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Contains fulltext : 306496.pdf (Publisher’s version ) (Open Access), Background: Offspring of parents with alcohol use disorder (AUD) are more susceptible to developing AUD, with an estimated heritability of around 50%. Vulnerability to AUD in first-degree relatives is influenced by biological factors, such as spontaneous brain activity, and high-risk psychosocial characteristics. However, existing resting-state EEG studies in AUD offspring have shown inconsistent findings regarding theta, alpha, and beta band frequencies. Additionally, research consistently demonstrates an increased risk of internalizing and externalizing disorders, self-regulation difficulties, and interpersonal issues among AUD offspring. Methods: This study aimed to investigate the absolute power of theta, alpha, and beta frequencies in young adult offspring with a family history of AUD compared to individuals without family history. The psychosocial profiles of the offspring were also examined in relation to individuals without a family history of AUD. Furthermore, the study sought to explore the potential association between differences in frequency bands and psychosocial variables. Resting-state EEG recordings were obtained from 31 young adult healthy offspring of alcohol-dependent individuals and 43 participants with no family history of AUD (age range: 16-25 years). Participants also completed self-report questionnaires assessing anxiety and depressive symptoms, impulsivity, emotion regulation, and social involvement. Results: The results revealed no significant differences in spontaneous brain activity between the offspring and participants without a family history of AUD. However, in terms of psychosocial factors, the offspring exhibited significantly lower social involvement than the control group. Conclusions: This study does not provide evidence suggesting vulnerability in offspring based on differences in spontaneous brain activity. Moreover, this investigation highlights the importance of interventions aimed at enhancing social connections in offsprin, 10 p.

We present a 3D mapping of the Wolf-Rayet (WR) nebula M1-67 around WR124. We obtained high-resolution San Pedro M\'{a}rtir (SPM) Manchester Echelle Spectrograph (MES) observations along 17 long-slit positions covering all morphological features in M1-67. We are able to unveil the true morphology of M1-67 and its kinematics by interpreting the SPM MES observations by means of the 3D modelling tool for Astrophysics SHAPE. Our SHAPE model that best reproduces the SPM MES data includes three concentric bipolar structures composed by a hollow ellipsoidal structure and a torus. In addition, the model requires the presence of expanding jets and broken blisters in order to reproduce specific spectral features. Our results are consistent with the idea that M1-67 and its progenitor star WR124 have formed through a common envelope scenario that occurred 11.8$^{+4.6}_{-0.8}$ kyr ago. Our bipolar model strongly questions previous suggestions of the presence of a bow shock structure surrounding M1-67. We interpret that the bright structures detected in the spectra extracted from the central regions are produced by wind compression at the receding region of the innermost structure in M1-67. Furthermore, WR124 is moving through a low-density region above the Galactic plane that has negligibly affected the formation history of M1-67., Comment: 9 pages, 7 figures, 2 tables; Accepted to MNRAS

Born-again planetary nebulae (PNe) are extremely rare cases in the evolution of solar-like stars. It is commonly accepted that their central stars (CSPN) experienced a very late thermal pulse (VLTP), ejecting H-deficient material inside the evolved H-rich PN. Given the short duration of this event and the fast subsequent evolution of the CSPN, details of the mass ejection are unknown. We present the first morpho-kinematic model of the H-deficient material surrounding a born-again PN, namely A30. New San Pedro M\'{a}rtir observations with the Manchester Echelle Spectrograph were recently obtained to map its inner regions of A30 which are interpreted by means of the software SHAPE in conjunction with HST WFC3 images. The SHAPE morpho-kinematic model that best reproduces the observations is composed by a disrupted disk tilted 37$^\circ$ with respect to the line of sight and a pair of orthogonal opposite bipolar ejections. We confirm previous suggestions that the structures closer to the CSPN present the highest expansion velocities, that is, the disrupted disk expands faster than the farther bipolar features. We propose that the current physical structure and abundance discrepancy of the H-deficient clumps around the CSPN of A30 can be explained by a common envelope (CE) phase following the VLTP event. Our proposed scenario is also compared with other known born-again PNe (A58, A78, HuBi1 and the Sakurai's Object)., Comment: 9 pages, 6 figures, 1 table; submitted to MNRAS (comments are welcome)

Theory predicts that the temperature of the X-ray-emitting gas (∼106 K) detected from planetary nebulae (PNe) is a consequence of mixing or thermal conduction when in contact with the ionized outer rim (∼104 K). Gas at intermediate temperatures (∼105 K) can be used to study the physics of the production of X-ray-emitting gas, via C IV, N V, and O VI ions. Here, we model the stellar atmosphere of the CSPN of NGC 1501 to demonstrate that even this hot H-deficient [WO4]-type star cannot produce these emission lines by photoionization. We use the detection of the C IV lines to assess the physical properties of the mixing region in this PNe in comparison with its X-ray-emitting gas, rendering NGC 1501 only the second PNe with such characterization. We extend our predictions to the hottest [WO1] and cooler [WC5] spectral types and demonstrate that most energetic photons are absorbed in the dense winds of [WR] CSPN and highly ionized species can be used to study the physics behind the production of hot bubbles in PNe. We found that the UV observations of NGC 2452, NGC 6751, and NGC 6905 are consistent with the presence mixing layers and hot bubbles, providing excellent candidates for future X-ray observations. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

Born-again planetary nebulae (PNe) are extremely rare cases in the evolution of solar-like stars. It is commonly accepted that their central stars (CSPN) experienced a very late thermal pulse (VLTP), ejecting H-deficient material inside the evolved H-rich PN. Given the short duration of this event and the fast subsequent evolution of the CSPN, details of the mass ejection are unknown. We present the first morphokinematic model of the H-deficient material surrounding a born-again PN, namely A 30. New San Pedro Mártir observations with the Manchester Echelle Spectrograph were recently obtained to map the inner region of A 30 which are interpreted by means of the software SHAPE in conjunction with HST WFC3 images. The SHAPE morphokinematic model that best reproduces the observations is composed by a disrupted disc tilted 37° with respect to the line of sight and a pair of orthogonal opposite bipolar ejections. We confirm previous suggestions that the structures closer to the CSPN present the highest expansion velocities, that is, the disrupted disc expands faster than the farther bipolar features. We propose that the current physical structure and abundance discrepancy of the H-deficient clumps around the CSPN of A 30 can be explained by a common envelope phase following the VLTP event. Our proposed scenario is also compared with other known born-again PNe (A 58, A 78, HuBi 1, and the Sakurai’s Object). © 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

