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The Latin American Integration Route – RILA, also known as the Bioceanic Route or Bioceanic Corridor, consists of a road integration project between Brazil, Paraguay, Argentina and Chile. The intention, through this initiative, is to establish a direct route of transit between the Brazilian ports on the Atlantic and the Chilean ports on the Pacific, reducing the distance and time of transport and, consequently, the logistical costs. In addition to its strategic character from a commercial point of view, the completion of the Corridor works carries the hope of making the development of the regions viable, as well as the cultural, social, linguistic, political, legal and environmental integration of Latin American countries. Faced with this emerging transformative scenario, the need to design an Observatory was recognized, with the intention of producing and disseminating data and information that would allow for the monitoring and evaluation of the various processes surrounding the Route. Therefore, this article aims to contextualize and present the UniRILA Interdisciplinary Observatory - OBSUNIRILA, through theoretical contributions from published articles and books, as well as journalistic publications, videos and lives on the subject. It is, therefore, an exploratory research with a qualitative approach, carried out through a bibliographic review and document analysis. As a result, the current actions of OBSUNIRILA and its future plans and projects are presented, with the aim of collaborating for the understanding of the specificities experienced along the Bioceanic Route, as well as appearing as an open and democratic space capable of building critical thinking and innovative solutions. [ABSTRACT FROM AUTHOR]

The COVID-19 pandemic had a significant impact on the living and working conditions of the entire population of Brazil, having a different and more intense effect on groups considered to be vulnerable. The objective of this article is to present an overview of the evolution of the pandemic in the country according to the bulletins of the Covid-19 Fiocruz Observatory in the period between the declarations of the beginning and end of the Public Health Emergency of National Concern (ESPIN, in Portuguese), February 2020 to April 2022. Several of the indicators adopted in the 69 bulletins published for the analysis of the pandemic were used, such as cases and deaths due to SARIs and COVID-19, age groups, % of occupancy of ICU beds, and vaccination, among others. The evolution analysis was organized between years and phases of the pandemic, seeking to highlight what characterized each moment. The closing statement of ESPIN in Brazil coincides with the discussions on the transition from a pandemic to an endemic scenario, without this representing the elimination of the virus, infections, and disease, posing the challenges of advances in vaccination processes in Brazil and around the world, as well as living with scenarios that may require the adoption of temporary protection measures in epidemic periods and periods of greater risk for vulnerable groups. [ABSTRACT FROM AUTHOR]

The article discusses the eleventh edition of the Jan Jędrzejewicz Award to recognize the most outstanding Polish-language publication in the field of the history of science and technology. It is reported that the award honors the best monographs and scientific works by Polish authors, serving as a tribute to Jan Walery Jędrzejewicz (1835–1887), a figure passionate about astronomy and meteorology, a physician, and the owner of a private observatory in Płońsk.

In this study, a comprehensive analysis of the reflection grating spectrometer (RGS) data (energy range 0.33 keV to 2.5 keV) of GX 13+1 from the XMM-Newton space observatory was conducted. Numerous absorption lines have been described in earlier publications, although the majority of these investigations focused on the energy range between 3 keV and 10 keV. We considered all ten on-axis observations for spectral analysis, but during timing analysis, off-axis observations were also analysed. A fresh dip in off-axis observation 0122340701(B) was observed together with the previously reported dip in on-axis observation 0505480501(F). No burst or eclipsing was observed in any of the observations. The spectral analysis revealed the presence of the highly ionized elements, Si XIII 1s2–1s2p and 1s2–1s3p transitions with energies of 2.02 keV and 2.24 keV, respectively, as well as Mg XII 1s–6p transitions with energies of 1.91 keV and Al XIII 1s–4p transitions with energies of 2.15 keV. Before this study, no analyses of XMM-Newton data reported Mg XII and Al XIII elements. Moreover, the 1s–6p transitions of Mg XII and 1s–4p transitions of Al XIII were not even reported in any Chandra data analysis. The equivalent hydrogen column densities obtained (2.35 × 1022 cm−2 to 4.18 × 1022 cm−2) are consistent with previously reported values. The equivalent widths of neighbouring observations are found to be nearly the same. This supports us in suggesting that the absorptions may be due to the presence of an interstellar medium (ISM) in the line of sight (LOS) of the source. [ABSTRACT FROM AUTHOR]

During eruptions, volcanoes produce air‐pressure waves inaudible for the human ear called infrasound, which are very helpful for detecting early signs of magma at the surface. Compared to violent ash‐rich explosions, recording more discrete atmospheric disturbances from effusive eruptions remains a practical challenge depending on the distance to the source. At Nyiragongo volcano (D.R. Congo), towering above a 1‐million urban area, we analyzed local infrasonic records between January 2018 and April 2022. An acoustic signature from this open‐vent volcano is detected up to the volcano observatory facilities in Goma city center about 17 km from its crater. We compared infrasound signals with space‐based observations of the intra‐crater activity (SO2 emissions, thermal anomalies, crater depth/radius). We thus obtain a comprehensive picture of Nyiragongo's eruptive activity during this period, encompassing the drainage of its lava lake during its third known flank eruption on 22 May 2021. Plain Language Summary: Similar to seismic waves propagating within the solid Earth, acoustic waves propagate in the atmosphere as a result of near‐surface volcanic activity. In contrast with powerful volcanic explosions, close‐range deployment of instruments around the active vent (for instance <15 km) is generally needed for continuously monitoring long‐living lava effusion or degassing as observed at open‐vent volcanoes, such as Kīlauea (Hawaii) or Nyiragongo (D.R. Congo). Nyiragongo hosted the world's largest lava lake up to 2021, which was drained during the third known flank eruption of this volcano on 22 May 2021. While watching for possible reawakening, we detected the infrasound signature of a nascent lava lake four months later, highlighting the crucial role of infrasound monitoring. Remote observations from space (ground deformation, gas emissions, thermal anomalies) can also provide essential information about the eruptive state of a volcano and were jointly analyzed with infrasound records. Knowing that Nyiragongo towers above the 1‐million inhabitant city of Goma, such an approach has significant implications for optimizing future monitoring efforts in a harsh field environment. Key Points: Nyiragongo volcano (D.R. Congo) is a permanent emitter of infrasound that pauses during rare flank eruptionsIntra‐crater lava eruptions (lava lake, spatter cone, lava pond) are detected up to the observatory in a dense urban area ∼17 km awayJoint analysis with space‐based observations over the period 2018–2022 provides a clear picture of the persistent unrest at this volcano [ABSTRACT FROM AUTHOR]

