The large-scale environment of low surface brightness galaxies

Abstract

Context. The exact formation scenarios and evolutionary processes that led to the existence of the class of low surface brightness galaxies (LSBs) have not yet been understood completely. There is evidence that the lack of star formation expected to be typical of LSBs can only occur if the LSBs were formed in low-density regions. Aims. Since the environment of LSBs has been studied before only on small scales (below 2 Mpc), a study of the galaxy content in the vicinity of LSB galaxies on larger scales could add a lot to our understanding of the origin of this galaxy class. Methods. We used the spectroscopic main galaxy sample of the SDSS DR4 to investigate the environmental galaxy density of LSB galaxies compared to the galaxy density in the vicinity of high surface brightness galaxies (HSBs). To avoid the influence of evolutionary effects depending of redshift and to minimize completeness issues within the SDSS, we limited the environment studies to the local universe with a redshift of z ≤ 0.1. At first we studied the luminosity distribution of the LSB sample obtained from the SDSS within two symmetric redshift intervals (0.01 < z ≤ 0.055 and 0.055 < z ≤ 0.1). Results. It was found that the lower redshift interval is dominated by small, low-luminosity LSBs, whereas the LSB sample in the higher redshift range mainly consists of larger, more luminous LSBs. This comes from selection effects of the SDSS spectroscopic sample. The environment studies, also divided into these two redshift bins, show that both the low mass, and the more massive LSBs possess an environment with a lower galaxy density than HSBs. The differences in the galaxy density between LSBs and HSBs are significant on scales between 2 and 5 Mpc, the scales of groups and filaments. To quantify this, we have introduced for the first time the LSB-HSB Antibias. The obtained LSB-HSB Antibias parameter has a value of 10%-15%. Conclusions. From these results we conclude that LSBs formed in low-density regions of the initial universe and have drifted until now to the outer parts of the filaments and walls of the large-scale structure. Furthermore, our results, together with actual cosmological simulations, show that LSBs are caused by a mixture of nature and nurture.

Star Forming Dwarf Galaxies

“…146]. Both have low metallicities and high gas mass fractions and reside in similar environments [128,134]. If BCGs are bursting, clearly their progenitors must be either irregulars or LSBGs.…”

The properties of the Malin 1 galaxy giant disk

“…They also proposed that another galaxy in the area, 350 kpc away from Malin 1 may have interacted with the LSBG 1 Gyr ago. Interactions and companions, however, are not limited to or typical of LSBG that live in less dense environments than their high surface brightness counterparts (Rosenbaum & Bomans 2004;Rosenbaum et al 2009). …”

The star formation histories of red and blue low surface brightness disk galaxies

“…Zackrisson et al 2005;Vorobyov et al 2009), which means that they appear to have a lower metallicity Haberzettl et al 2007), lower star formation rate (O'Neil et al 2007), are evolving much more slowly (van den Hoek et al 2000), have larger gas fraction Schombert et al 2001), lower galaxy density (Rosenbaum et al 2009) and larger amounts of dark matter than what is typically found in normal galaxies.…”