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fMRI correlates of subjective reversals in ambiguous structure-from-motion
We used fMRI to examine the neural correlates of subjective reversals for bistable structure-from-motion. We compared transparent random-dot kinematograms depicting either a cylinder rotating in depth or two flat surfaces translating in opposite directions at apparently different depths. For both such stimuli, the motion of dots on the different apparent depth planes typically appears to reverse direction periodically on prolonged viewing. Yet for cylindrical but not flat stimuli, such subjective reversals also coincide with apparent reversal of 3D rotation direction. We hypothesized that the lateral occipital complex (region LOC), sensitive to 3D form, might show greater event-related activity for subjective reversals of cylindrical than flat stimuli; conversely, motion-sensitive hMT+/V5 should respond in common to subjective reversals for either type of stimuli, as both are perceived as changes in planar motion. We obtained an event-related measure of neural activity associated with subjective reversals after first factoring out block-related differences between cylindrical versus flat stimuli (and thereby the associated low-level blocked stimulus differences). In support of our hypothesis, only the cylindrical stimuli produced reversal-related activity in contralateral human LOC. In contrast, the hMT+/V5 complex was activated alike by subjective reversals for both cylindrical and flat stimuli. Intriguingly, V1 also showed (contralateral) specificity for rotational reversals, suggesting a possible feedback influence from LOC. These results reveal specific neural correlates for subjective switches of 3D rotation versus translation, as distinct from subjective reversals in general
Can the Future Influence the Present?
One widely accepted model of classical electrodynamics assumes that a moving charged particle produces both retarded and advanced fields. This formulation first appeared at least 75 years ago. It was popularized in the 1940\u27s by work of Wheeler and Feynman. But the most fundamental question associated with the model has remained unanswered: When (if ever) does the two-body problem have a unique solution? The present paper gives an answer in one special case. Imagine two identical charged particles alone in the universe moving symmetrically along the x axis. One is at x(t) and the other is at −x(t). Their motion is then governed by a system of functional differential equations involving both retarded and advanced arguments. This system together with the Newtonian initial data x(0)=x0\u3e0 and x′(0)=0 has a unique solution for all time provided x0 is sufficiently large. Perhaps the existence and uniqueness proof given for this special case will pave the way for more general results on this curious two-body problem
A scanning tunnelling microscopy study of C and N adsorption phases on the vicinal Ni(100) surfaces Ni(810) and Ni(911)
The influence of N and C chemisorption on the morphology and local structure of nominal Ni(810) and Ni(911) surfaces, both vicinal to (100) but with [001] and 011¯ step directions, respectively, has been investigated using scanning tunnelling microscopy (STM) and low energy electron diffraction. Ni(911) undergoes substantial step bunching in the presence of both adsorbates, with the (911)/N surface showing (411) facets, whereas for Ni(810), multiple steps 2–4 layers high are more typical. STM atomic-scale images show the (2×2)pg ‘clock’ reconstruction on the (100) terraces of the (810) surfaces with both C and N, although a second c(2×2) structure, most readily reconciled with a ‘rumpling’ reconstruction, is also seen on Ni(810)/N. On Ni(911), the clock reconstruction is not seen on the (100) terraces with either adsorbate, and these images are typified by protrusions on a (1×1) mesh. This absence of clock reconstruction is attributed to the different constraints imposed on the lateral movements of the surface Ni atoms adjacent to the up-step edge of the terraces with a [011] step direction
Phase transformation in Si from semiconducting diamond to metallic beta-Sn phase in QMC and DFT under hydrostatic and anisotropic stress
Silicon undergoes a phase transition from the semiconducting diamond phase to
the metallic beta-Sn phase under pressure. We use quantum Monte Carlo
calculations to predict the transformation pressure and compare the results to
density functional calculations employing the LDA, PBE, PW91, WC, AM05, PBEsol
and HSE06 exchange-correlation functionals. Diffusion Monte Carlo predicts a
transition pressure of 14.0 +- 1.0 GPa slightly above the experimentally
observed transition pressure range of 11.3 to 12.6 GPa. The HSE06 hybrid
functional predicts a transition pressure of 12.4 GPa in excellent agreement
with experiments. Exchange-correlation functionals using the local-density
approximation and generalized-gradient approximations result in transition
pressures ranging from 3.5 to 10.0 GPa, well below the experimental values. The
transition pressure is sensitive to stress anisotropy. Anisotropy in the stress
along any of the cubic axes of the diamond phase of silicon lowers the
equilibrium transition pressure and may explain the discrepancy between the
various experimental values as well as the small overestimate of the quantum
Monte Carlo transition pressure
Hubble Space Telescope Counts of Elliptical Galaxies: Constraints on Cosmological Models ?