Carbon dioxide (CO2) is the most important anthropogenic greenhouse gas. Its atmospheric concentration has increased by almost 50% since the beginning of the industrial era, causing climate change. Fossil fuel combustion is responsible for most of the atmospheric CO2 increase, which originates to a large extent from localized sources such as power stations. Independent estimates of the emissions from these sources are key to tracking the effectiveness of implemented climate policies to mitigate climate change. We developed a procedure to quantify CO2 emissions from localized sources based on a cross-sectional mass-balance approach and applied it to infer CO2 emissions from the Bełchatów Power Station, in Poland, using atmospheric observations from the Orbiting Carbon Observatory 3 (OCO-3) in its Snapshot Area Map (SAM) mode. As a result of the challenge of identifying CO2 emission plumes from satellite data with adequate accuracy, we located and constrained the shape of emission plumes using TROPOspheric Monitoring Instrument (TROPOMI) NO2 column densities. We analysed all available OCO-3 overpasses over the Bełchatów Power Station from July 2019 to November 2022 and found a total of 9 that were suitable for the estimation of CO2 emissions using our method. The mean uncertainty of the obtained estimates was 5.8 Mt CO2y-1 (22.0%), mainly driven by the dispersion of the cross-sectional fluxes downwind of the source, e.g. due to turbulence. This dispersion uncertainty was characterized using a semivariogram, possible thanks to the OCO-3 imaging capability over a target region in SAM mode, which provides observations containing plume information up to several tens of kilometres downwind of the source. A bottom-up emission estimate was computed based on the hourly power plant generated power and emission factors to validate the satellite-based estimates. We found that the two independent estimates agree within their 1σ uncertainty in 8 out of 9 analysed overpasses and have a high Pearson's correlation coefficient of 0.92. Our results confirm the potential for monitoring large localized CO2 emission sources from space-based observations and the usefulness of NO2 estimates for plume detection. They illustrate as well the potential to improve CO2 monitoring capabilities with the planned Copernicus Anthropogenic CO2 Monitoring (CO2M) satellite constellation, which will provide simultaneously retrieved XCO2 and NO2 maps. [ABSTRACT FROM AUTHOR]

The ultraviolet multi-filter rotating shadowband radiometer (UV-MFRSR) is a seven-channel radiometer with narrowband filters centered between wavelengths 300 and 368 nm. Four of the middle wavelengths in this device are near those used in the Dobson spectrometer to retrieve ozone column abundance. In this paper measurements from Mauna Loa Observatory (MLO) were used, first, to calibrate the instrument using the Langley plot method, and, subsequently, to derive column ozone and aerosol optical depths. The ozone derived from the UV-MFRSR was compared to the ozone measured by a Dobson spectrophotometer that operates daily at the MLO resulting in column values within about 1 DU on average for 43 days in 2018. The aerosol optical depth (AOD) retrievals are more challenging. Generally, the AOD increases with wavelength between 305 and 332 nm; not what is expected given the typical AOD wavelength dependence at visible wavelengths. An example of this behavior is discussed, and research by others is cited that indicates similar behavior at these wavelengths, at least for the low aerosol optical depth conditions encountered at high altitude sites. [ABSTRACT FROM AUTHOR]

Carbon dioxide (CO2) is the most important anthropogenic greenhouse gas. Its atmospheric concentration has increased by almost 50 % since the beginning of the industrial era, causing climate change. Fossil fuel combustion is responsible for most of the atmospheric CO2 increase, which originates to a large extent from localized sources such as power stations. Independent estimates of the emissions from these sources are key to tracking the effectiveness of implemented climate policies to mitigate climate change. We developed a procedure to quantify CO2 emissions from localized sources based on a cross-sectional mass-balance approach and applied it to infer CO2 emissions from the Bełchatów Power Station, in Poland, using atmospheric observations from the Orbiting Carbon Observatory 3 (OCO-3) in its Snapshot Area Map (SAM) mode. As a result of the challenge of identifying CO2 emission plumes from satellite data with adequate accuracy, we located and constrained the shape of emission plumes using TROPOspheric Monitoring Instrument (TROPOMI) NO2 column densities. We analysed all available OCO-3 overpasses over the Bełchatów Power Station from July 2019 to November 2022 and found a total of 9 that were suitable for the estimation of CO2 emissions using our method. The mean uncertainty of the obtained estimates was 5.8 Mt CO2 y−1 (22.0 %), mainly driven by the dispersion of the cross-sectional fluxes downwind of the source, e.g. due to turbulence. This dispersion uncertainty was characterized using a semivariogram, possible thanks to the OCO-3 imaging capability over a target region in SAM mode, which provides observations containing plume information up to several tens of kilometres downwind of the source. A bottom-up emission estimate was computed based on the hourly power plant generated power and emission factors to validate the satellite-based estimates. We found that the two independent estimates agree within their 1 sigma uncertainty in 8 out of 9 analysed overpasses and have a high Pearson's correlation coefficient of 0.92. Our results confirm the potential for monitoring large localized CO2 emission sources from space-based observations and the usefulness of NO2 estimates for plume detection. They illustrate as well the potential to improve CO2 monitoring capabilities with the planned Copernicus Anthropogenic CO2 Monitoring (CO2M) satellite constellation, which will provide simultaneously retrieved XCO2 and NO2 maps. [ABSTRACT FROM AUTHOR]

We present results from long-term spectroscopic monitoring of 21 T-Tauri stars located in the Taurus–Auriga star-forming region (SFR). We combine medium and high-dispersion Echelle spectroscopy obtained at the Stará Lesná, Skalnaté Pleso (both in Slovakia), and Tautenburg (Germany) observatories with low-resolution flux-calibrated spectra from Asiago (Italy) observatory all taken between 2015 and 2018. We extend the coverage by additional medium-resolution spectra from Stará Lesná obtained in 2022. In the previous paper, we measured photometric periods of these targets in a range of 0.7–3.1 d, which could be due to the rotation of a spotted surface or binarity. Here, we use the broadening-function technique to determine the radial and projected rotational velocities to reveal any close binary companion. Our analysis concludes that no such companion is present with an orbital period equal to the photometric period. We focus our analysis primarily on determining atmospheric parameters such as surface gravity log  g , effective temperature T eff, and metallicity [Fe/H]. Additionally, we measure the equivalent width of H α, Li i , and interstellar Na i lines. We also investigate the effect of possible reddening on individual targets and construct the HR diagram of our sample. Using pre-main-sequence evolutionary models, we determine the age of our targets. This analysis hints at ages younger than 50 Myr with mean age 5 ± 3 Myr, masses between 0.75 and 2.10 M⊙, and minimum radii in the range 0.60–3.17 R⊙. Altogether, the results are consistent with expected young stars with larger radii than those of main-sequence stars. [ABSTRACT FROM AUTHOR]

We measure the mean-squared polarization fraction of a sample of 6282 Galactic cold clumps at 353 GHz, consisting of Planck Galactic cold clump (PGCC) catalogue category 1 objects [flux densities measured with signal-to-noise ratio (S/N) > 4]. At 353 GHz, we find the mean-squared polarization fraction, which we define as the mean-squared polarization divided by the mean-squared intensity, to be (4.79 ± 0.44) × 10−4 equation to an |$11\, \sigma$| detection of polarization. We test if the polarization fraction depends on the clumps' physical properties, including flux density, luminosity, Galactic latitude, and physical distance. We see a trend towards increasing polarization fraction with increasing Galactic latitude, but find no evidence that polarization depends on the other tested properties. The Simons Observatory, with angular resolution of order 1 arcmin and noise levels between 22 and |$54\, \mu$| K−arcmin at high frequencies, will substantially enhance our ability to determine the magnetic field structure in Galactic cold clumps. At |$\ge 5\, \sigma$| significance, we predict the Simons Observatory will detect at least ∼12 000 cold clumps in intensity and ∼430 cold clumps in polarization. This number of polarization detections would represent a two orders of magnitude increase over the current Planck results. We also release software that can be used to mask these Galactic cold clumps in other analyses. [ABSTRACT FROM AUTHOR]

