# On the characteristics of tidal structures of interacting galaxies

Research output: Contribution to journalArticleResearchpeer-review

2 Citations (Scopus)

### Abstract

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
Original language English 670-678 Astronomy Letters 37 10 https://doi.org/10.1134/S1063773711100045 Published - 2011

### Keywords

• galaxies
• interacting galaxies
• morphology
• kinematics

### Cite this

@article{35822c743b804a12ade214e9d03c6fa3,
title = "On the characteristics of tidal structures of interacting galaxies",
abstract = "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",
keywords = "galaxies, interacting galaxies, morphology, kinematics",
author = "Y.H. Mohamed and V.P. Reshetnikov and N.Ya. Sotnikova",
year = "2011",
doi = "10.1134/S1063773711100045",
language = "English",
volume = "37",
pages = "670--678",
journal = "Astronomy Letters",
issn = "1063-7737",
publisher = "МАИК {"}Наука/Интерпериодика{"}",
number = "10",

}

In: Astronomy Letters, Vol. 37, No. 10, 2011, p. 670-678.

Research output: Contribution to journalArticleResearchpeer-review

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 -