Simultaneous ram pressure and tidal stripping; how dwarf spheroidals lost their gas

By Lucio Mayer, C. Mastropietro, James Wadsley, Joachim Stadel, B. Moore. 2005

334 citations recorded by the source corpus.

We perform high-resolution N-body+SPH (smoothed particle hydrodynamics) simulations of gas-rich dwarf galaxy satellites orbiting within a Milky Way-sized halo and study for the first time the combined effects of tides and ram pressure. The structure of the galaxy models and the orbital configurations are chosen in accordance with those expected in a Lambda cold dark matter (ACDM) universe. While tidal stirring of disky dwarfs produces objects whose stellar structure and kinematics resembles that of dwarf spheroidals after a few orbits, ram pressure stripping is needed to entirely remove their gas component. Gravitational tides can aid ram pressure stripping by diminishing the overall potential of the dwarf, but tides also induce bar formation which funnels gas inwards making subsequent stripping more difficult. This inflow is particularly effective when the gas can cool radiatively. Assuming a low density of the hot Galactic corona consistent with observational constraints, dwarfs with V peak 30 km s -1 lose most or all of their gas content only if a heating source keeps the gas extended, partially counteracting the bar-driven inflow. We show that the ionizing radiation from the cosmic ultraviolet (UV) background at z > 2 can provide the required heating. In these objects, most of the gas is removed or becomes ionized at the first pericenter passage, explaining the early truncation of the star formation observed in Draco and Ursa Minor. Galaxies on orbits with larger pericenters and/or falling into the Milky Way halo at lower redshift can retain significant amounts of the centrally concentrated gas. These dwarfs would continue to form stars over a longer period of time, especially close to pericenter passages, as observed in Fornax and other dwarf spheroidal galaxies (dSphs) of the Local Group. The stripped gas breaks up into individual clouds pressure confined by the outer gaseous medium that have masses, sizes and densities comparable to the H I clouds recently discovered around M31.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

THE SAGITTARIUS DWARF GALAXY: A MODEL FOR EVOLUTION IN A TRIAXIAL MILKY WAY HALO (2010, background): “…two-component King-profile stellar core com- bined with an extended NFW dark matter halo), or consider the possible conversion of an originally disky dwarf to a dSph via tidal stirring (e.g., Mayer et al. 2006) the mass loss history could also be very different (see, e.g., Read et al. 2006ab).”
Cold gas stripping in satellite galaxies: from pairs to clusters (2016, background): “…in significant amounts over many gigayears; however, such effects are expected to be dominant in dwarf galaxies, i.e. those with circular velocities 30 km s−1, which are smaller than the galaxies we are studying here (see Mastropietro et al. 2005; Mayer et al. 2006; Tomozeiu, Mayer & Quinn 2016).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “…which acts to remove the supply of cold gas in a satellite galaxy, or dynamical effects such as tidal disruption or harassment, responsible for switching off the star formation these galaxies (Gunn & Gott 1972; Moore et al. 1996; Balogh et al. 2004b; Wilman et al. 2005a; Mayer et al. 2006).”
Small scale problems of the $\Lambda$CDM model: a short review (2016, background): “st solving the problem (see Figure13, bottom right panel). c. Photo-ionisation from stellar and supernova feedback (e.g., Refs. [303,387,388]), and generally stripping gas by ram pressure (e.g., Ref. [389]). Because of the photo-ionisation threshold, UFDs’ baryons to stars conversion efﬁciency lies ”
Gaia DR2 proper motions of dwarf galaxies within 420 kpc (2018, background): “…(UFDs) lose their gas due to internal stellar feedback or due to a combination of internal and external effects, such as UVbackground heating and/or tidal and ram-pressure stripping from the large Local Group spirals (e.g. Mayer et al. 2006; Bermejo-Climent et al. 2018; Revaz & Jablonka 2018)?”
THE ACS NEARBY GALAXY SURVEY TREASURY. VIII. THE GLOBAL STAR FORMATION HISTORIES OF 60 DWARF GALAXIES IN THE LOCAL VOLUME (2011, background): “Instead, Mayer et al. (2001a, 2006) advocate a more complex approach in which a combination of ram pressure stripping and stellar mass loss due to tidal effects provide a plausible model, ‘tidal stirring’, for the transformation of gas-rich dIs into gas-poor dSphs.”
Are the Magellanic Clouds on Their First Passage about the Milky Way? (2007, background): “The SMC’s ability to retain such a highgas fraction on an orbit with a pericenter of only 60 kpc suggests that it was accreted at a low redshift (Mayer et al. 2006).”
The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR (2009, background): “This strongly supports stripping of the gas by external gravitational and/or hydrodynamical interactions (see for example, Mayer et al. 2006), even though the bulk of the galaxy formation could be determined by their initial conditions.”
Gaseous Galaxy Halos (2012, background): “Since most galaxies are likely to be stripped at radii > 20 kpc (Grcevich & Putman, 2009; Mayer et al., 2006; Nichols & Bland-Hawthorn, 2011), much of the cold gas will be integrated into the diffuse galactic halo before eventually recooling at the disk (see §5).”
THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I. HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS (2014, methodology): “…CVn I, Carina, Sculptor) suggest that the environmental history of individual galaxies are also important (e.g., tidal and ram pressure stripping, Mayer et al. 2001, 2006), and should be considered in any evolutionary model of dSphs. Finally, we briefly comment on the dichotomy between…”
Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters (2007, methodology): “…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; 2007).”
The Velocity Dispersion Profile of the Remote Dwarf Spheroidal Galaxy Leo I: A Tidal Hit and Run? (2007, methodology): “This behavior is reflected in some of the models of Mayer et al. (2001a, 2001b, 2006) although these authors did not explore orbits quite as eccentric as we are considering for Leo I.”
Dark Matter Subhalos and the Dwarf Satellites of the Milky Way (2008, background): “Bullock et al. 2000; Benson et al. 2002; Somerville 2002; Kravtsov et al. 2004; Moore et al. 2006), supernova feedback (e.g. Dekel & Silk 1986; Mac Low & Ferrara 1999; Mori et al. 2002), and gas stripping by ram pressure (e.g. Mayer et al. 2006) as favourite suppression mechanisms.”
PRE-REIONIZATION FOSSILS, ULTRA-FAINT DWARFS, AND THE MISSING GALACTIC SATELLITE PROBLEM (2008, background): “In the tidal model (Mayer et al. 2007, 2006), And XII and And XIV would be expected to still harbor significant reservoirs of gas, however, observations show And XIV has MHI < 3 × 103M (Chapman et al. 2007) and And XII has no detected H i (Martin et al. 2006).”
THE LEAST-LUMINOUS GALAXY: SPECTROSCOPY OF THE MILKY WAY SATELLITE SEGUE 1 (2008, result): “This limit is consistent with other dSphs around the Milky Way in which any gas has been presumably removed via ram pressure stripping or used up via tidally-induced star formation (Mayer et al. 2006).”
A lower bound on the mass of dark matter particles (2008, background): “Such a feedback is thought to be responsible to the formation of dwarf spheroidals from gasrich dwarf spiral/irregular galaxies [139–143].”
THE UNIVERSAL STELLAR MASS–STELLAR METALLICITY RELATION FOR DWARF GALAXIES (2013, methodology): “This is best achieved in hydrodynamical simulations (e.g., Mayer et al. 2006; Gatto et al. 2013).”