The Earth's albedo is the fraction of short-wave solar radiation that is reflected back to space, and is key to understand the observed trends in climate change. Although there have been many observational approaches to estimate the Earth's albedo, different methods have their own drawbacks, for example, artificial satellites have a finite life time, and are operating in a hard environment that could quickly degrade the detectors. The Moon, the only natural satellite of Earth, offers an additional platform for monitoring the Earth's albedo. In this paper, we calculate the global TOA (top-of-atmosphere) albedo that would be observed by a theoretical observatory on the Moon, and compare it with long-term trends derived from CERES (Clouds and the Earth's Radiant Energy System, 2000–2020) and earthshine data (1999–2017). We find that the global hourly mean albedo observed in the direction of the Moon is more variable because of the orbital movement of the Moon. However, the regional and long-term global mean albedo anomalies that would be observed by CERES and has a good general agreement by a lunar observer over 20 years the data spans. Similarly, earthshine data show a steady decline during two decades of about 0.7 W / m 2 which is in line with the decline of 0.5 W / m 2 that would be observed from the Moon. Besides, to compare the regional changes of albedo with CERES, the spatially-resolved decadal anomalies in the albedo are also calculated for analysis. We find that a lunar-based observatory would be capable of detecting similar changes seen from CERES. Thus, it is a a practical option to monitor the long-term trends in albedo from the point of view of capturing the variability in the TOA fluxes of the Earth's atmosphere. [ABSTRACT FROM AUTHOR]

Classical novae are thermonuclear explosions in stellar binary systems, and important sources of 26Al and 22Na. While γ rays from the decay of the former radioisotope have been observed throughout the Galaxy, 22Na remains untraceable. Its half-life (2.6 yr) would allow the observation of its 1.275 MeV γ-ray line from a cosmic source. However, the prediction of such an observation requires good knowledge of its nucleosynthesis. The 22Na(p, γ)23Mg reaction remains the only source of large uncertainty about the amount of 22Na ejected. Its rate is dominated by a single resonance on the short-lived state at 7785.0(7) keV in 23Mg. Here, we propose a combined analysis of particle-particle correlations and velocity-difference profiles to measure femtosecond nuclear lifetimes. The application of this method to the study of the 23Mg states, places strong limits on the amount of 22Na produced in novae and constrains its detectability with future space-borne observatories. The authors report a particle-particle correlation and velocity-difference profile method to measure nuclear lifetime. The results obtained for excited states of 23Mg are used to constrain the production of 22Na in the astrophysical novae explosions. [ABSTRACT FROM AUTHOR]

Women with schizophrenia have specific health needs that differ from those of men and that change through successive life stages. We aimed to review the biopsychosocial literature on schizophrenia that addresses clinically important questions related to the treatment of women, including somatic morbi-mortality, hyperprolactinemia, comorbid substance use disorders, social risk factors, and medication effectiveness/safety. Data search terms were as follows: (Morbidity AND mortality) OR hyperprolactinemia OR ("substance use disorders" OR addictions) OR ("social risk factors") OR ("drug safety" OR prescription) AND women AND schizophrenia. A secondary aim was to describe a method of monitoring and interdisciplinary staff strategies. Schizophrenia patients show an increased risk of premature death from cardiovascular/respiratory disease and cancer compared to the general population. The literature suggests that close liaisons with primary care and the introduction of physical exercise groups reduce comorbidity. Various strategies for lowering prolactin levels diminish the negative long-term effects of hyperprolactinemia. Abstinence programs reduce the risk of victimization and trauma in women. Stigma associated with women who have serious psychiatric illness is often linked to reproductive functions. The safety and effectiveness of antipsychotic drug choice and dose differ between men and women and change over a woman's life cycle. Monitoring needs to be multidisciplinary, knowledgeable, and regular. [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 invited memoir looks back on my scientific career that straddles the solar and stellar branches of astrophysics, with sprinklings of historical context and personal opinion. Except for a description of my life up to my Ph.D. phase, the structure is thematic rather than purely chronological, focusing on those topics that I worked on throughout substantial parts of my life: stars like the Sun and the Sun-as-a-star, surface field evolution, coronal structure and dynamics, heliophysics education, and space weather. Luck and a broadly inquisitive frame of mind shaped a fortunate life on two continents, taking me from one amazing mentor, colleague, and friend to another, working in stimulating settings to interpret data from state-of-the-art space observatories. [ABSTRACT FROM AUTHOR]

We present a comprehensive analysis of the physical parameters and relationships of umbral dots (UDs), which assists in our understanding of the physical properties of the Sun. This study is based on a detailed analysis of UDs detected in 12 umbras belonging to 10 different sunspots using high-resolution data recorded by the Goode Solar Telescope at Big Bear Solar Observatory. We obtained the physical parameters (total intensity, diameter, eccentricity, lifetime, and dynamic velocity) of each UD and calculated correlation coefficients using linear and nonlinear approaches to reveal the relationships between these parameters. We found that: i) The diameter of UDs vary between 92.2 km and 246.5 km, the eccentricity varies between 0.02 and 0.65, the lifetimes of UDs vary from 0.75 to 120.00 min and the dynamic velocities vary from 0.01 km s−1 to 3.80 km s−1. ii) The intensity–diameter and diameter–eccentricity relationships show the highest degree of correlation, while the lowest linear correlation was obtained for the diameter–lifetime relationship and the lowest nonlinear correlation was obtained for the eccentricity–lifetime relationship. iii) In general, the nonlinear correlation coefficients are higher than the linear correlation without exception. iv) The linear and nonlinear correlation coefficients are very close to each other in the case of the diameter–eccentricity relation. v) While the average diameter, intensity, and eccentricity are related to the umbral area, the average lifetime and dynamic velocity of UDs are not dependent on the umbral area. [ABSTRACT FROM AUTHOR]

We report on the first comprehensive study of the coronal mass ejections (CMEs) associated with ∼ 25 MeV solar energetic-proton (SEP) events in 1980 – 2013 observed in the low/inner corona by the Mauna Loa Solar Observatory (MLSO) Mk3 and Mk4 coronameters. Where possible, these observations are combined with space-based observations from the Solar Maximum Mission C/P, P78-1 SOLWIND, or SOHO/LASCO coronagraphs. The aim of the study is to understand directly measured (rather than inferred from proxies) CME motions in the low to midcorona and their association with SEP acceleration, and hence attempt to identify early signatures that are characteristic of SEP acceleration in ground-based CME observations that may be used to warn of impending SEP events. Although we find that SEP events are associated with CMEs that are on average faster and wider than typical CMEs observed by MLSO, a major challenge turns out to be determining reliable estimates of the CME dynamics in the low corona from the 3-min cadence Mk3/4 observations since different analysis techniques can produce inconsistent results. This complicates the assessment of what early information on a possible SEP event is available from these low-coronal observations. [ABSTRACT FROM AUTHOR]

