Context. To understand the structure and evolution of massive stars, systematic surveys of the Local Group galaxies have been undertaken, to find these objects...
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PublicaciónThe young stellar population of IC 1613. II. Physical properties of OB associations
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PublicaciónThe young stellar population of IC 1613. III. New O-type stars unveiled by GTC-OSIRIS
Context. Very low-metallicity massive stars are key to understanding the reionization epoch. Radiation-driven winds, chief agents in the evolution of massive...
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PublicaciónThermochemical properties of C60Br24
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PublicaciónThree-dimensional decomposition of galaxies with bulge and long bar
Context. Some observations indicate that the Milky Way has two inner components, a bulge and a long bar, which present a misalignment of Δα ≃ 20° that is...
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PublicaciónTidally induced velocity gradients in the Milky Way dwarf spheroidal satellites
We present a kinematic study of six dwarf spheroidal galaxies (dSph) satellites of the Milky Way (MW), namely Carina, Draco, Fornax, Sculptor, Sextans, and Ursa...
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PublicaciónTidally trapped pulsations in a close binary star system discovered by TESS
It has long been suspected that tidal forces in close binary stars could modify the orientation of the pulsation axis of the constituent stars. Such stars have...
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PublicaciónTime-domain Study of the Young Massive Cluster Westerlund 2 with the Hubble Space Telescope. I
Time-domain studies of pre-main-sequence (PMS) stars have long been used to investigate star properties during their early evolutionary phases and to trace the...
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PublicaciónTiming the Evolution of the Galactic Disk with NGC 6791: An Open Cluster with Peculiar High-α Chemistry as Seen by APOGEE
We utilize elemental-abundance information for Galactic red giant stars in five open clusters (NGC 7789, NGC 6819, M67, NGC 188, and NGC 6791) from the Apache...
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PublicaciónTo clump or not to clump. The impact of wind inhomogeneities on the optical and NIR spectroscopic analysis of massive OB stars
Context. Winds of massive stars have density inhomogeneities (clumping) that may affect the formation of spectral lines in different ways, depending on their...