230 research outputs found
Testing for lack of fit in inverse regression - with applications to photonic imaging.
Regression; Problems; Lack-of-fit; Applications;
A sharp look at the gravitationally lensed quasar SDSS J0806+2006 with Laser Guide Star Adaptive Optics
We present the first VLT near-IR observations of a gravitationally lensed
quasar, using adaptive optics and laser guide star. These observations can be
considered as a test bench for future systematic observations of lensed quasars
with adaptive optics, even when bright natural guide stars are not available in
the nearby field. With only 14 minutes of observing time, we derived very
accurate astrometry of the quasar images and of the lensing galaxy, with 0.05
\arcsec spatial resolution, comparable to the Hubble Space Telescope (HST). In
combination with deep VLT optical spectra of the quasar images, we use our
adaptive optics images to constrain simple models for the mass distribution of
the lensing galaxy. The latter is almost circular and does not need any strong
external shear to fit the data. The time delay predicted for SDSS0806+2006,
assuming a singular isothermal ellipsoid model and the concordance cosmology,
is Delta t \simeq 50 days. Our optical spectra indicate a flux ratio between
the quasar images of A/B=1.3 in the continuum and A/B=2.2 in both the MgII and
in the CIII] broad emission lines. This suggests that microlensing affects the
continuum emission. However, the constant ratio between the two emission lines
indicates that the broad emission line region is not microlensed. Finally, we
see no evidence of reddening by dust in the lensing galaxy.Comment: 4 pages, Published in Astronomy and Astrophysics. Discussion slightly
expanded with respect to v1. Typos correcte
Characterizing Entanglement Sources
We discuss how to characterize entanglement sources with finite sets of
measurements. The measurements do not have to be tomographically complete, and
may consist of POVMs rather than von Neumann measurements. Our method yields a
probability that the source generates an entangled state as well as estimates
of any desired calculable entanglement measures, including their error bars. We
apply two criteria, namely Akaike's information criterion and the Bayesian
information criterion, to compare and assess different models (with different
numbers of parameters) describing entanglement-generating devices. We discuss
differences between standard entanglement-verificaton methods and our present
method of characterizing an entanglement source.Comment: This submission, together with the next one, supersedes
arXiv:0806.416
Spectroscopic Redshifts for Seven Lens Galaxies
We report VLT observations of 11 lensed quasars, designed to measure the
redshifts of their lens galaxies. We successfully determined the redshifts for
seven systems, five of which were previously unknown. The securely measured
redshifts for the lensing galaxies are: HE0047-1756 z=0.408; PMNJ0134-0931
z=0.766; HE0230-2130 z=0.522; HE0435-1223 z=0.455; SDSS0924+021 z=0.393;
LBQS1009-025 z=0.871; and WFIJ2033-472 z=0.658. For four additional systems
(BRI0952-0115, Q1017-207, Q1355-2257 and PMNJ1632-003) we estimate tentative
redshifts based on some features in their spectra.Comment: 8 pages, ApJ, submitte
Testing a new analytic model for gravitational lensing probabilities
We study gravitational lensing with a multiple lens plane approach, proposing
a simple analytical model for the probability distribution function (PDF) of
the dark matter convergence, kappa, for the different lens planes in a given
cosmology as a function of redshift and smoothing angle, theta. The model is
fixed solely by the variance of kappa, which in turn is fixed by the amplitude
of the power spectrum, sigma_8. We test the PDF against a high resolution
Tree-Particle-Mesh simulation and find that it is far superior to the Gaussian
or the lognormal, especially for small values of theta << 1 arcmin and at large
values of kappa relevant to strong lensing. With this model, we predict the
probabilities of strong lensing by a single plane or by multiple planes. We
find that for theta ~ 10 arcsec, a single plane accounts for almost all (~ 98%)
of the strong lensing cases for source redshift unity. However, for a more
typical source redshift of 4, about 12% of the strong lensing cases will result
from the contribution of a secondary clump of matter along the line of sight,
introducing a systematic error in the determination of the surface density of
clusters, typically overestimating it by about 2-5%. We also find that matter
inhomogenieties introduce a dispersion in the value of the angular diameter
distance about its cosmological mean. The probable error relative to the mean
increases with redshift to a value of about 8% for z ~ 6 and theta ~ 10 arcsec.Comment: Accepted for publication in ApJ, 13 pages, 12 figures, revised
version, references added, section 6 expande
Finding rare objects and building pure samples: Probabilistic quasar classification from low resolution Gaia spectra
We develop and demonstrate a probabilistic method for classifying rare
objects in surveys with the particular goal of building very pure samples. It
works by modifying the output probabilities from a classifier so as to
accommodate our expectation (priors) concerning the relative frequencies of
different classes of objects. We demonstrate our method using the Discrete
Source Classifier, a supervised classifier currently based on Support Vector
Machines, which we are developing in preparation for the Gaia data analysis.