The Ion Velocity Meter (IVM) on NASA's Ionospheric Connection Explorer (ICON) reports the in-situ ion density, ion temperature and 3-component ion drift velocity, retrieved from measurements by a retarding potential analyzer and an ion drift meter. ICON was launched during a deep solar minimum in late 2019, followed by a solar quiet (F10.7 < 80) period until September 2020. In order to quantify the uncertainties in the IVM's drift velocity in a low plasma density environment, we compared IVM's vertical drift velocity with eastward electric field (EEF) obtained from Swarm's equatorial electrojet current measurements, the vertical drift from ground-based incoherent scatter radar (ISR) at Jicamarca Radio Observatory (JRO) and from Jicamarca Unattended Long-term studies of Ionosphere and Atmosphere (JULIA) coherent mode. The main results of this study show that (1) the vertical drift derived from Swarm's EEF and ISR are in good agreement with the zonal electric field derived from JULIA's vertical drift regardless of the F10.7 value. (2) The zonal electric field derived from IVM's meridional drift is in good agreement with Swarm's EEF in 2021, whereas the distribution is highly scattered in the deepest solar minimum in 2020. (3) An ad hoc IVM correction based on the 24-hour running mean of meridional drift can bring the IVM data into better agreement with Swarm and JULIA. An additional quality control based on O+ fractional composition may be needed for some studies using IVM's vertical drift. By using the same methodology presented in this work, future missions could calibrate their drift measurements to facilitate meaningful integration with ICON/IVM observations through the comparision with ground-based measurements. [ABSTRACT FROM AUTHOR]

This paper introduces a group of three articles that bring together object stories relating to observatory history and networks. The three articles ('Instrumental networks', 'Object itineraries' and 'Observatory audiences') each bring together three object stories by different authors that contribute to the article theme. Here the genesis of the collection at the workshops of the Observatory Sites and Networks project is discussed, along with the approaches taken and the kind of insights that studies of material culture can shed on histories of observatories and the observatory sciences. The arrangement of the stories into three themes is outlined while common threads and recurring motifs that create connections and synergies across the thematic sections are highlighted. Together the collected papers make an argument for the use of objects in research, demonstrating the fruitfulness of investigating their histories and showing how they can expand our understanding of the networks of people, organisations and objects that were interested in or essential to the successful functioning of observatories. They also demonstrate the breadth and variety of interests and resources that were drawn into these networks, offering new ways of understanding and interpreting both observatory sites and museum objects. [ABSTRACT FROM AUTHOR]

In this paper, each contribution uses an object biography -- or object itinerary -- methodology, tracking their chosen objects from conception and purchase, across time and space, to today. The function of each object could change significantly over time, and these stories serve to remind us of the range of projects and activities that observatories might support or host, including overseas astronomical expeditions, a local time service, mathematical calculations, measurement of photographic plates, magnetic, meteorological and seismological observation, the hosting and dining of visitors, and the display and promotion of the observatory's status. In each case, the object's movements and location within particular spaces point the reader to consider a wide range of people, whether located within the observatory, beyond its walls, or within international scientific networks. The objects considered here are a London-made marine chronometer purchased by the Palermo Observatory, which was not used for navigation but was nevertheless well travelled; a large wooden table placed in the Octagon Room of the Royal Observatory Greenwich; and a British seismograph set up in at the Meteorological and Magnetic Observatory of the University of Coimbra. These itineraries also show how the value attached to objects changes over time: they shift from functional tools to obsolescence, then regain significance as their histories have been recovered and re-examined. This paper forms part of the collection 'Revealing observatory networks through object stories' where object stories are presented in three themed papers (with further papers being 'Instrumental networks' and 'Observatory audiences'). The genesis of the collection is described in the 'Introduction'. [ABSTRACT FROM AUTHOR]

Like the contributions to the other papers in this collection ('Object itineraries' and 'Instrumental networks'), those in this final section explore instrumental networks and object itineraries in order to tell new histories of observatory sites and their associated networks. (For a discussion of the genesis and thinking behind the collection of papers see the 'Introduction'). Here, however, they focus on object stories that highlight the opportunities for and importance of communicating with those outside the scientific community. They show, however, a wide range of potential and actual audiences to be mediated between, from closely associated scientific institutions and those holding the purse strings within government, to groups making up the local civic society and a wider and more diffuse audience for scientific outputs and achievements. The objects explored here are an 1850s model of electrically triggered time signals, associated with those at the Royal Observatory, Edinburgh; a late nineteenth-century astrographic telescope that, with approval of scientific and governmental audiences, brought the National Astronomical Observatory of Mexico into an international project and subsequently found new audiences through public display and artistic intervention; and a photoelectric relay that advertised the Yerkes Observatory to the Chicago and visiting public by forming part of a stunt, whereby the light of a distant star triggered the lighting of the 1933 Century of Progress Exposition. [ABSTRACT FROM AUTHOR]

This paper presents three pieces that use objects, or object types, to reveal the material, personal, institutional and commercial networks that surrounded the introduction and successful use of instruments, systems and techniques. The objects explored are: the Hourly Signal Relay, used within the time signal system of the Royal Observatory, Greenwich, from the mid-nineteenth century; photographic glass plates from the British 1874 transit of Venus expeditions; and an electronic imaging tube, Lallemand's camera, developed in Paris and used at the Lick Observatory in California in the 1960s. Each story uses examples of failure as a means of highlighting a lack of robustness in or effort required to maintain these networks. Once created, however, such networks could, as the second two stories note, go on to develop and support alternative approaches, helping to create success from apparent failure. Nevertheless, complexity, failure and fragility have also led to the underrepresentation or obscurity of these objects in museum collections, until given focused attention in these studies. The paper forms part of a collection of articles: Revealing observatory networks through object stories. The other papers in the collection are 'Object itineraries', and 'Observatory audiences' and the genesis of the collection is discussed in the 'Introduction'. [ABSTRACT FROM AUTHOR]

We explain the details of the photometric operation mode of the ASTRONICAM near-IR spectrograph camera mounted on the 2.5-m telescope of the Caucasian Mountain Observatory of the Sternberg Astronomical Institute and describe algorithms used for primary correction and overall pipeline reduction of the acquired data. We present the transformation equations from the 2MASS photometric system to the instrumental -band system. We derive color transformation coefficients between the instrumental photometric system and standard MKO-NIR (Mauna Kea Observatories Near-Infrared) system for the , , and -band filters and show that the camera system is close to the standard photometric system. We found that in the case of observations at zenith, average background brightness level, and seeing the stars with , , can be measured with a 3000-s exposure at the signal-to-noise ratio . [ABSTRACT FROM AUTHOR]

