Multi-wavelength structure analysis of local cluster galaxies. The WINGS project. (arXiv:1909.03256v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Psychogyios_A/0/1/0/all/0/1">A. Psychogyios</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vika_M/0/1/0/all/0/1">M. Vika</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charmandaris_V/0/1/0/all/0/1">V. Charmandaris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bamford_S/0/1/0/all/0/1">S. Bamford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fasano_G/0/1/0/all/0/1">G. Fasano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haussler_B/0/1/0/all/0/1">B. Häußler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moretti_A/0/1/0/all/0/1">A. Moretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poggianti_B/0/1/0/all/0/1">B. Poggianti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vulcani_B/0/1/0/all/0/1">B. Vulcani</a>
We present a multi-wavelength analysis of the galaxies in nine clusters
selected from the WINGS dataset, examining how galaxy structure varies as a
function of wavelength and environment using the state of the art software
GALAPAGOSII. We simultaneously fit single S’ersic functions on three optical
(u, B and V) and two near-infrared (J and K) bands thus creating a
wavelength-dependent model of each galaxy. We measure the magnitudes, effective
radius ($R_{e}$) the S’ersic index ($n$), axis ratio and position angle in
each band. The sample contains 790 cluster members (located close to the
cluster center < 0.64 R$_{200}$ and 254 non-member galaxies that we further
separate based on their morphology into ellipticals, lenticulars and spirals.
We find that the S’ersic index of all galaxies inside clusters remains
nearly constant with wavelength while $R_{e}$ decreases as wavelength increases
for all morphological types. We do not observe a significant variation on n and
$R_{e}$ as a function of projected local density and distance from the clusters
center. Comparing the n and $R_{e}$ of bright cluster galaxies with a subsample
of non-member galaxies we find that bright cluster galaxies are more
concentrated (display high $n$ values) and are more compact (low $R_{e}$).
Moreover, the light profile ($mathcal{N}$) and size ($mathcal{R}$) of bright
cluster galaxies does not change as a function of wavelength in the same manner
as non-member galaxies.
We present a multi-wavelength analysis of the galaxies in nine clusters
selected from the WINGS dataset, examining how galaxy structure varies as a
function of wavelength and environment using the state of the art software
GALAPAGOSII. We simultaneously fit single S’ersic functions on three optical
(u, B and V) and two near-infrared (J and K) bands thus creating a
wavelength-dependent model of each galaxy. We measure the magnitudes, effective
radius ($R_{e}$) the S’ersic index ($n$), axis ratio and position angle in
each band. The sample contains 790 cluster members (located close to the
cluster center < 0.64 R$_{200}$ and 254 non-member galaxies that we further
separate based on their morphology into ellipticals, lenticulars and spirals.
We find that the S’ersic index of all galaxies inside clusters remains
nearly constant with wavelength while $R_{e}$ decreases as wavelength increases
for all morphological types. We do not observe a significant variation on n and
$R_{e}$ as a function of projected local density and distance from the clusters
center. Comparing the n and $R_{e}$ of bright cluster galaxies with a subsample
of non-member galaxies we find that bright cluster galaxies are more
concentrated (display high $n$ values) and are more compact (low $R_{e}$).
Moreover, the light profile ($mathcal{N}$) and size ($mathcal{R}$) of bright
cluster galaxies does not change as a function of wavelength in the same manner
as non-member galaxies.
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