Cluster winds blow along supercluster axes

Novikov, D.; Melott, Adrian L.; Wilhite, Brian C.; Kaufman, Michael J.; Burns, Jack O.; Miller, Christopher J.; Batuski, D. J.

doi:10.1046/j.1365-8711.1999.02428.x

Cited by 21 publications

(21 citation statements)

References 22 publications

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“…Hence, the direction of the jets of CWAT-01 is almost perpendicular also to the long axis of LSS 17. This is in disagreement with the correlation of the alignment between the direction of the jets and (1) the central X-ray emission elongation Gomez et al 1997) and (2) the supercluster axis as defined by the distribution of the nearby Abell clusters (Novikov et al 1999). Nevertheless, the misalignment seen in CWAT-01's orientation compared to the parent cluster and to LSS 17 elongations may not be unexpected if we assume an early stage of cluster formation.…”

Section: Galaxy Cluster Assemblycontrasting

confidence: 56%

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A Wide‐Angle Tail Radio Galaxy in the COSMOS Field: Evidence for Cluster Formation

Smolčić¹,

Schinnerer²,

Finoguenov³

et al. 2007

ASTROPHYS J SUPPL S

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We have identified a complex galaxy cluster system in the COSMOS field via a wide-angle tail (WAT ) radio galaxy, consistent with the idea that WAT galaxies can be used as tracers of clusters. The WAT galaxy, CWAT-01, is coincident with an elliptical galaxy resolved in the HST ACS image. Using the COSMOS multiwavelength data set, we derive the radio properties of CWAT-01 and use the optical and X-ray data to investigate its host environment. The cluster hosting CWAT-01 is part of a larger assembly consisting of a minimum of four X-ray luminous clusters within $2 Mpc distance. We apply hydrodynamic models that combine ram pressure and buoyancy forces on CWAT-01. These models explain the shape of the radio jets only if the galaxy's velocity relative to the intracluster medium (ICM) is in the range of about 300-550 km s À1 , which is higher than expected for brightest cluster galaxies (BCGs) in relaxed systems. This indicates that the CWAT-01 host cluster is not relaxed but is possibly dynamically young. We argue that such a velocity could have been induced through subcluster merger within the CWAT-01 parent cluster and/or cluster-cluster interactions. Our results strongly indicate that we are witnessing the formation of a large cluster from an assembly of multiple clusters, consistent with the hierarchical scenario of structure formation. We estimate the total mass of the final cluster to be approximately 20% of the mass of the Coma Cluster.

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Section: Galaxy Cluster Assemblycontrasting

confidence: 56%

“…Although LSS 17 spatially extends $4 Mpc in the north-south direction, the direction of its long axis (as defined in, e.g., Novikov et al 1999) is in the northwest-southeast direction (see Fig. 3 in Scoville et al 2007b).…”

Section: Galaxy Cluster Assemblymentioning

confidence: 99%

A Wide‐Angle Tail Radio Galaxy in the COSMOS Field: Evidence for Cluster Formation

Smolčić¹,

Schinnerer²,

Finoguenov³

et al. 2007

ASTROPHYS J SUPPL S

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“…Clusters are often elongated within their group [40] and aligned within their supercluster [41]. This filamentary network [45] (.e.g.…”

Section: The Virial Theorem and Large Astrophysical Structuresmentioning

confidence: 99%

Ellipsoidal configurations in the de Sitter spacetime

Balaguera-Antolínez

Mota

Nowakowski

2006

Class. Quantum Grav.

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Abstract. The cosmological constant Λ modifies certain properties of large astrophysical rotating configurations with ellipsoidal geometries, provided the objects are not too compact. Assuming an equilibrium configuration and so using the tensor virial equation with Λ we explore several equilibrium properties of homogeneous rotating ellipsoids. One shows that the bifurcation point, which in the oblate case distinguishes the Maclaurin ellipsoid from the Jacobi ellipsoid, is sensitive to the cosmological constant. Adding to that, the cosmological constant allows triaxial configurations of equilibrium rotating the minor axis as solutions of the virial equations. The significance of the result lies in the fact that minor axis rotation is indeed found in nature. Being impossible for the oblate case, it is permissible for prolate geometries, with Λ zero and positive. For the triaxial case, however, an equilibrium solution is found only for non-zero positive Λ. Finally, we solve the tensor virial equation for the angular velocity and display special effects of the cosmological constant there.PACS numbers: 95.30. Sf, 98.62.Dm, 98.80.Jk, 98.52.Eh, 98.56.Ew Ellipsoidal configurations in the de Sitter spacetime 2

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“…Several studies of clusters of galaxies have provided evidence that properties of rich clusters depend on their large scale environment (Novikov et al 1999;Chambers et al 2002;Einasto et al 2001;Schuecker et al 2001;and Plionis & Basilakos 2002) up to a distance of about 20 h −1 Mpc. This distance is close to the so-called "pancake scale" (Melott & Shandarin 1993), and corresponds to the mean thickness of superclusters (Einasto et al 1994b(Einasto et al , 1997Jaaniste et al 1998).…”

Section: Comparison With Observationsmentioning

confidence: 99%

Environmental enhancement of DM haloes

Einasto¹,

Suhhonenko

Heinämäki

et al. 2005

A&A

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Abstract. We study the properties of dark matter haloes of a LCDM model in different environments. Using the distance of the 5th nearest neighbour as an environmental density indicator, we show that haloes in a high density environment are more massive, richer and have larger radii and larger velocity dispersions than haloes in a low density environment. Haloes in high density regions move with larger velocities, and are more spherical than haloes in low density regions. In addition, low mass haloes in the vicinity of the most massive haloes are themselves more massive, larger and have larger rms velocities and larger 3D velocities than low mass haloes far from massive haloes. The velocities of low mass haloes near massive haloes increase with the parent halo mass. Our results are in agreement with recent findings about environmental effects for groups and clusters of galaxies from deep (SDSS and LCRS) surveys.

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Cluster winds blow along supercluster axes

Cited by 21 publications

References 22 publications

A Wide‐Angle Tail Radio Galaxy in the COSMOS Field: Evidence for Cluster Formation

A Wide‐Angle Tail Radio Galaxy in the COSMOS Field: Evidence for Cluster Formation

Ellipsoidal configurations in the de Sitter spacetime

Environmental enhancement of DM haloes

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