace in Bulgaria, with a specific shape and orientation in space, which are part of the characteristic representatives of the archeoastronomical sites on the Balkan Peninsula from the period of 4000–4500 BCE. Earlier societies focused on the triad "astronomical instrument"—celestial objects—trained observers. When choosing sites for the construction of oriented stone complexes for astronomical observations, prehistoric people were interested in the number of clear days and nights within the tropical year, which is connected with the paleoclimate of the region and to the astroclimate, which determines the possibility of observing heavenly bodies. Here we examine 13 prehistoric astronomical observatories using the methods of archaeoastronomy in order to determine the period of their operation. Since the existence of a large number of such objects is indirect evidence of a good astroclimate, we make an assessment of the paleoclimate in the relevant era in the Bulgarian lands in order to find out if it was suitable for astronomical observations. The estimations are made according to the geological data and solar insolation luminescence proxy records of the evolution of cave speleothems from Duhlata cave in the village of Bosnek, Pernik municipality, which is still the only available experimental record of past solar insolation in Europe covering the last 20,000 years. The number of clear days and nights are estimated, and a critical assessment of the possibility of successful observations of the Sun during equinoxes and solstices is made using the methods of "horizon" astronomy and meridional culminations. It is also shown that the climate at the end of the Ice Age was cooler than today. About 11,700 years ago (11,700 radiocarbon years before 1950 CE or 11,700 BP), the climate began to warm, and forest vegetation developed on the territory liberated from the glaciers. During the Upper Atlantic (6–8 thousand years BCE), the average annual temperature on the Balkan Peninsula and in particular in Bulgaria was about 2–2.5 °C higher than it is today. This climate allows some very good astroclimatic conditions for observations of the Sun near the horizon and increases the accuracy of the observational data in determining the time of occurrence in its extreme positions on the horizon. We show that changes in climate (and astroclimate accordingly) influence the type of prehistoric astronomical observatories. [ABSTRACT FROM AUTHOR]

"Planetarien: Wunder der Technik—Techniken des Wunderns" by Helen Ahner is a book that explores the history and significance of planetariums as places of popular science education and entertainment. The author focuses on the period between 1925 and 1930 and examines case studies in Munich, Jena, Vienna, and Hamburg. Ahner argues that the planetarium experience was associated with wonder and amazement, and that the physical experience of the audience was more important than the content of the shows. The book also discusses the planetarium's role in modernity and its ability to condense central themes of the time. [Extracted from the article]

The Haystack Telescope is an antenna with a diameter of 37 m and an elevation-dependent surface accuracy of ≤ 100 μ m that is capable of millimeter-wave observations. The radome-enclosed instrument serves as a radar sensor for space situational awareness, with about one-third of the time available for research by MIT Haystack Observatory. Ongoing testing with the K-band (18–26 GHz) and W-band receivers (currently 85–93 GHz) is preparing the inclusion of the telescope into the Event Horizon Telescope (EHT) array and the use as a single-dish research telescope. Given its geographic location, the addition of the Haystack Telescope to current and future versions of the EHT array would substantially improve the image quality. [ABSTRACT FROM AUTHOR]

This work deals with a new theoretical method proposed with the intent of improving the quality of astronomical polarimetric data. The theoretical method is applied to one of the simplest possible birefringent type polarizer device constructs, being a hybrid measurement procedure between the fixed position angles and the continuous rotation records of the modulator (in our case, the quarter-wave plate) methods. It can be suitable for some astronomical applications in Planetary Science and Stellar Astrophysics, as their polarimetric parameters (polarization degree, polarization angle and Stokes parameters) have relatively stable values, allowing for the iterative proposed procedure. The validity of the procedure is expected to be practically proven by comparing the quality of the polarization parameters obtained with it, on the proposed instrument, with the results obtained with a similar standardized instrument on the market. [ABSTRACT FROM AUTHOR]

Copyright of Bulletin of History of Arts / Muvészettörténeti Értesíto is the property of Akademiai Kiado and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

The Perseverance rover landed in Jezero crater, Mars, in February 2021. We used the Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) instrument to perform deep-ultraviolet Raman and fluorescence spectroscopy of three rocks within the crater. We identify evidence for two distinct ancient aqueous environments at different times. Reactions with liquid water formed carbonates in an olivine-rich igneous rock. A sulfate-perchlorate mixture is present in the rocks, which probably formed by later modifications of the rocks by brine. Fluorescence signatures consistent with aromatic organic compounds occur throughout these rocks and are preserved in minerals related to both aqueous environments. [ABSTRACT FROM AUTHOR]

This essay examines the problems associated with the installation of a precision instrument at the National Astronomical Observatory of Chile, starting before its construction and following the process through its installation to its later useful life. Between 1908 and 1913, the director of the observatory, Friedrich W. Ristenpart, corresponded with the German manufacturer, A. Repsold & Söhne in Hamburg, trying to identify the critical points pertinent to the installation of the instrument in Chile. These communications reveal how the installation of the instrument required the stabilization of local knowledge (location, adjustment, calibration, and staging) that would allow the data it obtained to be universally validated. This correspondence between user and manufacturer also reveals that the phenomenon of the mobility of instruments implies much more than simply transporting something from one place to another: there is no movement without some type of coordination between the extraction of an object from a certain place and context and its insertion into a new place and set of relationships. [ABSTRACT FROM AUTHOR]

