US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia; Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; National Science Foundation [AST-1138766]; University of California at Santa Cruz; University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago, University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; European Research Council [FP7/291329]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union [240672, 291329, 306478]
The X-Ray Imaging and Spectroscopy Mission (XRISM) is a joint mission between the Japan Aerospace Exploration Agency (JAXA) and the National Aeronautics and Space Administration (NASA) in collaboration with the European Space Agency (ESA). In addition to the three space agencies, universities and research institutes from Japan, North America, and Europe have joined to contribute to developing satellite and onboard instruments, data-processing software, and the scientific observation program. XRISM is the successor to the ASTRO-H (Hitomi) mission, which ended prematurely in 2016. Its primary science goal is to examine astrophysical problems with precise, high-resolution X-ray spectroscopy. XRISM promises to discover new horizons in X-ray astronomy. It carries a 6 × 6 pixelized X-ray microcalorimeter on the focal plane of an X-ray mirror assembly (Resolve) and a co-aligned X-ray CCD camera (Xtend) that covers the same energy band over a large field of view. XRISM utilizes the Hitomi heritage, but all designs were reviewed. The attitude and orbit control system was improved in hardware and software. The spacecraft was launched from the JAXA Tanegashima Space Center on 2023 September 6 (UTC). During the in-orbit commissioning phase, the onboard components were activated. Although the gate valve protecting the Resolve sensor with a thin beryllium X-ray entrance window was not yet opened, scientific observation started in 2024 February with the planned performance verification observation program. The nominal observation program commenced with the following guest observation program beginning in 2024 September.
Buracos negros são objetos astrofísicos com propriedades muito particulares e fascinante. A partir de hipóteses genéricas, como a validade da teoria da relatividade geral, é possível provar teoremas que garantem a existência e propriedades desses objetos. Porém, apenas a observação e os experimentos são capazes de testar e verificar afirmações sobre fenômenos naturais. Seguindo este raciocínio, iremos desenvolver os conceitos básicos do que é um buraco negro, explicitar algumas de suas propriedades peculiares e por fim pontuar as observações que comprovaram a existência desses objetos compactos.
Desde a descoberta dos primeiros planetas fora do Sistema Solar, os chamados exoplanetas, na década de 90, mais de 5000 exoplanetas já foram descobertos, além dos milhares de candidatos sendo analisados. A descoberta de que existem sistemas planetários ao redor de outras estrelas, suscita naturalmente o questionamento sobre a possibilidade de que esses exoplanetas possam hospedar vida. É nesse contexto que ganha cada vez mais destaque a astrobiologia, área de pesquisa multidisciplinar que consiste no estudo da origem e evolução da vida no Universo. Neste artigo apresentaremos uma breve revisão sobre a procura por exoplanetas e os principais resultados interessantes do ponto de vista da astrobiologia até o momento. Iniciaremos pela definição do conceito de zona habitável estelar, região em torno de uma estrela na qual é, em princípio, possível manter água no estado líquido na superfície de um planeta rochoso. Comentaremos sobre a procura por vida no Sistema Solar, descreveremos os principais métodos de detecção de exoplanetas e apresentaremos exemplos de exoplanetas com particular interesse astrobiológico. Finalizaremos comentando sobre a procura pelas chamadas bioassinaturas e tecnoassinaturas, indicadores da existência de vida fora da Terra, e as missões presentes e futuras com maior potencial para novas descobertas na área da astrobiologia.
O Museu da Amazônia, o Musa, é um museu vivo, a céu aberto na Reserva Ducke, uma floresta primária na cidade de Manaus. Os ecossistemas, a fauna e a flora desta floresta, têm sido estudados há mais de cinquenta anos pelos pesquisadores do INPA. O Musa está empenhado em divulgar para o grande público os segredos desta floresta. Mostrar ao vivo, em seu habitat natural, as plantas, os pássaros, insetos, flores e polinizadores. É propósito do Musa em suas exposições valorizar os saberes das culturas indígenas que habitaram e ainda habitam as florestas amazônicas. No Musa são também cultivadas e divulgadas práticas agrícolas compatíveis com a presença da floresta, explorando assim modos antigos de compreender o mundo que propiciam o ‘viver juntos’ de culturas e saberes de humanos e não humanos.
The aim of this paper is to underline the most important aspects of advanced lung cancer therapy.The described trends and problems were presented during ASTRO 59 Conference in San Diego.
Abstract Spin-dipole (SD) nuclear matrix elements (NMEs) M ± ( SD 2 ) for unique first forbidden β ± 2 − → 0 + ground-state-to-ground-state transitions are studied by using effective microscopic two-nucleon interactions in realistic single-particle model spaces. The observed values of the NMEs M exp ± ( SD 2 ) are compared with the values of the single-quasiparticle NMEs M qp ± ( SD 2 ) without nucleon spin–isospin ( στ ) correlation and the QRPA NMEs M QRPA ± ( SD 2 ) with the στ correlation. The observed SD matrix elements are found to be reduced by the factor k ≈ 0.2 with respect to M qp ± ( SD 2 ) and by the factor k NM ≈ 0.5 with respect to M QRPA ± ( SD 2 ) . We then infer that the SD NME is reduced considerably partly by the nucleon στ correlations and partly by other non-nucleonic and nucleonic correlations which are not explicitly included in the QRPA. Impact of the found reduction factors on the magnitudes of the NMEs involved in neutrino-less double beta decays and astro-neutrino interactions are discussed.
The next generation X-ray observatory ASTRO-H will open up a new dimension in the study of galaxy clusters by achieving for the first time the spectral resolution required to measure velocities of the intracluster plasma, and extending at the same time the spectral coverage to energies well beyond 10 keV. This white paper provides an overview of the capabilities of ASTRO-H for exploring gas motions in galaxy clusters including their cosmological implications, the physics of AGN feedback, dynamics of cluster mergers as well as associated high-energy processes, chemical enrichment of the intracluster medium, and the nature of missing baryons and unidentified dark matter.
To realize a broadband, large-line-spacing astro-comb, suitable for wavelength calibration of astrophysical spectrographs, from a narrowband, femtosecond laser frequency comb ("source-comb"), one must integrate the source-comb with three additional components: (1) one or more filter cavities to multiply the source-comb's repetition rate and thus line spacing; (2) power amplifiers to boost the power of pulses from the filtered comb; and (3) highly nonlinear optical fiber to spectrally broaden the filtered and amplified narrowband frequency comb. In this paper we analyze the interplay of Fabry-Perot (FP) filter cavities with power amplifiers and nonlinear broadening fiber in the design of astro-combs optimized for radial-velocity (RV) calibration accuracy. We present analytic and numeric models and use them to evaluate a variety of FP filtering schemes (labeled as identical, co-prime, fraction-prime, and conjugate cavities), coupled to chirped-pulse amplification (CPA). We find that even a small nonlinear phase can reduce suppression of filtered comb lines, and increase RV error for spectrograph calibration. In general, filtering with two cavities prior to the CPA fiber amplifier outperforms an amplifier placed between the two cavities. In particular, filtering with conjugate cavities is able to provide 300 nm wavelength coverage. Such superior performance will facilitate the search for and characterization of Earth-like exoplanets, which requires <10 cm/s RV calibration error.