Onderzoeksvragen

In 2024 October, JWST observed a transit of Kepler-167 e, a Jupiter-analog planet on a 1000+ day orbit. These observations, recorded over a long baseline of nearly 60 hr, were designed to search for signatures of planetary oblateness and/or exomoons comparable to Ganymede. In this first in a series of studies analyzing these data, we…

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We present new Rosseland and Planck mean opacity tables relevant to the shallow interiors and atmospheres of giant planets. The tables span metallicities from 0.31 to 50 times solar, temperatures from $100 – 6000 rm K$, and pressures from $10^{-6} – 10^{5} rm bar$, thereby covering a wider parameter space than previous data sets. Our…

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Correctly interpreting JWST spectra of close-in exoplanets requires a measurement of the X-ray and ultraviolet light that the planets receive from their host stars. Here, we provide spectral energy distributions (SEDs) covering the range ≍5─1 × 107 Å for 20 transiting exoplanet host stars observed in JWST Cycle 1. The SEDs are constructed out of…

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The XRISM/Resolve microcalorimeter directly measured the gas velocities in the core of the Virgo Cluster, the closest example of active galactic nucleus (AGN) feedback in a cluster. This proximity allows us to resolve the kinematic impact of feedback on scales down to 5 kpc. Our spectral analysis reveals a high velocity dispersion of σv=262−38+45 km…

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Aims. The identification of active galactic nuclei (AGNs) is extremely important for understanding galaxy evolution and its connection with the assembly of supermassive black holes (SMBHs). With the advent of deep- and high-angular-resolution imaging surveys such as those conducted with the James Webb Space Telescope (JWST), it is now possible to identify galaxies with a…

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Using XRISM/Resolve 439 ks time-averaged spectra of the well-known Seyfert-1.5 active galactic nucleus (AGN) in NGC 3783, we investigated the nature of the Fe Kα emission line at 6.4 keV, the strongest and most common X-ray line observed in AGNs. Even the narrow component of the line is resolved with evident Fe Kα1 (6.404 keV)…

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