Tidal Triggering of Star Formation by the Galaxy Cluster Potential

Henriksen, M. J.; Byrd, G. G.

doi:10.1086/176870

Cited by 77 publications

(91 citation statements)

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“…When the galaxy velocity becomes comparable to or exceeds that of the sound in the inter-galactic medium, effects of the compressibility of the fluid become important, and shock waves can occur within the galaxy or backward throughout the ISM (e.g., Landau & Lifshitz 1959). In the literature these concepts find application in problems related to the free fall of galaxies in rich clusters of galaxies (e.g., Henriksen & Byrd 1996, their Eq. 6).…”

Section: Galaxy Model and Plasma Distributionmentioning

confidence: 99%

“…Generally, environmental effects are important in groups and clusters of galaxies and are believed to contribute to the origin of the density-morphology relation (e.g., Oemler 1974;Dressler 1980;Dressler et al 1997) or to the Butcher-Oemler effect (Butcher & Oemler 1978;Couch et al 1998;Goto et al 2003). The mechanism of tidal compression exerted by the gravitational potential of a galaxy cluster is known to increase the velocity dispersion of the molecular clouds falling in disk galaxies (e.g., Valluri 1993;Byrd & Valtonen 1990), thus inducing star formation episodes (e.g., Henriksen & Byrd 1996;Evrard 1991). Tidal compression is also responsible for the so-called galaxy-harassment phenomenon in the case of dwarf galaxies (Moore et al 1996(Moore et al , 1998(Moore et al , 1999 or late-type systems A&A 542, A17 (2012) (see e.g., Murali 2000;Nidever et al 2010), where the authors constrained the density of the coronal gas to be n < 10 −5 cm −3 at the distance of 50 kpc in order to let the Stream clouds survive up to 2.5 Gyr or at least a minimum of 0.5 Gyr.…”

Section: Introductionmentioning

confidence: 99%

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Dissipative phenomena in extended-body interactions

Pasetto

Bertelli

Grebel

et al. 2012

A&A

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Aims. Dissipative phenomena occurring during the orbital evolution of a dwarf satellite galaxy around a host galaxy may leave signatures in the star formation activity and signatures in the colour-magnitude diagram of the galaxy stellar content. Our goal is to reach a simple and qualitative description of these complicated phenomena. Methods. We develop an analytical and numerical technique able to study the ram pressure, Kelvin-Helmholtz instability, RayleighTaylor, and tidal forces acting on the star formation processes in molecular clouds. We consider it with synthetic colour-magnitude diagram techniques. Results. We developed a method of investigating the connections between gas consumption processes and star formation processes in the context of the two extended-body interactions, paying special attention to the dwarf galaxies dynamical regime.

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Section: Galaxy Model and Plasma Distributionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Dissipative phenomena in extended-body interactions

Pasetto

Bertelli

Grebel

et al. 2012

A&A

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“…Physical processes could drive these differences, but luckily, as galaxies are accreted and orbit within a cluster, each physical process may leave characteristic low surface brightness signatures. Gravitational effects, including mergers and low-energy interactions (Mihos 2004(Mihos , 2005, tidal stripping (Henriksen & Byrd 1996), and high-speed harassment (Moore et al 1998), will strip or eject stellar material into the intracluster medium (ICM). This was recently statistically studied within the CLASH sample (Postman et al 2012) by Burke et al (2015), who concluded that the growth of stellar mass in the ICL is larger than can be provided by the brightest cluster galaxy (BCG) close companions, and that the majority of the ICL mass must come from galaxies which fall from outside of the core of the clusters.…”

