Ram Pressure Stripping and Galaxy Orbits: The Case of the Virgo Cluster

By B. Vollmer, V. Cayatte, C. Balkowski, W. J. D. M. F. Radioastronomie, Bonn, Germany, Daec, O. Paris, France, Ita and 1 more. 2001

326 citations recorded by the source corpus.

We investigate the role of ram pressure stripping in the Virgo Cluster using N-body simulations. Radial orbits within the Virgo Cluster's gravitational potential are modeled and analyzed with respect to ram pressure stripping. The N-body model consists of 10,000 gas cloud complexes that can have inelastic collisions. Ram pressure is modeled as an additional acceleration on the clouds located at the surface of the gas distribution in the direction of the galaxy's motion within the cluster. We made several simulations, changing the orbital parameters in order to recover different stripping scenarios using realistic temporal ram pressure profiles. We investigate systematically the influence of the inclination angle between the disk and the orbital plane of the galaxy on the gasdynamics. We show that ram pressure can lead to a temporary increase of the central gas surface density. In some cases a considerable part of the total atomic gas mass (several 108 M☉) can fall back onto the galactic disk after the stripping event. A quantitative relation between the orbit parameters and the resulting H I deficiency is derived containing explicitly the inclination angle between the disk and the orbital plane. The comparison between existing H I observations and the results of our simulations shows that the H I deficiency depends strongly on galaxy orbits. It is concluded that the scenario in which ram pressure stripping is responsible for the observed H I deficiency is consistent with all H I 21 cm observations in the Virgo Cluster.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/24437ce4b8f8ead5a34c2c12a00d70517c6b63d4

