421 research outputs found
Refining MOND interpolating function and TeVeS Lagrangian
The phenomena customly called Dark Matter or Modified Newtonian Dynamics
(MOND) have been argued by Bekenstein (2004) to be the consequences of a
covariant scalar field, controlled by a free function (related to the MOND
interpolating function) in its Lagrangian density. In the context of this
relativistic MOND theory (TeVeS), we examine critically the interpolating
function in the transition zone between weak and strong gravity. Bekenstein's
toy model produces too gradually varying functions and fits rotation curves
less well than the standard MOND interpolating function. However, the latter
varies too sharply and implies an implausible external field effect (EFE).
These constraints on opposite sides have not yet excluded TeVeS, but made the
zone of acceptable interpolating functions narrower. An acceptable "toy"
Lagrangian density function with simple analytical properties is singled out
for future studies of TeVeS in galaxies. We also suggest how to extend the
model to solar system dynamics and cosmology, and compare with strong lensing
data (see also astro-ph/0509590).Comment: accepted for publication in ApJ Letter
Cyclosporin A in skin samples from in vitro penetration studies may be assayed by a simple HPLC method
Neste estudo foi desenvolvido um método simples utilizando Cromatografia Líquida de Alta Eficiência (CLAE) com detecção no UV para quantificação de Ciclosporina A (CysA) em amostras de pele após estudos de penetração cutânea in vitro. O peptídeo foi extraído do estrato córneo e da epiderme sem estrato córneo + derme ([E+D]) através de agitação em vórtex e sonicação utilizando um solvente extrator (metanol). A recuperação da CysA de ambas as camadas da pele foi de 85%, conforme estimado por CLAE utilizando coluna RP-18, detecção em 210 nm e fase móvel composta de acetonitrila e água (67:33, v/v). O limite de quantificação do peptídeo utilizando este método cromatográfico foi de 150 ng/mL. O método mostrou-se linear na faixa de 0,15-500 mig/mL. A precisão e exatidão intra e inter-ensaio foram avaliadas utilizando três concentrações distintas (1, 10 e 20 mig/mL). Os valores de coeficiente de variação e o desvio do valor teórico foram inferiores a 5%. O método descrito pode ser utilizado para determinação da CysA após estudos de penetração cutânea in vitro utilizando pele de porco como modelo de membranaA simple High Performance Liquid Chromatographic method with UV detection was developed for quantification of Cyclosporin A (CysA) in skin samples after in vitro penetration studies. The peptide was recovered from two different layers of skin, the stratum corneum and the epidermis plus dermis ([E+D]), by vortex homogenization and bath sonication in an organic solvent (methanol). Recovery of CysA from skin was about 85%, and CysA was estimated by HPLC using a RP-18 column, UV detection at 210 nm and acetonitrile:water (67:33 v/v) as the mobile phase. The quantification limit was 150ng/mL. The assay was linear from 0.15-500 mg/muL. The within-day and between-day assay precision and accuracy were studied at three concentration levels (1, 10 and 20 mug/mL). The coefficients of variation and deviation from the theoretical values were lower than 5%. The method described has a potential application to in vitro penetration studies of CysA using porcine skin as a biological membrane model
The canonical 8-form on manifolds with holonomy group Spin(9)
An explicit expression of the canonical 8-form on a Riemannian manifold with
a Spin(9)-structure, in terms of the nine local symmetric involutions involved,
is given. The list of explicit expressions of all the canonical forms related
to Berger's list of holonomy groups is thus completed. Moreover, some results
on Spin(9)-structures as G-structures defined by a tensor and on the curvature
tensor of the Cayley planes, are obtained
First Results from the KMOS Lens-Amplified Spectroscopic Survey (KLASS): Kinematics of Lensed Galaxies at Cosmic Noon
We present the first results of the KMOS Lens-Amplified Spectroscopic Survey
(KLASS), a new ESO Very Large Telescope (VLT) large program, doing multi-object
integral field spectroscopy of galaxies gravitationally lensed behind seven
galaxy clusters selected from the HST Grism Lens-Amplified Survey from Space
(GLASS). Using the power of the cluster magnification we are able to reveal the
kinematic structure of 25 galaxies at , in four
