Eventos

About a decade ago, the upgrade from the classic Very Large Array into the EVLA, i.e. the Karl G. Jansky Very Large Array (VLA), made it possible to observe fainter radio continuum emission than ever before. The project Continuum Halos in Nearby Galaxies - an EVLA Survey (CHANG-ES, PI: J.

Polarimetry is a very important technique for understanding magnetic fields and high-energy processes in the Universe.

El jueves 27 de abril a las 12:00 CEST, el Cherenkov Telescope Array Observatory (CTAO) y el Instituto de Astrofísica de Andalucía (IAA-CSIC) celebrarán un evento gratuito y abierto para investigadores interesados en la Ciencia Abierta y posibles sinergias con el CTAO, así como para estudiantes d

The processes that explain the evolution of galaxies from the blue cloud to the red sequence are still under discussion.

During the last two decades, multiple observation techniques have enabled the study of exoplanet atmospheres, informing us about their chemical composition, thermal distribution and transport processes.

The angular size of a star is a critical factor in determining its basic properties. Together with the distance, it provides the physical diameter of the star which can be used to yield luminosity and mass estimates.

Gamma-ray emission produced by interactions of cosmic rays with interstellar matter and radiation fields is a probe of non-thermal particles in galaxies.

Active galactic nuclei (AGN) feedback is the effect that nuclear activity produces in the interstellar and circumgalactic medium of galaxies.

School visit

In their early stages, massive stars have a profound impact on their hosting cloud as reflected by signposts like shocks, bars and shells of swept material resulting from prominent stellar winds, or photo-ionized (HII) regions produced by energetic irradiance.

Accretion is vital for understanding the properties of a number of astrophysical objects, including massive young stars and black holes. For the former, accretion drives the stellar mass growth and multiplicity through gas fragmentation.

This talk will cover two distinct topics in progress, one programmatic and the other science: I will first discuss the ALMA Wideband Sensitivity Upgrade (WSU), and then I'll talk about ALMA followup of the highest redshift HI detection in the COSMOS HI Large Extragalactic Survey (CHILES) made wit

Thanks to ultra-precise space missions, we are living an era of big scientific discoveries in the stellar and planetary physics fields. PLATO will capitalise on the developments of successful past missions such as CoRoT, Kepler/K2, TESS and CHEOPS that studied stars and their planetary systems.

It is a posit of modern astrophysics that most massive galaxies host a super- massive black hole (millions to billions of times more massive than the Sun).  These black holes affect the evolution of galaxies well beyond their  gravitational sphere of influence (which does not extend wider than 1/

CARMENES is a dual (VIS: 550 to 950 nm; NIR: 950 to 1700 nm) high-resolution spectrograph installed at the 3.5 m telescope at the Calar Alto Observatory (CAHA, Almería, Spain). The NIR channel spectrograph uses the radial-velocity method for detecting exoplanets around low-mass stars.

Observational tests of strong field gravity are improving rapidly. This allows us to test whether the compact objects observed in the sky are truly black holes as described in general relativity or some other "exotic" objects.

The Milky Way nuclear star cluster (NSC) is located within the nuclear stellar disc (NSD) in the Galactic centre. The NSC and NSD are distinct structures of the Milky Way, but also connected to the larger Milky Way structures, e.g.

The ASTRI Collaboration is building at the Teide Astronomical Observatory in Tenerife an array of 9 small Cherenkov telescopes capable of observing with good flux sensitivity, energy and angular resolution the gamma-ray sky above an energy threshold of several hundreds of GeV.

In this talk I will present the design of the Integral Field Unit TARSIS, recently selected to be the next generation multi-object spectrograph for the 3.5m telescope at Calar Alto.