The interpretation of galaxy number counts in terms of cosmological models is
fraught with difficulty due to uncertainties in the overall galaxy population
(mix of morphological types, luminosity functions etc.) and in the observations
(loss of low surface brightness images, image blending etc.). Many of these can
be overcome if we use deep high resolution imaging of a single class of high
surface brightness galaxies, whose evolution is thought to be fairly well
understood. This is now possible by selecting elliptical and S0 galaxies using
Hubble Space Telescope images from the Medium Deep Survey and other ultradeep
WFPC2 images. In the present paper, we examine whether such data can be used to
discriminate between open and closed universes, or between conventional
cosmological models and those dominated by a cosmological constant. We find,
based on the currently available data, that unless elliptical galaxies undergo
very strong merging since (and/or very large errors exist in the
morphological classifications), then flat models dominated by a cosmological
constant are ruled out. However, both an Einstein-de Sitter ()
model with standard passive stellar evolution and an open ()
model with no net evolution ({\it i.e.} cancelling stellar and dynamical
evolution) predict virtually identical elliptical and S0 galaxy counts.
Based on these findings and the recent reportings of km/s
Mpc/s, we find that the maximum acceptable age of the universe is 13.3 Gyrs and
a value of Gyrs favored. A flat------universe is
therefore {\it not} a viable solution to the /globular cluster age
problem.Comment: Accepted for publication in the Astrophysical Journal (April, 1996).
34 pages (including 4 figures) of gzip compressed and uuencoded PS. Also
available at http://www.phys.unsw.edu.au/~spd/bib.htm
The Faint End Slopes Of Galaxy Luminosity Functions In The COSMOS 2-Square Degree Field
We examine the faint-end slope of the rest-frame V-band luminosity function
(LF), with respect to galaxy spectral type, of field galaxies with redshift
z<0.5, using a sample of 80,820 galaxies with photometric redshifts in the
Cosmic Evolution Survey (COSMOS) field. For all galaxy spectral types combined,
the LF slope, alpha, ranges from -1.24 to -1.12, from the lowest redshift bin
to the highest. In the lowest redshift bin (0.02<z<0.1), where the magnitude
limit is M(V) ~ -13, the slope ranges from ~ -1.1 for galaxies with early-type
spectral energy distributions (SEDs), to ~ -1.9 for galaxies with
low-extinction starburst SEDs. In each galaxy SED category (Ell, Sbc, Scd/Irr,
and starburst), the faint-end slopes grow shallower with increasing redshift;
in the highest redshift bin (0.4<z<0.5), the slope is ~ -0.5 and ~ -1.3 for
early-types and starbursts respectively. The steepness of alpha at lower
redshift could be qualitatively explained by large numbers of faint dwarf
galaxies, perhaps of low surface brightness, which are not detected at higher
redshifts.Comment: 24 pages including 5 figures, accepted to ApJ
The Millennium Galaxy Catalogue: The connection between close pairs and asymmetry; implications for the galaxy merger rate
We compare the use of galaxy asymmetry and pair proximity for measuring
galaxy merger fractions and rates for a volume limited sample of 3184 galaxies
with -21 < M(B) -5 log h < -18 mag. and 0.010 < z < 0.123 drawn from the
Millennium Galaxy Catalogue. Our findings are that:
(i) Galaxies in close pairs are generally more asymmetric than isolated
galaxies and the degree of asymmetry increases for closer pairs. At least 35%
of close pairs (with projected separation of less than 20 h^{-1} kpc and
velocity difference of less than 500 km s^{-1}) show significant asymmetry and
are therefore likely to be physically bound.