Theory predicts that the temperature of the X-ray-emitting gas ($\sim$10$^{6}$ K) detected from planetary nebulae (PNe) is a consequence of mixing or thermal conduction when in contact with the ionized outer rim ($\sim$10$^{4}$ K). Gas at intermediate temperatures ($\sim$10$^{5}$ K) can be used to study the physics of the production of X-ray-emitting gas, via C IV, N V and O VI ions. Here we model the stellar atmosphere of the CSPN of NGC 1501 to demonstrate that even this hot H-deficient [WO4]-type star cannot produce these emission lines by photoionization. We use the detection of the C IV lines to assess the physical properties of the mixing region in this PNe in comparison with its X-ray-emitting gas, rendering NGC 1501 only the second PNe with such characterization. We extend our predictions to the hottest [WO1] and cooler [WC5] spectral types and demonstrate that most energetic photons are absorbed in the dense winds of [WR] CSPN and highly ionized species can be used to study the physics behind the production of hot bubbles in PNe. We found that the UV observations of NGC 2452, NGC 6751 and NGC 6905 are consistent with the presence mixing layers and hot bubbles, providing excellent candidates for future X-ray observations., Comment: To appear in MNRAS; 14 pages, 10 figures, 6 tables

We present a 3D mapping of the Wolf–Rayet (WR) nebula M 1-67 around WR 124. We obtained high-resolution San Pedro Mártir (SPM) Manchester Echelle Spectrograph (MES) observations along 17 long-slit positions covering all morphological features in M 1-67. We are able to unveil the true morphology of M 1-67 and its kinematics by interpreting the SPM MES observations by means of the 3D modelling tool for Astrophysics SHAPE. Our SHAPE model that best reproduces the SPM MES data includes three concentric bipolar structures composed by a hollow ellipsoidal structure and a torus. In addition, the model requires the presence of expanding jets and broken blisters in order to reproduce specific spectral features. Our results are consistent with the idea that M 1-67 and its progenitor star WR 124 have formed through a common envelope scenario that occurred 11.8+4.6−0.8 kyr ago. Our bipolar model strongly questions previous suggestions of the presence of a bow shock structure surrounding M 1-67. We interpret that the bright structures detected in the spectra extracted from the central regions are produced by wind compression at the receding region of the innermost structure in M 1-67. Furthermore, WR 124 is moving through a low-density region above the Galactic plane that has negligibly affected the formation history of M 1-67. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

We present a multiwavelength characterization of the planetary nebula (PN) NGC 6905 and its [Wolf–Rayet]-type ([WR]) central star (CSPN) HD 193949. Our Nordic Optical Telescope Alhambra Faint Object Spectrograph and Camera (ALFOSC) spectra and images unveil in unprecedented detail the high-ionization structure of NGC 6905. The high-quality spectra of HD 193949 allowed us to detect more than 20 WR features including the characteristic O-bump, blue bump, and red bump, which suggests a spectral type no later than a [WO2]-subtype. Moreover we detect the Ne VII and Ne VIII broad emission lines, rendering HD 193949 yet another CSPN with Teff ≲ 150 kK exhibiting such stellar emission lines. We studied the physical properties (Te and ne) and chemical abundances of different regions within NGC 6905 including its low-ionization clumps; abundances are found to be homogeneous. We used the PoWR stellar atmosphere code to model the spectrum of HD 193949, which is afterwards used in a photoionization model performed with CLOUDY that reproduces the nebular and dust properties for a total mass in the 0.31–0.47 M⊙ range and a mass of C-rich dust of ∼2 × 10−3 M⊙. Adopting a current stellar mass of 0.6 M⊙, our model suggests an initial mass ∼1 M⊙ for HD 193949, consistent with the observations. © 2021 The Author(s).

Born-again planetary nebulae (PNe) are extremely rare cases in the evolution of solar-like stars. It is commonly accepted that their central stars (CSPN) experienced a very late thermal pulse (VLTP), ejecting H-deficient material inside the evolved H-rich PN. Given the short duration of this event and the fast subsequent evolution of the CSPN, details of the mass ejection are unknown. We present the first morpho-kinematic model of the H-deficient material surrounding a born-again PN, namely A30. New San Pedro M\'{a}rtir observations with the Manchester Echelle Spectrograph were recently obtained to map the inner region of A30 which are interpreted by means of the software SHAPE in conjunction with HST WFC3 images. The SHAPE morpho-kinematic model that best reproduces the observations is composed by a disrupted disk tilted $37^\circ$ with respect to the line of sight and a pair of orthogonal opposite bipolar ejections. We confirm previous suggestions that the structures closer to the CSPN present the highest expansion velocities, that is, the disrupted disk expands faster than the farther bipolar features. We propose that the current physical structure and abundance discrepancy of the H-deficient clumps around the CSPN of A30 can be explained by a common envelope phase following the VLTP event. Our proposed scenario is also compared with other known born-again PNe (A58, A78, HuBi1 and the Sakurai's Object)., Comment: 9 pages, 6 figures, 1 table; Accepted to MNRAS

We present a 3D mapping of the Wolf-Rayet (WR) nebula M1-67 around WR124. We obtained high-resolution San Pedro M\'{a}rtir (SPM) Manchester Echelle Spectrograph (MES) observations along 17 long-slit positions covering all morphological features in M1-67. We are able to unveil the true morphology of M1-67 and its kinematics by interpreting the SPM MES observations by means of the 3D modelling tool for Astrophysics SHAPE. Our SHAPE model that best reproduces the SPM MES data includes three concentric bipolar structures composed by a hollow ellipsoidal structure and a torus. In addition, the model requires the presence of expanding jets and broken blisters in order to reproduce specific spectral features. Our results are consistent with the idea that M1-67 and its progenitor star WR124 have formed through a common envelope scenario that occurred 11.8$^{+4.6}_{-0.8}$ kyr ago. Our bipolar model strongly questions previous suggestions of the presence of a bow shock structure surrounding M1-67. We interpret that the bright structures detected in the spectra extracted from the central regions are produced by wind compression at the receding region of the innermost structure in M1-67. Furthermore, WR124 is moving through a low-density region above the Galactic plane that has negligibly affected the formation history of M1-67., Comment: 9 pages, 7 figures, 2 tables; Accepted to MNRAS

We present the latest developments of our High-Order Spectral Element Solver (HORSES3D), an open source high-order discontinuous Galerkin framework, capable of solving a variety of flow applications, including compressible flows (with or without shocks), incompressible flows, various RANS and LES turbulence models, particle dynamics, multiphase flows, and aeroacoustics. We provide an overview of the high-order spatial discretisation (including energy/entropy stable schemes) and anisotropic p-adaptation capabilities. The solver is parallelised using MPI and OpenMP showing good scalability for up to 1000 processors. Temporal discretisations include explicit, implicit, multigrid, and dual time-stepping schemes with efficient preconditioners. Additionally, we facilitate meshing and simulating complex geometries through a mesh-free immersed boundary technique. We detail the available documentation and the test cases included in the GitHub repository.

