424 research outputs found
Model-Independent Mass Reconstruction of the Hubble Frontier Field Clusters with MARS \\ Based on Self-Consistent Strong Lensing Data
We present new strong-lensing (SL) mass reconstruction of the six Hubble
Frontier Fields (HFF) clusters with the MAximum-entropy ReconStruction () algorithm. is a new free-form inversion method, which
suppresses spurious small-scale fluctuations while achieving excellent
convergence in positions of multiple images. For each HFF cluster, we obtain a
model-independent mass distribution from the compilation of the self-consistent
SL data in the literature. With multiple images per cluster, we
reconstruct solutions with small scatters of multiple images in both source
(~0".01) and image planes (~0."05), which are lower than the previous results
by an order of magnitude. An outstanding case is the MACS J0416.1-2403 mass
reconstruction, which is based on the largest high-quality SL dataset where all
236 multiple images/knots have spectroscopic redshifts. Although our solution
is smooth on a large scale, it reveals group/galaxy-scale peaks where the
substructures are required by the data. We find that in general, these mass
peaks are in excellent spatial agreement with the member galaxies, although
{\tt MARS} never uses the galaxy distributions as priors. Our study
corroborates the flexibility and accuracy of the algorithm and
demonstrates that is a powerful tool in the JWST era, when
times larger number of multiple image candidates become available for SL mass
reconstruction, and self-consistency within the dataset becomes a critical
issue.Comment: 19 pages, 7 figures, 7 tables, submitted to Ap
MC: Multi-wavelength and dynamical analysis of the merging galaxy cluster ZwCl 0008.8+5215: An older and less massive Bullet Cluster
We analyze a rich dataset including Subaru/SuprimeCam, HST/ACS and WFC3,
Keck/DEIMOS, Chandra/ACIS-I, and JVLA/C and D array for the merging galaxy
cluster ZwCl 0008.8+5215. With a joint Subaru/HST weak gravitational lensing
analysis, we identify two dominant subclusters and estimate the masses to be
M
and 1.2 M. We estimate the
projected separation between the two subclusters to be
924 kpc. We perform a clustering analysis on
confirmed cluster member galaxies and estimate the line of sight velocity
difference between the two subclusters to be 92164 km s. We
further motivate, discuss, and analyze the merger scenario through an analysis
of the 42 ks of Chandra/ACIS-I and JVLA/C and D polarization data. The X-ray
surface brightness profile reveals a remnant core reminiscent of the Bullet
Cluster. The X-ray luminosity in the 0.5-7.0 keV band is
1.70.110 erg s and the X-ray
temperature is 4.900.13 keV. The radio relics are polarized up to 40.
We implement a Monte Carlo dynamical analysis and estimate the merger velocity
at pericenter to be 1800 km s. ZwCl
0008.8+5215 is a low-mass version of the Bullet Cluster and therefore may prove
useful in testing alternative models of dark matter. We do not find significant
offsets between dark matter and galaxies, as the uncertainties are large with
the current lensing data. Furthermore, in the east, the BCG is offset from
other luminous cluster galaxies, which poses a puzzle for defining dark matter
-- galaxy offsets.Comment: 22 pages, 19 figures, accepted for publication in the Astrophysical
Journal on March 13, 201
Dark Matter in the Galaxy Cluster CL J1226+3332 at Z=0.89
We present a weak-lensing analysis of the galaxy cluster CL J1226+3332 at
z=0.89 using Hubble Space Telescope Advanced Camera for Surveys images. The
cluster is the hottest (>10 keV), most X-ray luminous system at z>0.6 known to
date. The relaxed X-ray morphology, as well as its high temperature, is unusual
at such a high redshift. Our mass reconstruction shows that on a large scale
the dark matter distribution is consistent with a relaxed system with no
significant substructures. However, on a small scale the cluster core is
resolved into two mass clumps highly correlated with the cluster galaxy
distribution. The dominant mass clump lies close to the brightest cluster
galaxy whereas the other less massive clump is located ~40" (~310 kpc) to the
southwest. Although this secondary mass clump does not show an excess in the
X-ray surface brightness, the gas temperature of the region is much higher
(12~18 keV) than those of the rest. We propose a scenario in which the less
massive system has already passed through the main cluster and the X-ray gas
has been stripped during this passage. The elongation of the X-ray peak toward
the southwestern mass clump is also supportive of this possibility. We measure
significant tangential shears out to the field boundary (~1.5 Mpc), which are
well described by an Navarro-Frenk-White profile with a concentration parameter
of c200=2.7+-0.3 and a scale length of rs=78"+-19" (~600 kpc) with
chi^2/d.o.f=1.11. Within the spherical volume r200=1.6 Mpc, the total mass of
the cluster becomes M(r<r200)=(1.4+-0.2) x 10^15 solar mass. Our weak-lensing
analysis confirms that CL1226+3332 is indeed the most massive cluster known to
date at z>0.6.Comment: Accepted for publication in Ap
Morphology with Light Profile Fitting of Confirmed Cluster Galaxies at z=0.84
We perform a morphological study of 124 spectroscopically confirmed cluster
galaxies in the z=0.84 galaxy cluster RX J0152.7-1357. Our classification
scheme includes color information, visual morphology, and 1-component and
2-component light profile fitting derived from Hubble Space Telescope riz
imaging. We adopt a modified version of a detailed classification scheme
previously used in studies of field galaxies and found to be correlated with
kinematic features of those galaxies. We compare our cluster galaxy
morphologies to those of field galaxies at similar redshift. We also compare
galaxy morphologies in regions of the cluster with different dark-matter
density as determined by weak-lensing maps. We find an early-type fraction for
the cluster population as a whole of 47%, about 2.8 times higher than the
field, and similar to the dynamically young cluster MS 1054 at similar
redshift. We find the most drastic change in morphology distribution between
the low and intermediate dark matter density regions within the cluster, with
the early type fraction doubling and the peculiar fraction dropping by nearly
half. The peculiar fraction drops more drastically than the spiral fraction
going from the outskirts to the intermediate-density regions. This suggests
that many galaxies falling into clusters at z~0.8 may evolve directly from
peculiar, merging, and compact systems into early-type galaxies, without having
the chance to first evolve into a regular spiral galaxy.Comment: 13 pages, 11 figures, accepted for publication in A&
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