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Citations in the corpus

Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters (2007, background): “…star formation rates (and redder colours) of cluster spirals relative to their field counterparts (e.g., Abadi et al. 1999; Quilis et al. 2000; Vollmer et al. 2001; Okamoto & Nagashima 2003; Mayer et al. 2006; Roediger et al. 2006; Hester 2006; Jachym et al. 2007; Roediger & Brüggen 2006;…”
On the influence of ram-pressure stripping on the star formation of simulated spiral galaxies (2008, background): “The stripping radius with respect to acting ram pressure and galaxy properties was investigated (e.g. Abadi et al. 1999, Vollmer et al. 2001, Roedig r & Hensler 2005) and a reasonable agreement between the analytically estimated stripping radius and the stripping radius from numerical simulations…”
VLA H I Observations of Gas Stripping in the Virgo Cluster Spiral NGC 4522 (2004, background): “Simulations suggest stripping rates which vary approximately as cos2i (Vollmer et al. 2001 ; Schulz & Struck 2001).”
The gravitational and hydrodynamical interaction between the Large Magellanic Cloud and the Galaxy (2004, background): “The dependence of ram pressure on the satellite orientation is not a simple function of the angle between the disc plane and the orbital velocity (Vollmer et al. 2001) and can depend on the ram pressure and the structure of the satellite (Abadi, Moore & Bower 1999; Quilis et al. 2000; Schulz &…”
The effect of ram pressure on the star formation, mass distribution and morphology of galaxies (2009, background): “The dependence of the stripping radius on the external ram pressure and the galaxy properties was investigated (e.g. Abadi et al. 1999; Vollmer et al. 2001; Roediger & Hensler 2005) and a remarkable agreement between analytical estimates and numerical simulations was found.”
MUSE sneaks a peek at extreme ram-pressure stripping events - I. A kinematic study of the archetypal galaxy ESO137-001 (2014, methodology): “In synergy with models and numerical simulations (e.g. Gunn & Gott 1972; Nulsen 1982; Moore et al. 1996; Quilis et al. 2000; Schulz & Struck 2001; Vollmer et al. 2001a; Bekki & Couch 2003; Kronberger et al. 2008; Tonnesen & Bryan 2010; Ruszkowski et al. 2014), these pculiar systems are in fact…”
Pre-Processing of Galaxies before Entering a Cluster (2003, background): “…of an ingredient of stars (Gunn, Gott 1972; Balsara et al. 1994; Fujita, Nagashima 1999; Abadi et al. 1999; Quilis et al. 2000; Mori, Burkert 2000; Vollmer et al. 2001; Bicker et al. 2002), although ram-pressure may cause a mild increase of star formation of a galaxy (Fujita, Nagashima 1999) or a…”
Ram pressure stripping of disc galaxies orbiting in clusters – I. Mass and radius of the remaining gas disc (2007, background): “Interestingly, the sticky-particle simulations of Vollmer et al. (2001) where the galaxies were also exposed to a varying ram pressure found gas backfall of up to 5×108M⊙ after pericentre passage, primarily for edge-on galaxies.”
The Origin of Dwarf Ellipticals in the Virgo Cluster (2008, methodology): “The gas-loss rate adopted is then equal to ǫ Σgas Σpotential , with the efficiency ǫ following a Gaussian having a maximum ǫ0 at the time trp, chosen to mimic the variation of the ram pressure suggested by Vollmer et al. (2001).”
Virgo Galaxies with Long One-sided H I Tails (2007, methodology): “…have been estimated assuming the β-model (Schindler, Binggeli & Böhringer 1999) with the same coefficients for the Virgo cluster presented as in Vollmer et al. (2001). its GALEX (Galaxy Evolution Explorer) image shows a UV tail from the SW end of the optical disk along the Hi to the NW,…”
The effect of the environment on the Hi scaling relations (2011, background): “The ram pressure stripping event is simulated by assuming a gas- loss rate inversely proportional to the potential of the galaxy, with an efficiency depending on the density of the intracluster medium (taken from Vollmer et al. 2001).”
Hα Tail, Intracluster H II Regions, and Star Formation: ESO 137-001 in Abell 3627 (2007, background): “ESO 137-001 was undetected in the HI observations with ATCA by Vollmer et al. (2001).”
The role of dwarf galaxy interactions in shaping the Magellanic System and implications for Magellanic Irregulars (2012, unknown): “Following Martin et al. (2002), the initial mass function (IMF) averaged metallicity of SNe ejecta is ZO,SN ∼ 8 times solar for oxygen.”
A large H I cloud near the centre of the Virgo cluster (2005, unknown): “Indeed, NGC 4388 is often discussed as a good example of a galaxy undergoing rampressure stripping (Vollmer et al. 2001; Vollmer & Huchtmeier 2003).”
BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, background): “Although it is well-known that their formula is best at predicting the stripping radius in the case of face-on stripping, other inclination angles (with respect to the infall trajectory) can lead to more complex behaviour (e.g. Abadi et al. 1999; Vollmer et al. 2001).”
Environmental Effects on Late‐Type Galaxies in Nearby Clusters (2006, background): “In the case of edge-on stripping, more than 50% of the stripped gas can be reaccreted, whereas in face-on encounters, the fraction of reaccreted gas is significantly smaller (Vollmer et al. 2001b).”
Ram pressure stripping of disk galaxies. From high to low density environments (2005, background): “In further papers (Vollmer et al. 2000, 2001a, 1999; Vollmer 2003) this group tried to explain the features of individual galaxies by comparing simulation results with observations and specifying the ram pressure, inclination angle and the moment of the stripping event.”
GASP. I. Gas Stripping Phenomena in Galaxies with MUSE (2017, background): “…it is a good approximation of the cluster virial radius. assuming a smooth static ICM, r r= + b-⎡ ⎣ ⎢⎢ ⎛ ⎝⎜ ⎞ ⎠⎟ ⎤ ⎦ ⎥⎥( ) ( )r r r 1 , 4 c cl 0 cl 2 3 2 ICM with core radius =r 13.4 kpcc , slope parameter β=0.5, and central density r = ´ -4 10 cm0 2 3 (the same values used in Vollmer et al. 2001).”