We performed photometric observations of the S 255, S 257, S 140, NGC 7358, and the Orion Bar photo-dissociation regions (PDRs) at 2 m using narrow-band filters centered on the Br , H , and [Fe II] lines, as well as the narrow-band and the broad-band filters for continuum subtraction. The observations were done with the 2.5-m telescope of the SAI Caucasian Mountain Observatory and the near-infrared camera and spectrograph ASTRONIRCAM. We find several high-density arc-like structures in the Br and [Fe II] images of the ionized gas in NGC 7538 and extended shells and arcs visible through the H emission. The H ionization front and H dissociation front are merged in NGC 7538. In S 255 and S 257 we detected only Br emission from the H II regions and bright H emission from the PDRs. The projected distance between the H ionization and H dissociation fronts is approximately 0.3–0.4 pc, which cannot be explained using models of a uniform medium. Most probably, the ionized and neutral gas in these PDRs is clumpy. The H I-to-H transitions in the NGC 7538, S 255, S 257 and S 140 PDRs are gradual with no sharp borders. This conclusion also agrees with the suggestion of a clumpy medium. [ABSTRACT FROM AUTHOR]

We report the results of optical spectroscopy of eight highly variable X-ray sources—AGN candidates from all-sky survey of the eROSITA telescope of the Spectrum-Roentgen-Gamma Space Observatory—performed with the TDS spectrograph (3600–7500 Å, ) attached to the 2.5-m telescope of the Caucasian Mountain Observatory of Sternberg Astronomical Institute of M.V. Lomonosov Moscow State University. We determined the redshifts of the sources from the emission and absorption lines in their spectra. At least five objects can be classified as Seyfert galaxies. We performed pilot infrared photometry of three distant quasars with using the ASTRONIRCAM camera and show that on the " " diagram the distant quasars studied can be confidently distinguished from Galactic red and brown dwarfs. This result proves the possibility of preliminary classification of distant X-ray quasar candidates by their IR colors for further detailed spectroscopic study on large telescopes. [ABSTRACT FROM AUTHOR]

This review presents the results of observations of high-mass and low-mass X-ray binaries carried out at the Caucasus Mountain Observatory of SAI MSU over the past five years. Interpretation of these observations within the framework of complex unconventional models has led to a number of interesting results. In particular, on the basis of the secular evolutionary increase in the orbital period of the microquasar SS 433 that we discovered, we managed to prove that the relativistic object here is a black hole, and the SS 433 system itself evolves as a semi-detached system due to the fact that the distance between its components increases with time, which prevents the formation of a common envelope. In the microquasar Cyg X-3, an anomalous behavior of IR color indices with the phase of the orbital period was detected. Modeling is carried out and estimates of the parameters of this system are given. In low-mass X-ray binaries (X-ray novae), black hole masses are estimated, spectra of advection-dominated disks are constructed, and an observational justification is given for modern results of three-dimensional gas-dynamic calculations for interacting binaries. [ABSTRACT FROM AUTHOR]

This work reports a novel method of determining the atmospheric water vapour feedback by utilizing the simultaneously retrieved atmospheric column concentrations of carbon dioxide (xCO2), the total column of water vapour (H2O) and the temperature (T7) at 700 hPa obtained from Orbiting Carbon Observatory-2 (OCO-2) and Orbiting Carbon Observatory-3 (OCO-3) data. The study areas are the tropical land cover of India and the surrounding deep seas. The methodology involves annual mean values for xCO2, H2O and T7 defined by averaging over a full year. The practical range of variation of saturation vapour pressure with surface temperature allows a linear approximation of the annual mean H2O versus xCO2. The linear correlation of the annual mean xCO2 and H2O values over the years 2016–2022 for OCO-2 and 2020–2022 for both OCO-2 and OCO-3 revealed an opposite trend of temporal variation for populated land and unpopulated deep sea regions. A feedback for water vapour was defined in terms of the long-term variation of annual mean H2O with annual mean xCO2 over years 2016–2022 and the corresponding variation with annual mean T7. The water vapour feedback for each ppm increase of annual mean xCO2 was equivalent to approximately 0.015 W m−2 and 0.007 W m−2 for populated and deep sea regions, respectively. The corresponding changes in T7 were an increase of 0.0267 K and a decrease of 0.0044 K, respectively. [ABSTRACT FROM AUTHOR]

Since its launch in 2000, the Cluster fleet visited a vast domain of the circum‐terrestrial environment, from the upstream solar wind and the distant tail, down to the plasmasphere, scanning in detail all magnetospheric regions during over two solar cycles. This led to an unprecedentedly rich data collection of multi‐point measurements which will be used for years to come to decipher the mechanisms of Solar‐Terrestrial interactions. The large volume of data gathered by Cluster requires special strategies to make efficient use of it. To address this issue we constructed a browsable database containing parameters of the detected Ultra low frequency waves and of the spacecraft formation geometry. The primary data used to derive the parameters are the magnetic field, the electric field and the electron density. The data is resampled to a cadence of 1 s and processed using a sliding analysis window of 2,048 s with a step of 256 s over 24 hr intervals. This results in time‐frequency arrays for each parameter covering the 0.5 mHz to 0.5 Hz frequency range. The database is accessible at http://plasma.spacescience.ro/cluster.html. In total there are 47 wave parameters in the database, among them being the ellipticity, the degree of polarization, the (unsigned) wave vector direction, and the Poynting vector. Plots for the planarity, elongation, and degeneration of the Cluster tetrahedron are also available. At the moment, the database covers measurements made between 01 January 2001 and 31 December 2020 with more data being added in time. Here we present this database, discuss the methods used to derive the parameters and give practical examples. Plain Language Summary: This work describe an on‐line database containing data and plots of physical quantities characterizing low frequency waves detected by the Cluster spacecraft fleet in the space plasma around the Earth. These quantities are derived using measurements of the magnetic field, electric field, and particles taken by the four spacecraft over 20 years. The plots can be used to quickly assess the plasma waves activity over a certain time interval, while the data can be used for further analysis. Key Points: The Cluster Virtual Observatory (CVO) is an on‐line archive of low frequency wave parameters based on Cluster measurementsThe CVO also provides the tetrahedron geometrical configuration parametersThe waves and configuration parameters are available as quick‐plots as well as binary Hierarchical Data Format data [ABSTRACT FROM AUTHOR]

Cheomseongdae in Gyeongju is the oldest astronomical observatory in the world and a representative scientific cultural heritage in Korea. However, in the mid twentieth century, suspicions were raised that Cheomseongdae might not be an observatory. As these suspicions piled up, a heated debate began about Cheomseongdae, which is still ongoing. I will examine the situation of the Cheomseongdae debate based on re- cent research results. First, some researchers interpreted the name Cheomseongdae as an astronomical observatory. However, other researchers interpreted the term “Chumseong[瞻星]” and the word “Dae[臺]” as symbolic. Second, many researchers view the shape of Cheomseongdae as a well since the shape of the top of Cheomseongdae resembles the letter “jeong(井),” which means a well. Third, there were conflicting interpretations of the unique structure of Cheomseongdae. Some said that it could not be seen as an observatory because it was inconvenient to climb to the top. On the contrary, some viewed it as an observatory because one could go up to the top of Cheomseongdae. The Cheomseongdae debate is unlikely to end easily. In order to end the Cheomseongdae debate, it is necessary to accurately distinguish between the factual contents of Cheomseongdae and the imagination felt after seeing it. And historical data should not be interpreted based on personal speculation or improper grounds. [ABSTRACT FROM AUTHOR]

