56 research outputs found
Necrosis avascular secundaria al tratamiento de la luxación congénita de cadera: relación entre factores terapéuticos y secuelas radiológicas
Se presentan 108 casos de Luxación Congénita de Cadera (LCC) unilateral tratados
con la misma metódica terapéutica: tracción más reducción abierta o cerrada dependiendo
de los hallazgos artrográficos. Tras un seguimiento medio de 7 años (Rango: 5-13),
5 (5%) tenían una coxa magna, 14 (13%) mostraban disminución de la altura epifisaria, 22
(20%) tenían una coxa magna con disminución de la altura epifisaria 10 (9%) presentaban
lesión fisaria residual. El análisis estadístico demostró asociación significativa (p<0,05 ) entre
el desarrollo de coxa magna con disminución de la altura epifisaria y la ausencia de descenso
cefálico al terminar la tracción, así como con la reducción abierta. La lesión fisaria residual,
se encontró asociada significativamente a LCC Tipo IV de Tönnis, caderas que estuvieron más
de 5 semanas en tracción, fallo en el descenso cefálico al finalizar la tracción y reducción abierta.
En conclusión, se recomienda la tracción preoperatoria «efectiva», que desciende la cabeza
femoral a nivel del cotilo, para disminuir las alteraciones radiológicas finales, secuelas de necrosis
avascular.A total of 108 patients with unilateral congenital dislocation of the hip treated
by the same therapeutic approach, are reviewed. The protocol for treatment consisted in traction
and open or closed reduction, depending of the arthrographic findings. After 7-year follow-up
(range, 5-13), 5 (5%) had coxa magna, 14 (13%) showed a decrease in epiphyseal height, 22
(20%) exhibited both coxa magna and decreased epiphyseal height, and 10 (9%) showed physeal
damage. The statistical analysis revealed a significant relationship (p < 0,05) between the development
of coxa magna with decreased epiphyseal height and both an absence of femoral head
descent after traction and an open reduction of the hip. Physeal damage was found to be associated
to Tönnis type-IV congenital dislocation, to hips undergoing more than 5 weeks traction, to
failed cephalic descent following traction and an open reduction procedure. In conclusion, a
effective preoperative hip traction allowing an appropriate descent of the femoral head to the
acetabulum is recommended in order to prevent radiological alterations induced by avascular
necrosis
The search for galaxy cluster members with deep learning of panchromatic HST imaging and extensive spectroscopy
Context. The next generation of extensive and data-intensive surveys are bound to produce a vast amount of data, which can be efficiently dealt with using machine-learning and deep-learning methods to explore possible correlations within the multi-dimensional parameter space. Aims. We explore the classification capabilities of convolution neural networks (CNNs) to identify galaxy cluster members (CLMs) by using Hubble Space Telescope (HST) images of fifteen galaxy clusters at redshift 0.19≲ z≲ 0.60, observed as part of the CLASH and Hubble Frontier Field programmes. Methods. We used extensive spectroscopic information, based on the CLASH-VLT VIMOS programme combined with MUSE observations, to define the knowledge base. We performed various tests to quantify how well CNNs can identify cluster members on ht basis of imaging information only. Furthermore, we investigated the CNN capability to predict source memberships outside the training coverage, in particular, by identifying CLMs at the faint end of the magnitude distributions. Results. We find that the CNNs achieve a purity-completeness rate ≳ 90%, demonstrating stable behaviour across the luminosity and colour of cluster galaxies, along with a remarkable generalisation capability with respect to cluster redshifts. We concluded that if extensive spectroscopic information is available as a training base, the proposed approach is a valid alternative to catalogue-based methods because it has the advantage of avoiding photometric measurements, which are particularly challenging and time-consuming in crowded cluster cores. As a byproduct, we identified 372 photometric cluster members, with mag(F814) < 25, to complete the sample of 812 spectroscopic members in four galaxy clusters RX J2248-4431, MACS J0416-2403, MACS J1206-0847 and MACS J1149+2223. Conclusions. When this technique is applied to the data that are expected to become available from forthcoming surveys, it will be an efficient tool for a variety of studies requiring CLM selection, such as galaxy number densities, luminosity functions, and lensing mass reconstruction
Candidate Cluster Members with Deep learning
