1,245 research outputs found
The LSST Data Mining Research Agenda
We describe features of the LSST science database that are amenable to
scientific data mining, object classification, outlier identification, anomaly
detection, image quality assurance, and survey science validation. The data
mining research agenda includes: scalability (at petabytes scales) of existing
machine learning and data mining algorithms; development of grid-enabled
parallel data mining algorithms; designing a robust system for brokering
classifications from the LSST event pipeline (which may produce 10,000 or more
event alerts per night); multi-resolution methods for exploration of petascale
databases; indexing of multi-attribute multi-dimensional astronomical databases
(beyond spatial indexing) for rapid querying of petabyte databases; and more.Comment: 5 pages, Presented at the "Classification and Discovery in Large
Astronomical Surveys" meeting, Ringberg Castle, 14-17 October, 200
All degree six local unitary invariants of k qudits
We give explicit index-free formulae for all the degree six (and also degree
four and two) algebraically independent local unitary invariant polynomials for
finite dimensional k-partite pure and mixed quantum states. We carry out this
by the use of graph-technical methods, which provides illustrations for this
abstract topic.Comment: 18 pages, 6 figures, extended version. Comments are welcom
SUPERVISING MICROWAVE TELECOMMUNICATION NETWORKS WITH THE REALEX EXPERT SYSTEM SHELL
To effectively supervise a telecommunication network, an intelligent supervisory system is proposed consisting of a traditional process monitoring. a fault diagnostic, a communication handler and a database manager subsystem. The whole system is based on a generic expert system shell designed to operate in industrial environment. The diagnostic subsystem contains a two-level inference engine to operate on structural information and traditional if-then rules. To ensure easy mapping of the supervisory system to any telecommunication network a configuration environment consisting of several compilers integrated into a multi-window editor was also developed. The system was implemented on two interconnected IBM PC-s running MS WINDOWS 3.0
Distribution of Maximal Luminosity of Galaxies in the Sloan Digital Sky Survey
Extreme value statistics (EVS) is applied to the distribution of galaxy luminosities in the Sloan Digital Sky Survey (SDSS). We analyze the DR8 Main Galaxy Sample (MGS), as well as the Luminous Red Galaxies (LRG). Maximal luminosities are sampled from batches consisting of elongated pencil beams in the radial direction of sight. For the MGS, results suggest a small and positive tail index , effectively ruling out the possibility of having a finite maximum cutoff luminosity, and implying that the luminosity distribution function may decay as a power law at the high luminosity end. Assuming, however, , a non-parametric comparison of the maximal luminosities with the Fisher-Tippett-Gumbel distribution (limit distribution for variables distributed by the Schechter fit) indicates a good agreement provided uncertainties arising both from the finite batch size and from the batch size distribution are accounted for. For a volume limited sample of LRGs, results show that they can be described as being the extremes of a luminosity distribution with an exponentially decaying tail, provided the uncertainties related to batch-size distribution are taken care of
ParadigmavĂĄltĂĄs a csontmetasztĂĄzisok sebĂŠszetĂŠben. I. VĂŠgtagi ĂŠs medencelokalizĂĄciĂłjĂş ĂĄttĂŠtek
According to the statistical data of tumor registries the incidence of cancer has increased in the last decade, however the mortality shows only a slight change due to the new and effective multimodal treatments. The aim of our overview article is to present the changes in the survival of the metastatic patients, and to demonstrate which factors influence their prognosis. The improvement of survival resulted in a more active surgical role both in metastases of the bone of the extremities and the pelvis. We present a diagnostic flow chart and current options for the reconstruction of the different regions of the bone and skeleton, and we will discuss their potential advantages, disadvantages and complications. It is evident that apart from the impending and pathological fracture surgery it is not the first choice of treatment but rather a palliative measure. The aim of surgery is to alleviate pain, to regain mobility and improve quality of life. If possible minimal invasive techniques are performed, as they are less demanding and allow fast rehabilitation for the patient, and they are solutions that last for a lifetime. In optimal conditions radical curative surgery can be performed in about 10 to 15 per cent of the cases, and better survival is encouraging. Orv Hetil. 2017; 158(40): 1563-1569
Superclustering at Redshift Z=0.54
We present strong evidence for the existence of a supercluster at a redshift
of z=0.54 in the direction of Selected Area 68. From the distribution of
galaxies with spectroscopic redshifts we find that there is a large
over-density of galaxies (a factor of four over the number expected in an
unclustered universe) within the redshift range 0.530 < z < 0.555. By
considering the spatial distribution of galaxies within this redshift range
(using spectroscopic and photometric redshifts) we show that the galaxies in
SA68 form a linear structure passing from the South-West of the survey field
through to the North-East (with a position angle of approximately 35 deg East
of North). This position angle is coincident with the positions of the X-ray
clusters CL0016+16, RX J0018.3+1618 and a new X-ray cluster, RX J0018.8+1602,
centered near the radio source 54W084. All three of these sources are at a
redshift of approximately z=0.54 and have position angles, derived from their
X-ray photon distributions, consistent with that measured for the supercluster.