In Alzheimer’s disease (AD), a single-nucleotide polymorphism in the gene encoding brain-derived neurotrophic factor (BDNFVal66Met) is associated with worse impact of primary AD pathology (beta-amyloid, Aβ) on neurodegeneration and cognitive decline, rendering BDNFVal66Met an important modulating factor of cognitive impairment in AD. However, the effect of BDNFVal66Met on functional networks that may underlie cognitive impairment in AD is poorly understood. Using a cross-validation approach, we first explored in subjects with autosomal dominant AD (ADAD) from the Dominantly Inherited Alzheimer Network (DIAN) the effect of BDNFVal66Met on resting-state fMRI assessed functional networks. In seed-based connectivity analysis of six major large-scale networks, we found a stronger decrease of hippocampus (seed) to medial-frontal connectivity in the BDNFVal66Met carriers compared to BDNFVal homozogytes. BDNFVal66Met was not associated with connectivity in any other networks. Next, we tested whether the finding of more pronounced decrease in hippocampal-medial-frontal connectivity in BDNFVal66Met could be also found in elderly subjects with sporadically occurring Aβ, including a group with subjective cognitive decline (N = 149, FACEHBI study) and a group ranging from preclinical to AD dementia (N = 114, DELCODE study). In both of these independently recruited groups, BDNFVal66Met was associated with a stronger effect of more abnormal Aβ-levels (assessed by biofluid-assay or amyloid-PET) on hippocampal-medial-frontal connectivity decreases, controlled for hippocampus volume and other confounds. Lower hippocampal-medial-frontal connectivity was associated with lower global cognitive performance in the DIAN and DELCODE studies. Together these results suggest that BDNFVal66Met is selectively associated with a higher vulnerability of hippocampus-frontal connectivity to primary AD pathology, resulting in greater AD-related cognitive impairment.

We present a multi-wavelength characterisation of the planetary nebula (PN) NGC 6905 and its [Wolf-Rayet]-type ([WR]) central star (CSPN) HD 193949. Our Nordic Optical Telescope (NOT) Alhambra Faint Object Spectrograph and Camera (ALFOSC) spectra and images unveil in unprecedented detail the high-ionization structure of NGC 6905. The high-quality spectra of HD 193949 allowed us to detect more than 20 WR features including the characteristic O-bump, blue bump and red bump, which suggests a spectral type no later than a [WO2]-subtype. Moreover we detect the Ne VII and Ne VIII broad emission lines, rendering HD 193949 yet another CSPN with $T_\mathrm{eff}\lesssim150$ kK exhibiting such stellar emission lines. We studied the physical properties ($T_\mathrm{e}$ and $n_\mathrm{e}$) and chemical abundances of different regions within NGC 6905 including its low-ionization clumps; abundances are found to be homogeneous. We used the PoWR stellar atmosphere code to model the spectrum of HD 193949, which is afterwards used in a photoionization model performed with Cloudy that reproduces the nebular and dust properties for a total mass in the 0.31-0.47 M$_{\odot}$ range and a mass of C-rich dust of $\sim$2 $\times10^{-3}$ M$_{\odot}$. Adopting a current stellar mass of 0.6 M$_{\odot}$, our model suggests an initial mass $\sim$1 M$_\odot$ for HD 193949, consistent with the observations., Comment: To appear in MNRAS; 17 pages, 9 figures, 10 tables

We present a multi-wavelength characterisation of the planetary nebula (PN) NGC 6905 and its [Wolf-Rayet]-type ([WR]) central star (CSPN) HD 193949. Our Nordic Optical Telescope (NOT) Alhambra Faint Object Spectrograph and Camera (ALFOSC) spectra and images unveil in unprecedented detail the high-ionization structure of NGC 6905. The high-quality spectra of HD 193949 allowed us to detect more than 20 WR features including the characteristic O-bump, blue bump and red bump, which suggests a spectral type no later than a [WO2]-subtype. Moreover we detect the Ne VII and Ne VIII broad emission lines, rendering HD 193949 yet another CSPN with $T_\mathrm{eff}\lesssim150$ kK exhibiting such stellar emission lines. We studied the physical properties ($T_\mathrm{e}$ and $n_\mathrm{e}$) and chemical abundances of different regions within NGC 6905 including its low-ionization clumps; abundances are found to be homogeneous. We used the PoWR stellar atmosphere code to model the spectrum of HD 193949, which is afterwards used in a photoionization model performed with Cloudy that reproduces the nebular and dust properties for a total mass in the 0.31-0.47 M$_{\odot}$ range and a mass of C-rich dust of $\sim$2 $\times10^{-3}$ M$_{\odot}$. Adopting a current stellar mass of 0.6 M$_{\odot}$, our model suggests an initial mass $\sim$1 M$_\odot$ for HD 193949, consistent with the observations., Comment: To appear in MNRAS; 17 pages, 9 figures, 10 tables

We present the analysis of XMM-Newton European Photon Imaging Camera (EPIC) observations of the nova shell IPHASX J210204.7$+$471015. We detect X-ray emission from the progenitor binary star with properties that resemble those of underluminous intermediate polars such as DQ Her: an X-ray-emitting plasma with temperature of $T_\mathrm{X}=(6.4\pm3.1)\times10^{6}$ K, a non-thermal X-ray component, and an estimated X-ray luminosity of $L_\mathrm{X}=10^{30}$ erg s$^{-1}$. Time series analyses unveil the presence of two periods, the dominant with a period of $2.9\pm0.2$ hr, which might be attributed to the spin of the white dwarf, and a secondary of $4.5\pm0.6$ hr that is in line with the orbital period of the binary system derived from optical observations. We do not detect extended X-ray emission as in other nova shells probably due to its relatively old age (130-170 yr) or to its asymmetric disrupted morphology which is suggestive of explosion scenarios different to the symmetric ones assumed in available numerical simulations of nova explosions., Comment: 6 pages and 5 Figures; Accepted to MNRAS

We present the analysis of XMM–Newton European Photon Imaging Camera (EPIC) observations of the nova shell IPHASX J210204.7+471015. We detect X-ray emission from the progenitor binary star with properties that resemble those of underluminous intermediate polars such as DQ Herculis (DQ Her): an X-ray-emitting plasma with temperature of TX = (6.4 ± 3.1) × 106 K, a non-thermal X-ray component, and an estimated X-ray luminosity of LX = 1030 erg s−1. Time series analyses unveil the presence of two periods, the dominant with a period of 2.9 ± 0.2 h, which might be attributed to the spin of the white dwarf, and a secondary of 4.5 ± 0.6 h that is in line with the orbital period of the binary system derived from optical observations. We do not detect extended X-ray emission as in other nova shells probably due to its relatively old age (130–170 yr) or to its asymmetric disrupted morphology that is suggestive of explosion scenarios different to the symmetric ones assumed in available numerical simulations of nova explosions. © 2021 The Author(s).