The next generation of extensive and data-intensive surveys are bound to produce a vast amount of data, which can be efficiently dealt with using machine-learning and deep-learning methods to explore possible correlations within the multi-dimensional parameter space. We explore the classification capabilities of convolution neural networks (CNNs) to identify galaxy cluster members (CLMs) by using Hubble Space Telescope (HST) images of fifteen galaxy clusters at redshift 0.19≲z≲0.60, observed as part of the CLASH and Hubble Frontier Field programmes. We used extensive spectroscopic information, based on the CLASH-VLT VIMOS programme combined with MUSE observations, to define the knowledge base. We performed various tests to quantify how well CNNs can identify cluster members on ht basis of imaging information only. Furthermore, we investigated the CNN capability to predict source memberships outside the training coverage, in particular, by identifying CLMs at the faint end of the magnitude distributions. We find that the CNNs achieve a purity-completeness rate ≳90%, demonstrating stable behaviour across the luminosity and colour of cluster galaxies, along with a remarkable generalisation capability with respect to cluster redshifts. We concluded that if extensive spectroscopic information is available as a training base, the proposed approach is a valid alternative to catalogue-based methods because it has the advantage of avoiding photometric measurements, which are particularly challenging and time-consuming in crowded cluster cores. As a byproduct, we identified 372 photometric cluster members, with mag(F814)<25, to complete the sample of 812 spectroscopic members in four galaxy clusters RX J2248-4431, MACS J0416-2403, MACS J1206-0847 and MACS J1149+2223. When this technique is applied to the data that are expected to become available from forthcoming surveys, it will be an efficient tool for a variety of studies requiring CLM selection, such as galaxy number densities, luminosity functions, and lensing mass reconstruction
New high-precision strong lensing modeling of Abell 2744. Preparing for JWST observations
We present a new strong lensing (SL) model of the Hubble Frontier Fields
galaxy cluster Abell 2744, at z=0.3072, by exploiting archival Hubble Space
Telescope (HST) multi-band imaging and Multi Unit Spectroscopic Explorer (MUSE)
follow-up spectroscopy. The lens model considers 90 spectroscopically confirmed
multiple images (from 30 background sources), which represents the largest
secure sample for this cluster field prior to the recently acquired James Webb
Space Telescope observations. The inclusion of the sub-structures within
several extended sources as model constraints allows us to accurately
characterize the inner total mass distribution of the cluster and the position
of the cluster critical lines. We include the lensing contribution of 225
cluster members, 202 of which are spectroscopically confirmed. We also measure
the internal velocity dispersion of 85 cluster galaxies to independently
estimate the role of the subhalo mass component in the lens model. We
investigate the effect of the cluster environment on the total mass
reconstruction of the cluster core with two different mass parameterizations.
We consider the mass contribution from three external clumps, either based on
previous weak-lensing studies, or extended HST imaging of luminous members
around the cluster core. In the latter case, the observed positions of the
multiple images are better reproduced, with a remarkable accuracy of 0.37", a
factor of smaller than previous lens models. We develop and make
publicly available a Strong Lensing Online Tool (SLOT) to exploit the
predictive power and the full statistical information of this and future
models, through a simple graphical interface. We plan to apply our
high-precision SL model to the first analysis of the GLASS-JWST-ERS program,
specifically to measure the intrinsic physical properties of high- galaxies
from robust magnification maps.Comment: 14 pages, 9 figures, 4 table
Searching for galaxy-scale strong-lenses in galaxy clusters with deep networks -- I: methodology and network performance
Galaxy-scale strong lenses in galaxy clusters provide a unique tool to
investigate their inner mass distribution and the sub-halo density profiles in
the low-mass regime, which can be compared with the predictions from
cosmological simulations. We search for galaxy-galaxy strong-lensing systems in
HST multi-band imaging of galaxy cluster cores from the CLASH and HFF programs
by exploring the classification capabilities of deep learning techniques.