Assuming a redshift of 0.54 for the distribution of galaxies and a FWHM
dispersion in redshift of 0.020 this represents a coherent structure with a
radial extent of 31 Mpc, transverse dimension of 12 Mpc, and a thickness of
approximately 4 Mpc. The detection of this possible supercluster demonstrates
the power of using X-ray observations, combined with multicolor observations,
to map the large scale distribution of galaxies at intermediate redshifts.Comment: 12 pages, 3 figures, Latex, aaspp4.sty, accepted for publication in
Ap J Letters. Figure 3 and followup observations can be found at
http://tarkus.pha.jhu.edu/~ajc/papers/supercluster
Peaks theory and the excursion set approach
We describe a model of dark matter halo abundances and clustering which
combines the two most widely used approaches to this problem: that based on
peaks and the other based on excursion sets. Our approach can be thought of as
addressing the cloud-in-cloud problem for peaks and/or modifying the excursion
set approach so that it averages over a special subset, rather than all
possible walks. In this respect, it seeks to account for correlations between
steps in the walk as well as correlations between walks. We first show how the
excursion set and peaks models can be written in the same formalism, and then
use this correspondence to write our combined excursion set peaks model. We
then give simple expressions for the mass function and bias, showing that even
the linear halo bias factor is predicted to be k-dependent as a consequence of
the nonlocality associated with the peak constraint. At large masses, our model
has little or no need to rescale the variable delta_c from the value associated
with spherical collapse, and suggests a simple explanation for why the linear
halo bias factor appears to lie above that based on the peak-background split
at high masses when such a rescaling is assumed. Although we have concentrated
on peaks, our analysis is more generally applicable to other traditionally
single-scale analyses of large-scale structure.Comment: 10 pages, 4 figures; v2 -- minor changes, added discussion in sec2.2,
fixed a typo. Accepted in MNRA
Galaxy Zoo : Building the low-mass end of the red sequence with local post-starburst galaxies
We present a study of local post-starburst galaxies (PSGs) using the photometric and spectroscopic observations from the Sloan Digital Sky Survey and the results from the Galaxy Zoo project. We find that the majority of our local PSG population have neither early- nor late-type morphologies but occupy a well-defined space within the colour-stellar mass diagram, most notably, the low-mass end of the 'green valley' below the transition mass thought to be the mass division between low-mass star-forming galaxies and high-mass passively evolving bulge-dominated galaxies. Our analysis suggests that it is likely that local PSGs will quickly transform into 'red', low-mass early-type galaxies as the stellar morphologies of the 'green' PSGs largely resemble that of the early-type galaxies within the same mass range. We propose that the current population of PSGs represents a population of galaxies which is rapidly transitioning between the star-forming and the passively evolving phases. Subsequently, these PSGs will contribute towards the build-up of the low-mass end of the 'red sequence' once the current population of young stars fade and stars are no longer being formed. These results are consistent with the idea of 'downsizing' where the build-up of smaller galaxies occurs at later epochs.Peer reviewe
Galaxy Zoo Green Peas: discovery of a class of compact extremely star-forming galaxies
âThe definitive version is available at www3.interscience.wiley.com '. Copyright Royal Astronomical Society. DOI: 10.1111/j.1365-2966.2009.15383.xWe investigate a class of rapidly growing emission line galaxies, known as 'Green Peas', first noted by volunteers in the Galaxy Zoo project because of their peculiar bright green colour and small size, unresolved in Sloan Digital Sky Survey imaging. Their appearance is due to very strong optical emission lines, namely [O iii]Îť5007 Ă
, with an unusually large equivalent width of up to âź1000 Ă
. We discuss a well-defined sample of 251 colour-selected objects, most of which are strongly star forming, although there are some active galactic nuclei interlopers including eight newly discovered narrow-line Seyfert 1 galaxies. The star-forming Peas are low-mass galaxies (Mâź 108.5â1010 Mâ) with high star formation rates (âź10 Mâ yrâ1) , low metallicities (log[O/H]+ 12 âź 8.7) and low reddening [ E(BâV) ⤠0.25 ] and they reside in low-density environments. They have some of the highest specific star formation rates (up to âź10â8 yrâ1 ) seen in the local Universe, yielding doubling times for their stellar mass of hundreds of Myr. The few star-forming Peas with Hubble Space Telescope imaging appear to have several clumps of bright star-forming regions and low surface density features that may indicate recent or ongoing mergers. The Peas are similar in size, mass, luminosity and metallicity to luminous blue compact galaxies. They are also similar to high-redshift ultraviolet-luminous galaxies, e.g. Lyman-break galaxies and LyÎą emitters, and therefore provide a local laboratory with which to study the extreme star formation processes that occur in high-redshift galaxies. Studying starbursting galaxies as a function of redshift is essential to understanding the build up of stellar mass in the Universe.Peer reviewe
An Inversion Method for Measuring Beta in Large Redshift Surveys
A precision method for determining the value of Beta= Omega_m^{0.6}/b, where
b is the galaxy bias parameter, is presented. In contrast to other existing
techniques that focus on estimating this quantity by measuring distortions in
the redshift space galaxy-galaxy correlation function or power spectrum, this
method removes the distortions by reconstructing the real space density field
and determining the value of Beta that results in a symmetric signal. To remove
the distortions, the method modifies the amplitudes of a Fourier plane-wave
expansion of the survey data parameterized by Beta. This technique is not
dependent on the small-angle/plane-parallel approximation and can make full use
of large redshift survey data. It has been tested using simulations with four
different cosmologies and returns the value of Beta to +/- 0.031, over a factor
of two improvement over existing techniques.Comment: 16 pages including 6 figures Submitted to The Astrophysical Journa
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