Astronomy and Astrophysics, volume 620A, 166-166 (2018/12-1)
Stellar systems in the direction of Pegasus I. I. Low surface brightness galaxies.
GONZALEZ N.M., SMITH CASTELLI A.V., FAIFER F.R., ESCUDERO C.G. and CELLONE S.A.
Abstract (from CDS):
Context. In spite of the numerous studies of low-luminosity galaxies in different environments, there is still no consensus about their formation scenario. In particular, a large number of galaxies displaying extremely low surface brightnesses have been detected in recent years and the nature of these objects is still under discussion.
Aims. In order to enlarge the sample of known low-surface-brightness (LSB) galaxies and to try to provide clues about their nature, we report the detection of eight such objects (µeff,g'~=27mag/arcsec2) towards the group of galaxies Pegasus I. They are located, in projection, within a radius of ∼200 kpc in the very center of Pegasus I, close to the dominant elliptical galaxies NGC 7619 and NGC 7626.
Methods. We analyzed deep, high-quality GEMINI-GMOS images with ELLIPSE within IRAF in order to obtain their brightness profiles and structural parameters. We also fit Sersic functions to these profiles in order to compare their properties with those of typical early-type galaxies.
Results. Assuming that these galaxies are at the distance of Pegasus I, we have found that their sizes are intermediate among similar objects reported in the literature. In particular, we found that three of these galaxies can be classified as ultra-diffuse galaxies and a fourth one displays a nucleus. The eight new LSB galaxies show significant color dispersion around the extrapolation towards faint luminosities of the color-magnitude relation defined by typical early-type galaxies. In addition, they display values of the Sersic index below 1 (concave brightness profiles in linear scale), in agreement with values obtained for LSB galaxies in other environments.
Conclusions. We show that there seems to be a bias effect in the size distributions of the detected LSBs in different environments, in the sense that more distant groups/clusters lack small reff objects, while large systems are not found in the Local Group and nearby environments. While there may be an actual shortage of large LSB galaxies in low-density environments like the Local Group, the non-detection of small (and faint) systems at large distances is clearly a selection effect. As an example, LSB galaxies with similar sizes to those of the satellites of Andromeda in the Local Group will be certainly missed in a visual identification at the distance of Pegasus I.
© ESO 2018
methods: observational - techniques: photometric - galaxies: groups: individual: Pegasus I - galaxies: star clusters: general - galaxies: dwarf
Tables 3-4: [GSF2018] PEG JHHMMSS+DDMMSS.s N=8.
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