THE VELOCITY FUNCTION IN THE LOCAL ENVIRONMENT FROM ΛCDM AND ΛWDM CONSTRAINED SIMULATIONS

By J. Zavala, Yipeng Jing, A. Faltenbacher, G. Yepes, Y. Hoffman, S. Gottlober, B. Catinella. 2009

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Using constrained simulations of the local universe for generic cold dark matter (CDM) and for 1 keV warm dark matter (WDM), we investigate the difference in the abundance of dark matter halos in the local environment. We find that the mass function (MF) within 20 h−1 Mpc of the Local Group is ∼2 times larger than the universal MF in the 109–1013 h−1 M☉ mass range. Imposing the field of view of the ongoing H i blind survey Arecibo Legacy Fast ALFA (ALFALFA) in our simulations, we predict that the velocity function (VF) in the Virgo-direction region (VdR) exceeds the universal VF by a factor of 3. Furthermore, employing a scheme to translate the halo VF into a galaxy VF, we compare the simulation results with a sample of galaxies from the early catalog release of ALFALFA. We find that our simulations are able to reproduce the VF in the 80–300 km s-1 velocity range, having a value ∼10 times larger than the universal VF in the VdR. In the low-velocity regime, 35–80 km s-1, the WDM simulation reproduces the observed flattening of the VF. In contrast, the simulation with CDM predicts a steep rise in the VF toward lower velocities; for Vmax = 35 km s-1, it forecasts ∼10 times more sources than the ones observed. If confirmed by the complete ALFALFA survey, our results indicate a potential problem for the CDM paradigm or for the conventional assumptions about energetic feedback in dwarf galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8ebacb1561111260c3b33e41334a5e357806dcfd

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Citations in the corpus

Too big to fail? The puzzling darkness of massive Milky Way subhaloes (2011, background): “…of σ8 and ns. Modifying the dark matter power spectrum on sub-galactic scales – for example, through Warm Dark Matter (WDM) with a characteristic scale of 40 to 50 km s−1 – would result in both fewer massive subhaloes (e.g., Zavala et al. 2009) and lower central densities in such subhaloes.”
Subhaloes in self-interacting galactic dark matter haloes (2012, methodology): “…is “warm”, i.e., where DM particles have larger primordial thermal velocities, are able to alleviate the overabundance problem (e.g. Bode et al. 2001; Zavala et al. 2009) and at the same time, if their masses are & 1 keV, avoid current constraints on the matter power spectrum as measured by the…”
Non-linear evolution of cosmological structures in warm dark matter models (2011, unknown): “…Avila-Reese & Valenzuela 2000; White & Croft 2000; Avila-Reese et al. 2001; Bode et al. 2001; Bullock, Kravtsov & Colı́n 2002; Zentner & Bullock 2003; Colı́n, Valenzuela & Avila-Reese 2008; Zavala et al. 2009; Macciò & Fontanot 2010; Dunstan et al. 2011; Lovell et al. 2012; Viel et al. 2011).”
Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations (2016, background): “…circular velocity function (dnh/d log Vmax)—is recognized as a sensitive probe of dark matter (Cole & Kaiser 1989; Shimasaku 1993; Gonzalez et al. 2000; Zavala et al. 2009; Papastergis et al. 2011; Trujillo-Gomez et al. 2011; Schneider et al. 2014; Klypin et al. 2015; Papastergis et al. 2015).”
Constraining self-interacting dark matter with the Milky Way’s dwarf spheroidals (2012, background): “…gas physics is the next step of SIDM simulations, a challenge to make SIDM an even more attractive alternative to CDM is the prospect of explaining the observed scarcity of MW satellites and field dwarfs (e.g. Klypin et al. 1999; Zavala et al. 2009) without invoking extreme baryonic processes.”
Cores in warm dark matter haloes: a Catch 22 problem (2012, methodology): “Furthermore, recent studies (Tikhonov et al. 2009; Zavala et al. 2009; Peebles & Nusser 2010) re-emphasized that also the population of dwarf galaxies within voids is in strong contradiction with CDM predictions.”
The warm dark matter halo mass function below the cut-off scale (2013, background): “…of Milky-Way satellites (Boylan-Kolchin et al. 2011; Lovell et al. 2012), the velocity ∗ reangulo@stanford.edu † hahn@phys.ethz.ch ‡ tabel@stanford.edu function of HI selected galaxies (Zavala et al. 2009), and the abundance of low mass galaxies at low and high redshifts (Menci et al. 2012).”
The SAMI Galaxy Survey: Instrument specification and target selection (2014, background): “This scaling (effectively between stellar mass and dynamical mass) underpins models of galaxy evolution, and becomes particularly interesting for v < 100 km s−1 where the velocity functions predicted by CDM and warm dark matter (WDM) models deviate significantly (Zavala et al. 2009).”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “2007; Bullock 2010), the ‘cusp-core problem’ (Li and Chen 2009; Simon et al. 2005; Zavala et al. 2009) and sizes of mini-voids (Tikhonov et al.”
Small-Scale Challenges to the ΛCDM Paradigm (2017, background): “This version of too-big-to-fail in the field is also manifested in the velocity function of field galaxies4 (Zavala et al. 2009; Klypin et al. 2015; Trujillo-Gomez et al. 2016; Schneider 4We note that the mismatch between the observed and predicted velocity function can also…”
The flattening of the concentration–mass relation towards low halo masses and its implications for the annihilation signal boost (2013, background): “In this regard, allowed Warm Dark Matter (WDM) models with a filtering mass near this scale would predict a different formation scenario for dwarfs (Zavala et al. 2009). c© 2002 RAS scribed above, where the halo formation epoch fully reflects the adopted underlying cosmological model.”
Is there a "too big to fail" problem in the field? (2014, methodology): “Both the galactic VF and WF have been used extensively in the literature to testΛCDM on galactic scales (Obreschkow et al. 2009; Zavala et al. 2009; Zwaan et al. 2010; Papastergis et al. 2011; Trujillo-Gomez et al. 2011; Obreschkow et al. 2013; Schneider et al. 2014; Klypin et al. 2014).”
Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology (2010, background): “A number of authors have suggested that the suppression of small-scale structure expected in a warm dark matter model might reduce the abundance of low-mass halos enough to alleviate the tension (e.g. Bode et al. 2001; Zavala et al. 2009; Macciò et al. 2010).”
THE VELOCITY WIDTH FUNCTION OF GALAXIES FROM THE 40% ALFALFA SURVEY: SHEDDING LIGHT ON THE COLD DARK MATTER OVERABUNDANCE PROBLEM (2011, methodology): “Also note that the simulation is complete only down to vhalo = 50 km s −1, and a power-law extrapolation is used at lower velocities (which is however expected to hold, see for example §4.2 in Zavala et al. 2009).”