The distribution of dark matter in the Perseus cluster

Eyles, C. J.; Watt, Mark; Bertram, D. S.; Church, M. J.; Ponman, T. J.; Skinner, G. K.; Willmore, A. P.

doi:10.1086/170251

Cited by 59 publications

(50 citation statements)

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“…Because the x-ray-emitting gas in a cluster is expected to be in hydrostatic equilibrium, kT plays the role of mV2 in the virial analysis and is a good tracer of the cluster gravitational potential. From the x-ray data, Eyles et al (53) find that the total gravitational cluster mass is 30-65% less than that obtained from the application of the virial theorem, in part because the distribution of mass does not follow the distribution of galaxies. Moreover, while the dark matter is more centrally condensed than the galaxies and is the dominant mass component out to =1 Mpc, the x-ray gas is less so.…”

Section: Section III Dwarf Spirals Contain Mostly Dark Mattermentioning

confidence: 96%

Galaxy dynamics and the mass density of the universe.

Rubin

1993

Proc. Natl. Acad. Sci. U.S.A.

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Dynamical evidence accumulated over the past 20 years has convinced astronomers that luminous matter in a spiral galaxy constitutes no more than 10% of the mass of a galaxy. An additional 90% is inferred by its gravitational effect on luminous material. Here I review recent observations concerning the distribution of luminous and nonluminous matter in the Milky Way, in galaxies, and in galaxy clusters. Observations of neutral hydrogen disks, some extending in radius several times the optical disk, confirm that a massive dark halo is a major component of virtually every spiral. A recent surprise has been the discovery that stellar and gas motions in ellipticals are enormously complex. To date, only for a few spheroidal galaxies do the velocities extend far enough to probe the outer mass distribution. But the diverse kinematics of inner cores, peripheral to deducing the overall mass distribution, offer additional evidence that ellipticals have acquired gas-rich systems after initial formation. Dynamical results are consistent with a low-density universe, in which the required dark matter could be baryonic. On smallest scales of galaxies [10 kiloparsec (kpc); H. = 50 kmsec'lmegaparsec'11 the luminous matter constitutes only 1% of the closure density. On scales greater than binary galaxies (i.e., .100 kpc) all systems indicate a density -10% of the closure density, a density consistent with the low baryon density in the universe. If large-scale motions in the universe require a higher mass density, these motions would constitute the first dynamical evidence for nonbaryonic matter in a universe of higher density.Twenty years ago, astronomers started accumulating observations that indicated that orbital velocities of stars and gas in spiral galaxies remained high out to the limits of the observable galaxy. By 1982, after a decade of initial disquiet, most astronomers reluctantly accepted the conclusion that a galaxy consists of much more than the luminous stars, gas, and dust that can be observed at various wavelengths. In fact, at least 90% of a galaxy consists of dark matter, matter that is undetectable at any wavelength and that is deduced only by its gravitational influence on the orbits of the stars and the gas that we can see. But not all astronomers were reluctant to accept the evidence. "There are reasons, increasing in number and quality, to believe that the masses of ordinary galaxies may have been underestimated by a factor of 10 or more," stated Ostriker, Peebles, and Yahill (1) in a truly prescient sentence.This revolution in our understanding came about because theoretical arguments revealed the necessity of stabilizing the disks of galaxies with invisible halos (2), because observations with optical (3, 4) and with radio (5) telescopes showed uniformly high rotation velocities, and because an enormously influential review of the inferred distribution of

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Section: Section III Dwarf Spirals Contain Mostly Dark Mattermentioning

confidence: 96%

Galaxy dynamics and the mass density of the universe.

Rubin

1993

Proc. Natl. Acad. Sci. U.S.A.

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“…An X-ray analysis of the Coma cluster had suggested that the mass distribution might be more concentrated than the galaxy distribution (Henriksen and Mushotzky 1985), in agreement with mass models from velocity-dispersion data (The and White 1986). More recently, it has become possible to measure both the temperature and density profiles of the gas in a cluster, and this has led to a direct determination of the distribution of gravitating mass in Perseus by Eyles et al (1991) and in Coma by Briel et al ( 1992). To determine the distribution of DM, Eyles et al ( 1991 ) subtracted out the contribution from the galaxies and the X-ray emitting gas.…”

Section: Cluster-mass Distribution From X Raysmentioning

confidence: 99%

Decaying neutrinos and the nature of the dark matter in galaxy clusters

Sciama

Peršić

Salucci

1993

PASP

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ABSTRACT. It is widely believed that Sciama's (1990) decaying-neutrino theory has been disproved by the failure of Davidsen et al. ( 1991 ) to detect an unidentified emission line at ~ 15 eV (in the rest frame) from the dark matter in the cluster of galaxies A665 (e.g., Trimble 1992). Here we show that recent X-ray data for A665 favor models in which the dark matter in the regions of the cluster observed by Davidsen et al. is mainly baryonic. Thus the decaying-neutrino theory continues to be viable.

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“…sequent analyses of mass estimates based on optical and X-ray data indicated smaller values : M/L B \ 190 h M _ /L _ for A194 by Chapman, Geller, & Huchra (1988) ; M/L B \ 200 for the Perseus cluster by Eyles et al (1991) David, Jones, & Forman (1995) ;…”

Section: Introductionmentioning

confidence: 98%

Optical Luminosities and Mass‐to‐Light Ratios of Nearby Galaxy Clusters

Girardi

Borgani

Giuricin

et al. 2000

ApJ

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We analyze a sample of 105 clusters having virial mass homogeneously estimated and for which galaxy magnitudes are available with a well-deÐned high degree of completeness. In particular, we consider a subsample of 89 clusters with galaxy magnitudes taken from the COSMOS/UKST B j -band Southern Sky Object Catalog. After suitable magnitude corrections and uniform conversions to band, B j we compute cluster luminosities within several clustercentric distances, 0.5, 1.0, 1.5 h~1 Mpc and L Bj within the virialization radiusIn particular, we use the luminosity function and background counts R vir . estimated by Lumsden et al. on the Edinburgh/Durham Southern Galaxy Catalog, which is the wellcalibrated part of the COSMOS catalog. We analyze the e †ect of several uncertainties connected to photometric data, fore/background removal, and extrapolation below the completeness limit of the photometry, in order to assess the robustness of our cluster luminosity estimates. We draw our results on the relations between luminosity and dynamical quantities from the COSMOS sample by considering mass and luminosities determined within the virialization radius. We Ðnd a very good correlation between cluster luminosity, and galaxy velocity dispersion, with Our estimate of . the typical value for the mass-to-light ratio isWe do not Ðnd any correlation ofwith cluster morphologies, i.e., Rood-Sastry and Bautz-Morgan types, and only a weak signiÐcant M/L Bj correlation with cluster richness. We Ðnd that mass has a slight, but signiÐcant, tendency to increase faster than the luminosity does,We verify the robustness of this relation against a number M P L Bj 1.2h1.3. of possible systematics. We verify that this increasing trend of M/L with cluster mass cannot be entirely due to a higher spiral fraction in poorer clusters, thus suggesting that a similar result would also be found by using R-band galaxy magnitudes.

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The distribution of dark matter in the Perseus cluster

Cited by 59 publications

References 0 publications

Galaxy dynamics and the mass density of the universe.

Galaxy dynamics and the mass density of the universe.

Decaying neutrinos and the nature of the dark matter in galaxy clusters

Optical Luminosities and Mass‐to‐Light Ratios of Nearby Galaxy Clusters

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