Research output: Contribution to journal › Article › peer-review
On the characteristics of tidal structures of interacting galaxies. / Mohamed, Y.H.; Reshetnikov, V.P.; Sotnikova, N.Ya.
In: Astronomy Letters, Vol. 37, No. 10, 2011, p. 670-678.Research output: Contribution to journal › Article › peer-review
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TY - JOUR
T1 - On the characteristics of tidal structures of interacting galaxies
AU - Mohamed, Y.H.
AU - Reshetnikov, V.P.
AU - Sotnikova, N.Ya.
PY - 2011
Y1 - 2011
N2 - We present the results of our analysis of the geometrical tidal tail characteristics for nearby and distant interacting galaxies. The sample includes more than two hundred nearby galaxies and about seven hundred distant ones. The distant galaxies have been selected in several deep fields of the Hubble Space Telescope (HDF-N, HDF-S, HUDF, GOODS, GEMS) and they are at mean redshift z=0.65. We analyze the distributions of lengths and thicknesses for the tidal structures and show that the tails in distant galaxies are shorter than those in nearby ones. This effect can be partly attributed to observational selection effects, but, on the other hand, it may result from the general evolution of the sizes of spiral galaxies wih z. The location of interacting galaxies on the galaxy luminosity ($L$) -- tidal tail length ($l$) plane are shown to be explained by a simple geometrical model, with the upper envelope of the observed distribution being $l \propto \sqrt{L}$. We have solved the problem on the relationship betwee
AB - We present the results of our analysis of the geometrical tidal tail characteristics for nearby and distant interacting galaxies. The sample includes more than two hundred nearby galaxies and about seven hundred distant ones. The distant galaxies have been selected in several deep fields of the Hubble Space Telescope (HDF-N, HDF-S, HUDF, GOODS, GEMS) and they are at mean redshift z=0.65. We analyze the distributions of lengths and thicknesses for the tidal structures and show that the tails in distant galaxies are shorter than those in nearby ones. This effect can be partly attributed to observational selection effects, but, on the other hand, it may result from the general evolution of the sizes of spiral galaxies wih z. The location of interacting galaxies on the galaxy luminosity ($L$) -- tidal tail length ($l$) plane are shown to be explained by a simple geometrical model, with the upper envelope of the observed distribution being $l \propto \sqrt{L}$. We have solved the problem on the relationship betwee
KW - galaxies
KW - interacting galaxies
KW - morphology
KW - kinematics
U2 - 10.1134/S1063773711100045
DO - 10.1134/S1063773711100045
M3 - Article
VL - 37
SP - 670
EP - 678
JO - Astronomy Letters
JF - Astronomy Letters
SN - 1063-7737
IS - 10
ER -
ID: 5137510