Large–scale structure and matter in the Universe

Peacock, J. A.

doi:10.1098/rsta.2003.1288

Cited by 12 publications

(6 citation statements)

References 39 publications

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“…For instance, a hot dark matter (HDM) particle candidate with mass of a few to 15 eV would have a free-streaming length of about ∼ 100 Mpc, leading to too little power at the small-scale end of the matter power spectrum. The existence of galaxies at redshift z ∼ 6 implies that the coherence length should have been smaller than 100 kpc or so, meaning that even warm dark matter (WDM) particles with masses between 1 and 10 keV are close to being ruled out as well (see, e.g., [349]). ΛCDM thus presently remains the state-of-the-art in Cosmology, although some of the challenges listed below in Sect.…”

Section: Cold Dark Matter (Cdm)mentioning

confidence: 99%

Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions

Famaey

McGaugh

2012

Living Rev. Relativ.

874

1,303

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A wealth of astronomical data indicate the presence of mass discrepancies in the Universe. The motions observed in a variety of classes of extragalactic systems exceed what can be explained by the mass visible in stars and gas. Either (i) there is a vast amount of unseen mass in some novel form — dark matter — or (ii) the data indicate a breakdown of our understanding of dynamics on the relevant scales, or (iii) both. Here, we first review a few outstanding challenges for the dark matter interpretation of mass discrepancies in galaxies, purely based on observations and independently of any alternative theoretical framework. We then show that many of these puzzling observations are predicted by one single relation — Milgrom’s law — involving an acceleration constant a0 (or a characteristic surface density Σ† = a0/G) on the order of the square-root of the cosmological constant in natural units. This relation can at present most easily be interpreted as the effect of a single universal force law resulting from a modification of Newtonian dynamics (MOND) on galactic scales. We exhaustively review the current observational successes and problems of this alternative paradigm at all astrophysical scales, and summarize the various theoretical attempts (TeVeS, GEA, BIMOND, and others) made to effectively embed this modification of Newtonian dynamics within a relativistic theory of gravity.

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Section: Cold Dark Matter (Cdm)mentioning

confidence: 99%

Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions

Famaey

McGaugh

2012

Living Rev. Relativ.

874

1,303

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“…For lighter particle candidates, the damping scale becomes too large: for instance, a hot DM (HDM) particle candidate (m HDM ≈ few eV) would have a free-streaming length of ≈ 100 Mpc leading to too little power at the small-scale end of the matter power spectrum. The existence of galaxies at redshift z ≈ 6 implies that the coherence scale should have been smaller than 100 kpc or so, meaning that warm DM (WDM) particles with mass m WDM ≈ 1 − 10 keV are close to being ruled out (Peacock 2003).…”

Section: Introductionmentioning

confidence: 99%

Local-Group tests of dark-matter Concordance Cosmology: Towards a new paradigm for structure formation

Kroupa,

Famaey,

de Boer

et al. 2010

Preprint

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Predictions of the concordance cosmological model (CCM) of the structures in the environment of large spiral galaxies are compared with observed properties of Local Group galaxies. Five new most probably irreconcilable problems are uncovered: 1) A great variety of published CCM models consistently predict some form of relation between dark-mattermass and luminosity for the Milky Way (MW) satellite galaxies, but none is observed. 2) The mass function of luminous sub-halos predicted by the CCM contains too few satellites with dark matter (DM) mass ≈ 10 7 M ⊙ within their innermost 300 pc than in the case of the MW satellites. 3) The Local Group galaxies and data from extragalactic surveys indicate there is a correlation between bulge-mass and the number of luminous satellites that is not predicted by the CCM. 4) The 13 new ultra-faint MW satellites define a disc-of-satellites (DoS) that is virtually identical to the DoS previously found for the 11 classical MW satellites, implying that most of the 24 MW satellites are correlated in phase-space. 5) The occurrence of two MW-type DM halo masses hosting MW-like galaxies is unlikely in the CCM. However, the properties of the Local Group galaxies provide information leading to a solution of the above problems. The DoS and bulge-satellite correlation suggest that dissipational events forming bulges are related to the processes forming phase-space correlated satellite populations. These events are well known to occur since in galaxy encounters energy and angular momentum are expelled in the form of tidal tails, which can fragment to form populations of tidal-dwarf galaxies (TDGs) and associated star clusters. If Local Group satellite galaxies are to be interpreted as TDGs then the substructure predictions of the CCM are internally in conflict. All findings thus suggest that the CCM does not account for the Local Group observations and that therefore existing as well as new viable alternatives have to be further explored. These are discussed and natural solutions for the above problems emerge.

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“…Blind surveys for galaxies and galaxy clusters have been performed in the optical waveband for many years. The most recent galaxy redshift surveys (2dFGRS and SDSS) have yielded significant constraints on cosmological parameters via measurements of the power spectrum and redshift-space distortions, as well as a wealth of understanding of the properties of the individual galaxies (Peacock 2003;Tegmark et al 2004). If deep redshift surveys using H I could be performed they would open up a new window on the Universe which could have some technical advantages (and inevitably some disadvantages) over optical approaches.…”

Section: Introductionmentioning

confidence: 99%

Neutral hydrogen surveys for high-redshift galaxy clusters and protoclusters

Battye

Davies

Weller

2004

Monthly Notices of the Royal Astronomical Society

154

134

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We discuss the possibility of performing blind surveys to detect large‐scale features of the Universe using 21‐cm emission. Using instruments with ∼5–10 arcmin resolution currently in the planning stage, it should be possible to detect virialized galaxy clusters at intermediate redshifts using the combined emission from their constituent galaxies, as well as less overdense structures, such as protoclusters and the ‘cosmic web’, at higher redshifts. Using semi‐analytic methods, we compute the number of virialized objects and those at turnaround which might be detected by such surveys. We find that there is a surprisingly large number of objects even using small (∼5 per cent) bandwidths and elaborate on some issues pertinent to optimizing the design of the instrument and the survey strategy. The main uncertainty is the fraction of neutral gas relative to the total dark matter within the object. We discuss this issue in the context of the observations which are currently available.

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Large–scale structure and matter in the Universe

Cited by 12 publications

References 39 publications

Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions

Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions

Local-Group tests of dark-matter Concordance Cosmology: Towards a new paradigm for structure formation

Neutral hydrogen surveys for high-redshift galaxy clusters and protoclusters

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