Hierarchical formation of bulgeless galaxies: why outflows have low angular momentum

By C. Brook, Fabio Governato, Rok Roskar, G. Stinson, A. Brooks, James Wadsley, Thomas P. Quinn, Bradley K Gibson, O. Snaith, K. Pilkington and 2 more. 2010

201 citations recorded by the source corpus.

Using high resolution, fully cosmological smoothed particle hydrodynamical simulations of dwarf galaxies in a Lambda cold dark matter Universe, we show how high redshift gas outflows can modify the baryon angular momentum distribution and allow pure disc galaxies to form. We outline how galactic outflows preferentially remove low angular momentum material due a combination of (a) star formation peaking at high redshift in shallow dark matter potentials, an epoch when accreted gas has relatively low angular momentum, (b) the existence of an extended reservoir of high angular momentum gas in the outer disc to provide material for prolonged SF at later times and (c) the tendency for outflows to follow the path of least resistance which is perpendicular to the disc. We also show that outflows are enhanced during mergers, thus expelling much of the gas which has lost its angular momentum during these events, and preventing the formation of ‘classical’, merger driven bulges in low-mass systems. Stars formed prior to such mergers form a diffuse, extended stellar halo component similar to those detected in nearby dwarfs.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9935fd441a3c3434a284cce0e7ed1fd42ad95fa4