The James Webb Space Telescope (JWST) has discovered an abundance of ultraviolet (UV) light from young galaxies and luminous black holes, challenging previous theories about the ionization of the universe. Astronomers have long debated how the neutral hydrogen gas in the early universe became ionized, a process that requires high-energy UV light. JWST's findings suggest that there may be an oversupply of UV light, leading to a reevaluation of when and how the epoch of reionization occurred. The telescope has also found evidence of smaller galaxies emitting significant amounts of UV light, potentially contributing to the ionization process. The role of active galactic nuclei (AGNs) as drivers of reionization is also being reconsidered, as JWST has discovered more AGNs than previously thought. Overall, JWST's observations have opened up new possibilities and raised more questions about the ionization of the universe. [Extracted from the article]

This paper introduces a group of three articles that bring together object stories relating to observatory history and networks. The three articles (‘Instrumental networks’, ‘Object itineraries’ and ‘Observatory audiences’) each bring together three object stories by different authors that contribute to the article theme. Here the genesis of the collection at the workshops of the Observatory Sites and Networks project is discussed, along with the approaches taken and the kind of insights that studies of material culture can shed on histories of observatories and the observatory sciences. The arrangement of the stories into three themes is outlined while common threads and recurring motifs that create connections and synergies across the thematic sections are highlighted. Together the collected papers make an argument for the use of objects in research, demonstrating the fruitfulness of investigating their histories and showing how they can expand our understanding of the networks of people, organisations and objects that were interested in or essential to the successful functioning of observatories. They also demonstrate the breadth and variety of interests and resources that were drawn into these networks, offering new ways of understanding and interpreting both observatory sites and museum objects.

Like the contributions to the other papers in this collection (‘Object itineraries’ and ‘Instrumental networks’), those in this final section explore instrumental networks and object itineraries in order to tell new histories of observatory sites and their associated networks. (For a discussion of the genesis and thinking behind the collection of papers see the ‘Introduction’). Here, however, they focus on object stories that highlight the opportunities for and importance of communicating with those outside the scientific community. They show, however, a wide range of potential and actual audiences to be mediated between, from closely associated scientific institutions and those holding the purse strings within government, to groups making up the local civic society and a wider and more diffuse audience for scientific outputs and achievements. The objects explored here are an 1850s model of electrically triggered time signals, associated with those at the Royal Observatory, Edinburgh; a late nineteenth-century astrographic telescope that, with approval of scientific and governmental audiences, brought the National Astronomical Observatory of Mexico into an international project and subsequently found new audiences through public display and artistic intervention; and a photoelectric relay that advertised the Yerkes Observatory to the Chicago and visiting public by forming part of a stunt, whereby the light of a distant star triggered the lighting of the 1933 Century of Progress Exposition.

This paper presents three pieces that use objects, or object types, to reveal the material, personal, institutional and commercial networks that surrounded the introduction and successful use of instruments, systems and techniques. The objects explored are: the Hourly Signal Relay, used within the time signal system of the Royal Observatory, Greenwich, from the mid-nineteenth century; photographic glass plates from the British 1874 transit of Venus expeditions; and an electronic imaging tube, Lallemand’s camera, developed in Paris and used at the Lick Observatory in California in the 1960s. Each story uses examples of failure as a means of highlighting a lack of robustness in or effort required to maintain these networks. Once created, however, such networks could, as the second two stories note, go on to develop and support alternative approaches, helping to create success from apparent failure. Nevertheless, complexity, failure and fragility have also led to the underrepresentation or obscurity of these objects in museum collections, until given focused attention in these studies. The paper forms part of a collection of articles: Revealing observatory networks through object stories. The other papers in the collection are ‘Object itineraries’, and ‘Observatory audiences’ and the genesis of the collection is discussed in the ‘Introduction’.

Aims. Since it launched on 22 March 2021, the 1U-sized CubeSat GRBAlpha operates and collects scientific data on high-energy transients, making it the smallest astrophysical space observatory to date. GRBAlpha is an in-orbit demonstration of a gamma-ray burst (GRB) detector concept suitably small to fit into a standard 1U volume. As was demonstrated in a companion paper, GRBAlpha adds significant value to the scientific community with accurate characterization of bright GRBs, including the recent outstanding event of GRB 221009A. Methods. The GRB detector is a 75 × 75 × 5 mm CsI(Tl) scintillator wrapped in a reflective foil (ESR) read out by an array of SiPM detectors, multi-pixel photon counters by Hamamatsu, driven by two separate redundant units. To further protect the scintillator block from sunlight and protect the SiPM detectors from particle radiation, we applied a multi-layer structure of Tedlar wrapping, anodized aluminium casing, and a lead-alloy shielding on one edge of the assembly. The setup allows observations of gamma radiation within the energy range of 70–890 keV with an energy resolution of ~30%. Results. Here, we summarize the system design of the GRBAlpha mission, including the electronics and software components of the detector, some aspects of the platform, and the current semi-autonomous operations. In addition, details are given about the raw data products and telemetry in order to encourage the community to expand the receiver network for our initiatives with GRBAlpha and related experiments. [ABSTRACT FROM AUTHOR]

In order to complement the picture of the atmospheric water cycle in the Southern Ocean, we have continuously monitored water vapor isotopes since January 2020 in Amsterdam Island (37.7983 °S, 77.5378 °E) in the Indian Ocean. We present here the first 2-year-long water vapor isotopic record monitored on this site. We show that the vapor isotopic composition largely follows the vapor mixing ratio, as expected in marine boundary layers. However, we evidence 11 cold front periods of a few days where there is a strong loss of correlation between water vapor δ18O and mixing ratio. These periods are associated with abrupt negative excursions of water vapor δ18Ο, often occurring toward the end of precipitation events. Six of these events show a decrease in gaseous elemental mercury suggesting subsidence of air from higher altitude. Accurately representing the water isotopic signal during these cold fronts is a real challenge for the atmospheric components of Earth System models equipped with water isotopes. While the ECHAM6-wiso model was able to reproduce most of the sharp negative water vapor δ18O excursions, the LMDZ-iso model at 2° (3°) resolution was only able to reproduce 7 (1) of the negative excursions. Based on a detail model-data comparison, we conclude that the most plausible explanations for such isotopic excursions are rain-vapor interactions associated with subsidence at the rear of a precipitation event. [ABSTRACT FROM AUTHOR]

