Gas stripping in galaxy clusters: a new SPH simulation 
approach

Jáchym, Pavel; Palouš, J.; Köppen, J.; Combes, F.

doi:10.1051/0004-6361:20066442

Cited by 63 publications

(96 citation statements)

References 27 publications

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“…In Jáchym et al (2007) for an example the stripped ISM does not show clumps of cool gas. In the eulerian grid simulations of Roediger et al (2006) the wake does show cooler, dense regions, but the number is much less as in the simulations presented here.…”

Section: Comparison To Other Simulations Of Ram-pressure Strippingmentioning

confidence: 99%

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies

Kapferer¹,

Sluka²,

Schindler³

et al. 2009

A&A

208

253

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Aims. We investigate the dependence of star formation and the distribution of the components of galaxies on the strength of ram pressure. Several mock observations in X-ray, Hα and HI wavelength for different ram-pressure scenarios are presented. Methods. By applying a combined N-body/hydrodynamic description (GADGET-2) with radiative cooling and a recipe for star formation and stellar feedback 12 different ram-pressure stripping scenarios for disc galaxies were calculated. Special emphasis was put on the gas within the disc and in the surroundings. All gas particles within the computational domain having the same mass resolution. The relative velocity was varied from 100 km s −1 to 1000 km s −1 in different surrounding gas densities in the range from 1 × 10 −28 to 5 × 10 −27 g/cm 3 . The temperature of the surrounding gas was initially 1 × 10 7 K. Results. The star formation of a galaxy is enhanced by more than a magnitude in the simulation with a high ram-pressure (5 × 10 −11 dyn/cm 2 ) in comparison to the same system evolving in isolation. The enhancement of the star formation depends more on the surrounding gas density than on the relative velocity. Up to 95% of all newly formed stars can be found in the wake of the galaxy out to distances of more than 350 kpc behind the stellar disc. Continuously stars fall back to the old stellar disc, building up a bulge-like structure. Young stars can be found throughout the stripped wake with surface densities locally comparable to values in the inner stellar disc. Ram-pressure stripping can shift the location of star formation from the disc into the wake on very short timescales. As the gas in a galaxy has a complex velocity pattern due to the rotation and spiral arms, the superposition of the internal velocity field and the ram pressure causes complex structures in the gaseous wake which survive dynamically up to several 100 Myr. Finally we provide simulated X-ray, Hα and HI observations to be able to compare our results with observations in these wavebands. These simulated observations show many features which depend strongly both on the strength and the duration of the external ram pressure.

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Section: Comparison To Other Simulations Of Ram-pressure Strippingmentioning

confidence: 99%

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies

Kapferer¹,

Sluka²,

Schindler³

et al. 2009

A&A

208

253

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“…The buildup of HI and enhancement of radio continuum emission in NGC 1961's southeastern ridge could then be accounted for by an edge-on stripping geometry. For such a geometry, simulations predict that a galaxy encountering an intragroup medium for the first time should have its H I extended on the side where the galactic rotation adds to the velocity relative to the IGM and the gas is more stripped on the other side (see the explanation of this paradox in Roediger & Brüggen 2006;Jachym et al 2007Jachym et al , 2009). For NGC 1961, which is falling into its group from the northwest, we see an extended H I structure on the northern side of the galaxy, coming from the west (Haan et al 2008).…”

Section: A Possible Minor Mergermentioning

confidence: 99%

Molecular gas in NUclei of GAlaxies (NUGA)

Combes

Baker²,

Schinnerer³

et al. 2009

A&A

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We present high-resolution maps of the CO(1-0) and CO(2-1) emission from the LINER 2 galaxy NGC 1961. This galaxy is unusual among late-type (Sc) disk galaxies in having a very large radial extent and inferred dynamical mass. We propose a head-on collision scenario to explain the perturbed morphology of this galaxy -both the off-centered rings and the inflated radius. This scenario is supported by the detection of a steep velocity gradient in the CO(1-0) map at the position of a southwest peak in radio continuum and near-infrared emission. This peak would represent the remnant of the disrupting companion. We use numerical models to demonstrate the plausibility of the scenario. While ram pressure stripping could in principle be important for shocking the atomic gas and produce the striking head-tail morphology, the non detection of this small galaxy group in X-ray emission suggests that any hot intragroup medium has too low a density. A prediction of the collision model is the propagation of ring waves from the center to the outer parts, superposed on a probable pre-existing m = 2 barred spiral feature, accounting for the observed complex structure of rings and spokes. This lopsided wave accounts for the sharp boundary observed in the atomic gas on the southern side. Through dynamical friction, the collision finishes quickly in a minor merger, the best fit being for a companion with a mass ratio 1:4. We argue that NGC 1961 has a strongly warped disk, which gives the false impression of a nearly face-on system; the main disk is actually more edge-on, and this error in the true inclination has led to the surprisingly high dynamical mass for a morphologically late-type galaxy. In addition, the outwardly propagating ring artificially enlarges the disk. The collision de-stabilizes the inner disk and can provide gas inflow to the active nucleus.

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“…Numerical modeling has shown that ram pressure stripping is a very efficient process for removing the gaseous content of cluster galaxies (e.g., Vollmer et al 2001;Roediger & Hensler 2005;Jáchym et al 2007Jáchym et al , 2009. Simulations also predict that material IC3418 M87 M86 0.5 deg Fig.…”

Section: Introductionmentioning

confidence: 95%

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

Jáchym¹,

Kenney²,

Růžička³

et al. 2013

A&A

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We present IRAM 30m sensitive upper limits on CO emission in the ram pressure stripped dwarf Virgo galaxy IC3418 and in a few positions covering H ii regions in its prominent 17 kpc UV/Hα gas-stripped tail. In the central few arcseconds of the galaxy, we report a possible marginal detection of about 1 × 10 6 M ⊙ of molecular gas (assuming a Galactic CO-to-H 2 conversion factor) that could correspond to a surviving nuclear gas reservoir. We estimate that there is less molecular gas in the main body of IC3418, by at least a factor of 20, than would be expected from the pre-quenching UV-based star formation rate assuming the typical gas depletion timescale of 2 Gyr. Given the lack of star formation in the main body, we think the H 2 -deficiency is real, although some of it may also arise from a higher CO-to-H 2 factor typical in low-metallicity, low-mass galaxies. The presence of H ii regions in the tail of IC3418 suggests that there must be some dense gas; however, only upper limits of < 1 × 10 6 M ⊙ were found in the three observed points in the outer tail. This yields an upper limit on the molecular gas content of the whole tail < 1 × 10 7 M ⊙ , which is an amount similar to the estimates from the observed star formation rate over the tail. We also present strong upper limits on the X-ray emission of the stripped gas in IC3418 from a new Chandra observation. The measured X-ray luminosity of the IC3418 tail is about 280 times lower than that of ESO 137-001, a spiral galaxy in a more distant cluster with a prominent ram pressure stripped tail. Non-detection of any diffuse X-ray emission in the IC3418 tail may be due to a low gas content in the tail associated with its advanced evolutionary state and/or due to a rather low thermal pressure of the surrounding intra-cluster medium.

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Gas stripping in galaxy clusters: a new SPH simulation approach

Cited by 63 publications

References 27 publications

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies

Molecular gas in NUclei of GAlaxies (NUGA)

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

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