Convolutional neural networks are trained utilising highly-realistic
simulations of galaxy-scale strong lenses injected into the HST cluster fields
around cluster members. To this aim, we take advantage of extensive
spectroscopic information on member galaxies in 16 clusters and the accurate
knowledge of the deflection fields in half of these from high-precision strong
lensing models. Using observationally-based distributions, we sample
magnitudes, redshifts and sizes of the background galaxy population. By placing
these sources within the secondary caustics associated with cluster galaxies,
we build a sample of ~3000 galaxy-galaxy strong lenses which preserve the full
complexity of real multi-colour data and produce a wide diversity of strong
lensing configurations. We study two deep learning networks processing a large
sample of image cutouts in three HST/ACS bands, and we quantify their
classification performance using several standard metrics. We find that both
networks achieve a very good trade-off between purity and completeness
(85%-95%), as well as good stability with fluctuations within 2%-4%. We
characterise the limited number of false negatives and false positives in terms
of the physical properties of the background sources and cluster members. We
also demonstrate the neural networks' high degree of generalisation by applying
our method to HST observations of 12 clusters with previously known
galaxy-scale lensing systems.Comment: 17 pages, 13 figures, to be published on A&
The Kormendy relation of early-type galaxies as a function of wavelength in Abell S1063, MACS J0416.1-2403 and MACS J1149.5+2223
The wavelength dependence of the Kormendy relation (KR) is well characterised
at low-redshift, but poorly studied at intermediate redshifts. The KR provides
information on the evolution of the population of early-type galaxies (ETGs),
therefore, by studying it, we may shed light on the assembly processes of these
objects and their size evolution. Since studies at different redshifts are
generally conducted in different rest-frame wavebands, investigating whether
there is a wavelength dependence of the KR is fundamental to interpret the
conclusions we might draw from it. We analyse the KRs of the three Hubble
Frontier Fields clusters, Abell S1063 (z = 0.348), MACS J0416.1-2403 (z =
0.396), and MACS J1149.5+2223 (z = 0.542), as a function of wavelength. This is
the first time the KR of ETGs has been explored consistently in such a large
range of wavelength at intermediate redshifts. We exploit very deep HST
photometry, ranging from the observed B-band to the H-band, and VLT/MUSE
integral field spectroscopy. We improve the structural parameters estimation we
performed in a previous work (Tortorelli et al. 2018) by means of a newly
developed Python package called morphofit (Tortorelli&Mercurio 2023). With its
use on cluster ETGs, we find that the KR slopes smoothly increase with
wavelength from the optical to the near-infrared bands in all three clusters,
with the intercepts getting fainter at lower redshifts due to the passivisation
of the ETGs population. The slope trend is consistent with previous findings at
lower redshifts. The slope increase with wavelength implies that smaller size
ETGs are more centrally concentrated than larger size ETGs in the near-infrared
with respect to the optical regime. Since different bands probe different
stellar populations in galaxies, the slope increase also implies that smaller
ETGs have stronger internal gradients with respect to larger ETGs.Comment: Submitted to Astronomy and Astrophysics in the form of letter to the
Editor, 5 pages, 1 figure, 1 tabl
Euclid Preparation TBD. Characterization of convolutional neural networks for the identification of galaxy-galaxy strong lensing events
Forthcoming imaging surveys will increase the number of known galaxy-scale strong lenses by several orders of magnitude. For this to happen, images of billions of galaxies will have to be inspected to identify potential candidates. In this context, deep-learning techniques are particularly suitable for finding patterns in large data sets, and convolutional neural networks (CNNs) in particular can efficiently process large volumes of images. We assess and compare the performance of three network architectures in the classification of strong-lensing systems on the basis of their morphological characteristics. In particular, we implemented a classical CNN architecture, an inception network, and a residual network. We trained and tested our networks on different subsamples of a data set of 40 000 mock images whose characteristics were similar to those expected in the wide survey planned with the ESA mission Euclid, gradually including larger fractions of faint lenses. We also evaluated the importance of adding information about the color difference between the lens and source galaxies by repeating the same training on single- and multiband images. Our models find samples of clear lenses with ≳90% precision and completeness. Nevertheless, when lenses with fainter arcs are included in the training set, the performance of the three models deteriorates with accuracy values of ~0.87 