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Citations in the corpus

A UNIVERSAL, LOCAL STAR FORMATION LAW IN GALACTIC CLOUDS, NEARBY GALAXIES, HIGH-REDSHIFT DISKS, AND STARBURSTS (2011, unknown): “Finally, we note that our discussion does not address the issue of what density resolution is required for a correct treatment of star formation feedback (e.g. Governato et al. 2010; Brook et al. 2011).”
Stellar Feedback in Galaxies and the Origin of Galaxy-scale Winds (2011, background): “Often cooling (along with star formation and other hydrodynamic processes) is ‘turned off’ for an extended period of time (Thacker & Couchman 2000; Governato et al. 2007; Brook et al. 2011).”
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations (2015, background): “…the efficiency of feedback still impacts upon galaxy sizes: feedback preferentially ejects the lowest angular momentum gas in galaxies (e.g. Brook et al. 2011, 2012), so the heating (and concomitant ejection) of more gas per unit stellar mass formed in the StrongFB model with respect to…”
Constraining sub-grid physics with high-redshift spatially-resolved metallicity distributions (2013, methodology): “The MaGICC feedback prescription is outlined in a series of papers (Brook et al. 2011, 2012a,b,c; Pilkington et al. 2012b; Stinson et al. 2012, 2013).”
THE BIMODAL METALLICITY DISTRIBUTION OF THE COOL CIRCUMGALACTIC MEDIUM AT z ≲ 1 (2013, background): “…galaxy disks (e.g., Dekel & Birnboim 2006; Stewart et al. 2011b; Rubin et al. 2012; Shen et al. 2013), while on the other hand, stellar feedback in galaxies tends to be bi-conical, near perpendicular to the galaxy major axis (e.g., Strickland et al. 2004; Bouché et al. 2012; Brook et al. 2011).”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, background): “…Brook et al. 2007; Stinson et al. 2006; Sijacki et al. 2007; Scannapieco et al. 2009; Agertz et al. 2009; Schaye et al. 2010; Agertz et al. 2011; Brook et al. 2011) with improved descriptions of cooling, star formation, black hole formation, and luminous, mechanical and material feedback from…”
Four phases of angular-momentum buildup in high-z galaxies: from cosmic-web streams through an extended ring to disc and bulge (2014, background): “…gas from the dense central regions where the SFR is high and the AGN activity takes place, and therefore the outflows tend to increase the effective sAM of the remaining gas in the disc (e.g. Maller & Dekel 2002; Governato et al. 2010; Brook et al. 2011; Brooks et al. 2011; Guedes et al. 2011).”
HIGH-RESOLUTION MASS MODELS OF DWARF GALAXIES FROM LITTLE THINGS (2015, background): “…in galaxies can be substantially redistributed by frequent explosions of supernovae (SNe) (Larson 1974; Navarro et al. 1996a; Dekel et al. 2003; Mo & Mao 2004; Mashchenko et al. 2008; de Souza et al. 2011; Brook et al. 2011; Pontzen & Governato 2012; Di Cintio et al. 2014; Ogiya & Mori 2014 etc.).”
REPRODUCING THE STELLAR MASS/HALO MASS RELATION IN SIMULATED ΛCDM GALAXIES: THEORY VERSUS OBSERVATIONAL ESTIMATES (2012, background): “As discussed in Brook et al. (2011) and Pontzen & Governato (2012), a bursty SFH is necessary to remove low angular momentum baryons and create the fast outflows able to transfer energy from baryons to the DM component and create DM cores (Governato et al. 2010).”
Self-regulated star formation in galaxies via momentum input from massive stars (2011, background): “For this reason, in order to make SN feedback have any significant effect (even in MW-like galaxies), simulators often ‘turn-off’ cooling (often along with star formation and/or other hydrodynamic processes) for an extended period of time, much longer than τ cool (cooling is typically suppressed for”
MaGICC discs: matching observed galaxy relationships over a wide stellar mass range (2012, methodology): “We have previously shown that the outflows in our model remove low angular momentum gas (Brook et al. 2011), resolving the ‘angular momentum problem’ which has plagued simulations (e.g. Navarro & Steinmetz 2000; Piontek & Steinmetz 2011).”
The origin of discs and spheroids in simulated galaxies (2011, background): “…that morphologies can be radically altered when even modest changes in the strength of feedback or its implementation are introduced (Okamoto et al. 2005; Scannapieco et al. 2008; Ceverino & Klypin 2009; Sales et al. 2010; Agertz, Teyssier & Moore 2011; Brook et al. 2011; Piontek & Steinmetz 2011).”
The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time (2016, background): “The adoption of any of these schemes ultimately removes low-angular momentum gas from the central regions of the galaxy (Governato et al. 2010; Brook et al. 2011) and prevents the overcooling of gas and the growth of massive stellar bulges.”
Cuspy No More: How Outflows Affect the Central Dark Matter and Baryon Distribution in Lambda CDM Galaxies (2012, background): “These outflows efficiently remove gas from the inner kpc of protogalaxies (Brook et al. 2011) and, in smaller galaxies, are able to expel a large fraction of gas from the galaxy altogether.”
Galaxies on FIRE (Feedback In Realistic Environments): stellar feedback explains cosmologically inefficient star formation (2013, background): “…particularly true of models which invoke only energetic feedback via supernovae (SNe), which is efficiently radiated in the dense gas where star formation actually occurs (see e.g. Guo et al. 2010; Powell et al. 2011; Brook et al. 2011; Nagamine 2010; Bournaud et al. 2011, and references therein).”
BARYONS MATTER: WHY LUMINOUS SATELLITE GALAXIES HAVE REDUCED CENTRAL MASSES (2012, methodology): “…because the effect of energetic feedback from supernovae (SNe) can reduce the baryonic (Dekel & Silk 1986; Maller & Dekel 2002; Dekel et al. 2003a; Brook et al. 2011; Guedes et al. 2011) and DM mass at the centers of galaxies (Navarro et al. 1996; Read & Gilmore 2005; Mashchenko et al. 2006,…”
Toy models for galaxy formation versus simulations (2013, background): “…way angular momentum is transported into the disc by cold streams from the cosmic web (Kimm et al. 2011; Pichon et al. 2011; Danovich et al. 2012; Stewart et al. 2013), and (b) because outflows tend to preferentially carry away low-angular-momentummaterial (Maller & Dekel 2002; Brook et al. 2011).”
ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, background): “Recent work in numerical simulations of disk galaxy formation has emphasized how outflows might remove low-jg material, which counteracts j-loss through tidal torques during galaxy collapse, and maintains a high net level of fj (e.g., Brook et al. 2011; Guedes et al. 2011).”