A Simulation Atlas of Tidal Features in Galaxies

Howard, S.; Keel, William C.; Byrd, G. G.; Burkey, Jordan M.

doi:10.1086/173329

Cited by 52 publications

(69 citation statements)

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“…The radio bridge was discovered at 1465 MHz by van der Hulst & Hummel (1985, A&A, 150, 17). We find that the bridge has a fairly steep spectrum with a spectral index α (S ∝ ν α ) of −1.8 +0.3 −0.2 which is much steeper than the −0.8 quoted by van der Hulst & Hummel (1985); b) detection of other tidal features like the tilted HI and radio continuum disk of NGC 2814, a HI streamer and a radio continuum tail arising from the south of NGC 2814. We also report the detection of a possible tidal dwarf galaxy in HI; c) sharp truncation in the HI distribution in the south of NGC 2820 and in the HI and radio continuum distribution in the north of NGC 2814.…”

contrasting

confidence: 53%

“…Additionally, a bridge connecting the triplet is also detected at 330 MHz. This bridge was first reported by van der Hulst and Hummel (1985) at 1465 MHz. We have marginal detection of the bridge at 610 and 240 MHz.…”

Section: Radio Continuummentioning

confidence: 52%

“…1a, we have detected the bridge connecting the triplet at 330 MHz. Using the 1465 MHz result of van der Hulst and Hummel (1985) along with our data at 330 MHz we estimate a spectral index of −1.8 +0.3 −0.2 for the bridge. This spectral index is much steeper than the value of −0.8 quoted by van der Hulst & Hummel (1985) which might possibly have been corrupted by disk emission at their lower frequency.…”

Section: Tidal Bridgementioning

confidence: 89%

“…van der Hulst & Hummel (1985) were the first to detect a radio continuum bridge connecting the triplet in Ho 124 at 1465 MHz. Since then radio bridges have been detected in many other systems, a famous one being the Taffy galaxies (Condon et al 1993) in which one-half the total radio synchrotron emission of the system arises in the bridge.…”

Section: Tidal Effectsmentioning

confidence: 99%

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GMRT observations of the group Holmberg 124: Evolution by tidal forces and ram pressure?

Kantharia

Ananthakrishnan

Nityananda

et al. 2005

A&A

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Abstract. We report new radio continuum and 21 cm HI observations using the Giant Metrewave Radio Telescope (GMRT) of the group Holmberg 124 (Ho 124) comprising four late-type galaxies, namely NGC 2820, Mrk 108, NGC 2814 and NGC 2805. The three galaxies, NGC 2820, Mrk 108 and NGC 2814 which are closely located in the sky plane have clearly undergone tidal interactions as seen from the various morphological tidal signatures and debris. Moreover we note various features in the group members which we believe might be due to ram pressure. In this paper, we describe four interesting results emerging from our observations: a) detection of the tidal radio continuum bridge at 330 MHz connecting the galaxies NGC 2820+Mrk 108 with NGC 2814. The radio bridge was discovered at 1465 MHz by van der Hulst & Hummel (1985, A&A, 150, 17). We find that the bridge has a fairly steep spectrum with a spectral index α (S ∝ ν α ) of −1.8 +0.3 −0.2 which is much steeper than the −0.8 quoted by van der Hulst & Hummel (1985); b) detection of other tidal features like the tilted HI and radio continuum disk of NGC 2814, a HI streamer and a radio continuum tail arising from the south of NGC 2814. We also report the detection of a possible tidal dwarf galaxy in HI; c) sharp truncation in the HI distribution in the south of NGC 2820 and in the HI and radio continuum distribution in the north of NGC 2814. The optical disks in both the cases look undisturbed. As pointed out by Davis et al. (1997, AJ, 114, 613), ram pressure affects different components of the interstellar medium to varying degrees. Simple estimates of pressure in different components of the interstellar medium (radio continuum, Hα and HI) in NGC 2820 indicate that ram pressure will significantly influence HI; d) detection of a large one-sided HI loop to the north of NGC 2820. No radio continuum emission or Hα emission is associated with the HI loop. We discuss various scenarios for the origin of this loop including a central starburst, ram pressure stripping and tidal interaction. We do not support the central starburst scenario since the loop is not detected in ionized gas. Using the upper limit on X-ray luminosity of Ho 124 (Mulchaey et al. 2003, ApJS, 145, 39), we estimate an upper limit on the intragroup medium (IGrM) density of 8.8 × 10 −4 cm −3 . For half this electron density, we estimate the ram pressure force of the IGrM to be comparable to the gravitational pull of the disk of NGC 2820. Since tidal interaction has obviously influenced the group, we suggest that the loop could have formed by ram pressure stripping if tidal effects had reduced the surface density of HI in NGC 2820. From the complex observational picture of Ho 124 and the numerical estimates, we suggest that the evolution of the Ho 124 group may be governed by both tidal forces due to the interaction and the ram pressure due to motion of the member galaxies in the IGrM and that the IGrM densities should not be too low (i.e. ≥4 × 10 −4 ). However this needs to be verified by further observations.

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contrasting

confidence: 53%

Section: Radio Continuummentioning

confidence: 52%

Section: Tidal Bridgementioning

confidence: 89%

Section: Tidal Effectsmentioning

confidence: 99%

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GMRT observations of the group Holmberg 124: Evolution by tidal forces and ram pressure?

Kantharia

Ananthakrishnan

Nityananda

et al. 2005

A&A

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“…with a zero-inclination. The highly inclined configurations, called polar orbits, give generally birth to a single tail, as opposed to the bridge/tail pairs (Howard et al, 1993). In short, because an observed tidal effect does not only depend on the strength of the differential forces, but also on the duration of their existence, long tails are associated with prograde configurations.…”

Section: Spin-orbit Couplingmentioning

confidence: 99%

Tides in Colliding Galaxies

Duc

Renaud

2013

Lecture Notes in Physics

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Long tails and streams of stars are the most noticeable upshots of galaxy collisions. Their origin as gravitational, tidal, disturbances has however been recognized only less than fifty years ago and more than ten years after their first observations. This Review describes how the idea of galactic tides emerged, in particular thanks to the advances in numerical simulations, from the first ones that included tens of particles to the most sophisticated ones with tens of millions of them and state-of-the-art hydrodynamical prescriptions. Theoretical aspects pertaining to the formation of tidal tails are then presented. The third part of the review turns to observations and underlines the need for collecting deep multi-wavelength data to tackle the variety of physical processes exhibited by collisional debris. Tidal tails are not just stellar structures, but turn out to contain all the components usually found in galactic disks, in particular atomic / molecular gas and dust. They host star-forming complexes and are able to form star-clusters or even second-generation dwarf galaxies. The final part of the review discusses what tidal tails can tell us (or not) about the structure and content of present-day galaxies, including their dark components, and explains how tidal tails may be used to probe the past evolution of galaxies and their mass assembly history. On-going deep wide-field surveys disclose many new lowsurface brightness structures in the nearby Universe, offering great opportunities for attempting galactic archeology with tidal tails.

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References for 9.2

Huchtmeier¹

Interstellar Matter, Galaxy, Universe

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A Simulation Atlas of Tidal Features in Galaxies

Cited by 52 publications

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GMRT observations of the group Holmberg 124: Evolution by tidal forces and ram pressure?

GMRT observations of the group Holmberg 124: Evolution by tidal forces and ram pressure?

Tides in Colliding Galaxies

References for 9.2

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