THE COUPLING BETWEEN THE CORE/CUSP AND MISSING SATELLITE PROBLEMS

By J. Peñarrubia, Andrew Pontzen, M. Walker, Sergey E. Koposov. 2012

171 citations recorded by the source corpus.

We calculate the energy that baryons must inject into cold dark matter (CDM) halos in order to remove centrally divergent DM cusps on scales relevant to observations of dwarf spheroidal galaxies (dSphs). We estimate that the CDM halos often associated with the Milky Way's dSphs (Mvir/M☉ ∼ 109–10) require ΔE ∼ 1053–55 erg in order to form cores on scales comparable to the luminous size of these galaxies. While supernova Type II (SNeII) explosions can in principle generate this energy, the actual contribution is limited by the low star formation efficiency implied by the abundance of luminous satellites. Considering that CDM's well-known “core/cusp” and “missing satellite” problems place opposing demands on star formation efficiencies, existing observational evidences for large cores in the most luminous dSphs require that CDM models invoke some combination of the following: (1) efficient (of the order of unity) coupling of SNeII energy into dark matter particles, (2) star formation histories peaking at unexpectedly high redshifts (z ≳ 6), (3) a top-heavy stellar initial mass function, and/or (4) substantial satellite disruption or other stochastic effects to ease the substructure abundance constraints. Our models show that the tension between CDM problems on small scales would increase if cored DM profiles were to be found in fainter dwarfs.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/aa24502452ed106a2d972dc733d9c5762f413d2c

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Citations in the corpus

NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time (2015, methodology): “This is a still quite debated topic in the literature and our simulations can be used to determine the validity of different analytic approaches (e.g. Peñarrubia et al. 2012 and Maxwell et al. 2015).”
Core formation in dwarf haloes with self-interacting dark matter: no fine-tuning necessary (2014, result): “In contrast, Peñarrubia et al. (2012) and Garrison-Kimmel et al. (2013) have argued that the M?”
The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations (2015, background): “…matter profiles (Blumenthal et al. 1986; Navarro et al. 1996; El-Zant et al. 2001; Gnedin et al. 2004; Read & Gilmore 2005; Governato et al. 2010; Peñarrubia et al. 2012; Governato et al. 2012; Pontzen & Governato 2012; Macciò et al. 2012b; Teyssier et al. 2013; Di Cintio et al. 2014; Pontzen &…”
Forged in FIRE: cusps, cores and baryons in low-mass dwarf galaxies (2015, background): “As pointed out by Peñarrubia et al. (2012), these two requirements are at odds with each other: the need to lower the efficiency of star formation means that there will be less supernovae energy available to create dark matter cores.”
Dwarf galaxies in CDM and SIDM with baryons: observational probes of the nature of dark matter (2014, background): “…mechanism seemingly produces intermediate-mass galaxies (halo mass ∼5−10 × 1010 M ) with realistic cores and stellar-tohalo mass ratios (Governato et al. 2010, 2012), it is questionable if it is energetically viable for lower mass galaxies (Peñarrubia et al. 2012; Garrison-Kimmel et al. 2013).”
Double-Disk Dark Matter (2013, background): “This is in tension with the low star-formation efficiency suggested by the missing satellites problem [122].”
Dark matter cores all the way down (2015, methodology): “Peñarrubia et al. (2012) assume either rc = 1 kpc or rc = 0.1rs.”
WHY BARYONS MATTER: THE KINEMATICS OF DWARF SPHEROIDAL SATELLITES (2012, background): “…halos lead to DM core creation prior to infall (see also Read & Gilmore 2005; Macciò et al. 2012b; Pontzen & Governato 2012; Teyssier et al. 2012b; Peñarrubia et al. 2012; Garrison-Kimmel et al. 2013).1 Many subhalos lose most of their gas after infall and are gas-free by z = 0.2 While some…”
Constraining self-interacting dark matter with the Milky Way’s dwarf spheroidals (2012, methodology): “We note that Peñarrubia et al. (2012) already used Eq.”
The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores (2013, result): “This flattening is 2 UsingMhalo taken from the dark matter only run provides similar results, as the halo mass amongst DM and SPH simulations changes by only a few percent. c© 2010 RAS, MNRAS000, 1–10 due to the increasing energy available from SNe explosions,as derived in Peñarrubia et al. (2012).”
The hidden giant: discovery of an enormous Galactic dwarf satellite in Gaia DR2 (2018, background): “…would be sufficiently large to give each object a ‘normal’ half-light to halo radius ratio correspond to M200 values so large that the ratio of stellar mass to halo mass plummets, rendering the process of core formation energetically implausible (see Peñarrubia et al. 2012; Di Cintio et al. 2014).”
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure (2012, background): “…of star formation could have possibly blown out enough gas to reduce the densities of dwarf spheroidal galaxies to the level required to match observations (Boylan-Kolchin et al. 2011b; Teyssier et al. 2012; Zolotov et al. 2012; Peñarrubia et al.2012; Garrison-Kimmel et al., in preparation).”
Bar formation and evolution in disc galaxies with gas and a triaxial halo: morphology, bar strength and halo properties (2012, background): “…de Blok et al. 2001, 2008; de Blok & Bosma 2002; de Blok, Bosma & McGaugh 2003; Simon et al. 2003; Kuzio de Naray et al. 2006; Battaglia et al. 2008; Kuzio de Naray, McGaugh & de Blok 2008; Oh et al. 2008; de Blok 2010; Walker & Peñarrubia 2011; Amorisco & Evans 2012; Peñarrubia et al. 2012).”
A mass-dependent density profile for dark matter haloes including the influence of galaxy formation (2014, unknown): “The star formation efﬁciency at which the cusp/core transition happens in our simulations is in agreement with the analytic calculation of Pe˜narrubia et al. (2012), who compared the energy needed to remove a cusp with the energy liberated by SNII explosions.”
Too big to fail in the Local Group (2014, background): “Moreover, unless these galaxies formed with top-heavy initial mass functions or live in much smaller haloes than AM suggests, the energy available from supernovae is likely below that required to alter their density profiles significantly (Peñarrubia et al. 2012; GarrisonKimmel et al. 2013).”
A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, methodology): “…destruction have long been considered potential solutions to bring the number of predicted satellites in line with the number of observed satellites (Bullock et al. 2000; Somerville 2002; Kravtsov et al. 2004; Simon & Geha 2007; Koposov et al. 2009; Nickerson et al. 2011; Peñarrubia et al. 2012).”
Small scale problems of the $\Lambda$CDM model: a short review (2016, methodology): “e [378] produces the solid line with diamonds. The model of baryonic corrections applied to VL2 subhaloes yields the abundance shown by the dotted line (ﬁgure reproduced from [403]). classical dwarfs [291,301], while isolated galaxies do not clearly present baryonic physics solutions to the TBTF pro”
Gravitational probes of dark matter physics (2017, background): “The halo mass scale on which baryons can affect the central density of dark matter is around Mhalo ∼ 10(9)M − 10(15)M , where the bottom of the range is uncertain by about an order of magnitude because of the uncertainty on the scale on which baryons significantly affect halo structure [358, 381, 35”
Can feedback solve the too-big-to-fail problem? (2013, background): “Another way to characterize the problem inherent in lowering the densities in the faintest dwarfs is to consider the energy required to bring densities into accordance with observations (Peñarrubia et al. 2012).”