The Descendants of Lyman Break Galaxies in Galaxy Clusters: Spatial Distribution and Orbital Properties | Zendy

Fabio Governato | Zendy; Sebastiano Ghigna | Zendy; Ben Moore | Zendy; Thomas Quinn | Zendy; Joachim Stadel | Zendy; George Lake | Zendy

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The Descendants of Lyman Break Galaxies in Galaxy Clusters: Spatial Distribution and Orbital Properties

Author(s) -

Fabio Governato,

Sebastiano Ghigna,

Ben Moore,

Thomas Quinn,

Joachim Stadel,

George Lake

Publication year - 2001

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/318431

Subject(s) - astrophysics , physics , velocity dispersion , virial mass , galaxy cluster , galaxy , brightest cluster galaxy , astronomy , luminosity , population , virial theorem , radius , halo , cluster (spacecraft) , elliptical galaxy , galaxy formation and evolution , type cd galaxy , medicine , computer security , environmental health , computer science , programming language

We combine semi-analytical methods with a ultra-high resolution simulation ofa galaxy cluster (of mass 2.3 10^14h-1Msolar, and 4 10^6 particles within itsvirial radius) formed in a standard CDM universe to study the spatialdistribution and orbital properties of the present-day descendents of LymanBreak Galaxies (LBGs). At the present time only five (out of 12) of haloscontaining LBGs survive as separate entities inside the cluster virial radius.Their circular velocities are in the range 200 - 550 km/sec. Seven halos mergedtogether to form the central object at the very center of the cluster. Usingsemi-analytical modeling of galaxy evolution we show that descendents of haloscontaining LBGs now host giant elliptical galaxies. Galaxy orbits are radial,with a pericenter to apocenter ratio of about 1:5. The orbital eccentricitiesof LBGs descendents are statistically indistinguishable from those of theaverage galaxy population inside the cluster, suggesting that the orbits ofthese galaxies are not significantly affected by dynamical friction decay afterthe formation of the cluster's main body. In this cluster, possibly due to itsearly formation time, the descendents of LBGs are contained within the central60% of the cluster virial radius and have an orbital velocity dispersion lowerthan the global galaxy population, originating a mild luminosity segregationfor the brightest cluster members. Mass estimates based only on LBGsdescendents (especially including the central cD) reflect this bias in spaceand velocity and underestimate the total mass of this well virialized clusterby up to a factor of two compared to estimates using at least 20 clustermembers.Comment: 6 Pages, 2 Postscript figures. Submitted to Ap

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