Herschel-ATLAS : The spatial clustering of low and high redshift submillimetre galaxies. (arXiv:1811.02870v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Amvrosiadis_A/0/1/0/all/0/1">A. Amvrosiadis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valiante_E/0/1/0/all/0/1">E. Valiante</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Nuevo_J/0/1/0/all/0/1">J. Gonzalez-Nuevo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maddox_S/0/1/0/all/0/1">S. J. Maddox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Negrello_M/0/1/0/all/0/1">M. Negrello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eales_S/0/1/0/all/0/1">S. A. Eales</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunne_L/0/1/0/all/0/1">L. Dunne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_L/0/1/0/all/0/1">L. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kampen_E/0/1/0/all/0/1">E. van Kampen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zotti_G/0/1/0/all/0/1">G. De Zotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_M/0/1/0/all/0/1">M. W. L. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andreani_P/0/1/0/all/0/1">P. Andreani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greenslade_J/0/1/0/all/0/1">J. Greenslade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tai_An_C/0/1/0/all/0/1">C. Tai-An</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Michalowski_M/0/1/0/all/0/1">M. J. Michałowski</a>
We present measurements of the angular correlation function of sub-millimeter
(sub-mm) galaxies (SMGs) identified in four out of the five fields of the
Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) – GAMA-9h,
GAMA-12h, GAMA-15h and NGP – with flux densities $S_{250mu m}$>30 mJy at 250
{mu}m. We show that galaxies selected at this wavelength trace the underlying
matter distribution differently at low and high redshifts. We study the
evolution of the clustering finding that at low redshifts sub-mm galaxies
exhibit clustering strengths of $r_0$ $sim$ 2 – 3 $h^{-1}$ Mpc, below z < 0.3.
At high redshifts, on the other hand, we find that sub-mm galaxies are more
strongly clustered with correlation lengths $r_0$ = 8.1 $pm$ 0.5, 8.8 $pm$
0.8 and 13.9 $pm$ 3.9 $h^{-1}$Mpc at z = 1 - 2, 2 - 3 and 3 - 5, respectively.
We show that sub-mm galaxies across the redshift range 1 < z < 5, typically
reside in dark-matter halos of mass of the order of ~ $10^{12.5}$ - $10^{13.0}$
$h^{-1} , M_{odot}$ and are consistent with being the progenitors of local
massive elliptical galaxies that we see in the local Universe.
We present measurements of the angular correlation function of sub-millimeter
(sub-mm) galaxies (SMGs) identified in four out of the five fields of the
Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) – GAMA-9h,
GAMA-12h, GAMA-15h and NGP – with flux densities $S_{250mu m}$>30 mJy at 250
{mu}m. We show that galaxies selected at this wavelength trace the underlying
matter distribution differently at low and high redshifts. We study the
evolution of the clustering finding that at low redshifts sub-mm galaxies
exhibit clustering strengths of $r_0$ $sim$ 2 – 3 $h^{-1}$ Mpc, below z < 0.3.
At high redshifts, on the other hand, we find that sub-mm galaxies are more
strongly clustered with correlation lengths $r_0$ = 8.1 $pm$ 0.5, 8.8 $pm$
0.8 and 13.9 $pm$ 3.9 $h^{-1}$Mpc at z = 1 – 2, 2 – 3 and 3 – 5, respectively.
We show that sub-mm galaxies across the redshift range 1 < z < 5, typically
reside in dark-matter halos of mass of the order of ~ $10^{12.5}$ – $10^{13.0}$
$h^{-1} , M_{odot}$ and are consistent with being the progenitors of local
massive elliptical galaxies that we see in the local Universe.
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