On the characteristics of tidal structures of interacting galaxies

Mohamed, Y. H.; Решетников, В. П.; Sotnikova, N. Ya.

doi:10.1134/s1063773711100045

Cited by 7 publications

(12 citation statements)

References 20 publications

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“…However, the properties described above are very basic geometric observables that relate quite directly to model characteristics. We also note that the available and adequately resolved observations are not sufficiently extensive to make detailed statistical comparisons (though global statistical properties have been studied recently by Smith et al 2007, 2010a; Mohamed, Reshetnikov & Sotnikova 2011).…”

Section: Comparisons To Observed Formsmentioning

confidence: 99%

The symmetries and scaling of tidal tails in galaxies

Struck¹,

Smith²

2012

Monthly Notices of the Royal Astronomical Society

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(Abriged) We present analytic models for the formation and evolution of tidal tails and related structures following impulsive disturbances in galaxy collisions. Since the epicyclic approximation is not valid for large radial excursions, we use orbital equations of the form we call p-ellipses. These have been shown to provide accurate representations of orbits in power-law halo potentials. In the case of a purely tidal disturbance the resulting tidal tails have simple structure. Scalings for their maximum lengths and other characteristics as functions of the tidal amplitude and the exponent of the power-law potentials are described. The analytic model shows that azimuthal caustics (orbit crossing zones) are produced generically in these tails at a fixed azimuth relative to the point of closest approach. Long tails, with high order caustics at their base are also produced at larger amplitudes. The analysis is extended to nonlinear disturbances and multiple encounters, which break the symmetries of tidal perturbations. As the strength of the nonlinear terms is varied the structure of the resulting forms varies from symmetric tails to one-armed plumes. Cases with two or more impulse disturbances are also considered as the simplest analytic models distinguishing between prograde and retrograde encounters. A specific mechanism for the formation of tidal dwarf galaxies at the end of tails is suggested as a consequence of resonance effects in prolonged encounters. Qualitative comparisons to Arp Atlas systems suggest that the limiting analytic cases are realized in real systems. We identify a few Arp systems which may have swallowtail caustics, where dissipative gas streams converge and trigger star formation. UV and optical images reveal luminous knots of young stars at these 'hinge clump' locations.Comment: MNRAS accepted, 24 pages, 21 figure

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Section: Comparisons To Observed Formsmentioning

confidence: 99%

The symmetries and scaling of tidal tails in galaxies

Struck¹,

Smith²

2012

Monthly Notices of the Royal Astronomical Society

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“…Moreover, star clusters and tidal dwarf galaxies (TDGs) can be formed in tidal tails (Barnes & Hernquist 1992;Bournaud & Duc 2006;Wetzstein, Naab & Burkert 2007). Previous observational studies of TDGs focused on individual objects or small sam-ples (Duc et al 2000;Duc & Mirabel 1998;Hancock et al 2009;Mohamed, Reshetnikov & Sotnikova 2011;Kaviraj et al 2012). A systematic investigation of tidal tails using a sufficiently large sample of merging galaxies is required to address how the tidal tails are created in reality, draw constraints on how spiral galaxies merge with each other in the cosmic web, and examine the formation of TDGs and star formation under these extreme conditions.…”

Section: Introductionmentioning

confidence: 99%

Long tidal tails in merging galaxies and their implications

Ren

Zheng

Valls–Gabaud

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We investigate the properties of long tidal tails using the largest to date sample of 461 merging galaxies with $\log (M_\ast /\rm M_\odot )\ge 9.5$ within 0.2 ≤ z ≤ 1 from the COSMOS survey in combination with Hubble Space Telescope imaging data. Long tidal tails can be briefly divided into three shape types: straight (41 per cent), curved (47 per cent) and plume (12 per cent). Their host galaxies are mostly at late stages of merging, although 31 per cent are galaxy pairs with projected separations d > 20 kpc. The high formation rate of straight tidal tails needs to be understood as the projection of curved tidal tails accounts for only a small fraction of the straight tails. We identify 165 tidal dwarf galaxies (TDGs), yielding a TDG production rate of 0.36 per merger. Combined with a galaxy merger fraction and a TDG survival rate from the literature, we estimate that ∼ 5 per cent of local dwarf galaxies are of tidal origin, suggesting the tidal formation is not an important formation channel for the dwarf galaxies. More than half of TDGs are located at the tip of their host tails. These TDGs have stellar masses in the range of $7.5\le \log (M_\ast /\rm M_\odot )\le 9.5$ and appear compact with half-light radii following the M* - Re relation of low-mass elliptical galaxies. However, their surface brightness profiles are generally flatter than those of local disc galaxies. Only 10 out of 165 TDGs have effective radii larger than 1.5 kpc and would qualify as unusually bright ultra-diffuse galaxies.

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“…The results of linear projected separation and relative velocities have presented in Table 4. Patton et al (2011) found that < The length and the thickness of a tidal tails and a tidal bridge are calculated using the method of Mohamed et al (2011). The results of the geometric properties of the interaction signs for each pair have been described in Table 5.…”

Section: Resultsmentioning

confidence: 99%

The morphological study of spiral/lenticular galaxies in some pairs

Hendy

Ali

2018

NRIAG Journal of Astronomy and Geophysics

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A B S T R A C TThis work presents the optical observations for three galaxy pairs. We have presented the isophotal contours and geometrical analysis (x-center shift (xc), y-center shift (yc), ellipticity (Ellip = 1 − b/a) and position angle (P.A.)) for each component of the pair. The projected linear separations r p and the relative velocity v Δ of each pair have been determined.This sample of galaxy pairs has been reported by Karachentsev Catalog without interaction signs. Our analysis shows that the galaxies had signs of interaction (tidal tail and tidal bridge or only tidal tail). The length and thickness of the tidal tails and tidal bridges have obtained and presented in this study.Our results show that two of the galaxy pairs are close pairs, i.e. contact systems ( < − r 30 h kpc p 70 1 and < v Δ 200 km/s) with the tidal interaction of tails and bridges. While the other pair is an intermediate pair ( < < − r 30 55 h kpc p 70 1 and < v Δ 5 km/s) with the tidal tail in the western side.

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On the characteristics of tidal structures of interacting galaxies

Cited by 7 publications

References 20 publications

The symmetries and scaling of tidal tails in galaxies

The symmetries and scaling of tidal tails in galaxies

Long tidal tails in merging galaxies and their implications

The morphological study of spiral/lenticular galaxies in some pairs

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