The Pierre Auger Observatory (PAO) and Telescope Array (TA) collaborations report significant differences in the observed energy spectra of ultra-high-energy cosmic rays (UHECRs) above 30 EeV. In this work we present a joint fit of TA and PAO data using the rigidity-dependent maximum energy model, including a full marginalization over all relevant parameters. We test two possible scenarios to explain these differences. One is that they are due to complex energy-dependent experimental systematics; the other is the presence of a local astrophysical source in the Northern Hemisphere, which is only visible by the TA experiment. We show that the astrophysical and systematic scenarios improve the explanation of the data equally well, compared to the scenario where both experiments observe the same UHECR flux from a cosmological source distribution and have energy-independent systematics. We test different mass compositions emitted from the local source and conclude that the data are best described by a source lying at a distance below 26 Mpc that emits cosmic rays dominated by the silicon mass group. We also discuss possible source candidates and the possible role of the putative local UHECR source in the observed TA anisotropy and in the differences in TA spectral data from different decl. bands. [ABSTRACT FROM AUTHOR]

The Western Channel Observatory (WCO) comprises a series of pelagic, benthic and atmospheric sampling sites within 40 km of Plymouth UK, which have been sampled by the Plymouth Institutes on a regular basis since 1903. This longevity of recording and the high frequency of observations provide a unique combination of data; for example temperature data were first collected in 1903 and the reference station L4 has been sampled on a weekly basis since 1988 where nearly 400 planktonic taxa have been enumerated. While the component datasets have been archived, here we provide the first summary database bringing together a wide suite of the observations. This provides monthly average values of some of the key pelagic and benthic measurements for the inshore site L4 (50° 15.00' N, 4° 13.02' W approx depth 55 m), the offshore site E1 (50° 02.00' N, 4° 22.00' W approx depth 75 m) and the intermediate L5 site (50° 10.80' N 4° 18.00' W approx depth 58 m. In brief, the data include: water temperature (from 1903); macronutrients (from 1934); dissolved inorganic carbon and total alkalinity (from 2008); methane and nitrous oxide (from 2011); chlorophyll a (from 1992); HPLC-derived pigments (from 1999); <20 µm plankton by flow cytometry including bacteria (8 functional groups from 2007); phytoplankton by microscopy (6 functional groups from 1992); microplankton and mesozooplankton from FlowCam (6 groups from 2012), Noctiluca sp. dinoflagellate (from 1997); mesozooplankton by microscopy (8 groups from 1988); Calanus helgolandicus egg production rates (from 1992); fish larvae from Young Fish Trawl survey (4 groups from 1924); benthic macrofauna (4 groups from 2008); demersal fish (19 families from 2008); blue shark, Prionace glauca (from 1958); 16S alpha diversity for sediment and water column (from 2012). These data have varying coverage in time and depth resolution. The metadata tables describe each data set, provide pointers to the source data and other related Western Channel Observatory data sets and outputs not compiled here. We provide summaries of the main trends in seasonality and some major, climate related shifts that have been revealed over the last century. The data are available from Data Archive for Seabed Species and Habitats (DASSH) via the link http://doi.org/10.17031/645110fb81749 (McEvoy and Atkinson, 2023). Making the data fully accessible and including units of both abundance and biomass will stimulate a variety of uptakes. These may include uses as an educational resource for projects, for models and budgets or for analysis of seasonality and long-term change in a coupled benthic-pelagic system and for supporting UK and Northeast Atlantic policy and management. [ABSTRACT FROM AUTHOR]

The space-based gravitational wave observatory mission consists of three drag-free controlled spacecraft, which form an equilateral triangle configuration. Due to the injection error, the configuration will deviate from the originally designed one, and the injection configuration cannot keep stability for a long term, which will affect the performance of the gravitational wave detection. In this study, we propose a method for reconfiguration using multiple-revolution Lambert solutions. In addition, assuming that the real-time data of spacecraft's motion states can be obtained with high accuracy and the propulsion system can ensure the magnitude and accuracy of maneuvers, and taking the cost of reconfiguration and configuration stability requirements into account, a novel method of redesigning configuration based on differential evolution algorithm is proposed. Finally, the numerical simulations show that the redesigned configuration not only can reduce the maneuver cost significantly, but also can meet the requirements of long-term stability requirements. [ABSTRACT FROM AUTHOR]

Modeling the interactions between atmosphere and soil at a forest site remains a challenging task. Using tower measurements from the Amazon Tall Tower Observatory (ATTO) in the rainforest, we evaluated the performance of the land surface model JSBACH, focusing especially on processes influenced by the forest canopy. As a first step, we analyzed whether high-resolution global reanalysis data sets are suitable to be used as land surface model forcing. Namely, we used data from the fifth-generation ECMWF atmospheric reanalysis of the global climate (ERA5) and the Modern-Era Retrospective analysis for Research and Applications version 2 (MERRA-2). Comparing 5 years of ATTO measurements to near-surface reanalysis data, we found a substantial underestimation of wind speeds by about 1 m s -1. ERA5 captures monthly mean temperatures quite well but overestimates annual mean precipitation by 30 %. Contrarily, MERRA-2 overestimates monthly mean temperatures in the dry season (August–October) by more than 1 K, while mean precipitation biases are small. To test how much the choice of reanalysis data set and the reanalysis biases affect the results of the land surface model, we performed spin-up and model runs using either ERA5 or MERRA-2 and with and without a bias correction for precipitation and wind speed and compared the results. The choice of reanalysis data set results in large differences of up to 1.3 K for soil temperatures and 20 % for soil water content, which are non-negligible, especially in the first weeks after spin-up. Correcting wind speed and precipitation biases also notably changes the land surface model results – especially in the dry season. Based on these results, we constructed an optimized forcing data set using bias-corrected ERA5 data for the spin-up period and ATTO measurements for a model run of 2 years and compared the results to observations to identify model shortcomings. Generally, the shape of the soil water profile is not reproduced correctly, which might be related to a lack of vertical variability of soil properties or of the root density. The model also shows a positive soil temperature bias and overestimates the penetration depth of the diurnal cycle. To tackle this issue, potential improvements can be made by improving the processes related to the storage and vertical transport of energy. For instance, incorporating a distinct canopy layer into the model could be a viable solution. [ABSTRACT FROM AUTHOR]

Atmospheric gaseous elemental mercury (GEM) concentrations in the Arctic exhibit a clear summertime maximum, while the origin of this peak is still a matter of debate in the community. Based on summertime observations during the Multidisciplinary drifting Observatory for the Study of Arctic Climate (MOSAiC) expedition and a modeling approach, we further investigate the sources of atmospheric Hg in the central Arctic. Simulations with a generalized additive model (GAM) show that long-range transport of anthropogenic and terrestrial Hg from lower latitudes is a minor contribution (~2%), and more than 50% of the explained GEM variability is caused by oceanic evasion. A potential source contribution function (PSCF) analysis further shows that oceanic evasion is not significant throughout the ice-covered central Arctic Ocean but mainly occurs in the Marginal Ice Zone (MIZ) due to the specific environmental conditions in that region. Our results suggest that this regional process could be the leading contributor to the observed summertime GEM maximum. In the context of rapid Arctic warming and the observed increase in width of the MIZ, oceanic Hg evasion may become more significant and strengthen the role of the central Arctic Ocean as a summertime source of atmospheric Hg. Oceanic evasion, which mainly occurs in the Marginal Ice Zone, is the main cause of the summertime maximum of gaseous elemental mercury in the central Arctic Ocean [ABSTRACT FROM AUTHOR]

