Simulations of the grand design galaxy M51: a case study for analysing tidally induced spiral structure

Dobbs, Clare; Theis, Ch.; Pringle, J. E.; Bate, Matthew R.

doi:10.1111/j.1365-2966.2009.16161.x

Cited by 178 publications

(262 citation statements)

References 97 publications

(199 reference statements)

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“…Barnes, 1988;Mihos et al, 1993;Hibbard & Mihos, 1995;Duc et al, 2000a;Barnes, 2004;Bekki, 2008;Renaud et al, 2008;Dobbs et al, 2010;Karl et al, 2010;Teyssier et al, 2010). Several pairs of interacting galaxies have been numerically reproduced (see an example in Figure 4) by putting the effort on finding a set of parameters that best describe the pair, generally by trial-and-error.…”

Section: Forty Years Of Numerical Simulationsmentioning

confidence: 99%

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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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Section: Forty Years Of Numerical Simulationsmentioning

confidence: 99%

“…Wetzstein et al, 2007;Bournaud et al, 2008a;Dobbs et al, 2010). In this respect, the tides play an important role on the physics of these subsystems.…”

Section: Forty Years Of Numerical Simulationsmentioning

confidence: 99%

Tides in Colliding Galaxies

Duc

Renaud

2013

Lecture Notes in Physics

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“…On the one hand, natural mechanisms for the generation of structures beyond the optical radius are those related to gas accretion (Dekel et al 2009), streams from gas-rich companions in close passages (Dobbs et al 2010), and, in general, tidal interactions with satellites or dwarf galaxies (Bullock & Johnston 2005). In these scenarios, the role of dark matter is not clear.…”

Section: Introductionmentioning

confidence: 99%

Spiral density waves in the outer galactic gaseous discs

Khoperskov

Bertin

2015

Monthly Notices of the Royal Astronomical Society

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Deep HI observations of the outer parts of disc galaxies demonstrate the frequent presence of extended, well-developed spiral arms far beyond the optical radius. To understand the nature and the origin of such outer spiral structure, we investigate the propagation in the outer gaseous disc of large-scale spiral waves excited in the bright optical disc. Using hydrodynamical simulations, we show that non-axisymmetric density waves, penetrating in the gas through the outer Lindblad resonance, can exhibit relatively regular spiral structures outside the bright optical stellar disc. For lowamplitude structures, the results of numerical simulations match the predictions of a simple WKB linear theory. The amplitude of spiral structure increases rapidly with radius. Beyond ≈ 2 optical radii, spirals become nonlinear (the linear theory becomes quantitatively and qualitatively inadequate) and unstable to Kelvin-Helmholtz instability. In numerical simulations, in models for which gas is available very far out, spiral arms can extend out to 25 disc scale-lengths. A comparison between the properties of the models we have investigated and the observed properties of individual galaxies may shed light into the problem of the amount and distribution of dark matter in the outer halo.

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“…The actual arms are imperfectly symmetric and may have azimuthal shifts of several tens of degrees relative to their average phase. Different models of star formation in the spiral arms (Dobbs et al 2010;Gittins & Clarke 2004;Kim & Ostriker 2002 have distinct predictions regarding the phase distribution of young clusters relative to the potential minimum of the arms. References.…”

Section: Spatial Distributionmentioning

confidence: 99%

Star formation in grand-design, spiral galaxies

Grosbøl

Dottori

2012

A&A

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Aims. Spiral structure is a prominent feature in many disk galaxies and is often outlined by bright, young objects. We study the distribution of young stellar clusters in grand-design spiral galaxies and thereby determine whether strong spiral perturbations can influence star formation. Methods. Deep, near-infrared JHK-maps were observed for ten nearby, grand-design, spiral galaxies using HAWK-I at the Very Large Telescope. Complete, magnitude-limited candidate lists of star-forming complexes were obtained by searching within the K-band maps. The properties of the complexes were derived from (H − K) -(J − H) diagrams including the identification of the youngest complexes (i.e. < ∼ 7 Myr) and the estimation of their extinction. Results. Young stellar clusters with ages < ∼ 7 Myr have significant internal extinction in the range of A V = 3-7 m , while older ones typically have A V < 1 m . The cluster luminosity function (CLF) is well-fitted by a power law with an exponent of around -2 and displays no evidence of a high luminosity cut-off. The brightest cluster complexes in the disk reach luminosities of M K = -15. m 5 or estimated masses of 10 6 M . At radii with a strong, two-armed spiral pattern, the star formation rate in the arms is higher by a factor of 2-5 than in the inter-arm regions. The CLF in the arms is also shifted towards brighter M K by at least 0. m 4. We also detect clusters with colors compatible with Large Magellanic Cloud intermediate age clusters and Milky Way globular clusters. The (J − K) -M K diagram of several galaxies shows, for the brightest clusters, a clear separation between young clusters that are highly attenuated by dust and older ones with low extinction. Conclusions. The gap in the (J − K) -M K diagrams implies that there has been a rapid expulsion of dust at an age around 7 Myr, possibly triggered by supernovae. Strong spiral perturbations concentrate the formation of clusters in the arm regions and shifts their CLF towards brighter magnitudes.

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Simulations of the grand design galaxy M51: a case study for analysing tidally induced spiral structure

Cited by 178 publications

References 97 publications

Tides in Colliding Galaxies

Tides in Colliding Galaxies

Spiral density waves in the outer galactic gaseous discs

Star formation in grand-design, spiral galaxies

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