Date and Time of the Query: 2019-06-25 T17:01:51 PDT
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Notes for object ABELL 3888

2 note(s) found in NED.

1. 2007AJ....134..466K
Re:ABELL 3888
A3888 is discussed in great detail in Paper I. To review, A3888 is a richness
class 2, Bautz-Morgan type I-II cluster at a redshift of 0.151. This cluster has
no cD galaxy; instead the core is comprised of three distinct subclumps of
multiple galaxies each. At least two galaxies in each of the subclumps are
confirmed members based on velocities (Teague et al. 1990; Pimbblet et al.
2002). The brightest cluster galaxy is only 0.12 +/- 0.04 mag brighter than the
second-ranked galaxy. XMM-Newton contours show an elongated distribution
centered roughly in the middle of the three clumps of galaxies. Reiprich &
Bohringer (2002) estimated mass from the X-ray luminosity to be M_200_ =
(25.5+/^10.5^_7.4_) * 10^14^ h^-1^_70_ M_{sun}_, where r_200_ = 2.8 h^-1^_70_
Mpc. This is consistent with the mass estimate from the published velocity
dispersion of 1102 +/-^137^_107_ (Girardi & Mezzetti 2001).
There is a clear red sequence of galaxies in the CMD of A3888. Using the CMD
as an indication of membership, we estimate the flux in cluster galaxies to be
(3.0 +/- 0.9) * 10^12^ L_{sun}_ in r and (7.2 +/- 2.2) * 10^11^ L_{sun}_ in B
inside of 0.92 h^-1^_70_ Mpc. We also determine galaxy flux using the Driver et
al. (1998) luminosity distribution, which is based on the statistical background
subtraction of noncluster galaxies to be (4.3 +/- 0.7) * 10^12^ L_{sun}_ in the
r-band and (3.4 +/- 0.6) * 10^12^ L_{sun}_ in V. The difference in these two
estimates is likely due to uncertainties in our membership identification (of
order 30%) and difference in detection thresholds of the two surveys.
Figure 9 shows the relevant plots for this cluster. There is a centralized
ICL component ranging from 26 to 29 mag arcsec^-2^ in r despite the fact that
there is no cD galaxy. The total flux in the ICL is (4.4 +/- 2.1) * 10^11^
L_{sun}_ in r and (8.6 +/- 2.5) * 10^10^ L_{sun }_ in B, which makes for ICL
fractions of 13% +/- 5% in r and 11% +/- 3% in B. The ICL has a red color
profile with an average color of V - r ~= 0.5 +/- 0.1, which is marginally
redder (0.2 mag) than the RCS. There is also a diffuse light component
surrounding a group of galaxies that is 1.4 h^-1^_70_ Mpc from the cluster
center that totals (1.7 +/- 0.5) * 10^10^^ L_{sun}_ in V and (2.6 +/- 1.2) *
10^10^ L_{sun}_ in r and has a color consistent with the main ICL component.

2. 1997ApJ...482...41G
Re:ABELL 3888
This is an almost regular cluster, but with an asymmetric velocity
distribution. The local dispersions are atypically high because of the
presence of numerous field galaxies uniformly distributed through the
whole extension of the cluster, thus suggesting a systematic
contamination effect.

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