First detection of Hα emission from KELT-9 b's escaping atmosphere shows double-peaked profile with self-absorption, indicating vigorous outflow with mass-loss rate above 10^13 g/s.
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40 Pith papers cite this work, alongside 1,677 external citations. Polarity classification is still indexing.
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abstract
We present a new library of high-resolution synthetic spectra based on the stellar atmosphere code PHOENIX that can be used for a wide range of applications of spectral analysis and stellar parameter synthesis. The spherical mode of PHOENIX was used to create model atmospheres and to derive detailed synthetic stellar spectra from them. We present a new self-consistent way of describing micro-turbulence for our model atmospheres. The synthetic spectra cover the wavelength range from 500AA to 50.000AA with resolutions of R=500.000 in the optical and near IR, R=100.000 in the IR and a step size of 0.1AA in the UV. The parameter space covers 2.300K<=Teff<=12.000K, 0.0<=log(g)<=+6.0, -4.0<=[Fe/H]<=+1.0, and -0.2<=[alpha/Fe]<=+1.2. The library is a work in progress and we expect to extend it up to Teff=25.000 K.
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High-resolution M-band spectroscopy detects super-stellar SiO in TWA 5 B, implying no significant magnesium-silicate clouds and formation consistent with core accretion beyond the CO snowline or gravitational instability with solid enrichment.
JWST observations at 15 and 25.5 μm reveal a smooth, radially broad debris disk around γ Ophiuchi extending to 250 au, interpreted as a steady-state collisional cascade from a wide planetesimal belt with possible low-eccentricity planetary perturbation.
Spectroscopic members of the M92 stream yield a Milky Way bar pattern speed of 29.1 +0.7/-0.4 km s^{-1} kpc^{-1}.
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DESI-HVS1 is the first reported old, low-mass, metal-poor hypervelocity star candidate whose reconstructed orbit points to a Galactic Center origin.
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Direct pixel-level extraction of NIRISS spectra for WASP-18b followed by cross-correlation yields 4.4σ CO, 3.4σ H2O, and 7.8σ OH detections, with improved abundance constraints from subsequent retrievals.
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Accounting for stellar and orbital uncertainties shows that predicted eclipse depths for bare-rock models of rocky exoplanets carry substantial uncertainty comparable to measurements, establishing a fundamental precision limit for atmospheric and compositional inferences.
DSEE is a flow-based emulator that generates stellar evolution tracks and isochrones as probabilistic outputs from a single model trained on millions of simulations, enabling fast interpolation and uncertainty-aware analyses.
Water-hydrogen demixing occurs on warm sub-Neptunes with envelope metallicities of 150-700 times solar, including TOI-270 d, implying layered interiors and underestimated bulk metallicities when using fully-miscible models.
NGC 6791 has an age of 8.46 ± 0.66 Gyr, [Fe/H] = +0.280 ± 0.079, and other parameters that favor an inner-Galaxy origin followed by outward migration.
Introduces a reflection spectroscopy metric and uses KELT-9 injection-recovery tests to demonstrate that rotational line broadening from rapid stellar rotation and large misalignments must be included when assessing detectability of exoplanet reflected spectra.
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Negative Ca II IRT residual indices in FGK stars arise mainly because synthetic photospheric templates miss chromospheric structure and NLTE effects that deepen the observed cores.
Tier 1 Ariel spectra suffice for sub-1.5 dex constraints on H2O and CO2 in giant-planet atmospheres, with higher tiers providing only incremental gains and more molecules in select cases.
Pandora simulations recover stellar photospheric temperatures to ~30 K with no bias and reduce simple spot contamination from 100-1000 ppm to under 10 ppm, but complex spot geometries leave ~1000 ppm residuals.
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