Dennis Edward Hyde, Letícia Pereira Alves, Daniel Rodrigues Costa Mello
et al.
This article presents the National Parks Astrotourism Potential Index (IASTRO), an innovative tool to evaluate and compare the potential for astro tourism in the 75 Brazilian national parks. IASTRO combines three crucial parameters: night sky quality, open sky probability, and tourism infrastructure, which encompasses the presence of guides and the availability of different experiences of overnight stays. The detailed methodology for data collection and IASTRO calculation is described, including the weighting of parameters, with night sky quality receiving greater weight for its fundamental importance for celestial observation. The results reveal a diverse distribution of IASTRO among the parks, highlighting those located in the Cerrado and Caatinga biomes, which present more favorable night sky and climatological conditions. The in-depth discussion explores the relationship between IASTRO and other factors, such as the number of visitors and the characteristics of the biomes, revealing an untapped potential for astro tourism in many national parks. The study also highlights the importance of tourism infrastructure and simulates how improvements in this aspect can boost astro tourism potential in various parks. The final considerations emphasize IASTRO as a valuable tool for protected area management and for the formulation of public policies, promoting the preservation of the starry sky and the development of astro tourism in a sustainable way. The article concludes that Brazil has enormous potential to become a world-class astro tourism destination, with its national parks offering exceptional conditions for celestial observation and connection with nature. This pioneering study contributes to the field of ecotourism by providing a comprehensive and innovative index to assess the astro tourism potential in national parks. IASTRO can be used by park managers, researchers, tourists, astronomy enthusiasts and policy makers to identify and prioritize parks with greater potential for this activity, assisting in the planning of actions and investments that promote the development of astro tourism in Brazil. In summary, the article presents an innovative index to assess the astro tourism potential in Brazilian national parks, highlighting the importance of night sky quality, open sky probability, and tourism infrastructure. The study reveals an untapped potential for astro tourism in many parks and highlights the importance of investments in tourism infrastructure to boost this activity. IASTRO is presented as a valuable tool for protected area management and for the formulation of public policies, aiming at the sustainable development of astro tourism in Brazil.
Baptiste Cecconi, Laura Debisschop, Sébastien Derrière
et al.
The astronomy communities are widely recognised as mature communities for their open science practices. However, while their data ecosystems are rather advanced and permit efficient data interoperability, there are still gaps between these ecosystems. Semantic artefacts (SAs) -- e.g., ontologies, thesauri, vocabularies or metadata schemas -- are a means to bridge that gap as they allow to semantically described the data and map the underlying concepts. The increasing use of SAs in astronomy presents challenges in description, selection, evaluation, trust, and mappings. The landscape remains fragmented, with SAs scattered across various registries in diverse formats and structures -- not yet fully developed or encoded with rich semantic web standards like OWL or SKOS -- and often with overlapping scopes. Enhancing data semantic interoperability requires common platforms to catalog, align, and facilitate the sharing of FAIR (Findable, Accessible, Interoperable and Reusable) SAs. In the frame of the FAIR-IMPACT project, we prototyped a SA catalogue for astronomy, heliophysics and planetary sciences. This exercise resulted in improved vocabulary and ontology management in the communities, and is now paving the way for better interdisciplinary data discovery and reuse. This article presents current practices in our discipline, reviews candidate SAs for such a catalogue, presents driving use cases and the perspective of a real production service for the astronomy community based on the OntoPortal technology, that will be called OntoPortal-Astro.
Savita Mathur, Angela R. G. Santos, Zachary R. Claytor
et al.
There is now a large sample of stars observed by the Kepler satellite with measured rotation periods and photometric activity index $S_{\rm ph}$. We use this data, in conjunction with stellar interiors models, to explore the interplay of magnetism, rotation, and convection. Stellar activity proxies other than $S_{\rm ph}$ are correlated with the Rossby number, $Ro$, or ratio of rotation period to convective overturn timescale. We compute the latter using the Yale Rotating Evolution Code stellar models. We observe different $S_{\rm ph}$-$Ro$ relationships for different stellar spectral types. Though the overall trend of decreasing magnetic activity versus $Ro$ is recovered, we find a localized dip in $S_{\rm ph}$ around $Ro/Ro_{\odot} \sim$\,0.3 for the G and K dwarfs. F dwarfs show little to no dependence of $S_{\rm ph}$ on $Ro$ due to their shallow convective zones; further accentuated as $T_{\rm eff}$ increases. The dip in activity for the G and K dwarfs corresponds to the intermediate rotation period gap, suggesting that the dip in $S_{\rm ph}$ could be associated with the redistribution of angular momentum between the core and convective envelope inside stars. For G-type stars, we observe enhanced magnetic activity above solar $Ro$. Compared to other Sun-like stars with similar effective temperature and metallicity, we find that the Sun's current level of magnetic activity is comparable to its peers and lies near the transition to increasing magnetic activity at high $Ro$. We confirm that metal-rich stars have a systematically larger $S_{\rm ph}$ level than metal-poor stars, which is likely a consequence of their deeper convective zones.
Desde tempos imemoriais que os seres humanos olham e tentam perceber o céu. Não sabiam bem o que eram aquelas luzes a brilhar e que se movimentavam de forma repetida. Hoje em dia parece muito fácil, mas demorou muito tempo a consolidar-se a imagem que atualmente temos do céu. E sobretudo, a sabermos qual era a sua composição química. Este artigo pretende fazer uma revisão de divulgação do conhecimento químico que temos do céu e mostrar que as informações químicas são indissociáveis do entendimento que temos hoje do universo.