to ~0.75, depending on the model. Specifically, the classical CNN and the inception network perform similarly in most of our tests, while the residual network generally produces worse results. Our analysis focuses on the application of CNNs to high-resolution space-like images, such as those that the Euclid telescope will deliver. Moreover, we investigated the optimal training strategy for this specific survey to fully exploit the scientific potential of the upcoming observations. We suggest that training the networks separately on lenses with different morphology might be needed to identify the faint arcs. We also tested the relevance of the color information for the detection of these systems, and we find that it does not yield a significant improvement. The accuracy ranges from ~0.89 to ~0.78 for the different models. The reason might be that the resolution of the Euclid telescope in the infrared bands is lower than that of the images in the visual band
CLASH-VLT: Abell S1063: Cluster assembly history and spectroscopic catalogue
Context. The processes responsible for galaxy evolution in different environments as a function of galaxy mass remain heavily debated. Rich galaxy clusters are ideal laboratories in which to distinguish the role of environmental versus mass quenching because they consist of a full range of galaxies and environments. Aims. Using the CLASH-VLT survey, we assembled an unprecedentedly large sample of 1234 spectroscopically confirmed members in Abell S1063. We found a dynamically complex structure at «zcl»= 0.3457 with a velocity dispersion σv = 1380-32+26 km s-1. We investigated cluster environmental and dynamical effects by analysing the projected phase-space diagram and the orbits as a function of galaxy spectral properties. Methods. We classified cluster galaxies according to the presence and strength of the [OII] emission line, the strength of the Hδ absorption line, and colours. We investigated the relation between the spectral classes of galaxies and their position in the projected phase-space diagram. We separately analysed red and blue galaxy orbits. By correlating the observed positions and velocities with the projected phase-space constructed from simulations, we constrained the accretion redshift of galaxies with different spectral types. Results. Passive galaxies are mainly located in the virialised region, while emission-line galaxies lie beyond r200 and are accreted into the cluster at a later time. Emission-line and post-starburst galaxies show an asymmetric distribution in projected phase-space within r200; emission-line galaxies are prominent at Δv/σ ≲ -1.5 and post-starburst galaxies at Δv/σ ≲ 1.5, suggesting that backsplash galaxies lie at high positive velocities. We find that low-mass passive galaxies are accreted into the cluster before high-mass galaxies. This suggests that we observe as passives only the low-mass galaxies that are accreted early into the cluster as blue galaxies. They had the time to quench their star formation. We also find that red galaxies move on more radial orbits than blue galaxies. This can be explained if infalling galaxies can remain blue by moving on tangential orbits
Euclid Preparation TBD. Characterization of convolutional neural networks for the identification of galaxy-galaxy strong lensing events
Forthcoming imaging surveys will potentially increase the number of known
galaxy-scale strong lenses by several orders of magnitude. For this to happen,
images of tens of millions of galaxies will have to be inspected to identify
potential candidates. In this context, deep learning techniques are
particularly suitable for the finding patterns in large data sets, and
convolutional neural networks (CNNs) in particular can efficiently process
large volumes of images. We assess and compare the performance of three network
architectures in the classification of strong lensing systems on the basis of
their morphological characteristics. We train and test our models on different
subsamples of a data set of forty thousand mock images, having characteristics
similar to those expected in the wide survey planned with the ESA mission
\Euclid, gradually including larger fractions of faint lenses. We also evaluate
the importance of adding information about the colour difference between the
lens and source galaxies by repeating the same training on single-band and
multi-band images. Our models find samples of clear lenses with
precision and completeness, without significant differences in the performance
of the three architectures. Nevertheless, when including lenses with fainter
arcs in the training set, the three models' performance deteriorates with
accuracy values of to depending on the model. Our
analysis confirms the potential of the application of CNNs to the
identification of galaxy-scale strong lenses. We suggest that specific training
with separate classes of lenses might be needed for detecting the faint lenses
since the addition of the colour information does not yield a significant
improvement in the current analysis, with the accuracy ranging from
to for the different models
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