159 research outputs found
Ultrastrong Magnon-Photon Coupling Achieved by Magnetic Films in Contact with Superconducting Resonators
Coherent coupling between spin wave excitations (magnons) and microwave
photons in a cavity may disclose new paths to unconventional phenomena as well
as for novel applications. Here, we present a systematic investigation on YIG
(Yttrium Iron Garnet) films on top of coplanar waveguide resonators made of
superconducting YBCO. We first show that spin wave excitations with frequency
higher than the Kittel mode can be excited by putting in direct contact a
5~m thick YIG film with the YBCO coplanar resonator (cavity frequency
~GHz). With this configuration, we obtain very large
values of the collective coupling strength ~GHz and
cooperativity . Transmission spectra are analyzed by a
modified Hopfield model for which we provide an exact solution that allows us
to well reproduce spectra by introducing a limited number of free parameters.
It turns out that the coupling of the dominant magnon mode with photons exceeds
0.2 times the cavity frequency, thus demonstrating the achievement of the
ultrastrong coupling regime with this architecture. Our analysis also shows a
vanishing contribution of the diamagnetic term which is a peculiarity of pure
spin systems
Mapping Susceptibility to Debris Flows Triggered by Tropical Storms: A Case Study of the San Vicente Volcano Area (El Salvador, CA)
In this study, an inventory of storm-triggered debris flows performed in the area of the San Vicente volcano (El Salvador, CA) was used to calibrate predictive models and prepare a landslide susceptibility map. The storm event struck the area in November 2009 as the result of the simultaneous action of low-pressure system 96E and Hurricane Ida. Multivariate Adaptive Regression Splines (MARS) was employed to model the relationships between a set of environmental variables and the locations of the debris flows. Validation of the models was performed by splitting 100 random samples of event and non-event 10 m pixels into training and test subsets. The validation results revealed an excellent (area under the receiver operating characteristic (ROC) curve (AUC) = 0.80) and stable (AUC std. dev. = 0.01) ability of MARS to predict the locations of the debris flows which occurred in the study area. However, when using the Youden’s index as probability threshold to discriminate between pixels predicted as positives and negatives, MARS exhibits a moderate ability to identify stable cells (specificity = 0.66). The final debris flow susceptibility map, which was prepared by averaging for each pixel the score of the 100 MARS repetitions, shows where future debris flows are more likely to occur, and thus may help in mitigating the risk associated with these landslides
Systematic search for lensed X-ray sources in the CLASH fields
We search for unresolved X-ray emission from lensed sources in the FOV of 11
CLASH clusters with Chandra data. We consider the solid angle in the lens plane
corresponding to a magnification , that amounts to a total of ~100
arcmin. Our main goal is to assess the efficiency of massive clusters as
cosmic telescopes to explore the faint end of X-ray extragalactic source
population. We search for X-ray emission from strongly lensed sources
identified in the optical, and perform an untargeted detection of lensed X-ray
sources. We detect X-ray emission only in 9 out of 849 lensed/background
optical sources. The stacked emission of the sources without detection does not
reveal any signal in any band. Based on the untargeted detection, we find 66
additional X-ray sources that are consistent with being lensed sources. After
accounting for completeness and sky coverage, we measure for the first time the
soft- and hard-band number counts of lensed X-ray sources. The results are
consistent with current modelization of the AGN population distribution. The
distribution of de-lensed fluxes of the sources identified in moderately deep
CLASH fields reaches a flux limit of ~ and ~ erg/s/cm
in the soft and hard bands, respectively. We conclude that, in order to match
the depth of the CDFS exploiting massive clusters as cosmic telescopes, the
required number of cluster fields is about two orders of magnitude larger than
that offered by the 20 years Chandra archive. A significant step forward will
be made when future X-ray facilities, with ~1' angular resolution and large
effective area, will allow the serendipitous discovery of rare, strongly lensed
high- X-ray sources, enabling the study of faint AGN activity in early
Universe and the measurement of gravitational time delays in the X-ray
variability of multiply imaged AGN.Comment: Accepted for publication in A&
Exploring the low-mass regime of galaxy-scale strong lensing: Insights into the mass structure of cluster galaxies
We aim at a direct measurement of the compactness of three galaxy-scale
lenses in massive clusters, testing the accuracy of the scaling laws that
describe the members in strong lensing (SL) models of galaxy clusters. We
selected the multiply imaged sources MACS J0416.12403 ID14 (), MACS
J0416.12403 ID16 (), and MACS J1206.20847 ID14 ().
Eight images were observed for the first SL system, and six for the latter two.
