Do model emission line galaxies live in filaments at z~1?. (arXiv:2001.06560v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Perez_V/0/1/0/all/0/1">V. Gonzalez-Perez</a> (LJMU), <a href="http://arxiv.org/find/astro-ph/1/au:+Cui_W/0/1/0/all/0/1">W. Cui</a> (ROE), <a href="http://arxiv.org/find/astro-ph/1/au:+Contreras_S/0/1/0/all/0/1">S. Contreras</a> (DIPC), <a href="http://arxiv.org/find/astro-ph/1/au:+Baugh_C/0/1/0/all/0/1">C. M. Baugh</a> (ICC), <a href="http://arxiv.org/find/astro-ph/1/au:+Comparat_J/0/1/0/all/0/1">J. Comparat</a> (MPE), <a href="http://arxiv.org/find/astro-ph/1/au:+Griffin_A/0/1/0/all/0/1">A. J. Griffin</a> (ICC), <a href="http://arxiv.org/find/astro-ph/1/au:+Helly_J/0/1/0/all/0/1">J. Helly</a> (ICC), <a href="http://arxiv.org/find/astro-ph/1/au:+Knebe_A/0/1/0/all/0/1">A. Knebe</a> (UAM), <a href="http://arxiv.org/find/astro-ph/1/au:+Lacey_C/0/1/0/all/0/1">C. Lacey</a> (ICC), <a href="http://arxiv.org/find/astro-ph/1/au:+Norberg_P/0/1/0/all/0/1">P. Norberg</a> (ICC)
Current and future cosmological surveys are targeting star-forming galaxies
at z~1 with nebular emission lines. In this work we use a state-of-the-art
model of galaxy formation and evolution to explore the large scale environment
of star-forming emission line galaxies (ELGs). Model galaxies are selected with
cuts such that the samples can be directly compared with the DEEP2, VVDS,
eBOSS-SGC and DESI surveys. Their large scale environment have been classified
using a velocity-shear-tensor and a tidal-tensor algorithms. Half of model ELGs
live in filaments and about a third in sheets. Model ELGs in knots have the
largest satellite fractions. We find that the shape of the mean halo occupation
distribution of model ELGs varies widely for different large scale
environments. To put these results in context, we have compared fixed number
density samples of galaxies, generated by either imposing an extra cut in
stellar mass, star formation rate (SFR) or L[OII] to the ELGs, or by imposing a
single cut in these quantities to the total model galaxy population. For the
fixed number density samples, ELGs are close to L[OII] and SFR selected samples
for densities above $10^{-4.2}h^{3}{rm Mpc}^{-3}$. ELGs with an extra cut in
stellar mass to fix their number density, present differences in sheets and
knots with respect to the other samples. ELGs, SFR and L[OII] selected samples
with equal number density, have similar large scale bias but their clustering
below separations of $1h^{-1}$Mpc is different.
Current and future cosmological surveys are targeting star-forming galaxies
at z~1 with nebular emission lines. In this work we use a state-of-the-art
model of galaxy formation and evolution to explore the large scale environment
of star-forming emission line galaxies (ELGs). Model galaxies are selected with
cuts such that the samples can be directly compared with the DEEP2, VVDS,
eBOSS-SGC and DESI surveys. Their large scale environment have been classified
using a velocity-shear-tensor and a tidal-tensor algorithms. Half of model ELGs
live in filaments and about a third in sheets. Model ELGs in knots have the
largest satellite fractions. We find that the shape of the mean halo occupation
distribution of model ELGs varies widely for different large scale
environments. To put these results in context, we have compared fixed number
density samples of galaxies, generated by either imposing an extra cut in
stellar mass, star formation rate (SFR) or L[OII] to the ELGs, or by imposing a
single cut in these quantities to the total model galaxy population. For the
fixed number density samples, ELGs are close to L[OII] and SFR selected samples
for densities above $10^{-4.2}h^{3}{rm Mpc}^{-3}$. ELGs with an extra cut in
stellar mass to fix their number density, present differences in sheets and
knots with respect to the other samples. ELGs, SFR and L[OII] selected samples
with equal number density, have similar large scale bias but their clustering
below separations of $1h^{-1}$Mpc is different.
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