The mass of the missing baryons in the X-ray forest of the warm–hot intergalactic medium

Nicastro, F.; Mathur, S.; Elvis, M.; Drake, J. J.; Fang, Taotao; Fruscione, A.; Krongold, Y.; Marshall, Herman L.; Williams, R.; Zezas, A.

doi:10.1038/nature03245

Cited by 186 publications

(193 citation statements)

References 24 publications

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“…In the cosmic baryon budget, it is now well known that only about 6% of them shine as stars and gas in galaxies (Fukugita et al 1998). Locally, UV absorption in front of background sources have shown that as much as 30% of baryons could be associated with the Lymanα forest and an uncertain fraction (5−10%) with the warm-hot medium (WHIM at 10 5 −10 6 K, Nicastro et al 2005;Danforth et al 2006). So about half of the baryons are not yet accounted for.…”

Section: Introductionmentioning

confidence: 99%

MOND and the dark baryons

Tiret¹,

Combes²

2009

A&A

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We consider for the first time the implications for the modified gravity MOND model of galaxies, of the presence of dark baryons, in the form of cold molecular gas in galaxy discs. We show that MOND models of rotation curves are still valid and universal, but the critical acceleration a 0 separating the Newtonian and MONDian regimes has a lower value. We quantify this modification as a function of the scale factor c between the total gas of the galaxy and the measured atomic gas. The main analysis concerns 43 resolved rotation curves and allows us to find the best pair (a 0 = 0.96 × 10 −10 m s −2 , c = 3), which is also compatible with the one obtained from a second method minimizing the scatter in the baryonic Tully-Fisher relation.

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Section: Introductionmentioning

confidence: 99%

MOND and the dark baryons

Tiret¹,

Combes²

2009

A&A

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“…If so, important objectives are (1) to investigate the intergalactic magnetic field strength and structure, (2) to determine the excitation state and metallicity of any associated warm-hot intergalactic medium (WHIM; e.g., Henry 2004;Nicastro et al 2005), (3) to understand the intergalactic cosmic-ray spectrum (e.g., , and (4) to define the propagation environment of ultraYhigh-energy cosmic rays (UHECRs; e.g., Sigl et al 2004). The achievement of these goals is ultimately important for solving important puzzles in high-energy astrophysics, astroparticle physics, the origin of cosmic magnetic fields, and the evolution of LSS.…”

Section: Introductionmentioning

confidence: 99%

Discovery of New Faint Radio Emission on 8o to 3′ Scales in the Coma Field, and Some Galactic and Extragalactic Implications

Kronberg

Kothes

Salter

et al. 2007

ApJ

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We present a deep, 8 diameter, 0.4 GHz radio image using a first-time combination of the NAIC Arecibo 305 m telescope in Puerto Rico and the wide-angle interferometer at the Dominion Radio Astrophysical Observatory at Penticton, Canada. Our observations are centered on the Coma Cluster of galaxies in the ''Great Wall'' of galaxies near the north Galactic pole. The complementary nature of these two instruments enables us to produce a distortion-free image that is sensitive to radiation on scales from 8 down to that of an individual galaxy halo at the 100 Mpc distance of the Great Wall. Newly revealed patches of distributed radio ''glow'' are seen well above the detection limit. One prominent such area coincides with groupings of radio galaxies near the Coma Cluster and indicates intergalactic magnetic fields in the range 0.2Y0.4 G on scales of up to $4 Mpc. Other patches of diffuse emission, not previously explored at these high latitudes on arcminute scales, probably consist of Galactic ''cirrus.'' A striking anticorrelation is found between low-level diffuse radio glow and some regions of enhanced optical galaxy surface density, suggesting that cosmological large-scale structure, normally defined by the baryonic (or dark) matter density, is not uniquely traced by faint continuum radio glow. Rather, intergalactic diffuse synchrotron radiation may be a proxy for IGM cosmic-ray and magnetic energy density, rather than matter density. The diffuse, arcminute-level structures over a large region of sky are potentially important pathfinders to CMB foreground radiation on high multipole scales. Subject headingg s: large-scale structure of universe -radio continuum: general

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“…19, this issue) must be used at their sensitivity limits and the most plausible detections (e.g. Nicastro et al 2005) are indeed still debated (Kaastra et al 2006). Firm detections are however of great relevance, because the existence of the WHIM and the estimate of its properties would be an extraordinary confirmation of the current model of structure formation.…”

Section: The Surrounding Whimmentioning

confidence: 99%

Clusters of Galaxies: Setting the Stage

2008

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Clusters of galaxies are self-gravitating systems of mass ∼ 10 14 -10 15 h −1 M and size ∼ 1-3h −1 Mpc. Their mass budget consists of dark matter (∼ 80%, on average), hot diffuse intracluster plasma ( 20%) and a small fraction of stars, dust, and cold gas, mostly locked in galaxies. In most clusters, scaling relations between their properties, like mass, galaxy velocity dispersion, X-ray luminosity and temperature, testify that the cluster components are in approximate dynamical equilibrium within the cluster gravitational potential well. However, spatially inhomogeneous thermal and non-thermal emission of the intracluster medium (ICM), observed in some clusters in the X-ray and radio bands, and the kinematic and morphological segregation of galaxies are a signature of non-gravitational processes, ongoing cluster merging and interactions. Both the fraction of clusters with these features, and the correlation between the dynamical and morphological properties of irregular clusters and the surrounding large-scale structure increase with redshift.In the current bottom-up scenario for the formation of cosmic structure, where tiny fluctuations of the otherwise homogeneous primordial density field are amplified by gravity, clusters are the most massive nodes of the filamentary large-scale structure of the cosmic web and form by anisotropic and episodic accretion of mass, in agreement with most of the observational evidence. In this model of the universe dominated by cold dark matter, at the present time most baryons are expected to be in a diffuse component rather than in stars and A. Diaferio ( ) Dipartimento

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The mass of the missing baryons in the X-ray forest of the warm–hot intergalactic medium

Cited by 186 publications

References 24 publications

MOND and the dark baryons

MOND and the dark baryons

Discovery of New Faint Radio Emission on 8o to 3′ Scales in the Coma Field, and Some Galactic and Extragalactic Implications

Clusters of Galaxies: Setting the Stage

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