The main factors that influence the success of observations in the infrared range (central wavelengths of the photometric bands at 3.75 and 4.8 m) on the multipurpose optical telescope are considered. Estimates of the sky background brightness are obtained for the Caucasus Mountain Observatory (CMO) of Moscow State University: photons/(s pixel) in the 3.75 m band and photons/(s pixel) in the 4.8 m; and the instrumental background for the 2.5-m CMO telescope at С: photons/(s pixel) in the 3.75 m band and photons/(s pixel) in the 4.8 m band. It is shown that at this background signal level with the currently available commercial cameras in the 3–5 m spectral range, the telescope–camera coupling capabilities for observing faint objects will still be limited by the thermal background. For different observational conditions, estimates of the limiting magnitudes of objects available for observations in the 3.75 and 4.8 m ranges are obtained. For average observation conditions (instrument temperature of C and stellar image size of ), the limit is and , respectively. [ABSTRACT FROM AUTHOR]

The period of the last third of 19th century was beneficial to a boom of observatories run by amateur astronomers. One of them was built in Hurbanovo. It is well known that place names have changed throughout history; sometimes more than one was used at the same time, and it often depended on the language in which the historical documents were written. These peculiarities can easily confuse the modern reader. For the sake of clarity, we have decided to use modern official geographical names. Even in Anglophone historiographical literature, modern names are usually used in the first place instead of historical ones. All other historical forms of place names are mentioned in parentheses when they first appear (first in Hungarian, then in German). Several names or variations of those names may be discovered in historical records pertaining to Hurbanovo, e.g.: Stará Ďala (in Slovak), Ó-Gyalla, O Gyalla, Ógyalla, Ogyalla, Ó Gyalla, Ó Gyala, Ó-Gyala, Ó Gyála (in Hungarian), Altdala (in German). The town was named Hurbanovo in 1948. (Slovakia) in 1871 by a local nobleman Nicolaus de Konkoly. The paper is divided into two main parts. The first part is focused on the development of instrumentation and domes of the observatory. The second one is focused on various kinds of astronomical and astrophysical observations performed by the observatory staff from the beginning of the observatory until the dissolution of the Austro-Hungarian Empire in 1918. [ABSTRACT FROM AUTHOR]

Echelle grating provides high spectral resolving power and diffraction efficiency in a broadband wavelength range by the Littrow mode. The spectrometer with the cross-dispersed echelle scheme has seen remarkable growth in recent decades. Rather than the conventional approach with common blazed grating, the cross-dispersed echelle scheme achieves the two-dimensional spatial distribution of the spectrum by one exposure without scanning in the broadband spectral range. It is the fastest and most sensitive spectroscopic technology as of now, and it has been extensively applied in commercial and astronomical spectrometers. In this review, we first highlight the characteristics of the echelle and then present the optical layout, detection approach, and method of calibration. Finally, we discuss the state-of-the-art implementations and applications of commercial and astronomical instruments. [ABSTRACT FROM AUTHOR]

A historical research study devoted to the elucidation of the historical facts about the activity of the Kharkiv Astronomical Observatory during the German–Soviet War is carried out. The astronomical community of Kharkiv suffered heavy losses: Professors O.I. Razdol'skii, M.S. Savron, and S.M. Semiletov, Researcher G.L. Strashnii, Yu.M. Fadeev, and V.O. Balanskii, and calculation specialist L.M. Kostirya died; young representatives of the Kharkiv astronomical community M. Azbel', F. Berezovskii, I. Tymoshenko, and O. Ubiivovk gave their lives in the battle with the enemy. During warfare, many observatory buildings, together with astronomical instruments and devices, were seriously damaged. The peculiarities of observatory operation during the studied period have been documented, and the biographical data of most of the employees of the Kharkiv Astronomical Observatory during the Nazi occupation of the city in 1941–1943 have been clarified. The stages of restoration of the observatory after the liberation of Kharkiv from the invaders were considered. [ABSTRACT FROM AUTHOR]

Copyright of Journal of History / Habaršy Tarihi Seriâsy is the property of Al-Farabi Kazakh National University and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Disputes over whether the Scientific Revolution contributed to the Industrial Revolution begin with the common assumption that natural philosophers and artisans formed distinct groups. In reality, these groups merged together through a diverse group of applied mathematics teachers, textbook writers, and instrument makers catering to a market ranging from navigators and surveyors to bookkeepers. Besides its direct economic contribution in diffusing useful numerical skills, this "practical mathematics" facilitated later industrialization in two ways. First, a large supply of instrument and watch makers provided Britain with a pool of versatile, mechanically skilled labor to build the increasingly complicated machinery of the late eighteenth century. Second, the less well-known but equally revolutionary innovations in machine tools—which, contrary to the Habbakuk thesis, occurred largely in Britain during the 1820s and 1830s to mass-produce interchangeable parts for iron textile machinery—drew on a technology of exact measurement developed for navigational and astronomical instruments. [ABSTRACT FROM AUTHOR]