cluster fields, with stellar masses . This sample includes 5 sources at with lower stellar masses
than in any previous kinematic IFU surveys. Our sample displays a diversity in
kinematic structure over this mass and redshift range. The majority of our
kinematically resolved sample is rotationally supported, but with a lower ratio
of rotational velocity to velocity dispersion than in the local universe,
indicating the fraction of dynamically hot disks changes with cosmic time. We
find no galaxies with stellar mass in our sample
display regular ordered rotation. Using the enhanced spatial resolution from
lensing, we resolve a lower number of dispersion dominated systems compared to
field surveys, competitive with findings from surveys using adaptive optics. We
find that the KMOS IFUs recover emission line flux from HST grism-selected
objects more faithfully than slit spectrographs. With artificial slits we
estimate slit spectrographs miss on average 60% of the total flux of emission
lines, which decreases rapidly if the emission line is spatially offset from
the continuum.Comment: Accepted for publication in Ap
A QUMOND galactic N-body code I: Poisson solver and rotation curve fitting
Here we present a new particle-mesh galactic N-body code that uses the full
multigrid algorithm for solving the modified Poisson equation of the Quasi
Linear formulation of Modified Newtonian Dynamics (QUMOND). A novel approach
for handling the boundary conditions using a refinement strategy is implemented
and the accuracy of the code is compared with analytical solutions of Kuzmin
disks. We then employ the code to compute the predicted rotation curves for a
sample of five spiral galaxies from the THINGS sample. We generated static
N-body realisations of the galaxies according to their stellar and gaseous
surface densities and allowed their distances, mass-to-light ratios (M/L) and
both the stellar and gas scale-heights to vary in order to estimate the best
fit parameters. We found that NGC 3621, NGC 3521 and DDO 154 are well fit by
MOND using expected values of the distance and M/L. NGC 2403 required a
moderately larger than expected and NGC 2903 required a substantially
larger value. The surprising result was that the scale-height of the dominant
baryonic component was well constrained by the rotation curves: the gas
scale-height for DDO 154 and the stellar scale-height for the others. In fact,
if the suggested stellar scale-height (one-fifth the stellar scale-length) was
used in the case of NGC 3621 and NGC 3521 it would not be possible to produce a
good fit to the inner rotation curve. For each of the four stellar dominated
galaxies, we calculated the vertical velocity dispersions which we found to be,
on the whole, quite typical compared with observed stellar vertical velocity
dispersions of face on spirals. We conclude that modelling the gas
scale-heights of the gas rich dwarf spiral galaxies will be vital in order to
make precise conclusions about MOND.Comment: 14 pages, 11 figures, MNRAS in pres
Can MOND take a bullet? Analytical comparisons of three versions of MOND beyond spherical symmetry
A proper test of Modified Newtonian Dynamics (MOND) in systems of non-trivial
geometries depends on modelling subtle differences in several versions of its
postulated theories. This is especially important for lensing and dynamics of
barely virialised galaxy clusters with typical gravity of scale . The original MOND formula, the classical single field
modification of the Poisson equation, and the multi-field general relativistic
theory of Bekenstein (TeVeS) all lead to different predictions as we stray from
spherical symmetry. In this paper, we study a class of analytical MONDian
models for a system with a semi-Hernquist baryonic profile. After presenting
the analytical distribution function of the baryons in spherical limits, we
develop orbits and gravitational lensing of the models in non-spherical
geometries. In particular, we can generate a multi-centred baryonic system with
a weak lensing signal resembling that of the merging galaxy cluster 1E 0657-56
with a bullet-like light distribution. We finally present analytical scale-free
highly non-spherical models to show the subtle differences between the single
field classical MOND theory and the multi-field TeVeS theory.Comment: 14 pages, 9 figures, accepted for publication in MNRA
Milky Way Mass Models and MOND
Using the Tuorla-Heidelberg model for the mass distribution of the Milky Way,
I determine the rotation curve predicted by MOND. The result is in good
