1997), LSBGs are currently broadly defined as galaxies fainter than the surface brightness detection limit of the Sloan Digital Sky Survey for objects of small apparent size, that is approximately 24 mag arcsec −2 in the g band.īecause of their inherent low surface brightness, the detection of new LSBGs is severely limited by depth and data processing, where correct flat-fielding and sky subtraction are crucial steps. 1988 Ferguson & Sandage 1988 Bothun et al. Traditionally, defined as those galaxies fainter than the surface brightness of the night sky, μ V > 22 mag arcsec −2 ( Sandage & Binggeli 1984 Impey et al. 2020) and provide important observational constraints for the Λ-CDM cosmological paradigm (e.g., Moore et al. Due to their low baryon density, LSBGs are an excellent laboratory for testing galactic formation and evolution models ( Bothun et al. Low-surface-brightness galaxies (LSBGs) are the dominant population of the faint end of the galaxy luminosity function (e.g., Blanton et al. Key words: galaxies: dwarf / galaxies: photometry / galaxies: groups: individual: NGC 1052 Our work expands the catalog of LSBGs with new interesting objects and provides a detailed environmental context for the study of LSBGs in this region.

possible effects derived from tidal interactions are worthy of further study. We argue that this is suggestive of a substructure with similar radial velocity in sight projection, but at a closer distance, to which some of these apparently larger LSBGs could be associated. However, when exploring the distribution of effective radius, we find an overpopulation of large LSBGs ( r eff > 15 arcsec) located close to the line of sight of NGC 1052. The spatial correlation analysis between the LSBGs and this large-scale structure suggests their association.

After analyzing the distribution of galaxies with available spectroscopy, we identified a large-scale structure of approximately 1 Mpc that is well isolated in redshift space and centered on NGC 1052. We marginally detected a GC system in RCP 32, and argue that this LSBG is of great interest for follow-up observations given its extremely low baryon density. We explored the presence of globular clusters (GCs) in the LSBGs. This makes RCP 32 one of the lowest surface brightness galaxies ever detected through integrated photometry, located at just 10 arcmin from the extensively studied NGC 1052-DF2. Among all the newly detected objects, RCP 32 stands out with extreme properties: r eff = 23.0 arcsec and ⟨ μ g⟩ eff = 28.6 mag arcsec −2. We detected 42 LSBGs with r eff > 5 arcsec and μ g(0) > 24 mag arcsec −2, of which 20 are previously undetected objects. We used public deep photometric data from the Dark Energy Camera Legacy Survey to carry out a comprehensive search for LSBGs over a wide region of 6 × 6 degrees, equivalent to 2 × 2 Mpc at the distance of NGC 1052. The environment of NGC 1052 has recently attracted much attention because of the presence of low-surface-brightness galaxies (LSBGs) with apparently “exotic” properties, making it a region of high interest for the detection of new objects. Universidad Internacional de Valencia (VIU), Pintor Sorolla 21, 46002 Valencia, Spain Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, 18008 Granada, SpainĮ-mail: de Astrofísica de Canarias, c/ Vía Láctea s/n, 38205 La Laguna, Tenerife, Spainĭepartamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain Javier Román 1 ,2 ,3, Aida Castilla 4 and Javier Pascual-Granado 1

Astronomical objects: linking to databases.

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Mgs 5 lower brightness