The first image of a new gaseous component in a planetary nebula.
False color image of the planetary nebula NGC 6778. In blue, the emission associated with weak lines of ion O++ recombination, taken with the OSIRIS tunable filter blue instrument in the GTC. In green, emission of the same ion in the excited lines by coll
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Jorge García Rojas: jogarcia_ext [at] iac.es (jogarcia_ext[at]iac[dot]es)
This Saturday, 29 March 2025, the Instituto de Astrofísica de Canarias (IAC) was able to follow the partial solar eclipse from the Teide Observatory in Tenerife. Although subtle to the naked eye, this eclipse was used by the IAC's outreach team to raise awareness of the phenomenon among a group of people from the ‘Friends of the IAC’ programme and IAC staff. At the same time, an observation was also made from the IAC Headquarters in La Laguna, which could be seen live on the centre's YouTube channel. The eclipse began at 09:14 UT and ended at 10:56 UT, with its maximum at 10:03 UT. For just
Una delegación de la Universidad de La Laguna (ULL), encabezada por el rector Francisco García, ha realizado una visita institucional al Instituto de Astrofísica de Canarias (IAC), reforzando así el compromiso de colaboración y la estrecha relación que mantienen ambas instituciones, claves para el desarrollo científico y tecnológico de Canarias. El encuentro ha servido para revisar el estado del convenio que mantienen ambas instituciones y revisar algunas áreas de mejora para la renovación del mismo en materia de investigación, docencia y divulgación científica, además de aspectos
Dormant black holes in X-ray transients can be identified by the presence of broad Hα emission lines from quiescent accretion discs. Unfortunately, short-period cataclysmic variables can also produce broad Hα lines, especially when viewed at high inclinations, and are thus a major source of contamination. Here we compare the full width at half maximum (FWHM) and equivalent width (EW) of the Hα line in a sample of 20 quiescent black hole transients and 354 cataclysmic variables (305 from SDSS I to IV) with secure orbital periods (Porb) and find that: (1) FWHM and EW values decrease with Porb
