32,157 research outputs found
Evolving Large-Scale Data Stream Analytics based on Scalable PANFIS
Many distributed machine learning frameworks have recently been built to
speed up the large-scale data learning process. However, most distributed
machine learning used in these frameworks still uses an offline algorithm model
which cannot cope with the data stream problems. In fact, large-scale data are
mostly generated by the non-stationary data stream where its pattern evolves
over time. To address this problem, we propose a novel Evolving Large-scale
Data Stream Analytics framework based on a Scalable Parsimonious Network based
on Fuzzy Inference System (Scalable PANFIS), where the PANFIS evolving
algorithm is distributed over the worker nodes in the cloud to learn
large-scale data stream. Scalable PANFIS framework incorporates the active
learning (AL) strategy and two model fusion methods. The AL accelerates the
distributed learning process to generate an initial evolving large-scale data
stream model (initial model), whereas the two model fusion methods aggregate an
initial model to generate the final model. The final model represents the
update of current large-scale data knowledge which can be used to infer future
data. Extensive experiments on this framework are validated by measuring the
accuracy and running time of four combinations of Scalable PANFIS and other
Spark-based built in algorithms. The results indicate that Scalable PANFIS with
AL improves the training time to be almost two times faster than Scalable
PANFIS without AL. The results also show both rule merging and the voting
mechanisms yield similar accuracy in general among Scalable PANFIS algorithms
and they are generally better than Spark-based algorithms. In terms of running
time, the Scalable PANFIS training time outperforms all Spark-based algorithms
when classifying numerous benchmark datasets.Comment: 20 pages, 5 figure
MC: Dynamical Analysis of the Merging Galaxy Cluster MACS J1149.5+2223
We present an analysis of the merging cluster MACS J1149.5+2223 using
archival imaging from Subaru/Suprime-Cam and multi-object spectroscopy from
Keck/DEIMOS and Gemini/GMOS. We employ two and three dimensional substructure
tests and determine that MACS J1149.5+2223 is composed of two separate mergers
between three subclusters occurring 1 Gyr apart. The primary merger gives
rise to elongated X-ray morphology and a radio relic in the southeast. The
brightest cluster galaxy is a member of the northern subcluster of the primary
merger. This subcluster is very massive
(16.7 M).
The southern subcluster is also very massive
(10.8 M),
yet it lacks an associated X-ray surface brightness peak, and it has been
unidentified previously despite the detailed study of this \emph{Frontier
Field} cluster. A secondary merger is occurring in the north along the line of
sight with a third, less massive, subcluster
(1.20 M).
We perform a Monte Carlo dynamical analysis on the main merger and estimate a
collision speed at pericenter of 2770 km
s. We show the merger to be returning from apocenter with core
passage occurring 1.16 Gyr before the observed
state. We identify the line of sight merging subcluster in a strong lensing
analysis in the literature and show that it is likely bound to MACS J1149
despite having reached an extreme collision velocity of 4000 km
s.Comment: 17 pages, 12 figure
The Cosmic Evolution Survey (COSMOS): a large-scale structure at z=0.73 and the relation of galaxy morphologies to local environment
We have identified a large-scale structure at z~0.73 in the COSMOS field,
coherently described by the distribution of galaxy photometric redshifts, an
ACS weak-lensing convergence map and the distribution of extended X-ray sources
in a mosaic of XMM observations. The main peak seen in these maps corresponds
to a rich cluster with Tx= 3.51+0.60/-0.46 keV and Lx=(1.56+/-0.04) x 10^{44}
erg/s ([0.1-2.4] keV band). We estimate an X-ray mass within
corresponding to M500~1.6 x 10^{14} Msun and a total lensing mass (extrapolated
by fitting a NFW profile) M(NFW)=(6+/-3) x 10^15 Msun. We use an automated
morphological classification of all galaxies brighter than I_AB=24 over the
structure area to measure the fraction of early-type objects as a function of
local projected density Sigma_10, based on photometric redshifts derived from
ground-based deep multi-band photometry. We recover a robust morphology-density
relation at this redshift, indicating, for comparable local densities, a
smaller fraction of early-type galaxies than today. Interestingly, this
difference is less strong at the highest densities and becomes more severe in
intermediate environments. We also find, however, local "inversions'' of the
observed global relation, possibly driven by the large-scale environment. In
particular, we find direct correspondence of a large concentration of disk
galaxies to (the colder side of) a possible shock region detected in the X-ray
temperature map and surface brightness distribution of the dominant cluster. We
interpret this as potential evidence of shock-induced star formation in
existing galaxy disks, during the ongoing merger between two sub-clusters.Comment: 15 pages (emulateapj style), 16 figs (low res.); to appear in the ApJ
Supplement COSMOS Special Issue. Low-resolution figures; full resolution
version available at:
http://www.astro.caltech.edu/~cosmos/publications/files/guzzo_0701482.pd
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