agreement with the observed terminal velocities interior to the solar radius
and with estimates of the Galaxy's rotation curve exterior thereto. There are
no fit parameters: given the mass distribution, MOND provides a good match to
the rotation curve. The Tuorla-Heidelberg model does allow for a variety of
exponential scale lengths; MOND prefers short scale lengths in the range 2.0 to
2.5 kpc. The favored value of scale length depends somewhat on the choice of
interpolation function. There is some preference for the `simple' interpolation
function as found by Famaey & Binney. I introduce an interpolation function
that shares the advantages of the simple function on galaxy scales while having
a much smaller impact in the solar system. I also solve the inverse problem,
inferring the surface mass density distribution of the Milky Way from the
terminal velocities. The result is a Galaxy with `bumps and wiggles' in both
its luminosity profile and rotation curve that are reminiscent of those
frequently observed in external galaxies.Comment: Accepted for publication in the Astrophysical Journal. 31 pages
including 8 figures and 3 table
MOND and the Universal Rotation Curve: similar phenomenologies
The Modified Newtonian Dynamics (MOND) and the Universal Rotation Curve (URC)
are two ways to describe the general properties of rotation curves, with very
different approaches concerning dark matter and gravity. Phenomenological
similarities between the two approaches are studied by looking for properties
predicted in one framework that are also reproducible in the other one. First,
we looked for the analogous of the URC within the MOND framework. Modifying in
an observationally-based way the baryonic contribution Vbar to the rotation
curve predicted by the URC, and applying the MOND formulas to this Vbar, leads
to a "MOND URC" whose properties are remarkably similar to the URC. Second, it
is shown that the URC predicts a tight mass discrepancy - acceleration
relation, which is a natural outcome of MOND. With the choice of Vbar that
minimises the differences between the URC and the "MOND URC" the relation is
almost identical to the observational one. This similarity between the
observational properties of MOND and the URC has no implications about the
validity of MOND as a theory of gravity, but it shows that it can reproduce in
detail the phenomenology of disk galaxies' rotation curves, as described by the
URC. MOND and the URC, even though they are based on totally different
assumptions, are found to have very similar behaviours and to be able to
reproduce each other's properties fairly well, even with the simple assumptions
made on the luminosity dependence of the baryonic contribution to the rotation
curve.Comment: Accepted for publication in ApJ. 8 pages, 5 figure
Constraining Lyman-alpha spatial offsets at from VANDELS slit spectroscopy
We constrain the distribution of spatially offset Lyman-alpha emission
(Ly) relative to rest-frame ultraviolet emission in high
redshift () Lyman-break galaxies (LBGs) exhibiting Ly emission
from VANDELS, a VLT/VIMOS slit-spectroscopic survey of the CANDELS Ultra Deep
Survey and Chandra Deep Field South fields (
total). Because slit spectroscopy compresses two-dimensional spatial
information into one spatial dimension, we use Bayesian inference to recover
the underlying Ly spatial offset distribution. We model the
distribution using a 2D circular Gaussian, defined by a single parameter
, the standard deviation expressed in polar
coordinates. Over the entire redshift range of our sample (), we find
kpc ( conf.),
corresponding to arcsec at . We also find that
decreases significantly with redshift. Because
Ly spatial offsets can cause slit-losses, the decrease in
with redshift can partially explain the increase
in the fraction of Ly emitters observed in the literature over this
same interval, although uncertainties are still too large to reach a strong
conclusion. If continues to decrease into the
reionization epoch, then the decrease in Ly transmission from galaxies
observed during this epoch might require an even higher neutral hydrogen
fraction than what is currently inferred. Conversely, if spatial offsets
increase with the increasing opacity of the IGM, slit losses may explain some
of the drop in Ly transmission observed at . Spatially resolved
observations of Ly and UV continuum at are needed to settle the
issue.Comment: Submitted to MNRA
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