We present the preliminary results of the sustainability survey carried out by the ``SEA Cero CO 2'' working group among Spanish astronomers. The survey aimed at studying, within a limited scope, the carbon footprint of astronomical research carried out in Spain, as well as to collect the opinion of Spanish astronomers about possible ways to reduce

Context. From a long-term Doppler monitoring campaign of 373 giant stars, we have identified ten giants with periodic radial velocity variations that are challenging to associate with planets. Similar cases in the literature are attributed to poorly understood intrinsic processes. Aims. Our goal is to confirm or refute the presence of planets

Aims. We analyze the clustering of galaxy clusters in a large contiguous sample, the Constrain Dark Energy with X-ray (CODEX) sample. We construct a likelihood for cosmological parameters by comparing the measured clustering signal and a theoretical prediction, and use this to obtain parameter constraints. Methods. We measured the three multipole

Chlorine (Cl) is a chemical element of the group of the halogens and is between the 17th and the 20th most abundant elements in the Solar System. It is thought to be produced from the capture of a proton or neutron by specific alpha-element isotopes during both hydrostatic and explosive oxygen burning, though some contribution may come from Type Ia

Planetary NebulAE(PNe) are known to host an energetic radiation environment that does not avoid the simultaneous presence of different types of molecules and single atoms. For this reason, PNe appear to be a unique laboratory where simple and complex molecules coexist. We will present our recent very sensitive and high-resolution mm observations of

Massive stars play a pivotal role in shaping the Universe. However, comparisons between observational data and theoretical models of massive stars have given rise to long-standing and new discrepancies that have questioned our understanding of these objects. A main uncertainty arises from the overdensity of B-type supergiants (BSGs) located beyond