A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM

By A. Brooks, Michael Kuhlen, A. Zolotov, D. Hooper. 2012

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It has been demonstrated that the inclusion of baryonic physics can alter the dark matter densities in the centers of low-mass galaxies, making the central dark matter slope more shallow than predicted in pure cold dark matter simulations. This flattening of the dark matter profile can occur in the most luminous subhalos around Milky Way mass galaxies. Zolotov et al. have suggested a correction to be applied to the central masses of dark matter-only satellites in order to mimic the affect of (1) the flattening of the dark matter cusp due to supernova feedback in luminous satellites and (2) enhanced tidal stripping due to the presence of a baryonic disk. In this paper, we apply this correction to the z = 0 subhalo masses from the high resolution, dark matter-only Via Lactea II (VL2) simulation, and find that the number of massive subhalos is dramatically reduced. After adopting a stellar mass to halo mass relationship for the VL2 halos, and identifying subhalos that are (1) likely to be destroyed by stripping and (2) likely to have star formation suppressed by photo-heating, we find that the number of massive, luminous satellites around a Milky Way mass galaxy is in agreement with the number of observed satellites around the Milky Way or M31. We conclude that baryonic processes have the potential to solve the missing satellites problem.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9ec6539b254c0b7f0b60106a264ecb508121b841

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Citations in the corpus

Dark matter cores all the way down (2015, background): “Such cored dwarfs are also much more efficiently tidally stripped, which can significantly alleviate the missing satellites problem (Read et al. 2006c; Peñarrubia et al. 2010; Zolotov et al. 2012; Brooks et al. 2013).”
A White Paper on keV sterile neutrino Dark Matter (2016, background): “Such a solution has recently been put forward by [55, 519, 520].”
WHY BARYONS MATTER: THE KINEMATICS OF DWARF SPHEROIDAL SATELLITES (2012, background): “There are fewer small satellite galaxies orbiting our Milky Way (MW) galaxy than predicted by the favored Cold Dark Matter (CDM) cosmological model (Moore et al. 1999; Klypin et al. 1999; Madau et al. 2008; Wadepuhl & Springel 2011; Brooks et al. 2013).”
The APOSTLE simulations: solutions to the Local Group's cosmic puzzles (2015, background): “While the observed kinematics of LG dwarf spheroidals are, in fact, consistent with either cores or cusps (Strigari, Frenk & White 2014), it has also been argued that cores are required to solve the too-big-to-fail problem (Brooks et al. 2013).”
HIGH-RESOLUTION MASS MODELS OF DWARF GALAXIES FROM LITTLE THINGS (2015, background): “…simulations and observations, the socalled ‘cusp/core’ problem has been one aspect of the small-scale crisis in ΛCDM cosmology which is likely connected to the ‘missing satellites’ problem (Brooks et al. 2013) and ‘too-big-to-fail’ problem (dense satellites; see Boylan-Kolchin et al. 2011, 2012).”
SEMI-ANALYTIC GALAXY EVOLUTION (SAGE): MODEL CALIBRATION AND BASIC RESULTS (2016, background): “…simulation are 7 This has been referred to in the literature as the “missing satellites problem” (Moore et al. 1999; Klypin et al. 1999), for which baryonic physical processes, including reionization heating, are capable of solving (e.g. Zolotov et al. 2012; Brooks et al. 2013). z0 = 8 and zr = 7.”
THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I. HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS (2014, methodology): “…in dSph SFHs has been known for over a decade (e.g., Grebel 1997; Mateo 1998; Grebel et al. 2003), and has motivated increasingly sophisticated model efforts to reproduce the properties of MW dSphs (e.g., Mayer et al. 2001, 2006; Zolotov et al. 2012; Brooks et al. 2013; Kazantzidis et al. 2013).”
ETHOS - an effective theory of structure formation: dark matter physics as a possible explanation of the small-scale CDM problems (2015, result): “…(e.g. Efstathiou 1992; Gnedin 2000; Benson et al. 2002; Koposov et al. 2008), although photoevaporation and photo-heating alone may not be enough to bring the predicted number of massive, luminous satellites into agreement with observations (e.g., Boylan-Kolchin et al. 2012; Brooks et al. 2013).”
Gravitational probes of dark matter physics (2017, background): “Despite differences in code and the implementation of semi-analytic star formation prescriptions, there are now largely consistent results about the sign of the effect of baryons on halos on dwarf scales [255, 284, 372, 373, 374, 375, 376, 377, 378, 379, 352, 261].”
A model for halo formation with axion mixed dark matter (2013, background): “…that the non-thermal solution both avoids this dilemma and also augurs well for a particle-orientated solution of MFP, a problem for which a feedback solution seems questionable (Garrison-Kimmel et al. 2013; Boylan-Kolchin, Bullock & Kaplinghat 2012), although not all agree (Brooks et al. 2013).”
Too big to fail in the Local Group (2014, background): “…ram pressure stripping, and tidal interactions, may account for the discrepancy (e.g. Del Popolo 2012; Pontzen & Governato 2012; Zolotov et al. 2012; Brooks et al. 2013; Gritschneder & Lin 2013; Amorisco, Zavala & de Boer 2014; Arraki et al. 2014; Brooks & Zolotov 2014; Del Popolo et al. 2014).”
Dwarf galaxies in CDM and SIDM with baryons: observational probes of the nature of dark matter (2014, background): “…effects such as tidal stripping might alleviate this stringent energetic condition in the case of satellite galaxies (Zolotov et al. 2012; Brooks et al. 2013; Arraki et al. 2014), the issue of low central DM densities seems relevant even for isolated galaxies (Ferrero et al. 2012; Kirby…”
The stellar mass-halo mass relation of isolated field dwarfs : a critical test of ΛCDM at the edge of galaxy formation (2016, background): “…of dwarfs from discs to spheroids (Mayer et al. 2001a; Lokas et al. 2012; Kazantzidis et al. 2013); and physically reshapes the dark matter halo mass function within groups (Peñarrubia et al. 2010; Zolotov et al. 2012; Brooks et al. 2013; Wetzel et al. 2016, and see the discussion in R16a).”