Nova shells can provide us with important information on their distance, their interactions with the circumstellar and interstellar media, and the evolution in morphology of the ejecta. We have obtained narrow-band images of a sample of five nova shells, namely DQHer, FHSer, TAur, V476Cyg, and V533Her, with ages in the range from 50 to 130 years. These images have been compared with suitable available archival images to derive their angular expansion rates. We find that all the nova shells in our sample are still in the free expansion phase, which can be expected, as the mass of the ejecta is 7-45 times larger than the mass of the swept-up circumstellar medium. The nova shells will keep expanding freely for time periods up to a few hundred years, reducing their time dispersal into the interstellar medium., Comment: 8 pages, 2 figures, 3 tables. Accepted for publication in ApJ

We present a comprehensive infrared (IR) study of the iconic Wolf-Rayet (WR) wind-blown bubble NGC6888 around WR136. We use Wide-field Infrared Survey Explorer (WISE), Spitzer IRAC and MIPS and Herschel PACS IR images to produce a sharp view of the distribution of dust around WR136. We complement these IR photometric observations with Spitzer IRS spectra in the 5-38 $\mu$m wavelength range. The unprecedented high-resolution IR images allowed us to produce a clean spectral energy distribution, free of contamination from material along the line of sight, to model the properties of the dust in NGC6888. We use the spectral synthesis code Cloudy to produce a model for NGC6888 that consistently reproduces its optical and IR properties. Our best model requires a double distribution with the inner shell composed only of gas, whilst the outer shell requires a mix of gas and dust. The dust consists of two populations of grain sizes, one with small sized grains $a_\mathrm{small}$=[0.002-0.008] $\mu$m and another one with large sized grains $a_\mathrm{big}$=[0.05-0.5] $\mu$m. The population of big grains is similar to that reported for other red supergiants stars and dominates the total dust mass, which leads us to suggest that the current mass of NGC6888 is purely due to material ejected from WR136, with a negligible contribution of swept up interstellar medium. The total mass of this model is 25.5$^{+4.7}_{-2.8}$ M$_{\odot}$, a dust mass of $M_\mathrm{dust}=$0.14$^{+0.03}_{-0.01}$ M$_{\odot}$, for a dust-to-gas ratio of $5.6\times10^{-3}$. Accordingly, we suggest that the initial stellar mass of WR136 was $\lesssim$50 M$_{\odot}$, consistent with current single stellar evolution models., Comment: 13 pages, 11 figures, 6 tables; Accepted to MNRAS

Nova shells can provide us with important information on their distance, their interactions with the circumstellar and interstellar media, and the evolution in morphology of the ejecta. We have obtained narrow-band images of a sample of five nova shells, namely DQHer, FHSer, TAur, V476Cyg, and V533Her, with ages in the range from 50 to 130 years. These images have been compared with suitable available archival images to derive their angular expansion rates. We find that all the nova shells in our sample are still in the free expansion phase, which can be expected, as the mass of the ejecta is 7-45 times larger than the mass of the swept-up circumstellar medium. The nova shells will keep expanding freely for time periods up to a few hundred years, reducing their time dispersal into the interstellar medium., Comment: 8 pages, 2 figures, 3 tables. Accepted for publication in ApJ

We present a comprehensive infrared (IR) study of the iconicWolf-Rayet (WR) wind-blown bubble NGC6888 around WR136. We use Wide-field Infrared Survey Explorer, Spitzer IRAC, and MIPS and Herschel PACS IR images to produce a sharp view of the distribution of dust around WR136. We complement these IR photometric observations with Spitzer IRS spectra in the 5-38-mu m wavelength range. The unprecedented high-resolution IR images allowed us to produce a clean spectral energy distribution, free of contamination from material along the line of sight, to model the properties of the dust in NGC6888. We use the spectral synthesis code CLOUDY to produce a model for NGC6888 that consistently reproduces its optical and IR properties. Our best model requires a double distribution with the inner shell composed only of gas, whilst the outer shell requires a mix of gas and dust. The dust consists of two populations of grain sizes, one with small-sized grains a(small) = [0.002-0.008] mu m and another one with large-sized grains a(big) = [0.05-0.5] mu m. The population of big grains is similar to that reported for other red supergiants stars and dominates the total dust mass, which leads us to suggest that the current mass of NGC6888 is purely due to material ejected from WR 136, with a negligible contribution of the swept up interstellar medium. The total mass of this model is 25.5(-2.8)+4.7 M-circle dot, a dust mass of M-dust = 0.14(-0.01)(+0.03) M circle dot, for a dust-to-gas ratio of 5.6 x 10(-3). Accordingly, we suggest that the initial stellar mass of WR 136 was less than or similar to 50 M-circle dot, consistent with current single stellar evolution models. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Surfactant-assisted seeded growth of metal nanoparticles (NPs) can be engineered to produce anisotropic gold nanocrystals with high chiroptical activity through the templating effect of chiral micelles formed in the presence of dissymmetric cosurfactants. Mixed micelles adsorb on gold nanorods, forming quasihelical patterns that direct seeded growth into NPs with pronounced morphological and optical handedness. Sharp chiral wrinkles lead to chiral plasmon modes with high dissymmetry factors (~0.20). Through variation of the dimensions of chiral wrinkles, the chiroptical properties can be tuned within the visible and near-infrared electromagnetic spectrum. The micelle-directed mechanism allows extension to other systems, such as the seeded growth of chiral platinum shells on gold nanorods. This approach provides a reproducible, simple, and scalable method toward the fabrication of NPs with high chiral optical activity.

Nova shells can provide important information on their distance, their interactions with circumstellar and interstellar media, and the evolution in morphology of the ejecta. We have obtained narrowband images of a sample of five nova shells, namely DQ Her, FH Ser, T Aur, V476 Cyg, and V533 Her, with ages ranging from 50 to 130 yr. These images have been compared with suitable available archival images to derive their angular expansion rates. We find that all the nova shells in our sample are still in the free expansion phase, which can be expected, as the mass of the ejecta is 7-45 times larger than the mass of the swept-up circumstellar medium. The nova shells will keep expanding freely for time periods up to a few hundred years, reducing their time dispersal into the interstellar medium. © 2020. The American Astronomical Society. All rights reserved.

We study a five-dimensional non-relativistic gravity theory whose action is composed of a gravitational sector and a sector of matter where the gravitational sector is given by the so called Newton--Chern--Simons gravity and where the matter sector is described by a perfect fluid. At time to do cosmology, the obtained field equations shows a close analogy with the projectable version of the Ho\v{r}ava--Lifshitz theory in (3+1)-dimensions. Solutions and their asymptotic limits are found. In particular a phantom solution with a future singularity reminiscent of a Litlle Big Rip future singularity is obtained.

