Evidence against dissipation-less dark matter from observations of galaxy haloes

Moore, Ben

doi:10.1038/370629a0

Cited by 1,065 publications

(1,056 citation statements)

References 28 publications

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“…Recognizing current uncertainties in the dark matter density profiles of low-mass galaxies (e.g. Moore 1994;de Blok et al 2001;Boylan-Kolchin, Bullock & Kaplinghat 2011, 2012, we also employ mass profiles derived from dynamical modeling of the observed HI kinematics for a subset of our systems, including NFW fits to the THINGS and Little THINGS samples from de Blok et al (2008) and Oh et al (2015) as well as fits to a Burkert profile (Burkert 1995) from Pace (2016).…”

Section: Estimating σGas(r) and M (R)mentioning

confidence: 99%

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Fillingham

Cooper

Pace

et al. 2016

Mon. Not. R. Astron. Soc.

117

123

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Recent studies of galaxies in the local Universe, including those in the Local Group, find that the efficiency of environmental (or satellite) quenching increases dramatically at satellite stellar masses below ∼ 10 8 M . This suggest a physical scale where quenching transitions from a slow "starvation" mode to a rapid "stripping" mode at low masses. We investigate the plausibility of this scenario using observed HI surface density profiles for a sample of 66 nearby galaxies as inputs to analytic calculations of ram-pressure and turbulent viscous stripping. Across a broad range of host properties, we find that stripping becomes increasingly effective at M * 10 8−9 M , reproducing the critical mass scale observed. However, for canonical values of the circumgalactic medium density (n halo < 10 −3.5 cm −3 ), we find that stripping is not fully effective; infalling satellites are, on average, stripped of only 40 − 60% of their cold gas reservoir, which is insufficient to match observations. By including a host halo gas distribution that is clumpy and therefore contains regions of higher density, we are able to reproduce the observed HI gas fractions (and thus the high quenched fraction and short quenching timescale) of Local Group satellites, suggesting that a host halo with clumpy gas may be crucial for quenching low-mass systems in Local Group-like (and more massive) host halos.

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Section: Estimating σGas(r) and M (R)mentioning

confidence: 99%

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Fillingham

Cooper

Pace

et al. 2016

Mon. Not. R. Astron. Soc.

117

123

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“…This disparity between the model and the data on the galaxy rotation curves requires the introduction of different fields and/or particles, including the DE as a candidate. Indeed, this disparity follows directly from the nature of collisionless particles, which have no physically associated length scale, with the result that DM halos should have zero effective core radii [20]. In order to generate cores in the DM distribution, additional physical properties are required, such as could be provided by Hot Dark Matter (in this case, the central density may be naturally limited by phase space constraints) or an universe dominated by dissipative baryonic matter.…”

Section: Possible Implications Of Quintessence Clumpinessmentioning

confidence: 99%

Sub-horizon perturbation behavior in extended quintessence

Perrotta

Baccigalupi

2003

Nuclear Physics B - Proceedings Supplements

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In the general context of scalar-tensor theories, we consider a model in which a scalar field coupled to the Ricci scalar in the gravitational sector of the Lagrangian, is also playing the role of an "Extended Quintessence" field, dominating the energy content of the Universe at the present time. In this framework, we study the linear evolution of the perturbations in the Quintessence energy density, showing that a new phenomenon, named here "gravitational dragging", can enhance the scalar field density perturbations as much as they reach the non-linear regime. The possibility of dark energy clumps formation is thus discussed.1. The growth of quintessence linear perturbations.The recent growing evidences for a vacuum energy component in the Universe [1,2] have lead to the development of a number of models, most of which tend to alleviate the theoretical difficulties of the well known "cosmological constant problem" (see [3] for a review). All these models are replacing the cosmological constant with a "dynamical vacuum energy" provided by an evolving scalar field, often named "Quintessence". This field should provide the present cosmic accelerating phase through its negative equation of state. Such "dark energy" component has also been modeled in the general framework of scalar-tensor theories of Gravity: in these "Extended Quintessence" (EQ) scenarios [4]-[11], the Quintessence scalar field is directly coupled to the Ricci scalar R in the Lagrangian of the theory: the canonical Ricci scalar term κ −1 R, with κ = 8πG * , is replaced by F (φ)R, where F (φ) is a function of the quintessence field φ. Here, G * is a "bare" gravitational constant, generally different from the Newton's constant G as it is measured by Cavendish-type experiments [12,13]. In EQ models, a scalar field has thus a double role: at any epoch, its value determines the effective gravitational constant, and the contribution in dark energy density. Of course, such a coupling is not arbitrary: it is instead subject to a number of constraints, mainly arising from the bounds on the time variations of the constants of nature, which must be taken into account. EQ scenarios have been analyzed from different points of view, and there are robust predictions about their possible imprints on the power spectrum of CMB anisotropies [4,5]. However, the important role of Dark Energy in modern cosmology opens the question of its relation with the other main dark component currently under investigation, the Dark Matter. One major point with Quintessence scenarios is whether a Dark Energy component could affect, in some way, the formation of Dark Matter clumps. In particular, one fundamental question is: can the Dark Energy itself form clumps on certain scales? If we restrict ourselves to minimally-coupled scalar fields, we have to deal with a very relativistic component: indeed, the sound speed of such component turns out to be identical to that of radiation [14]. As a consequence, an "ordinary" (i.e., minimally coupled) Quintessence component becomes homogeneou...

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“…As the relation between V vir and r vir is fully specified by the background cosmology, the independent parameters characterizing the model reduce from three to two (c and r s ). Let us stress that a high density Ω m = 1 model, with a concentration parameter c > 12, is definitely unable to account for the observed galaxy kinematics [11]. So far, due to the limited number of suitable RC's and to the serious uncertainties in deriving the actual amount of luminous matter inside the inner regions of spirals, it has been difficult to investigate the internal structure of dark halos.…”

Section: Introductionmentioning

confidence: 99%

The Intriguing Distribution of Dark Matter in Galaxies

Salucci

Borriello

2003

Particle Physics in the New Millennium

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Abstract. We review the most recent evidence for the amazing properties of the density distribution of the dark matter around spiral galaxies. Their rotation curves, coadded according to the galaxy luminosity, conform to an Universal profile which can be represented as the sum of an exponential thin disk term plus a spherical halo term with a flat density core. From dwarfs to giants, these halos feature a constant density region of size r0 and core density ρ0 related by ρ0 = 4.5 × 10 −2 (r0/kpc) −2/3 M⊙pc −3 . At the highest masses ρ0 decreases exponentially with r0, revealing a lack of objects with disk masses > 10 11 M⊙ and central densities > 1.5 × 10 −2 (r0/kpc) −3 M⊙pc −3 implying a maximum mass of ≈ 2 × 10 12 M⊙ for a dark halo hosting a stellar disk. The fine structure of dark matter halos is obtained from the kinematics of a number of suitable low-luminosity disk galaxies. The halo circular velocity increases linearly with radius out to the edge of the stellar disk, implying a constant dark halo density over the entire disk region. The properties of halos around normal spirals provide substantial evidence of a discrepancy between the mass distributions predicted in the Cold Dark Matter scenario and those actually detected around galaxies.

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Evidence against dissipation-less dark matter from observations of galaxy haloes

Cited by 1,065 publications

References 28 publications

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Sub-horizon perturbation behavior in extended quintessence

The Intriguing Distribution of Dark Matter in Galaxies

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