Formation of isolated dwarf galaxies with feedback

By T. Sawala, C. Scannapieco, Umberto De Maio, Simon D. M. White. 2009

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We present results of high resolution hydrodynamical simulations of the formation and evolution of dwarf galaxies. Our simulations start from cosmological initial conditions at high redshift. They include metal-dependent cooling, star formation, feedback from type II and type Ia supernovae and UV background radiation, with physical recipes identical to those applied in a previous study of Milky Way type galaxies. We find that a combination of feedback and the cosmic UV background results in the formation of galaxies with properties similar to the Local Group dwarf spheroidals, and that their effect is strongly moderated by the depth of the gravitational potential. Taking this into account, our models naturally reproduce the observed luminosities and metallicities. The final objects have halo masses between 2.3 × 10 8 and 1.1 × 10 9 M� , mean velocity dispersions between 6.5 and 9.7 kms −1 , stellar masses ranging from 5 × 10 5 to 1.2 ×10 7 M� , median metallicities between [Fe/H] = 1:8 and 1:1, and half-light radii of the order of 200 to 300 pc, all comparable with Local Group dwarf spheroidals. Our simulations also indicate that the dwarf spheroidal galaxies observed today lie near a halo mass threshold around 10 9 M� , in agreement with stellar kinematic data, where supernova feedback not only suffices to completely expel the i nterstellar medium and leave the residual gas-free, but where the combination of feedback, UV radiation and self-shielding establishes a dichotomy of age distributions similar to that observed in the Milky Way and M31 satellites.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c8b333cedd8c759e9c4676b5089407d3b43e4400

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Citations in the corpus

The APOSTLE simulations: solutions to the Local Group's cosmic puzzles (2015, background): “…hydrodynamic simulations which have confirmed the importance of baryonic effects have largely focused on individual dwarf galaxies, ignoring the LG environment (e.g. Stinson et al. 2009; Governato et al. 2010; Sawala et al. 2010, 2011; Nickerson et al. 2011; Shen et al. 2014; Wheeler et al. 2015).”
A Comprehensive Study of Galaxies at z ∼ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch (2022, background): “…radiation heats up H I gas in low-mass halos of Mh 108−9Me with negligible H I self-shielding, suppressing star formation at the EoR and post-EoR (Barkana & Loeb 2000; Susa & Umemura 2004; Hoeft et al. 2006; Mesinger et al. 2009; Pawlik & Schaye 2009; Sawala et al. 2010; BlandHawthorn et al. 2015).”
Constraints on star formation driven galaxy winds from the mass–metallicity relation at z= 0 (2010, result): “Regardless, this need for a high and mass-dependent wind efficiency is in broad agreement with previous studies (Dekel & Woo 2003; Dutton et al. 2010b; Sawala et al. 2010; Spitoni et al. 2010).”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, background): “This naturally results in self-regulated winds which are adapted to the depth of the potential well in which star formation is occurring (Scannapieco et al. 2006, 2009; Sawala et al. 2010, 2011; De Rossi et al. 2010).”
The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR (2009, methodology): “Sawala et al. (2010) used the multiphase scheme for the interstellar medium developed by Scannapieco et al. (2005, 2006), and constrained the fraction of metals given to the cold gas phase, later defining the final metallicity for a given stellar mass, on the metallicity-relation of dwarf galaxies.”
Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology (2010, background): “This results in a considerable sharpening of the constraints on galaxy formation within the ΛCDM model (Guo et al. 2010; Sawala et al. 2010), making it timely to reassess the viability of current models, in particular their ability to reproduce the faint end of the galaxy luminosity (or stellar…”
A METHOD FOR MEASURING (SLOPES OF) THE MASS PROFILES OF DWARF SPHEROIDAL GALAXIES (2011, background): “It is therefore instructive tocon- 2 sider recent high-resolution hydrodynamical simulationsby Sawala et al. (2010) and Parry et al. (2011).”
Quenching and ram pressure stripping of simulated Milky Way satellite galaxies (2017, background): “Studies of cosmologically isolated systems at this halo mass have demonstrated the photoevaporation of gas during reionization and the subsequent suppression of post-reionization gas accretion (Sawala et al. 2010; Simpson et al. 2013; Shen et al. 2014).”
THE TWO PHASES OF GALAXY FORMATION (2010, background): “…only a few high resolution galaxy formation calculations, using cosmological initial conditions, beginning to master the physics well enough to match either the winds seen in forming galaxies or the final metal distribution between galaxies and the IGM (Scannapieco et al. 2008; Sawala et al. 2010).”
THE COUPLING BETWEEN THE CORE/CUSP AND MISSING SATELLITE PROBLEMS (2012, background): “…feedback, inefficient cooling of inters llar media, cosmic reionization, UV radiation, and acousticoscillations have all been invoked to explain the suppressionof galaxy formation in low-mass satellite haloes (e.g. Tassiset al. 2008; Bovill & Riccotti 2009; Sawala et al. 2010; Bovy & Dvorkin 2012).”
The formation of disc galaxies in a ΛCDM universe (2010, background): “On the same topic, Sawala et al. (2010) argues that modern simulations of dwarf galaxy formation (Valcke et al. 2008; Stinson et al. 2009; Governato et al. 2010) all yield much larger stellar masses than expected from observations as well as gas-tostar conversion efficiencies almost an order of…”
MaGICC discs: matching observed galaxy relationships over a wide stellar mass range (2012, background): “…galaxies by increasing feedback had the trouble of ejecting their gas in high-redshift starbursts, resulting in isolated dwarf spheroidal galaxies (Sawala et al. 2010), rather than dwarfs with prolonged star formation histories and significant amounts of H I gas at z = 0, as observed in the field…”
BARYONS MATTER: WHY LUMINOUS SATELLITE GALAXIES HAVE REDUCED CENTRAL MASSES (2012, background): “The overall gas mass in these low mass subhalos is substantially reduced at early times, due to a combination of reionization and initial SF that ejects gas (see also Sawala et al. 2010).”
Numerical simulations of the dark universe: State of the art and the next decade (2012, background): “Feedback appears to be a crucial ingredient in explaining the macroscopic properties of individual galaxies [337, 352–355] as well as galaxy population statis-”