We study a five-dimensional non-relativistic gravity theory whose action is composed of a gravitational sector and a sector of matter where the gravitational sector is given by the so called Newton--Chern--Simons gravity and where the matter sector is described by a perfect fluid. At time to do cosmology, the obtained field equations shows a close analogy with the projectable version of the Ho\v{r}ava--Lifshitz theory in (3+1)-dimensions. Solutions and their asymptotic limits are found. In particular a phantom solution with a future singularity reminiscent of a Litlle Big Rip future singularity is obtained.

Objective: The aim was to establish if the balance adiponectin-oligomers, resolvin-E1 and chemerin levels could contribute to the insulin resistance (IR) setting of subjects with obesity, based on their serum levels and its relationship with inflammatory markers, metabolic profile and adiposopathy status. Methods: This study included 230 individuals, classified according to World Health Organization criteria by body mass index (BMI) kg/m2 in two groups: without-obesity (from 18.5 to 29.9) and with-obesity (from 30.0 to 39.9). Body fat mass distribution, metabolic and inflammatory markers were measured by anthropometric, enzymatic and immuno-turbidimetry methods, respectively. Serum insulin, resolvin-E1, chemerin, and adiponectin-oligomers were evaluating by ELISA method. Analysis performed were correlations IR-indexes with adiposity, receiver operating characteristic (ROC) curves and the adiponectin-oligomers, resolvin-E1 and chemerin tertiles. Results: Subjects’ with-obesity showed adiposopathy status, characterized by metabolic dysregulation and a subclinical inflammatory profile. They presented higher levels (`x ±SD, ng/mL) of resolvin-E1 (1227 ±668 versus 909 ±769, P= 0.017), chemerin (91 ±31 versus 79 ±23, P= 0.013) and LMW-Adiponectin (2257 ±797 versus 1030 ±1055, P= 0.011), whereas HMW-Adiponectin was lower (2470 ±1095 versus 3236 ±1848, P= 0.010), compared to the without-obesity individuals. Individuals’ with-obesity also displayed positive correlation of IR markers (rho from 0.163 to 0.479) along body fat measurements, metabolic and inflammation profiles. Moreover, a negative correlation of HMW-Adiponectin (rho from –0.564 to –0.214) with body fat measurements, metabolic and inflammation profiles. IR-indexes, LMW-Adiponectin and resolvin-E1/chemerin relationship showed differences between groups’ with-obesity and without-obesity, but not with gender. ROC curves shown potential ability of the LMW-Adiponectin levels to differentiate IR from non-IR individuals, Funding Agencies:CONACyT FOINS No. 2250-6 "Investigación en Fronteras de la Ciencia 2015-2" 4/XIV-E/2015 FON.INST./276/2016 to MVM/RENH. PNPC-CONACyT UdG Doctoral Training in Biomedical Sciences to FICM 2014-2017 Scholarship No. 305864. Grant No. 237662, UDG-Programa de Fortalecimiento de la Investigación y el Posgrado 2016 to MVM/RENH. Grant PRODEP No. 245256 to PMMR.

One of the major difficulties hindering the widespread application of colloidal anisotropic plasmonic nanoparticles is the limited robustness and reproducibility of multistep synthetic methods. We demonstrate herein that the reproducibility and reliability of colloidal gold nanorod (AuNR) synthesis can be greatly improved by disconnecting the symmetry-breaking event from the seeded growth process. We have used a modified silver-assisted seeded growth method in the presence of the surfactant hexadecyltrimethylammonium bromide and n-decanol as a co-surfactant to prepare small AuNRs in high yield, which were then used as seeds for the growth of high quality AuNR colloids. Whereas the use of n-decanol provides a more-rigid micellar system, the growth on anisotropic seeds avoids sources of irreproducibility during the symmetry breaking step, yielding uniform AuNR colloids with narrow plasmon bands, ranging from 600 to 1270 nm, and allowing the fine-tuning of the final dimensions. This method provides a robust route for the preparation of high quality AuNR colloids with tunable morphology, size, and optical response in a reproducible and scalable manner.

INTRODUCTION: Large variability among Alzheimer's disease (AD) cases might impact genetic discoveries and complicate dissection of underlying biological pathways. METHODS: Genome Research at Fundacio ACE (GR@ACE) is a genome-wide study of dementia and its clinical endophenotypes, defined based on AD's clinical certainty and vascular burden. We assessed the impact of known AD loci across endophenotypes to generate loci categories. We incorporated gene coexpression data and conducted pathway analysis per category. Finally, to evaluate the effect of heterogeneity in genetic studies, GR@ACE series were meta-analyzed with additional genome-wide association study data sets. RESULTS: We classified known AD loci into three categories, which might reflect the disease clinical heterogeneity. Vascular processes were only detected as a causal mechanism in probable AD. The meta-analysis strategy revealed the ANKRD31-rs4704171 and NDUFAF6-rs10098778 and confirmed SCIMP-rs7225151 and CD33-rs3865444. DISCUSSION: The regulation of vasculature is a prominent causal component of probable AD. GR@ACE meta-analysis revealed novel AD genetic signals, strongly driven by the presence of clinical heterogeneity in the AD series.

In the context of the non-relativistic theories, a generalization of the Chern--Weil-theorem allows us to show that extended Chern--Simons actions for gravity in d=4 invariant under some specific non-relativistic groups lead to modified Poisson equations. In some particular cases, these modified equations have the form of the so-called MOND approach to gravity. The modifications could be understood as due to the effects of dark matter. This result could leads us to think that dark matter can be interpreted as a non-relativistic limit of dark energy.

In the context of the non-relativistic theories, a generalization of the Chern--Weil-theorem allows us to show that extended Chern--Simons actions for gravity in d=4 invariant under some specific non-relativistic groups lead to modified Poisson equations. In some particular cases, these modified equations have the form of the so-called MOND approach to gravity. The modifications could be understood as due to the effects of dark matter. This result could leads us to think that dark matter can be interpreted as a non-relativistic limit of dark energy.