DSC classifies objects using their very low resolution optical spectra. We look
in detail at the problem of quasar classification, because identification of a
pure quasar sample is necessary to define the Gaia astrometric reference frame.
By varying a posterior probability threshold in DSC we can trade off sample
completeness and contamination. We show, using our simulated data, that it is
possible to achieve a pure sample of quasars (upper limit on contamination of 1
in 40,000) with a completeness of 65% at magnitudes of G=18.5, and 50% at
G=20.0, even when quasars have a frequency of only 1 in every 2000 objects. The
star sample completeness is simultaneously 99% with a contamination of 0.7%.
Including parallax and proper motion in the classifier barely changes the
results. We further show that not accounting for class priors in the target
population leads to serious misclassifications and poor predictions for sample
completeness and contamination. (Truncated)Comment: MNRAS accepte
Hevin is down-regulated in many cancers and is a negative regulator of cell growth and proliferation
We have cloned a human Hevin cDNA from omental adipose tissue of different patients by reverse transcription polymerase chain reaction and shown a sequence variation due to a possible polymorphism at amino acid position 161 (E/G). Hevin protein expressed in vitro showed molecular weights of approximately 75 kDa and 150 kDa, suggesting that Hevin may form a homodimer in vitro. Using Northern blots and a human expressed sequence tAg database analysis, Hevin was shown to be widely expressed in human normal or non-neoplastic diseased tissues with various levels. In contrast to this, its expression was strongly down-regulated in most neoplastic cells or tissues tested. However, neither the mechanism nor the physiological meaning of this down-regulation is known. As an initial step towards investigating the functional role of Hevin in cell growth and differentiation, we transiently or stably expressed this gene in cancer cells (HeLa 3S) that are devoid of endogenous Hevin and measured DNA synthesis (cell proliferation) by 5-bromo-2′-deoxyuridine incorporation. Hevin was shown to be a negative regulator of cell proliferation. Furthermore, we have shown that Hevin can inhibit progression of cells from G1 to S phase or prolong G1 phase. This is the first report which describes the function of Hevin in cell growth and proliferation. Through database analysis, Hevin was found to be located on chromosome 4 which contains loss of heterozygosity of many tumour suppressor genes. Taken together, these results suggest that Hevin may be a candidate for a tumour suppressor gene and a potential target for cancer diagnosis/therapy. © 2000 Cancer Research Campaig
Curvature of the Universe and Observed Gravitational Lens Image Separations Versus Redshift
In a flat, k=0 cosmology with galaxies that approximate singular isothermal
spheres, gravitational lens image separations should be uncorrelated with
source redshift. But in an open k=-1 cosmology such gravitational lens image
separations become smaller with increasing source redshift. The observed
separations do become smaller with increasing source redshift but the effect is
even stronger than that expected in an Omega=0 cosmology. The observations are
thus not compatible with the "standard" gravitational lensing statistics model
in a flat universe. We try various open and flat cosmologies, galaxy mass
profiles, galaxy merging and evolution models, and lensing aided by clusters to
explain the correlation. We find the data is not compatible with any of these
possibilities within the 95% confidence limit, leaving us with a puzzle. If we
regard the observed result as a statistical fluke, it is worth noting that we
are about twice as likely to observe it in an open universe (with 0<Omega<0.4)
as we are to observe it in a flat one. Finally, the existence of an observed
multiple image lens system with a source at z=4.5 places a lower limit on the
deceleration parameter: q_0 > -2.0.Comment: 21 pages, 4 figures, AASTeX
Gravitational Lensing, Dark Matter and the Optical Gravitational Lens Experiment
After briefly reviewing the history of gravitational lensing, we recall the basic principles of the theory. We then describe and use a simple optical gravitational lens experiment which has the virtue of accounting for all types of image configurations observed so far among the presently known gravitational lens systems. Finally, we briefly present the 4m International Liquid Mirror Telescope project in the context of a photometric monitoring of multiply imaged quasars
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