We focused on the main deflector of each galaxy-scale SL system (identified as
members 8971, 8785, and 3910, respectively), and modelled its total mass
distribution with a truncated isothermal sphere. We accounted for the lensing
effects of the remaining cluster components, and included the uncertainty on
the cluster-scale mass distribution through a bootstrapping procedure. We
measured a truncation radius value of ,
, and
for members 8971, 8785, and 3910, respectively. Alternative non-truncated
models with a higher number of free parameters do not lead to an improved
description of the SL system. We measured the stellar-to-total mass fraction
within the effective radius for the three members, finding ,
, and , respectively. We find that a parameterisation
of the properties of cluster galaxies in SL models based on power-law scaling
relations with respect to the total luminosity cannot accurately describe their
compactness over their full total mass range. Our results agree with modelling
of the cluster members based on the Fundamental Plane relation. Finally, we
report good agreement between our values of the stellar-to-total mass fraction
within and those of early-type galaxies from the SLACS Survey. Our work
significantly extends the regime of the current samples of lens galaxies.Comment: Astronomy & Astrophysics, 679, A124 (2023), 15 pages, 12 figures, 8
table
The Grism Lens-Amplified Survey from Space (GLASS) X. Sub-kpc resolution gas-phase metallicity maps at cosmic noon behind the Hubble Frontier Fields cluster MACS1149.6+2223
(Abridged) We combine deep HST grism spectroscopy with a new Bayesian method
to derive maps of gas-phase metallicity, nebular dust extinction, and
star-formation rate for 10 star-forming galaxies at high redshift
(). Exploiting lensing magnification by the foreground cluster
MACS1149.6+2223, we reach sub-kpc spatial resolution and push the stellar mass
limit associated with such high-z spatially resolved measurements below
for the first time. Our maps exhibit diverse morphologies,
indicative of various effects such as efficient radial mixing from tidal
torques, rapid accretion of low-metallicity gas, etc., which can affect the gas
and metallicity distributions in individual galaxies. Based upon an exhaustive
sample of all existing sub-kpc metallicity gradients at high-z, we find that
predictions given by analytical chemical evolution models assuming a relatively
extended star-formation profile in the early disk formation phase can explain
the majority of observed gradients, without involving galactic feedback or
radial outflows. We observe a tentative correlation between stellar mass and
metallicity gradient, consistent with the downsizing galaxy formation picture
that more massive galaxies are more evolved into a later phase of disk growth,
where they experience more coherent mass assembly at all radii and thus show
shallower metallicity gradients. In addition, we compile a sample of
homogeneously cross-calibrated integrated metallicity measurements spanning
three orders of magnitude in stellar mass at . We use this sample to
study the mass-metallicity relation (MZR) and test the fundamental metallicity
relation (FMR). The slope of the observed MZR can rule out the momentum-driven
wind model at 3- confidence level. We find no significant offset with
respect to the FMR, taking into account the intrinsic scatter and measurement
uncertainties.Comment: 26 pages, 14 figures, and 6 table
CLASH: Weak-Lensing Shear-and-Magnification Analysis of 20 Galaxy Clusters
We present a joint shear-and-magnification weak-lensing analysis of a sample
of 16 X-ray-regular and 4 high-magnification galaxy clusters at 0.19<z<0.69
selected from the Cluster Lensing And Supernova survey with Hubble (CLASH). Our
analysis uses wide-field multi-color imaging, taken primarily with Suprime-Cam
on the Subaru Telescope. From a stacked shear-only analysis of the
X-ray-selected subsample, we detect the ensemble-averaged lensing signal with a
total signal-to-noise ratio of ~25 in the radial range of 200 to 3500kpc/h. The
stacked tangential-shear signal is well described by a family of standard
density profiles predicted for dark-matter-dominated halos in gravitational
equilibrium, namely the Navarro-Frenk-White (NFW), truncated variants of NFW,
and Einasto models. For the NFW model, we measure a mean concentration of
at . We show this is in excellent agreement with Lambda
cold-dark-matter (LCDM) predictions when the CLASH X-ray selection function and
projection effects are taken into account. The best-fit Einasto shape parameter
is , which is consistent with the
NFW-equivalent Einasto parameter of . We reconstruct projected mass
density profiles of all CLASH clusters from a joint likelihood analysis of
shear-and-magnification data, and measure cluster masses at several
characteristic radii. We also derive an ensemble-averaged total projected mass
profile of the X-ray-selected subsample by stacking their individual mass
profiles. The stacked total mass profile, constrained by the
shear+magnification data, is shown to be consistent with our shear-based
halo-model predictions including the effects of surrounding large-scale
structure as a two-halo term, establishing further consistency in the context
of the LCDM model.Comment: Accepted by ApJ on 11 August 2014. Textual changes to improve clarity
(e.g., Sec.3.2.2 "Number-count Depletion", Sec.4.3 "Shape Measurement",
Sec.4.4 "Background Galaxy Selection"). Results and conclusions remain
unchanged. For the public release of Subaru data, see
http://archive.stsci.edu/prepds/clash
Hubble Space Telescope Combined Strong and Weak Lensing Analysis of the CLASH Sample: Mass and Magnification Models and Systematic Uncertainties
We present results from a comprehensive lensing analysis in HST data, of the
complete CLASH cluster sample. We identify new multiple-images previously
undiscovered allowing improved or first constraints on the cluster inner mass