Section: Introductionmentioning

confidence: 99%

The XXL Survey

Adami

Pompei

Sadibekova

et al. 2016

A&A

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Aims. Within a cluster, gravitational effects can lead to the removal of stars from their parent galaxies and their subsequent dispersal into the intracluster medium. Gas hydrodynamical effects can additionally strip gas and dust from galaxies; both gas and stars contribute to intracluster light (ICL). The properties of the ICL can therefore help constrain the physical processes at work in clusters by serving as a fossil record of the interaction history. Methods. The present study is designed to characterise this ICL for the first time in a ∼10 14 M and z ∼ 0.53 cluster of galaxies from imaging and spectroscopic points of view. By applying a wavelet-based method to CFHT Megacam and WIRCAM images, we detect significant quantities of diffuse light and are able to constrain their spectral energy distributions. These sources were then spectroscopically characterised with ESO Multi Unit Spectroscopic Explorer (MUSE) spectroscopic data. MUSE data were also used to compute redshifts of 24 cluster galaxies and search for cluster substructures.Results. An atypically large amount of ICL, equivalent in i to the emission from two brightest cluster galaxies, has been detected in this cluster. Part of the detected diffuse light has a very weak optical stellar component and apparently consists mainly of gas emission, while other diffuse light sources are clearly dominated by old stars. Furthermore, emission lines were detected in several places of diffuse light. Our spectral analysis shows that this emission likely originates from low-excitation parameter gas. Globally, the stellar contribution to the ICL is about 2.3 × 10 9 yr old even though the ICL is not currently forming a large number of stars. On the other hand, the contribution of the gas emission to the ICL in the optical is much greater than the stellar contribution in some regions, but the gas density is likely too low to form stars. These observations favour ram pressure stripping, turbulent viscous stripping, or supernovae winds as the origin of the large amount of intracluster light. Since the cluster appears not to be in a major merging phase, we conclude that ram pressure stripping is the most plausible process that generates the observed ICL sources. Conclusions. This is one of the first times that we are able to spectroscopically study diffuse light in such a distant and massive cluster, and it demonstrates the potential of MUSE observations for such studies.

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“…However, neither can gas stripping explain the many AGN observed in CG (e.g., Coziol et al 1998Coziol et al , 2000Martínez et al 2010). These AGN are related to the formation of numerous early-type galaxies through tidal triggering, a mechanism that funnels gas down directly into the center of galaxies, starting a sequence of bursts of star formation that increase the mass of the bulges, and forming, or feeding, a SMBH at their centers (Merritt 1983(Merritt , 1984Byrd & Valtonen 1990;Henriksen & Byrd 1996;Fujita 1998). However, because the level of these activities is generally low, we would then have to assume that these events have taken place sometime in the recent past, or possibly during the formation of the CG (Coziol et al 2004;Mendes de Oliveira et al 2005).…”

Section: Introductionmentioning

confidence: 99%

The star formation histories of Hickson compact group galaxies

Plauchu-Frayn

Olmo

Coziol

et al. 2012

A&A

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Aims. We study the star formation fistory (SFH) of 210 galaxy members of 55 Hickson compact groups (HCG) and 309 galaxies from the Catalog of Isolated Galaxies (CIG). The SFH traces the variation of star formation over the lifetime of a galaxy, and consequently yields a snapshot picture of its formation. Comparing the SFHs in these extremes in galaxy density allows us to determine the main effects of compact groups (CG) on the formation of galaxies. Methods. We fit our spectra using the spectral synthesis code STARLIGHT and obtained the stellar population contents and mean stellar ages of HCG and CIG galaxies in three different morphological classes: early-type galaxies (EtG), early-type spirals (EtS), and late-type spirals (LtS). Results. We find that EtG and EtS galaxies in HCG show higher contents of old and intermediate stellar populations as well as an important deficit of the young stellar population, which clearly implies an older average stellar age in early galaxies in HCG. For LtS galaxies we find similar mean values for the stellar content and age in the two samples. However, we note that LtS can be split into two subclasses, namely old and young LtS. In HCG we find a higher fraction of young LtS than in the CIG sample, in addition, most of these galaxies belong to groups in which most of the galaxies are also young and actively forming stars. The specific star formation rate (SSFR) of spiral galaxies in the two samples differ. The EtS in HCG show lower SSFR values, while LtS peak at higher values compared with their counterparts in isolation. We also measured the shorter star formation time scale (SFTS) in HCG galaxies, which indicates that they have a shorter star formation activity than CIG galaxies. We take these observations as evidence that galaxies in CG have evolved more rapidly than galaxies in isolation, regardless of their morphology. Our observations are consistent with the hierarchical galaxy formation model, which states that CGs are structures that formed recently from primordial small-mass density fluctuations. From the systematic difference in SFTS we deduce that the HCG have most probably formed ∼3 Gyr in the past. The galaxies in the HCG are not in equilibrium state, but merging without gas (i.e., under dissipationless conditions), which may explain their relatively long lifetime.

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Tidal Triggering of Star Formation by the Galaxy Cluster Potential

Cited by 77 publications

References 0 publications

Dissipative phenomena in extended-body interactions

Dissipative phenomena in extended-body interactions

The XXL Survey

The star formation histories of Hickson compact group galaxies

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