On the environment of Low Surface Brightness galaxies at different scales. (arXiv:1910.03078v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Perez_Montano_L/0/1/0/all/0/1">Luis Enrique Pérez-Montaño</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sodi_B/0/1/0/all/0/1">Bernardo Cervantes Sodi</a>
We select a volume-limited sample of galaxies derived from the SDSS-DR7 to
study the environment of low surface brightness (LSB) galaxies at different
scales, as well as several physical properties of the dark matter haloes where
the LSB galaxies of the sample are embedded. To characterize the environment we
make use of a number of publicly available value-added galaxy catalogues. We
find a slight preference for LSB galaxies to be found in filaments instead of
clusters, with their mean distance to the nearest filament typically larger
than for high surface brightness (HSB) galaxies. The fraction of isolated
central LSB galaxies is higher than the same fraction for HSB ones, and the
density of their local environment lower. The stellar-to-halo mass ratio using
four different estimates is up to $sim$20% for HSB galaxies. LSB central
galaxies present more recent assembly times when compared with their HSB
counterparts. Regarding the $lambda$ spin parameter, using six different
proxies for its estimation, we find that LSB galaxies present systematically
larger values of $lambda$ than the HSB galaxy sample, and constructing a
control sample with direct kinematic information drawn from ALFALFA, we confirm
that the spin parameter of LSB galaxies is 1.6 to 2 times larger than the one
estimated for their HSB counterparts.
We select a volume-limited sample of galaxies derived from the SDSS-DR7 to
study the environment of low surface brightness (LSB) galaxies at different
scales, as well as several physical properties of the dark matter haloes where
the LSB galaxies of the sample are embedded. To characterize the environment we
make use of a number of publicly available value-added galaxy catalogues. We
find a slight preference for LSB galaxies to be found in filaments instead of
clusters, with their mean distance to the nearest filament typically larger
than for high surface brightness (HSB) galaxies. The fraction of isolated
central LSB galaxies is higher than the same fraction for HSB ones, and the
density of their local environment lower. The stellar-to-halo mass ratio using
four different estimates is up to $sim$20% for HSB galaxies. LSB central
galaxies present more recent assembly times when compared with their HSB
counterparts. Regarding the $lambda$ spin parameter, using six different
proxies for its estimation, we find that LSB galaxies present systematically
larger values of $lambda$ than the HSB galaxy sample, and constructing a
control sample with direct kinematic information drawn from ALFALFA, we confirm
that the spin parameter of LSB galaxies is 1.6 to 2 times larger than the one
estimated for their HSB counterparts.
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