Deep neural networks are a powerful technique that have found ample applications in several branches of Physics. In this work, we apply machine learning algorithms to a specific problem of Cosmic Ray Physics: the estimation of the muon content of extensive air showers when measured at the ground. As a working case, we explore the performance of a deep neural network applied to the signals recorded by the water-Cherenkov detectors of the Surface Detector Array of the Pierre Auger Observatory. We apply deep learning architectures to large sets of simulated data. The inner structure of the neural network is optimized through the use of genetic algorithms. To obtain a prediction of the recorded muon signal in each individual detector, we train neural networks with a mixed sample of light, intermediate and heavy nuclei. When true and predicted signals are compared at detector level, the primary values of the Pearson correlation coefficients are above 95\%. The relative errors of the predicted muon signals are below 10\% and do not depend on the event energy, zenith angle, total signal size, distance range or the hadronic model used to generate the events., Comment: 22 pages, 16 figures. Version accepted for publication in Astroparticle Physics

Deep neural networks are a powerful technique that have found ample applications in several branches of Physics. In this work, we apply machine learning algorithms to a specific problem of Cosmic Ray Physics: the estimation of the muon content of extensive air showers when measured at the ground. As a working case, we explore the performance of a deep neural network applied to the signals recorded by the water-Cherenkov detectors of the Surface Detector Array of the Pierre Auger Observatory. We apply deep learning architectures to large sets of simulated data. The inner structure of the neural network is optimized through the use of genetic algorithms. To obtain a prediction of the recorded muon signal in each individual detector, we train neural networks with a mixed sample of light, intermediate and heavy nuclei. When true and predicted signals are compared at detector level, the primary values of the Pearson correlation coefficients are above 95\%. The relative errors of the predicted muon signals are below 10\% and do not depend on the event energy, zenith angle, total signal size, distance range or the hadronic model used to generate the events., Comment: 22 pages, 16 figures. Version accepted for publication in Astroparticle Physics

The non-relativistic versions of the generalized Poincar\'{e} algebras and generalized $AdS$-Lorentz algebras are obtained. This non-relativistic algebras are called, generalized Galilean algebras type I and type II and denoted by $\mathcal{G}\mathfrak{B}_{n}$ and $\mathcal{G}\mathfrak{L}_{_{n}}$ respectively. Using a generalized In\"{o}n\"{u}--Wigner contraction procedure we find that the generalized Galilean algebras type I can be obtained from the generalized Galilean algebras type II. The $S$-expansion procedure allows us to find the $\mathcal{G}\mathfrak{B}_{_{5}}$ algebra from the Newton--Hooke algebra with central extension. The procedure developed in Ref. \cite{newton} allow us to show that the non-relativistic limit of the five dimensional Einstein--Chern--Simons gravity is given by a modified version of the Poisson equation. The modification could be compatible with the effects of Dark Matter, which leads us to think that Dark Matter can be interpreted as a non-relativistic limit of Dark Energy., Comment: 16 pages, no figures in 755 (2016) 433-438

Acylethanolamides are a family of endogenous lipid mediators that are involved in physiological and behavioral processes associated with addiction. Recently, oleoylethanolamide (OEA) has been reported to reduce alcohol intake and relapse in rodents but the contribution of OEA and other acylethanolamides in alcohol addiction in humans is unknown. The present study is aimed to characterize the plasma acylethanolamides in alcohol dependence. Seventy-nine abstinent alcohol-dependent subjects (27 women) recruited from outpatient treatment programs and age-/sex-/body mass-matched healthy volunteers (28 women) were clinically assessed with the diagnostic interview PRISM according to the DSM-IV-TR after blood extraction for quantification of acylethanolamide concentrations in the plasma. Our results indicate that all acylethanolamides were significantly increased in alcohol-dependent patients compared with control subjects (p < 0.001). A logistic model based on these acylethanolamides was developed to distinguish alcohol-dependent patients from controls and included OEA, arachidonoylethanolamide (AEA) and docosatetraenoylethanolamide (DEA), providing a high discriminatory power according to area under the curve [AUC = 0.92 (95%CI: 0.87–0.96), p < 0.001]. Additionally, we found a significant effect of the duration of alcohol abstinence on the concentrations of OEA, AEA and DEA using a regression model (p < 0.05, p < 0.01 and p < 0.001, respectively), which was confirmed by a negative correlation (rho = −0.31, −0.40 and −0.44, respectively). However, acylethanolamides were not influenced by the addiction alcohol severity, duration of problematic alcohol use or diagnosis of psychiatric comorbidity. Our results support the preclinical studies and suggest that OEA, AEA and DEA are altered in alcohol-dependence during abstinence and that might act as potential markers for predicting length of alcohol abstinence., Depto. de Psicobiología y Metodología en Ciencias del Comportamiento, Fac. de Psicología, TRUE, pub

The non-relativistic versions of the generalized Poincar\'{e} algebras and generalized $AdS$-Lorentz algebras are obtained. This non-relativistic algebras are called, generalized Galilean algebras type I and type II and denoted by $\mathcal{G}\mathfrak{B}_{n}$ and $\mathcal{G}\mathfrak{L}_{_{n}}$ respectively. Using a generalized In\"{o}n\"{u}--Wigner contraction procedure we find that the generalized Galilean algebras type I can be obtained from the generalized Galilean algebras type II. The $S$-expansion procedure allows us to find the $\mathcal{G}\mathfrak{B}_{_{5}}$ algebra from the Newton--Hooke algebra with central extension. The procedure developed in Ref. \cite{newton} allow us to show that the non-relativistic limit of the five dimensional Einstein--Chern--Simons gravity is given by a modified version of the Poisson equation. The modification could be compatible with the effects of Dark Matter, which leads us to think that Dark Matter can be interpreted as a non-relativistic limit of Dark Energy., Comment: 16 pages, no figures in 755 (2016) 433-438

En este trabajo presentamos un modelo dinámico para el comportamiento global de crecimientos naturales (plantas, animales, personas, poblaciones, etc.), basado en una generalización de la segunda ley de Newton y de la mecánica analítica de Hamilton aplicadas a crecimientos naturales. El modelo puede ser usado para describir la dinámica de crecimiento de plantas y tallos o tubérculos con simetría cilíndrica o cónica, y en frutos con simetrías esferoide y elipsoide (prolatos y oblatos). Aplicamos el modelo para frutos de simetría esférica y se presentan los resultados obtenidos para los coeficientes de estímulo y de impulso al crecimiento, así como el potencial de crecimiento para frutos de naranjo, We present a dynamic model for the overall behavior of natural growths (plants, animals, people, populations, etc.), based on a generalization of the Newton’s second law and Hamilton’s analytic mechanics applied them to natural growths. The model can be used to describe the dynamics of growth for plants and stems or tubers with cylindrical or conical symmetry, and fruits with spheroid and ellipsoid (prolate and oblate) symmetries. We apply the model to fruits with spherical symmetry and the resulting stimulus’s coefficient and boost’s coefficient to growth and growth potential orange fruits are presented.

