News type: Research news

  • News
    The adequacy of stellar evolution models for the interpretation of the color-magnitude diagrams of resolved stellar populations
    Work by C. Gallart, M. Zoccali y A. Aparicio has been published in the Annual Review of Astronomy and Astrophysics. The article reviews current knowledge about...
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    The central molecular gas structure in LINERs with low luminosity AGN: evidence for gradual disappearance of the torus.
    We present observations of the molecular gas in the nuclear environment of three prototypical low luminosity AGN (LLAGN), based on VLT/SINFONI AO-assisted...
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    The changing-look optical wind of the flaring X-ray transient Swift J1858.6-0814
    The large amount of mass and angular momentum carried by disc winds makes them key processes to understand accretion onto compact objects, such as black holes...
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    The chemistry of Planetary Nebulae (PNe) and HII regions in the Local Group
    Chemical abundances have been measured of PNe and HII regions in Sex A and Sex B, two galaxies located on the outskirts of the Local Group. These PNe are the...
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    The cosmic assembly of stellar haloes in massive early-type Galaxies
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    The dark side of the fluffiest galaxies
    Ultra diffuse galaxies (UDGs) have the sizes of giants but the luminosities of dwarfs. A key to understanding their origins comes from their total masses, but...
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    The distribucion of electron densiy in the HII regions of the galaxies M51 and NGC 4449
    Using images of the Advanced Camera for Surveys" of the Hubble SpaceTelescope we have analyzed the global physical parameters of thepopulations of HII regions...
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    The distribution of gas and star formation in M 81.
    In this work we present the first complete CO J=3-2 map of M 81, observed as part of the Nearby Galaxies Legacy Survey. M 81 is a nearby spiral galaxy (3.64 Mpc...
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    The double-degenerate, super-Chandrasekhar nucleus of the planetary nebula Henize 2–428.
    The planetary nebula (PN) stage is the ultimate fate of stars with mass 1 to 8 solar masses (M⊙). The origin of their complex morphologies is poorly understood...