The Mass of the Virgo Cluster

Smith, Sinclair

doi:10.1086/143697

Cited by 216 publications

(166 citation statements)

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“…They provided the first line of evidence for the existence of dark matter (Zwicky, 1933;Smith, 1936), and cluster mass-to-light ratio measurements suggested that the matter density in the universe was sub-critical (Ω m < 1) as far back as the early 1970's (see Gott et al, 1974, and references therein). The evidence for low Ω m was substantially strengthened by baryon fraction measurements Evrard, 1997), and by the discovery of massive clusters at high (z ≈ 0.8) redshift (e.g., Henry, 1997;Eke et al, 1998;Donahue et al, 1998).…”

Section: General Principlesmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: General Principlesmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…Many attempts have been made to determine the amount and distribution of dark matter in clusters since Zwicky (1933Zwicky ( , 1937 and Smith (1936) concluded that the mass implied by the sum of the luminosities of the galaxies falls short of the total mass by as much as a factor of 10. In recent years, cosmological simulations have shown that dark matter halos have a universal density profile (Navarro, Frenk, & White 1996, but its precise form is still debated (Moore et al 1999, hereafter M99), while the ''universality'' of the mass density profile has also been questioned (Jing & Suto 2000;Thomas et al 2001;Ricotti 2003).…”

Section: Introductionmentioning

confidence: 99%

The ESO Nearby Abell Cluster Survey. XII. The Mass and Mass‐to‐Light Ratio Profiles of Rich Clusters

Katgert

Biviano

Mazure

2004

ApJ

117

173

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We determine the mass profile of an ensemble cluster built from 3056 galaxies in 59 nearby clusters observed in the ESO Nearby Abell Cluster Survey. The mass profile is derived from the distribution and kinematics of the early-type (elliptical and S0) galaxies only, with projected distances from the centers of their clusters 1.5r 200 . These galaxies are most likely to meet the conditions for the application of the Jeans equation, since they are the oldest cluster population and are thus quite likely to be in dynamical equilibrium with the cluster potential. In addition, the assumption that the early-type galaxies have isotropic orbits is supported by the shape of their velocity distribution. For galaxies of other types (the brightest elliptical galaxies, with M R À22 þ 5 log h, and the early and late spirals) these assumptions are much less likely to be satisfied. For the determination of the mass profile we also exclude early-type galaxies in subclusters. Application of the Jeans equation yields a nonparametric estimate of the cumulative mass profile M(

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“…At the beginning of the 1930s, F. Zwicky and other astronomers measured the total mass of a few clusters of galaxies and the masses of the luminous objects in these clusters of galaxies [10][11]. Their measurements showed that the masses of these clusters of galaxies required to gravitationally bind their galaxies are much larger than the sum of the luminous masses of their individual galaxies.…”

Section: Rotation Curves Of Spiral Galaxiesmentioning

confidence: 99%

“…However, measurements of the circular velocities of clouds of neutral hydrogen in galaxies by using their 21-cm emission showed that the rotation curves of spiral galaxies are flat (see Fig1) or even rising at distances far away from their stellar and gaseous components [7][8][9][10][11][12][13]. This implies the existence of a "dark halo" around the galaxy with a total mass profile [14].…”

Section: Rotation Curves Of Spiral Galaxiesmentioning

confidence: 99%

Untitled

2017

PAIJ

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Historically the observational evidence for the existence of Dark Matter came only from galactic dynamics and is gravitational. The following discussions in this section show that the observed luminous objects (stars, gas clouds, globular clusters, or even entire galaxies) can not have enough mass to support the observed gravitational effectsCeaseless efforts are being made for the last three decades towards revealing the mysteries regarding the nature of dark matter. A number of theoretical models have been proposed. On the basis of these models, experiments to search for dark matter and its nature are being planned and designed. Results of ongoing experiments are being analyzed and it is being constantly attempted to answer the question as what is the nature of dark matter. In the present chapter, it is attempted to review the developments in the search for dark matter.

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The Mass of the Virgo Cluster

Cited by 216 publications

References 0 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

The ESO Nearby Abell Cluster Survey. XII. The Mass and Mass‐to‐Light Ratio Profiles of Rich Clusters

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