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Wavefront Gravitational Lens

The galaxy cluster A bell 370 as observed in 1985 (left) with one of the first CCD cameras, in which the Ih-sl gravitation ally lensed arc wras later identified 81, 134 . The right image show the Hubble image of Abell 370. Most of the bright, galaxies seen are cluster members at j 0.375, whereas the arc, i.e. the highly elongated feature, is the image a galaxy at redshift 0.724 135 . North is on top, East to the left, field of view is roughly 40x60 arcsec2 could not immediately provide...

Dynamics of the Hot Intracluster Medium

Vikhlinin1, M. Markevitch1, M. Machacek1 and E. Churazov2 1 Center for Astrophysics, Cambridge, MA 02138, USA cjonesOcfa.harvard.edu 2 MPA, Garching, Germany Ki IKI, Moscow, Russia churazov mpa-garch.iiig. mpg. de Clusters of galaxies might well have been called something else, if they had been seen first in other than visible light, since the optically luminous galaxies make up only a small fraction (< 5 ) of the cluster mass. In clusters, most of the baryons are in...

Info

Measurements of changes in the apparent brightness temperature of the CMB as a function of declination in the three X-ray bright clusters CL 0016+16, Abell 665, and Abell 2218. The largest SZ effects are seen near the centres of the clusters, and the angular sizes of the effects are consistent with predictions based on the X-ray images. The horizontai fines mark the range of possibfe systematic errors in the zero levels on the data, and the error bars contain both random and systematic...

Pcc 100

Fig. 13. (Loft) The cluster radial slieMi profile ms fitted by a NFW model. The shear expectation for a SIS model, fitting the strong lensing constraints, is shown. (Right) The enclosed mass as a function of radius dark hashed region represents the lensing mass while the red hashed regions represent the light profile multiplied by a fix constant to match the mass profile. The blue dashed line show the mass profile of an SIS model fitting the weak lensing data only. The conclusion is that theie...

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Where vc is the local circular velocity (14). In this case, (7) reduces to a2 r(d0 dr) and so, the tangential velocity dispersion is simply the circular velocity, A word of caution is appropriate here just because we can find a solution, does not imply that it is stable. This is particularly critical for models built with circular orbits only. Fig. 7. Projection on the plane of the sky, with r the 3D radius, R the projected component on the plane of the sky radius and z the corresponding along...

References

Allen, S.W., Taylor, G.B., RNulsen, E.J., et al. MNRAS 324, 842 (2001) 2. Bacchi, M., Feretti, L., Giovannini, G., Govoni, F. ALA 400, 465 (2003) 3. Barrow, J.D., Ferreira, P.G., Silk, J. Phys. Rev. Let. 78, 3610 (1997) 4. Baum, S.A., O'Dea, C.P. MNRAS 250, 737 (1991) 5. Beck, R., Sukurov, A., Sokoloff, D., Wielebinski, R. A& A 411, 99 (2003) 6. Beck, R., Krause, M. Astron. Nachr. 326, 414 (2005) 7. Begelman, M.C., Rees, M.J., Blandford, R.D. Nature 279, 770 (1979) 8. Best, P.N. MNRAS 351,...