Comparing IMF-sensitive indices of intermediate-mass quiescent galaxies in various environments. (arXiv:1904.11493v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Eftekhari_E/0/1/0/all/0/1">Elham Eftekhari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mosleh_M/0/1/0/all/0/1">Moein Mosleh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vazdekis_A/0/1/0/all/0/1">Alexandre Vazdekis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tavasoli_S/0/1/0/all/0/1">Saeed Tavasoli</a>
Using samples drawn from the Sloan Digital Sky Survey, we study for the first
time the relation between large-scale environments (Clusters, Groups and Voids)
and the stellar Initial Mass Function (IMF). We perform an observational
approach based on the comparison of IMF-sensitive indices of quiescent galaxies
with similar mass in varying environments. These galaxies are selected within a
narrow redshift interval ($ 0.020 < z < 0.055 $) and spanning a range in
velocity dispersion from 100 to 200 kms$^{-1}$. The results of this paper are
based upon analysis of composite spectra created by stacking the spectra of
galaxies, binned by their velocity dispersion and redshift. The trends of
spectral indices as measured from the stacked spectra, with respect to velocity
dispersion, are compared in different environments. We find a lack of
dependence of the IMF on the environment for intermediate-mass galaxy regime.
We verify this finding by providing a more quantitative measurement of the IMF
variations among galactic environments using MILES stellar population models
with a precision of $DeltaGamma_{b}sim0.2$.
Using samples drawn from the Sloan Digital Sky Survey, we study for the first
time the relation between large-scale environments (Clusters, Groups and Voids)
and the stellar Initial Mass Function (IMF). We perform an observational
approach based on the comparison of IMF-sensitive indices of quiescent galaxies
with similar mass in varying environments. These galaxies are selected within a
narrow redshift interval ($ 0.020 < z < 0.055 $) and spanning a range in
velocity dispersion from 100 to 200 kms$^{-1}$. The results of this paper are
based upon analysis of composite spectra created by stacking the spectra of
galaxies, binned by their velocity dispersion and redshift. The trends of
spectral indices as measured from the stacked spectra, with respect to velocity
dispersion, are compared in different environments. We find a lack of
dependence of the IMF on the environment for intermediate-mass galaxy regime.
We verify this finding by providing a more quantitative measurement of the IMF
variations among galactic environments using MILES stellar population models
with a precision of $DeltaGamma_{b}sim0.2$.
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