Chemodynamical evolution of tidal dwarf galaxies – II. The long-term evolution and influence of a tidal field

Ploeckinger, Sylvia; Recchi, Simone; Hensler, G.; Kroupa, Pavel

doi:10.1093/mnras/stu2629

Cited by 44 publications

(53 citation statements)

References 74 publications

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“…For low SFRs this necessary condition can, however, not be fulfilled. As shown by Ploeckinger et al (2015) the IMF can hardly be fulfilled for star clusters of masses below 10 4 M ⊙ so that the stellar feedback is affected at low SFRs (Hensler et al 2017, see e.g. Steyrleithner et al, in prep.).…”

Section: Stellar Initial Mass Functionmentioning

confidence: 99%

“…The distribution function for mass ratios in binary systems is given by (Matteucci & Recchi 2001), where the parameter γ = 2 is based on statistical analyses that show mass ratios of one more likely. We implied this recipe to the cdFLASH code (Ploeckinger et al 2015). However, nowadays smaller γ is preferred and set here to γ ≃ 0.5 (Recchi, priv.…”

Section: Type Ia Supernovaementioning

confidence: 99%

“…In order to study the effect of RP we implemented a socalled wind module to the cdFLASH code (Mitchell et al 2013;Ploeckinger et al 2015). For the motion through the ICM its density varies according to the radial ICM density profile for the Virgo cluster of Vollmer et al (2001) as…”

Section: Wind Modulementioning

confidence: 99%

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The effect of ram-pressure stripping on dwarf galaxies

Steyrleithner

Hensler

Boselli

2020

Monthly Notices of the Royal Astronomical Society

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Ram-pressure stripping (RPS) is a well observed phenomenon of massive spiral galaxies passing through the hot intra-cluster medium (ICM) of galaxy clusters. For dwarf galaxies (DGs) within a cluster, the transformation from gaseous to gas-poor systems by RPS is not easily observed and must happen in the outskirts of clusters. In a few objects in close by galaxy clusters and the field, RPS has been observed. Since cluster early-type DGs also show a large variety of internal structures (unexpected central gas reservoirs, blue stellar cores, composite radial stellar profiles), we aim in this study to investigate how ram pressure (RP) affects the interstellar gas content and therefore the star-formation (SF) activity. Using a series of numerical simulations, we quantify the dependence of the stripped-off gas on the velocity of the infalling DGs and on the ambient ICM density. We demonstrated that SF can be either suppressed or triggered by RP depending on the ICM density and the DGs mass. Under some conditions, RP can compress the gas, so that it is unexpectedly retained in the central DG region and forms stars. When gas clouds are still bound against stripping but lifted from a thin disk and fall back, their new stars form an ellipsoidal (young) stellar population already with a larger velocity dispersion without the necessity of harassment. Most spectacularly, star clusters can form downstream in stripped-off massive gas clouds in the case of strong RP. We compare our results to observations.

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Section: Stellar Initial Mass Functionmentioning

confidence: 99%

Section: Type Ia Supernovaementioning

confidence: 99%

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The effect of ram-pressure stripping on dwarf galaxies

Steyrleithner

Hensler

Boselli

2020

Monthly Notices of the Royal Astronomical Society

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“…Although the applied recipe of SF by Koeppen et al (1995) already includes the selfregulation by stellar energy feedback, in recent simulations Ploeckinger et al (2015) we have implemented HII regions as additional effect on SF self-regulation. This recipe can also be used for momentum transfer and radiation-pressure driven turbulence (Renaud et al 2013).…”

Section: Stellar Radiationmentioning

confidence: 99%

Refuelled and shielded – the early evolution of tidal dwarf galaxies

Baumschlager

Hensler

Steyrleithner

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present, for the first time, numerical simulations of young tidal dwarf galaxies (TDGs), including a self-consistent treatment of the tidal arm in which they are embedded. Thereby, we do not rely on idealised initial conditions, as the initial data of the presented simulation emerge from a galaxy interaction simulation. By comparing models which are either embedded in or isolated form the tidal arm, we demonstrate its importance on the evolution of TDGs, as additional source of gas which can be accreted and is available for subsequent conversion into stars. During the initial collapse of the proto-TDG, with a duration of a few 100 Myr, the evolution of the embedded and isolated TDGs are indistinguishable. Significant differences appear after the collapse has halted and the further evolution is dominated by the possible accretion of material form the surroundings of the TDGs. The inclusion of the tidal arm in the simulation of TDGs results in roughly a doubling of the gas mass (M gas ) and gas fraction (f gas ), an increase in stellar mass by a factor of 1.5 and a ∼ 3 times higher star formation rate (SFR) compared to the isolated case. Moreover, we perform a parametric study on the influence of different environmental effects, i.e. the tidal field and ram pressure. Due to the orbit of the chosen initial conditions, no clear impact of the environmental effects on the evolution of TDG candidates can be found.

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“…Duc et al 2000;Bournaud & Duc 2006;Recchi et al 2007;Ploeckinger et al 2014Ploeckinger et al , 2015. For example, they should show a velocity gradient that is kinematically decoupled from the surrounding tidal debris, pointing to a local gravitational potential well.…”

Section: Introductionmentioning

confidence: 99%

Gas dynamics in tidal dwarf galaxies: Disc formation atz= 0

Lelli

Duc

Brinks

et al. 2015

A&A

124

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Tidal dwarf galaxies (TDGs) are recycled objects that form within the collisional debris of interacting and merging galaxies. They are expected to be devoid of non-baryonic dark matter, since they can only form from dissipative material ejected from the discs of the progenitor galaxies. We investigate the gas dynamics in a sample of six bona fide TDGs around three interacting and post-interacting systems: NGC 4694, NGC 5291, and NGC 7252 ("Atoms for Peace"). For NGC 4694 and NGC 5291, we analyse existing H I data from the Very Large Array (VLA), while for NGC 7252 we present new H I observations from the Jansky VLA, together with long-slit and integral-field optical spectroscopy. For all six TDGs, the H I emission can be described by rotating disc models. These H I discs, however, have undergone less than a full rotation since the time of the interaction/merger event, raising the question of whether they are in dynamical equilibrium. Assuming that these discs are in equilibrium, the inferred dynamical masses are consistent with the observed baryonic masses, implying that TDGs are devoid of dark matter. This puts constraints on putative "dark discs" (either baryonic or non-baryonic) in the progenitor galaxies. Moreover, TDGs seem to systematically deviate from the baryonic Tully-Fisher relation. These results provide a challenging test for alternative theories like MOND.

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Chemodynamical evolution of tidal dwarf galaxies – II. The long-term evolution and influence of a tidal field

Cited by 44 publications

References 74 publications

The effect of ram-pressure stripping on dwarf galaxies

The effect of ram-pressure stripping on dwarf galaxies

Refuelled and shielded – the early evolution of tidal dwarf galaxies

Gas dynamics in tidal dwarf galaxies: Disc formation atz= 0

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