868 research outputs found
Permutation branes and linear matrix factorisations
All the known rational boundary states for Gepner models can be regarded as
permutation branes. On general grounds, one expects that topological branes in
Gepner models can be encoded as matrix factorisations of the corresponding
Landau-Ginzburg potentials. In this paper we identify the matrix factorisations
associated to arbitrary B-type permutation branes.Comment: 43 pages. v2: References adde
The Effect of Variability on the Estimation of Quasar Black Hole Masses
We investigate the time-dependent variations of ultraviolet (UV) black hole
mass estimates of quasars in the Sloan Digital Sky Survey (SDSS). From SDSS
spectra of 615 high-redshift (1.69 < z < 4.75) quasars with spectra from two
epochs, we estimate black hole masses, using a single-epoch technique which
employs an additional, automated night-sky-line removal, and relies on UV
continuum luminosity and CIV (1549A) emission line dispersion. Mass estimates
show variations between epochs at about the 30% level for the sample as a
whole. We determine that, for our full sample, measurement error in the line
dispersion likely plays a larger role than the inherent variability, in terms
of contributing to variations in mass estimates between epochs. However, we use
the variations in quasars with r-band spectral signal-to-noise ratio greater
than 15 to estimate that the contribution to these variations from inherent
variability is roughly 20%. We conclude that these differences in black hole
mass estimates between epochs indicate variability is not a large contributer
to the current factor of two scatter between mass estimates derived from low-
and high-ionization emission lines.Comment: 76 pages, 15 figures, 2 (long) tables; Accepted for publication in
ApJ (November 10, 2007
Defect Perturbations in Landau-Ginzburg Models
Perturbations of B-type defects in Landau-Ginzburg models are considered. In
particular, the effect of perturbations of defects on their fusion is analyzed
in the framework of matrix factorizations. As an application, it is discussed
how fusion with perturbed defects induces perturbations on boundary conditions.
It is shown that in some classes of models all boundary perturbations can be
obtained in this way. Moreover, a universal class of perturbed defects is
constructed, whose fusion under certain conditions obey braid relations. The
functors obtained by fusing these defects with boundary conditions are twist
functors as introduced in the work of Seidel and Thomas.Comment: 46 page
Non-24-Hour Sleep-Wake Disorder Revisited – A Case Study
The human sleep-wake cycle is governed by two major factors: a homeostatic
hourglass process (process S), which rises linearly during the day, and a
circadian process C, which determines the timing of sleep in a ~24-h rhythm in
accordance to the external light–dark (LD) cycle. While both individual
processes are fairly well characterized, the exact nature of their interaction
remains unclear. The circadian rhythm is generated by the suprachiasmatic
nucleus (“master clock”) of the anterior hypothalamus, through cell-autonomous
feedback loops of DNA transcription and translation. While the phase length
(tau) of the cycle is relatively stable and genetically determined, the phase
of the clock is reset by external stimuli (“zeitgebers”), the most important
being the LD cycle. Misalignments of the internal rhythm with the LD cycle can
lead to various somatic complaints and to the development of circadian rhythm
sleep disorders (CRSD). Non-24-hour sleep-wake disorders (N24HSWD) is a CRSD
affecting up to 50% of totally blind patients and characterized by the
inability to maintain a stable entrainment of the typically long circadian
rhythm (tau > 24.5 h) to the LD cycle. The disease is rare in sighted
individuals and the pathophysiology less well understood. Here, we present the
case of a 40-year-old sighted male, who developed a misalignment of the
internal clock with the external LD cycle following the treatment for
Hodgkin’s lymphoma (ABVD regimen, four cycles and AVD regimen, four cycles). A
thorough clinical assessment, including actigraphy, melatonin profiles and
polysomnography led to the diagnosis of non-24-hour sleep-wake disorders
(N24HSWD) with a free-running rhythm of tau = 25.27 h. A therapeutic
intervention with bright light therapy (30 min, 10,000 lux) in the morning and
melatonin administration (0.5–0.75 mg) in the evening failed to entrain the
free-running rhythm, although a longer treatment duration and more intense
therapy might have been successful. The sudden onset and close timely
connection led us to hypothesize that the chemotherapy might have caused a
mutation of the molecular clock components leading to the observed elongation
of the circadian period
Atomic Resonance and Scattering
Contains reports on eleven research projects.U.S. Air Force - Office of Scientific Research (Grant AFOSR-81-0067
A Snapshot Survey for Gravitational Lenses Among z>=4.0 Quasars: I. The z>5.7 Sample
Over the last few years, the Sloan Digital Sky Survey (SDSS) has discovered
several hundred quasars with redshift between 4.0 and 6.4. Including the
effects of magnification bias, one expects a priori that an appreciable
fraction of these objects are gravitationally lensed. We have used the Advanced
Camera for Surveys on the Hubble Space Telescope to carry out a snapshot