Neste artigo explicamos o que são as ondas gravitacionais previstas pela teoria da relatividade geral de Einstein, falamos de suas fontes astrofísicas e cosmológicas e dos detectores que foram utilizados para a sua busca. Completamos o artigo com a menção aos detectores futuros, que estão sendo projetados para dar uma nova dimensão à astronomia de ondas gravitacionais e à astronomia multimensageira envolvendo ondas gravitacionais.
Discuto alguns aspectos do chamado “paradigma da luz cansada”, o qual representa uma das possíveis explicações para a dependência do desvio espectral para o vermelho de uma fonte cósmica distante com a sua distância até o observador. A mais popular representação fenomenológica do paradigma é apresentada em algum detalhe. Além disso, sendo o processo físico responsável pelo hipotético fenômeno ainda desconhecido, apresento também uma sugestão para a sua descoberta.
Building a large sample of kiloparsec (kpc)-scale dual active galactic nuclei (AGNs) amongst merging galaxies is of vital importance to understand the co-evolution between host galaxies and their central super massive black holes (SMBHs). Doing so, with just such a sample, we have developed an innovative method of systematically searching and identifying dual AGNs of amongst kpc scale merging galaxies and selected 222 candidates at redshifts $\leqslant$ 0.25. All the selected candidates have FIRST radio detection and at least one of two cores previously revealed as AGN spectroscopically. We report the first results from A SysTematic seaRch fOr Dual Agns in meRgINg Galaxies (ASTRO-DARING), which consist of spatially resolved long-slit spectroscopic observations of 41 targets selected from our merging galaxies sample carried out between November 2014 and February 2017, using the Yunnan Faint Object Spectrograph and Camera (YFOSC) mounted on the 2.4 meter telescope in Lijiang of Yunnan Observatories. Of these 16 are likely dual AGNs and 15 are newly identified. The efficiency of ASTRO-DARING is thus nearly 40 per cent. With this method, we plan to build the first even sample of more than 50 dual AGNs constructed using a consistent approach. Further analysis of the dual AGN sample shall provide vital clues for understanding the co-evolution of galaxies and SMBHs.
Apresentamos aqui uma breve e não-técnica introdução à teoria da relatividade geral, começando pelo conceito de espaço-tempo, passando pelo princípio de equivalência, e chegando nos testes clássicos que consagraram a teoria como uma das mais bonitas e bem-sucedidas da física.
Sophie C. Dubber, Annelies Mortier, Ken Rice
et al.
We present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely-populated category of exoplanet. We use {\it Kepler} light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine the semi-amplitude of the stellar reflex motion and, hence, the planet mass. For PH-2b we recover a 3.5-$σ$ mass estimate of $M_p = 109^{+30}_{-32}$ M$_\oplus$ and a radius of $R_p = 9.49\pm0.16$ R$_\oplus$. This means that PH-2b has a Saturn-like bulk density and is the only planet of this type with an orbital period $P > 200$ days that orbits a single star. We find that Kepler-103b has a mass of $M_{\text{p,b}} = 11.7^{+4.31}_{-4.72}$ M$_{\oplus}$ and Kepler-103c has a mass of $M_{\text{p,c}} = 58.5^{+11.2}_{-11.4}$ M$_{\oplus}$. These are 2.5$σ$ and 5$σ$ results, respectively. With radii of $R_{\text{p,b}} = 3.49^{+0.06}_{-0.05}$ R$_\oplus$, and $R_{\text{p,c}} = 5.45^{+0.18}_{-0.17}$ R$_\oplus$, these results suggest that Kepler-103b has a Neptune-like density, while Kepler-103c is one of the highest density planets with a period $P > 100$ days. By providing high-precision estimates for the masses of the long-period, intermediate-mass planets PH-2b and Kepler-103c, we increase the sample of long-period planets with known masses and radii, which will improve our understanding of the mass-radius relation across the full range of exoplanet masses and radii.
In general, modified gravity theories are modifications or extensions of Einstein's general relativity. Some of them give rise to additional scalar degrees of freedom in Nature. If these scalar fields exist and are light enough, they should cause a gravity-like fifth force that could, in principle, exceed gravity in its strength. However, there are tight constraints on fifth forces from Solar System-based tests. Screening mechanisms are popular means for avoiding these constraints by suppressing a fifth force in regions of high environmental mass density but allowing for phenomenologically interesting effects in environments of lower densities. In this thesis, scalar field models with screening mechanisms will be discussed and some astro- and quantum physical tests for their existence presented. At first, the impact of disformally coupled symmetrons on gravitational lensing by galaxies will be evaluated. Secondly, it will be shown how fluctuations of a chameleon scalar field induce the open dynamics of a quantum test particle. For this, tools from non-equilibrium quantum field theory will be introduced, developed and applied, and a quantum master equation derived.
X-ray spectra from cores of galaxy clusters can be strongly distorted by resonant scattering of line photons, affecting metal abundance and gas velocity measurements. We introduce simulated spectral models that take into account the resonant scattering effect, radial variations of thermodynamic properties of the hot gas, projection effects and small-scale isotropic gas motions. The key feature of the models is that all these effects are treated self-consistently for the whole spectrum, rather than for individual lines. The model spectra are publicly available and can be used for direct comparison with observed projected spectra. Comparison with the existing XMM-Newton and Chandra data of the Perseus Cluster shows that even though there is no strong evidence for the resonant scattering in Perseus, the low energy resolution of the X-ray CCDs is not sufficient to robustly distinguish spectral distortions due to the resonant scattering, different metal abundance profiles and different levels of gas turbulence. Future Astro-H data will resolve most of the problems we are facing with CCDs. With the help of our models, the resonant scattering analysis can be done self-consistently using the whole spectral information, constraining the level of gas turbulence already with a 100 ks observation with Astro-H.