En este trabajo presentamos un modelo dinámico para el comportamiento global de crecimientos naturales (plantas, animales, personas, poblaciones, etc.), basado en una generalización de la segunda ley de Newton y de la mecánica analítica de Hamilton aplicadas a crecimientos naturales. El modelo puede ser usado para describir la dinámica de crecimiento de plantas y tallos o tubérculos con simetría cilíndrica o cónica, y en frutos con simetrías esferoide y elipsoide (prolatos y oblatos). Aplicamos el modelo para frutos de simetría esférica y se presentan los resultados obtenidos para los coeficientes de estímulo y de impulso al crecimiento, así como el potencial de crecimiento para frutos de naranjo, We present a dynamic model for the overall behavior of natural growths (plants, animals, people, populations, etc.), based on a generalization of the Newton’s second law and Hamilton’s analytic mechanics applied them to natural growths. The model can be used to describe the dynamics of growth for plants and stems or tubers with cylindrical or conical symmetry, and fruits with spheroid and ellipsoid (prolate and oblate) symmetries. We apply the model to fruits with spherical symmetry and the resulting stimulus’s coefficient and boost’s coefficient to growth and growth potential orange fruits are presented.

En este trabajo presentamos un modelo dinámico para el comportamiento global de crecimientos naturales (plantas, animales, personas, poblaciones, etc.), basado en una generalización de la segunda ley de Newton y de la mecánica analítica de Hamilton aplicadas a crecimientos naturales. El modelo puede ser usado para describir la dinámica de crecimiento de plantas y tallos o tubérculos con simetría cilíndrica o cónica, y en frutos con simetrías esferoide y elipsoide (prolatos y oblatos). Aplicamos el modelo para frutos de simetría esférica y se presentan los resultados obtenidos para los coeficientes de estímulo y de impulso al crecimiento, así como el potencial de crecimiento para frutos de naranjo, We present a dynamic model for the overall behavior of natural growths (plants, animals, people, populations, etc.), based on a generalization of the Newton’s second law and Hamilton’s analytic mechanics applied them to natural growths. The model can be used to describe the dynamics of growth for plants and stems or tubers with cylindrical or conical symmetry, and fruits with spheroid and ellipsoid (prolate and oblate) symmetries. We apply the model to fruits with spherical symmetry and the resulting stimulus’s coefficient and boost’s coefficient to growth and growth potential orange fruits are presented.

The maker culture has created a dynamic in which designers are less responsible for the design and quality of the final product, but for the tools the consumer uses to create their own. While additive manufacturing (AM) is gaining acceptance among the general public, it is still seen as a prototyping tool instead of a high quality production technology. This limits its acceptance within co-design and maker culture. The research question is: How to create greater acceptance among the general public regarding the AM technology and its products? One way to create greater acceptance of digital design and manufacturing is to apply co-design principles on a local scale. By this means the public will be exposed and included in the design and production process, which will ensure the end product is better accepted. In time this could help spark a maker movement within the community. To validate these assumptions a test case was developed in which local design and production of simple wearables, small ready to wear garments like socks or hats, within an urban community will play a major role. During the research a digital design tool combined with a mobile digital knitting machine was developed to allow for a rapid codesign track. Wearables would be produced by the consumer themselves. The final design of the garment depends on the consumer’s choice of material, shape and pattern. A mobile setup provides the means to test the principle at different locations and allows the consumer to be intensively involved in the maker movement in their own neighbourhood. We implemented a small, low-cost knitting machine that was tested outdoors by park visitors. The anticipated results for this test case were: increased engagement in the production process, larger acceptance of digital design and an initial maker culture. Although the last result will be difficult to determine as it takes some time to develop. If successful, the maker culture will obtain greater exposure, acceptance and d, Design Engineering, Industrial Design Engineering

The maker culture has created a dynamic in which designers are less responsible for the design and quality of the final product, but for the tools the consumer uses to create their own. While additive manufacturing (AM) is gaining acceptance among the general public, it is still seen as a prototyping tool instead of a high quality production technology. This limits its acceptance within co-design and maker culture. The research question is: How to create greater acceptance among the general public regarding the AM technology and its products? One way to create greater acceptance of digital design and manufacturing is to apply co-design principles on a local scale. By this means the public will be exposed and included in the design and production process, which will ensure the end product is better accepted. In time this could help spark a maker movement within the community. To validate these assumptions a test case was developed in which local design and production of simple wearables, small ready to wear garments like socks or hats, within an urban community will play a major role. During the research a digital design tool combined with a mobile digital knitting machine was developed to allow for a rapid codesign track. Wearables would be produced by the consumer themselves. The final design of the garment depends on the consumer’s choice of material, shape and pattern. A mobile setup provides the means to test the principle at different locations and allows the consumer to be intensively involved in the maker movement in their own neighbourhood. We implemented a small, low-cost knitting machine that was tested outdoors by park visitors. The anticipated results for this test case were: increased engagement in the production process, larger acceptance of digital design and an initial maker culture. Although the last result will be difficult to determine as it takes some time to develop. If successful, the maker culture will obtain greater exposure, acceptance and d, Design Engineering, Industrial Design Engineering

Angiosperms, http://name.umdl.umich.edu/IC-HERB00IC-X-1542052%5DMICH-V-1542052, https://quod.lib.umich.edu/cgi/i/image/api/thumb/herb00ic/1542052/MICH-V-1542052/!250,250, The University of Michigan Library provides access to these materials for educational and research purposes. Some materials may be protected by copyright. If you decide to use any of these materials, you are responsible for making your own legal assessment and securing any necessary permission. If you have questions about the collection, please contact the Herbarium professional staff: herb-dlps-help@umich.edu. If you have concerns about the inclusion of an item in this collection, please contact Library Information Technology: libraryit-info@umich.edu., https://www.lib.umich.edu/about-us/policies/copyright-policy

Angiosperms, http://name.umdl.umich.edu/IC-HERB00IC-X-1529197%5DMICH-V-1529197, https://quod.lib.umich.edu/cgi/i/image/api/thumb/herb00ic/1529197/MICH-V-1529197/!250,250, The University of Michigan Library provides access to these materials for educational and research purposes. Some materials may be protected by copyright. If you decide to use any of these materials, you are responsible for making your own legal assessment and securing any necessary permission. If you have questions about the collection, please contact the Herbarium professional staff: herb-dlps-help@umich.edu. If you have concerns about the inclusion of an item in this collection, please contact Library Information Technology: libraryit-info@umich.edu., https://www.lib.umich.edu/about-us/policies/copyright-policy

Angiosperms, http://name.umdl.umich.edu/IC-HERB00IC-X-1542052%5DMICH-V-1542052, https://quod.lib.umich.edu/cgi/i/image/api/thumb/herb00ic/1542052/MICH-V-1542052/!250,250, The University of Michigan Library provides access to these materials for educational and research purposes. Some materials may be protected by copyright. If you decide to use any of these materials, you are responsible for making your own legal assessment and securing any necessary permission. If you have questions about the collection, please contact the Herbarium professional staff: herb-dlps-help@umich.edu. If you have concerns about the inclusion of an item in this collection, please contact Library Information Technology: libraryit-info@umich.edu., https://www.lib.umich.edu/about-us/policies/copyright-policy

Angiosperms, http://name.umdl.umich.edu/IC-HERB00IC-X-1529197%5DMICH-V-1529197, https://quod.lib.umich.edu/cgi/i/image/api/thumb/herb00ic/1529197/MICH-V-1529197/!250,250, The University of Michigan Library provides access to these materials for educational and research purposes. Some materials may be protected by copyright. If you decide to use any of these materials, you are responsible for making your own legal assessment and securing any necessary permission. If you have questions about the collection, please contact the Herbarium professional staff: herb-dlps-help@umich.edu. If you have concerns about the inclusion of an item in this collection, please contact Library Information Technology: libraryit-info@umich.edu., https://www.lib.umich.edu/about-us/policies/copyright-policy

Inflammatory and immune processes have been implicated in the etiopathology of schizophrenia. We demonstrate the existence of immune function alteration, assessed by serum cytokine's levels, not only in schizophrenia patients but also in their unaffected first-degree relatives. This finding may provide a new data for considering cytokines as schizophrenic disease biomarkers. © 2012 Elsevier Ireland Ltd.

