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A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS |
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The Main Sequence at z ∼ 1.3 Contains a Sizable Fraction of Galaxies with Compact Star Formation Sizes: A New Population of Early Post-starbursts? |
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Strong Evidence of Anomalous Microwave Emission from the Flux Density Spectrum of M31 |
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A near-infrared study of the multiphase outflow in the type-2 quasar J1509+0434 |
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Spectral Distortions of the CMB as a Probe of Inflation, Recombination, Structure Formation and Particle Physics |
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First detection of oscillations in the Halo giant HD 122563: Validation of seismic scaling relations and new parameters |
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Lower atmosphere and pressure evolution on Pluto from ground-based stellar occultations, 1988-2016 |
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Polarization of changing-look quasars |
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The CARMENES search for exoplanets around M dwarfs. Different roads to radii and masses of the target stars |
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The CORALIE survey for southern extrasolar planets. XVIII. Three new massive planets and two low-mass brown dwarfs at greater than 5 AU separation |
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The Fornax 3D project: Thick disks in a cluster environment |
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Extended Main-sequence Turnoffs in the Double Cluster h and χ Persei: The Complex Role of Stellar Rotation |
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ALMA Reveals Potential Evidence for Spiral Arms, Bars, and Rings in High-redshift Submillimeter Galaxies |
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Optically Faint Massive Balmer Break Galaxies at z > 3 in the CANDELS/GOODS Fields |
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Qatar Exoplanet Survey: Qatar-8b, 9b, and 10b—A Hot Saturn and Two Hot Jupiters |
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Measurement of the extragalactic background light using MAGIC and Fermi-LAT gamma-ray observations of blazars up to z = 1 |
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AGB dust and gas ejecta in extremely metal-poor environments |
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Torus model properties of an ultra-hard X-ray selected sample of Seyfert galaxies |
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The evolutionary status of Cataclysmic Variables: eclipse modelling of 15 systems |
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UNIT project: Universe N-body simulations for the Investigation of Theoretical models from galaxy surveys |
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A distance of 13 Mpc resolves the claimed anomalies of the galaxy lacking dark matter |
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System initial mass function of the 25 Ori group from planetary-mass objects to intermediate/high-mass stars |
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