galaxy dynamics in clash clusters
DESCRIPTION
Galaxy Dynamics in CLASH Clusters. Doron Lemze (Johns Hopkins). CLASH team + VLT team + Margaret Geller, Michael J. Kurtz, and Kenneth J. Rines. Clusters with reduced redshifts :. A963 - Hectospec (Margaret’s team) A2261 - Hectospec (Margaret’s team) - PowerPoint PPT PresentationTRANSCRIPT
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Galaxy Dynamics in CLASH Clusters
CLASH team + VLT team + Margaret Geller, Michael J. Kurtz, and Kenneth
J. Rines
Doron Lemze (Johns Hopkins)
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Clusters with reduced redshifts:
• A963 - Hectospec (Margaret’s team)• A2261 - Hectospec (Margaret’s team)• RXJ2129 - Hectospec (Margaret’s team)• MACS1206 – VLT & Magellan (Piero & DanK)
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Cluster members – removing interlopers
Why?
• Effects estimated quantities such as virial mass and concentration parameter.• Effects substructure measurements.• Effects estimating the level of relaxation.
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Cluster members – A963
# cluster members: 205
den Hartog & Katkert 1996
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Cluster members – RXJ2129
# cluster members: 195
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Cluster members – A2261
# cluster members: 213
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Cluster members – MACSJ1206
# cluster members: 311
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Substructure
2,2
,22 1
ilocalilocal
locali vvN
g
N
ii N
g
/1
2
Dressler & Shectman 1988 – a 3D method
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Substructure – A963
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Substructure – RXJ2129
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Substructure – A2261
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Substructure – MACSJ1206
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Substructure – summary
A2261 & MACSJ1206: substantial substructure
A963 & RXJ2129: some substructure level, but maybe not very significant?
Is it consistent with X-ray info?
Yes!
Out of the 20 relaxed CLASH clusters 8 have some evidence for substructure, among them A2261 & MACSJ1206 (Postman et al. 2011).
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Mass profiles
N
ji ij
N
i iv
R
vvGNrM
/123)(
N
iii
PMproj NvvR
GfrM /)( 2
r
c dRRAGF
rM0
2 )()(
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Mass profiles – A963
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Mass profiles – RXJ2129
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Mass profiles – MACSJ1206
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Mass profiles – A2261
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M – C relation
Coe et al.
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If at least some of the clusters are not fully relaxed, maybecomparing the unrelaxed clusters inferred concentrations to concentrations measured from simulated relaxed clusters is not comparing apples to apples.
However, since unrelaxed clusters should have slightly lower concentrations (Neto et al. 2007; Duffy et al. 2008), this actually increases the mass-concentration tension between observed inferred values and theoretical expectations.
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MACSJ1206 – Astronomy Picture of the Day