Le télescope spatial Hubble repère une galaxie ténue et diffuse

Le télescope spatial Hubble repère une galaxie ténue et diffuse
GAMA 526784

Le télescope spatial Hubble a capturé GAMA 526784, une galaxie ultra-diffuse qui apparaît comme une tache de lumière ténue sur cette image. Cet objet vaporeux se trouve dans la constellation de l’Hydre, à environ quatre milliards d’années-lumière de la Terre. Les galaxies ultra-diffuses telles que GAMA 526784 présentent un certain nombre de particularités. Crédit : ESA/Hubble & ; NASA, R. van der Burg, Remerciements : L. Shatz

Dans cette image du ;” data-gt-translate-attributes=”[{” attribute=””>NASA/ESA Hubble Space Telescope, the ultra-diffuse galaxy GAMA 526784 appears as a hazy patch of light. This wispy object is located in the constellation Hydra, approximately four billion light-years away from Earth.

Ultra-diffuse galaxies such as GAMA 526784 have a number of peculiarities. For example, their dark matter abundance can be either extremely low or extremely high — ultra-diffuse galaxies have been observed with an almost complete lack of dark matter, whereas others are comprised of almost nothing but dark matter. Another peculiarity of this class of galaxies is their unusual abundance of bright globular clusters, something not observed in other types of galaxies.

Hubble captured GAMA 526784 with the Advanced Camera for Surveys (ACS), which was installed in 2002 by astronauts during Hubble Servicing Mission 3B. Since then, the instrument has played a pivotal role in some of Hubble’s most impressive scientific results, including capturing the Hubble Ultra Deep Field. The ACS has also photographed Pluto in advance of the New Horizon mission, observed gargantuan gravitational lenses, and found fully formed galaxies in the early Universe.

This image comes from a set of Hubble observations designed to shed light on the properties of ultra-diffuse galaxies. Hubble’s keen vision allowed astronomers to study GAMA 526784 in high resolution at ultraviolet wavelengths, helping to gauge the sizes and ages of the compact star-forming regions studding the galaxy.

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