Background. Children with difficulties in processing and modulation sensory information, present difficulties in performing daily activities, developing habits, and daily routines in the performing academic and family roles, in correctly appreciating their abilities, and in taking responsibilities for their actions. Traditionally, assessment and intervention with these children has focused on the disability management. The ICF recognizes the individuality and the barriers and facilitators stemming from environmental and personal factors.Objectives. Compare the evaluation of children group with sensory integration deficit from the point of view of disability and CIF evaluation on daily activities deficits.Materials and Methods. The study was exploratory and descriptive, six pre-school and twenty-two students who attended SERH between September 2008 and March 2009. We compared and coded the score for each element of the sensory profile Based upon these; we evaluated bodily functioning and participation in daily activities.Results. The results demonstrate compatibility between the functions and participation activities and sections of sensory processing, but not, in relation to the factors for the specificity of the test. Characterization of sensory processing conditions is feasible with the combined use of references.Conclusion. This study shows that sensory stimulation can have a positive impact in development and performance of daily activities in disabled children. There is increasing need to provide appropriate treatment alternatives through proper professional and family education., Antecedentes Los niños con dificultades en el procesamiento y modulación sensorial, se han evaluado e intervenido en el ámbito de la discapacidad. La clasificación internacional del funcionamiento, la discapacidad y de la salud constituye un marco por el que estos niños pueden manejarse de forma integral.Objetivos. Describir los elementos que definen la condición de procesamiento sensorial desde las dimensiones de funcionamiento y actividades de participación y los elementos del procesamiento sensorial. Desde la CIF analizar la ocurrencia de las condiciones de procesamiento sensorial de un grupo de pre-escolares y escolares con dificultades en las actividades cotidianas.Material y métodos. Estudio exploratorio-descriptivo, de seis pre-escolares y 22 escolares que asistieron al SERH entre septiembre 2008 y marzo 2009. Se contrastó y codificó la lista de clasificación con cada elemento del perfil sensorial y se utilizó una matriz que contempló funciones corporales, actividades y participación con el código correspondiente.Resultados. Se encontró compatibilidad entre las funciones y actividades de participación y las secciones del procesamiento sensorial, pero no en relación con los factores por la especificidad de la prueba. La caracterización de las condiciones de procesamiento sensorial es viable con la utilización de referentes combinados.Conclusión. Para brindar alternativas apropiadas de manejo a los niños con dificultades sensoriales se requiere aumentar, mediar y difundir en los profesionales y familiares el conocimiento sobre el procesamiento sensorial y su funcionamiento, lo mismo que sobre la estimulación que se demanda para disminuir su impacto en las actividades cotidianas de los niños.

Background. Children with difficulties in processing and modulation sensory information, present difficulties in performing daily activities, developing habits, and daily routines in the performing academic and family roles, in correctly appreciating their abilities, and in taking responsibilities for their actions. Traditionally, assessment and intervention with these children has focused on the disability management. The ICF recognizes the individuality and the barriers and facilitators stemming from environmental and personal factors.Objectives. Compare the evaluation of children group with sensory integration deficit from the point of view of disability and CIF evaluation on daily activities deficits.Materials and Methods. The study was exploratory and descriptive, six pre-school and twenty-two students who attended SERH between September 2008 and March 2009. We compared and coded the score for each element of the sensory profile Based upon these; we evaluated bodily functioning and participation in daily activities.Results. The results demonstrate compatibility between the functions and participation activities and sections of sensory processing, but not, in relation to the factors for the specificity of the test. Characterization of sensory processing conditions is feasible with the combined use of references.Conclusion. This study shows that sensory stimulation can have a positive impact in development and performance of daily activities in disabled children. There is increasing need to provide appropriate treatment alternatives through proper professional and family education., Antecedentes Los niños con dificultades en el procesamiento y modulación sensorial, se han evaluado e intervenido en el ámbito de la discapacidad. La clasificación internacional del funcionamiento, la discapacidad y de la salud constituye un marco por el que estos niños pueden manejarse de forma integral.Objetivos. Describir los elementos que definen la condición de procesamiento sensorial desde las dimensiones de funcionamiento y actividades de participación y los elementos del procesamiento sensorial. Desde la CIF analizar la ocurrencia de las condiciones de procesamiento sensorial de un grupo de pre-escolares y escolares con dificultades en las actividades cotidianas.Material y métodos. Estudio exploratorio-descriptivo, de seis pre-escolares y 22 escolares que asistieron al SERH entre septiembre 2008 y marzo 2009. Se contrastó y codificó la lista de clasificación con cada elemento del perfil sensorial y se utilizó una matriz que contempló funciones corporales, actividades y participación con el código correspondiente.Resultados. Se encontró compatibilidad entre las funciones y actividades de participación y las secciones del procesamiento sensorial, pero no en relación con los factores por la especificidad de la prueba. La caracterización de las condiciones de procesamiento sensorial es viable con la utilización de referentes combinados.Conclusión. Para brindar alternativas apropiadas de manejo a los niños con dificultades sensoriales se requiere aumentar, mediar y difundir en los profesionales y familiares el conocimiento sobre el procesamiento sensorial y su funcionamiento, lo mismo que sobre la estimulación que se demanda para disminuir su impacto en las actividades cotidianas de los niños.

We develop a linearized five dimensional Kaluza-Klein theory as a gauge theory. By perturbing the metric around flat and the De Sitter backgrounds, we first discuss linearized gravity as a gauge theory in any dimension. In the particular case of five dimensions, we show that using the Kaluza-Klein mechanism, the field equations of our approach implies both linearized gauge gravity and Maxwell theory in flat and the De Sitter scenarios. As a possible further development of our formalism, we also discuss an application in the context of a gravitational polarization scattering by means of the analogue of the Mueller matrix in optical polarization algebra. We argue that this application can be of particular interest in gravitational waves experiments., Comment: 16 pages, Latex