There are some networks of SQM photometers that provide measures of the night sky brightness every night. The analysis of the data provided by the photometers allows the researchers to monitor the nightly, monthly and yearly evolution of the NSB and the relationship with light sources of pollution in intensity and distance. The photometers that are

Originally thought to explore the high redshift Universe, the extreme depth of the Frontier Fields survey provides also an excellent opportunity to explore with unprecedented detail the faintest component of the galaxy clusters: their intra-cluster light (ICL). In this contribution, we will show our analysis of the ICL of the cluster Abell 2744

We investigate the influence of interactions on the star formation by studying a sample of almost 1500 of the nearest galaxies, all within a distance of 40 Mpc. We define the massive star formation rate (SFR), as measured from far-IR emission, and the specific star formation rate (SSFR), which is the former quantity normalised by the stellar mass

We present high spatial resolution (≈ 60–90 mas) images of the molecular hydrogen emission in the planetary nebula (PN) NGC 2346. The data were acquired during the system verification of the Gemini Multi-conjugate Adaptive Optics System + Gemini South Adaptive Optics Imager. At the distance of NGC 2346, 700 pc, the physical resolution corresponds

We report contributions to cosmic infrared background (CIB) intensities originating from known galaxies and their faint companions at submillimeter wavelengths. Using the publicly available UltraVISTA catalog and maps at 250, 350, and 500 μm from the Herschel Multi-tiered Extragalactic Survey, we perform a novel measurement that exploits the fact

We have observed a sample of 12 interacting galaxies using the Fabry-Perot interferometer GHαFaS (Galaxy Hα Fabry-Perot system) on the 4.2m William Herschel Telescope (WHT) at the Observatorio del Roque de los Muchachos, La Palma, deriving maps in Hα surface brightness, velocity and velocity dispersion. We extracted the physical parameters (Hα