We describe a mode for two-dimensional UHF (445 MHz) radar observations of F-region irregularities using the 14-panel version of the advanced modular incoherent scatter radar (AMISR-14). We also present and discuss examples of observations made by this mode. AMISR-14 is installed at the Jicamarca Radio Observatory (JRO, 11.95°S, 76.87°W, ~ 0.5° dip latitude) in Peru and, therefore, allows studies of ionospheric irregularities at the magnetic equator. The new mode takes advantage of the electronic beam-steering capability of the system to scan the equatorial F-region in the east–west direction. Therefore, it produces two-dimensional views of the spatial distribution of sub-meter field-aligned density irregularities in the magnetic equatorial plane. The scans have a temporal resolution of 20 s and allow observations over a zonal distance of approximately 400 km at main F-region heights. While the system has a lower angular and range resolution than interferometric in-beam VHF radar imaging observations available at Jicamarca, it allows a wider field-of-view than that allowed with the VHF system. Here, we describe the mode, and present and discuss examples of observations made with the system. We also discuss implications of these observations for studies of ESF at the JRO. Keypoints: A new mode for two dimensional observations of F-region irregularities in the magnetic equatorial plane using AMISR-14 is described. Examples of observations are presented and illustrate the ability of the system to capture the genesis, evolution, and decay of sub-meter ESF irregularities. The benefits of the new mode are highlighted and implications of the new observations for studies and better understanding of ESF are discussed. [ABSTRACT FROM AUTHOR]

We use data from the Atmospheric Imaging Assembly (AIA) telescope on the Solar Dynamics Observatory (SDO) spacecraft in the 171 Å channel to investigate the spatial distribution of low-energy flares (nanoflashes). We have studied two periods: 05/20/2019 from 1200 UT to 1300 UT and 05/10/2020 from 1200 UT to 1300 UT. In total, we found 87 974 nanoflares with an average formation rate of 6.0 × 10‒21 cm–2 s–1. For solar latitudes from 0° up to 50° the nanoflare formation rate is approximately uniform with a standard deviation of about 25%. We have found an asymmetry in the rate of formation of nanoflares in the southern and northern hemispheres of the Sun: the rate of formation of nanoflares in the southern hemisphere was 34–42% higher than in the northern one. During this period, the same asymmetry was also observed for ordinary flares. We also found a weak dependence of the nanoflare formation rate on the solar cycle: the number of nanoflares increases with higher solar activity. [ABSTRACT FROM AUTHOR]

The results of analysis of measurements of the amplitudes and phases of the GQD (19.6 kHz) and GBZ (22.1 kHz) VLF transmitter signals at the Mikhnevo IGD observatory are presented to estimate of the influence of the solar flares X 2.2 and X 1.5 on June 10, 2014 on the electron concentration in the lower ionosphere. The flux of the X-rays in the more rigid spectral ranges of 0.01‒0.3, 0.01‒0.26, and 0.01‒0.22 nm was calculated based on the measurements of the X-ray emissions at wavelengths of 0.05–0.4 nm and 0.1–0.8 nm at the GOES satellite. That allowed us to find the ionization rate and the emission spectrum ranges that influenced the electron concentration dynamics most strongly. It is shown that if the duration of the forefront is substantially less than the characteristic recombination time, the change in the electron concentration profile in the lower ionosphere on the flare front is related linearly to the changes in the X-ray emission flux. [ABSTRACT FROM AUTHOR]

The spatial–temporal distributions of nitrogen dioxide (NO2) in a rural area of Tiber valley were evaluated over one year (March 2022–February 2023) using remote sensing and in situ measurements. Surface concentration monitoring was conducted using a Pandora-2s spectrometer and a chemiluminescence analyzer operated at the Liberti Observatory (CNR-IIA). In spring, when the growing season and the agricultural activities increase, NO2 peaks were detectable by the Pandora but not by the in situ analyzer. The tropospheric Pandora and TROPOMI VCD products showed similar temporal patterns as those of the analyzer at the Observatory. High TROPOMI VCD levels in spring were detected at the Observatory and at six sites selected as representative of rural, residential, and industrial environments. WRF simulations found that high pollution events, observed by the Pandora and analyzer, occurred in calm wind conditions, favouring the accumulation of NO2 locally emitted. The complementary dataset provided by remote sensing and in situ techniques efficiently captured the spatial–temporal NO2 variability in a rural site exposed to low emission sources, thus supporting future decisional policies and actions. [ABSTRACT FROM AUTHOR]

In 1639, the German naturalist Georg Marcgraf established the first astronomical observatory in the Americas, located in Recife (Brazil). There, he made the first daily systematic meteorological observations of wind direction, precipitation, fog, and thunder and lightning from 1640 to 1642. We outline the circumstances that led to this observatory being established and analyze the observations. The range of values obtained from all the variables recorded by Marcgraf corresponds well with Recife's current climate. However, wetter-than-normal conditions were recorded during 1640, while anomalous concentrations of foggy days occurred from May to December 1641. We hypothesize that these anomalous record foggy days could be associated with the highly explosive eruptions of the Komagatake and Parker volcanoes, both in 1640. [ABSTRACT FROM AUTHOR]

The Osservatorio Vesuviano (OV) is the oldest volcano observatory in the world having been founded in 1841 by the King of the Two Sicilies Ferdinand II of Bourbon. The historical building, located on the western slope of Vesuvius, hosts a museum with important collections of remarkable scientific, historical and artistic value, including pioneering instruments, rocks and minerals, photos and films of Vesuvius' eruptions and many other memorabilia. Visitors discover this heritage through permanent exhibitions, and a multimedia path, across the history of Vesuvius and the origin of volcano monitoring. The museum lies within the protected area of Vesuvius National Park, established in 1995. The park's network of trails allows visitors to enjoy the geodiversity of Somma-Vesuvius, whose activity has been intertwined with that of humans from Bronze Age to modern times, as testified by many important archaeological sites around the volcano, the most famous among them being Pompeii and Herculaneum. The "Grand Tour" was the cultural journey undertaken in the eighteenth century by European intellectuals, in which Italy was an essential destination; we consider the Museum of the OV an essential stop in a modern "Vesuvius Grand Tour", a journey through the geological and archaeological heritage of Vesuvius territory. Since 2001, the OV is the Naples section of the Istituto Nazionale di Geofisica e Vulcanologia (INGV), which is primarily tasked with monitoring the three active volcanoes of the Neapolitan area—Vesuvius, Campi Flegrei and Ischia—through an advanced surveillance network. [ABSTRACT FROM AUTHOR]