imaging survey of high-redshift SDSS quasars to search for gravitationally
split lenses. This paper, the first in a series reporting the results of the
survey, describes snapshot observations of four quasars at z = 5.74, 5.82, 5.99
and 6.30, respectively. We find that none of these objects has a lensed
companion within 5 magnitudes with a separation larger than 0.3 arcseconds;
within 2.5 magnitudes, we can rule out companions within 0.1 arcseconds. Based
on the non-detection of strong lensing in these four systems, we constrain the
z~6 luminosity function to a slope of beta>-4.63 (3 sigma), assuming a break in
the quasar luminosity function at M_{1450}^*=-24.0. We discuss the implications
of this constraint on the ionizing background due to quasars in the early
universe. Given that these quasars are not highly magnified, estimates of the
masses of their central engines by the Eddington argument must be taken
seriously, possibly challenging models of black hole formation.Comment: 23 pages, 8 figures, 2 tables, submitted to A
An Empirical Calibration of the Completeness of the SDSS Quasar Survey
Spectra of nearly 20000 point-like objects to a Galactic reddening corrected
magnitude of i=19.1 have been obtained to test the completeness of the SDSS
quasar survey. The spatially-unresolved objects were selected from all regions
of color space, sparsely sampled from within a 278 sq. deg. area of sky covered
by this study. Only ten quasars were identified that were not targeted as
candidates by the SDSS quasar survey (including both color and radio source
selection). The inferred density of unresolved quasars on the sky that are
missed by the SDSS algorithm is 0.44 per sq. deg, compared to 8.28 per sq. deg.
for the selected quasar density, giving a completeness of 94.9(+2.6,-3.8) to
the limiting magnitude. Omitting radio selection reduces the color-only
selection completeness by about 1%. Of the ten newly identified quasars, three
have detected broad absorption line systems, six are significantly redder than
other quasars at the same redshift, and four have redshifts between 2.7 and 3.0
(the redshift range where the SDSS colors of quasars intersect the stellar
locus). The fraction of quasars missed due to image defects and blends is
approximately 4%, but this number varies by a few percent with magnitude.
Quasars with extended images comprise about 6% of the SDSS sample, and the
completeness of the selection algorithm for extended quasars is approximately
81%, based on the SDSS galaxy survey. The combined end-to-end completeness for
the SDSS quasar survey is approximately 89%. The total corrected density of
quasars on the sky to i=19.1 is estimated to be 10.2 per sq. deg.Comment: 37 pages, 10 figures, accepted for publication in A
First Measurement of the Clustering Evolution of Photometrically-Classified Quasars
We present new measurements of the quasar autocorrelation from a sample of
\~80,000 photometrically-classified quasars taken from SDSS DR1. We find a
best-fit model of for the angular
autocorrelation, consistent with estimates from spectroscopic quasar surveys.
We show that only models with little or no evolution in the clustering of
quasars in comoving coordinates since z~1.4 can recover a scale-length
consistent with local galaxies and Active Galactic Nuclei (AGNs). A model with
little evolution of quasar clustering in comoving coordinates is best explained
in the current cosmological paradigm by rapid evolution in quasar bias. We show
that quasar biasing must have changed from b_Q~3 at a (photometric) redshift of
z=2.2 to b_Q~1.2-1.3 by z=0.75. Such a rapid increase with redshift in biasing
implies that quasars at z~2 cannot be the progenitors of modern L* objects,
rather they must now reside in dense environments, such as clusters. Similarly,
the duration of the UVX quasar phase must be short enough to explain why local
UVX quasars reside in essentially unbiased structures. Our estimates of b_Q are
in good agreement with recent spectroscopic results, which demonstrate the
implied evolution in b_Q is consistent with quasars inhabiting halos of similar
mass at every redshift. Treating quasar clustering as a function of both
redshift and luminosity, we find no evidence for luminosity dependence in
quasar clustering, and that redshift evolution thus affects quasar clustering
more than changes in quasars' luminosity. We provide a new method for
quantifying stellar contamination in photometrically-classified quasar catalogs
via the correlation function.Comment: 34 pages, 10 figures, 1 table, Accepted to ApJ after: (i) Minor
textual changes; (ii) extra points added to Fig.
Exploratory Chandra Observations of the Three Highest Redshift Quasars Known
We report on exploratory Chandra observations of the three highest redshift
quasars known (z = 5.82, 5.99, and 6.28), all found in the Sloan Digital Sky
Survey. These data, combined with a previous XMM-Newton observation of a z =
5.74 quasar, form a complete set of color-selected, z > 5.7 quasars. X-ray
emission is detected from all of the quasars at levels that indicate that the
X-ray to optical flux ratios of z ~ 6 optically selected quasars are similar to
those of lower redshift quasars. The observations demonstrate that it will be
feasible to obtain quality X-ray spectra of z ~ 6 quasars with current and
future X-ray missions.Comment: 15 pages, ApJL, in press; small revisions to address referee Comment
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