This section includes scientific and technological news from the IAC and its Observatories, as well as press releases on scientific and technological results, astronomical events, educational projects, outreach activities and institutional events.

  • Artist impression of WASP-189 and its planet. Credit: ESA.
    The CHEOPS mission measures the properties of one of the hottest and most extreme extrasolar planets

    CHEOPS, the new exoplanet mission of the European Space Agency (ESA), in which the Instituto de Astrofísica de Canarias (IAC) is participating, has observed a nearby planetary system which contains one of the hottest and most extreme extrasolar planets known until now: WASP-189 b. The result, the first from this mission, is being published in Astronomy & Astrophysics.

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  • Left and centre: Image of the region of the sky containing BOSS-EUVLG1, which stands out due to its blue colour. Credit: DESI Legacy Imaging Surveys. Right: Artist`s drawing of the burst of star formation in BOSS-EUVLG1, which contains a large number of young massive stars, and hardly any dust. Credit: Gabriel Pérez Díaz, SMM (IAC).
    Astronomers find the first galaxy whose ultraviolet luminosity is comparable to that of a quasar

    An international scientific team, led by researchers at the Centre for Astrobiology (CAB, CSIC-INTA) and with participation by the Instituto de Astrofísica de Canarias (IAC), have found the galaxy BOSS-EUVLG1. This is the galaxy with star formation but almost no dust, the most luminous of its type known up to now. It was found using observations made with the Gran Telescopio Canarias (GTC), at the Roque de los Muchachos Observatory, (Garafía, La Palma, Canary Islands), and with the ATACAMA Large Millimetre/submillimetre Array (ALMA), in Chile. The discovery was recently published in the

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  • Image illustrating the comparison between an active spiral galaxy (orange box) and its non-active twin (blue box). Credit: Gabriel Pérez Díaz, SMM (IAC).
    Large scale dynamical differences between active and non-active galaxies in the local Universe

    Observational evidences suggest a co-evolution of the central supermassive black holes and their host galaxies. In some of them, the black hole is ingesting the material surrounding it at a very high rate, emitting a large quantity of energy. In those cases we say that the galaxy has an active nucleus (AGN). Studying the mechanisms which control the relation between the active nucleus and the rest of the galaxy is essential to understand how these objects form and evolve, and to be able to throw light on this question we need to compare active and non-active galaxies. Here, we first identify

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  • Left: Colour image of the Large Magellanic Cloud, directly obtained from SMASH data. Right: Spatial distribution of the stellar mass fraction of stars younger (top) and older (bottom) than 2 billion years.
    Is the Large Magellanic Cloud spiral arm a stable structure?

    Some galaxies in the Universe display beautiful and appealing features known as "spiral arms". However, not all galaxies show spiral arms in the same manner. Among the variety of cases the Large Magellanic Cloud (LMC), a dwarf galaxy infalling towards the Milky Way, stands out. The LMC is the prototype of an entire family of galaxies, the Magellanic Spirals that are characterised by the presence of a barred stellar structure near their centres and a single spiral arm. Spiral patterns can form after galactic collisions, with subsequent star formation piling up in these arms. Nevertheless, we

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  • The spatial profiles of the observed and expected [O III] 4363 (orange and green, respectively), residuals from subtracting the expected collisional [O III] 4363 profile from the observed one (red), and the O II 4649 profile scaled (blue).
    The impact of strong recombination on temperature determination in planetary nebulae

    The long-standing difference in chemical abundances determined from optical recombination lines and collisionally excited lines raises questions about our understanding of atomic physics, as well as the assumptions made when determining physical conditions and chemical abundances in astrophysical nebulae. Here, we study the recombination contribution of [O III] 4363 and the validity of the line ratio [O III] 4363/4959 as a temperature diagnostic in planetary nebulae with a high abundance discrepancy. We derive a fit for the recombination coefficient of [O III] 4363 that takes into account

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  • Photogram from an animation which shows the ultrahot Neptune orbiting its star Credit: Ricardo Ramirez, University of Chile
    The first “ultrahot Neptune” is discovered

    A team of astronomers from the University of Chile, in collaboration with the Instituto de Astrofísica de Canarias (IAC) and the University of La Laguna (ULL), has discovered the first “ultrahot Neptune”, which is in orbita round the nearby star LTT 9779. The planet is so close to its star that its year lasts only 19 hours, and the star’s radiation heats the planet to more than 1,700 degrees centigrade. At those temperaturas, the heavy elements such as iron can be ionized in the atmosphere and molecules can dissociate, which makes this a unique laboratory for studying the chemistry of

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