(ii) Among asymmetric galaxies, we find that at least 80% are either
interacting systems or merger remnants. However, a significant fraction of
galaxies initially identified as asymmetric are contaminated by nearby stars or
are fragmented by the source extraction algorithm. Merger rates calculated via
asymmetry indices need careful attention in order to remove the above sources
of contamination, but are very reliable once this is carried out.
(iii) Close pairs and asymmetries represent two complementary methods of
measuring the merger rate. Galaxies in close pairs identify future mergers,
occurring within the dynamical friction timescale, while asymmetries are
sensitive to the immediate pre-merger phase and identify remnants.
(iv) The merger fraction derived via the close pair fraction and asymmetries
is about 2% for a merger rate of (5.2 +- 1.0) 10^{-4} h^3 Mpc^{-3} Gyr^{-1}.
These results are marginally consistent with theoretical simulations (depending
on the merger time-scale), but imply a flat evolution of the merger rate with
redshift up to z ~1.Comment: 10 pages, 10 figures, emulateapj format. ApJ, accepte
Risk assessment in open source systems
Adopting Open Source Software (OSS) components offers many advantages to organizations but also introduces risks related to the intrinsic fluidity of the OSS development projects. Choosing the right components is a critical decision, as it could contribute to the success of any adoption process. Making the right decision requires to evaluate the technical capabilities of the components and also related strategic aspects, including possible impacts on high level objectives. This can be achieved through a portfolio of risk assessment and mitigation methods. In this briefing we introduce the basic concepts related to OSS ecosystems and to risk representation and reasoning. We illustrate how risk management activities in OSS can benefit from the large amount of data available from OSS repositories and how they can be connected to business goals for strategic decision-making. The concepts are illustrated with a software platform developed in the context of the EU FP7 project RISCOSS.Peer ReviewedPostprint (author's final draft
ProFit : Bayesian profile fitting of galaxy images
We present ProFit, a new code for Bayesian two-dimensional photometric galaxy profile modelling. ProFit consists of a low-level c++ library (libprofit), accessible via a command-line interface and documented API, along with high-level R (ProFit) and Python (PyProFit) interfaces (available at github.com/ICRAR/libprofit, github.com/ICRAR/ProFit, and github.com/ICRAR/pyprofit, respectively). R ProFit is also available pre-built from cran; however, this version will be slightly behind the latest GitHub version. libprofit offers fast and accurate two-dimensional integration for a useful number of profiles, including Sérsic, Core-Sérsic, broken-exponential, Ferrer, Moffat, empirical King, point-source, and sky, with a simple mechanism for adding new profiles. We show detailed comparisons between libprofit and galfit. libprofit is both faster and more accurate than galfit at integrating the ubiquitous Sérsic profile for the most common values of the Sérsic index n (0.5 < n < 8). The high-level fitting code ProFit is tested on a sample of galaxies with both SDSS and deeper KiDS imaging. We find good agreement in the fit parameters, with larger scatter in best-fitting parameters from fitting images from different sources (SDSS versus KiDS) than from using different codes (ProFit versus galfit). A large suite of Monte Carlo-simulated images are used to assess prospects for automated bulge-disc decomposition with ProFit on SDSS, KiDS, and future LSST imaging. We find that the biggest increases in fit quality come from moving from SDSS- to KiDS-quality data, with less significant gains moving from KiDS to LSST.Publisher PDFPeer reviewe
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