distributions and profiles. We combine these strong-lensing constraints with
weak-lensing shape measurements within the HST FOV to jointly constrain the
mass distributions. The analysis is performed in two different common
parameterizations (one adopts light-traces-mass for both galaxies and dark
matter while the other adopts an analytical, elliptical NFW form for the dark
matter), to provide a better assessment of the underlying systematics - which
is most important for deep, cluster-lensing surveys, especially when studying
magnified high-redshift objects. We find that the typical (median), relative
systematic differences throughout the central FOV are in the
(dimensionless) mass density, , and in the magnification,
. We show maps of these differences for each cluster, as well as the mass
distributions, critical curves, and 2D integrated mass profiles. For the
Einstein radii () we find that all typically agree within
between the two models, and Einstein masses agree, typically, within
. At larger radii, the total projected, 2D integrated mass profiles
of the two models, within r\sim2\arcmin, differ by . Stacking the
surface-density profiles of the sample from the two methods together, we obtain
an average slope of , in the radial
range [5,350] kpc. Lastly, we also characterize the behavior of the average
magnification, surface density, and shear differences between the two models,
as a function of both the radius from the center, and the best-fit values of
these quantities.Comment: 35 pages (20 main text pages, plus 15 pages for additional figures
and tables); 2 Tables, 17 Figures. V3: accepted version; some minor
corrections and additions made. V4: corrected several entries in Table 2. All
mass models and magnification maps are made publicly available for the
communit
Dermatome mapping test in the analysis of anatomo-clinical correlations after inguinal hernia repair
Abstract
Background: Nerve identification is recommended in inguinal hernia repair to reduce or avoid postoperative pain.
The aim of this prospective observational study was to identify nerve prevalence and find a correlation between neuroanatomy
and chronic neuropathic postoperative inguinal pain (CPIP) after 6 months.
Material: A total of 115 patients, who underwent inguinal hernia mesh repair (Lichtenstein tension-free mesh
repair) between July 2018 and January 2019, were included in this prospective observational study. The mean age
and BMI respectively resulted 64 years and 25.8 with minimal inverse distribution of BMI with respect to age. Most
of the hernias were direct (59.1%) and of medium dimension (47.8%). Furthermore, these patients were undergoing
Dermatome Mapping Test in preoperatively and postoperatively 6 months evaluation.
Results: Identification rates of the iliohypogastric (IH), ilioinguinal (II) and genitofemoral (GF) nerves were 72.2%,
82.6% and 48.7% respectively. In the analysis of nerve prevalence according to BMI, the IH was statistically significant
higher in patients with BMI < 25 than BMI ≥ 25 P (< 0.05). After inguinal hernia mesh repair, 8 patients (6.9%) had
chronic postoperative neuropathic inguinal pain after 6 months. The CPIP prevailed at II/GF dermatome. The relation
between the identification/neurectomy of the II nerve and chronic postoperative inguinal pain after 6 months was
not significant (P = 0.542).
Conclusion: The anatomy of inguinal nerve is very heterogeneous and for this reason an accurate knowledge of
these variations is needed during the open mesh repair of inguinal hernias. The new results of our analysis is the statistically
significant higher IH nerve prevalence in patients with BMI < 25; probably the identification of inguinal nerve
is more complex in obese patients. In the chronic postoperative inguinal pain, the II nerve may have a predominant
role in determining postoperative long-term symptoms. Dermatome Mapping Test in an easy and safe method for
preoperative and postoperative 6 months evaluation of groin pain. The most important evidence of our analysis is
that the prevalence of chronic pain is higher when the nerves were not identified.
Keywords: Inguinal hernia, Inguinal nerves, Nerve identification, Pain, Follow-up
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The Contribution of Halos with Different Mass Ratios to the Overall Growth of Cluster-Sized Halos
We provide a new observational test for a key prediction of the \Lambda CDM
cosmological model: the contributions of mergers with different
halo-to-main-cluster mass ratios to cluster-sized halo growth. We perform this
test by dynamically analyzing seven galaxy clusters, spanning the redshift
range and caustic mass range M, with an average of 293 spectroscopically-confirmed
bound galaxies to each cluster. The large radial coverage (a few virial radii),
which covers the whole infall region, with a high number of spectroscopically
identified galaxies enables this new study. For each cluster, we identify bound
galaxies. Out of these galaxies, we identify infalling and accreted halos and
estimate their masses and their dynamical states. Using the estimated masses,
we derive the contribution of different mass ratios to cluster-sized halo
growth. For mass ratios between ~0.2 and ~0.7, we find a ~1 agreement
with \Lambda CDM expectations based on the Millennium simulations I and II. At
low mass ratios, , our derived contribution is underestimated
since the detection efficiency decreases at low masses,
M. At large mass ratios, , we do not
detect halos probably because our sample, which was chosen to be quite X-ray
relaxed, is biased against large mass ratios. Therefore, at large mass ratios,
the derived contribution is also underestimated.Comment: 25 pages, 16 figures, 6 tables, 2 machine readable tables, accepted
for publication in ApJ, updated acknowledgements and data table format
modifications mad
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