Water reservoirs monitoring through Google Earth Engine: application to Sentinel and Landsat imagery

Water reservoirs are subjected to increasing hydrological stresses, therefore continuous and accurate monitoring of these resources is essential to ensure their sustainable management. This work proposes a methodology to remotely monitor the surface extent of water reservoirs through the analysis of satellite multispectral and Synthetic Aperture Radar (SAR) images. In particular, a segmentation strategy was implemented within Google Earth Engine (GEE) to distinguish water bodies from the surrounding land surface and measure their extension, by applying three different approaches to Sentinel-1, Sentinel-2, and Landsat-8 imagery. The first approach is based on the use of the Automatic Water Extraction Index (AWEI) and the self-adaptive Otsu's thresholding method, the second approach is based on the image conversion from RGB (Red-Green-Blue) to HSV (Hue, Saturation, Value) and the use of a parametric threshold, the third approach is based on the use of SAR imagery and an empirically selected threshold. A "static"validation strategy was developed from scratch and standard segmentation metrics were computed to evaluate the accuracy of the three approaches. The average values of the F1 scores on the Sentinel imagery were equal to 0.95, 0.90, and 0.84 for the three approaches, respectively. The same metric on the Landsat imagery was 0.95 for the first approach and 0.93 for the second approach. The best approach, i.e. the AWEI-based method, was then applied to three water bodies in which the effects of the 2022 drought were particularly significant: Sawa lake (Iraq), Poyang lake (China), and Po river (Italy). The results visually highlighted the good performance of the approach in segmenting the water bodies from the surrounding areas

Numerical Analysis of Aluminium Façade Components

This paper commences with a scientific literature review of current research that underlines the environmental benefits to be gained from using smaller quantities of raw materials in the construction industry, with particular emphasis on a sustainable approach to façade design.  Life cycle assessment modelling is advocated to validate the sustainability of building structures to achieve optimal solutions. A real-life application of the design of an aluminium façade bracket is presented, demonstrating that a weight reduction of up to 35-45% is attainable by exploiting the post-elastic properties of a material. The work described ranges from a discussion of the current conventional numerical techniques adopted by the industry to the most recent and advanced computational methods permitted by the introduction of Eurocode 9. This code facilitates a substantial enhancement in structural performance by incorporating an evaluation of the material's elastic-hardening behaviour and allows for a noteworthy reduction in component size and increased geometric design flexibility

Lyα\alpha Halos Around z∼6z\sim6 Quasars

We present deep MUSE observations of five quasars within the first Gyr of the Universe ($z\gtrsim6$), four of which display extended Ly$\alpha$ halos. After PSF-subtraction, we reveal halos surrounding two quasars for the first time, as well as confirming the presence of two more halos for which tentative detections exist in long-slit spectroscopic observations and narrow-band imaging. The four Ly$\alpha$ halos presented here are diverse in morphology and size, they each display spatial asymmetry, and none are centred on the position of the quasar. Spectra of the diffuse halos demonstrate that none are dramatically offset in velocity from the systemic redshift of the quasars ($\Delta$ v $< 200$ kms$^{-1}$), however each halo shows a broad Ly$\alpha$ line, with a velocity width of order $\sim1000$ kms$^{-1}$. Total Ly$\alpha$ luminosities range between $\sim$ $2 \times 10^{43}$ erg s$^{-1}$ and $\sim$ $2 \times 10^{44}$ erg s$^{-1}$, reaching maximum radial extents of $13 - 30$ pkpc from the quasar positions. We find larger sizes and higher Ly$\alpha$ luminosities than previous literature results at this redshift, but find no correlation between the quasar properties and the Ly$\alpha$ halo, suggesting that the detected emission is most closely related to the physical properties of the circum-galactic mediumComment: 19 pages, Accepted for publication in Ap

Is GN-z11 powered by a super-Eddington massive black hole?

Observations of z∼6 quasars powered by super-massive black holes (SMBHs, MBH∼108−10M⊙) challenge our current understanding of early black hole formation and evolution. The advent of the James Webb Space Telescope (JWST) has enabled the study of massive black holes (MBHs, MBH∼106−7 M⊙) up to z∼11, thus bridging the properties of z∼6 quasars to their ancestors. JWST spectroscopic observations of GN-z11, a well-known z=10.6 star forming galaxy, have been interpreted with the presence of a super-Eddington (Eddington ratio ≡λEdd∼5.5) accreting MBH. To test this hypothesis we use a zoom-in cosmological simulation of galaxy formation and BH co-evolution. We first test the simulation results against the observed probability distribution function (PDF) of λEdd found in z∼6 quasars. Then, we select in the simulation those BHs that satisfy the following criteria: (a) 10106 M⊙. Finally we apply the Extreme Value Statistics to the PDF of λEdd resulting from the simulation and find that the probability of observing a z∼10−11 MBH, accreting with λEdd∼5.5, in the volume surveyed by JWST, is very low (<0.5%). We compare our predictions with those in the literature and further discuss the main limitations of our work. Our simulation cannot explain the JWST observations of GN-z11. This might be due to (i) missing physics in simulations, or (ii) uncertainties in the data analysis

Immunohistochemical analysis of chromatin remodeler DAXX in high grade urothelial carcinoma

Background/Aims: The chromatin remodeler DAXX, a predominantly nuclear protein, regulates the status of chromatin organization. The aim of this exploratory immunohistochemical study was to evaluate DAXX protein expression in high grade invasive urothelial carcinoma (UC) of the bladder as a biological regulator of aggressiveness. Methods: Quantitative analysis was made on DAXX immunostained nuclei in tissue sections from 5 cases of bladder normal urothelium (NU) and 5 cases of bladder pT1 UC. Carcinoma in situ (CIS) and high grade papillary carcinoma (HGPCa) were identified in 2 out of 5 UC cases. Results: The nuclei in UC show an open configuration of the chromatin composed of granules varying in size and distribution and a mean nuclear area 1.7 times greater than that in NU (UC: mean and SD 24.4 ± 11.4 square microns; NU: 14.8 6.5 square microns. The differences are statistically significant). 70% of the NU nuclei are immunostained, whereas 90% of UC nuclei are positive. The mean gray level value in UC, related to the intensity of nuclear immunostaining, is lower than in NU by a factor of 0.94 (UC: mean and SD 100 ± 15; NU: 106 ± 15. The differences are statistically significant). In particular, the value in the nuclei adjacent to the stroma in UC is slightly lower than in the intermediate cell layers by factor of 0.98, whereas in NU it is slightly greater by a factor 1.02 and 1.04 compared to the intermediate and superficial cell layers. The values in CIS and HGPCa are similar to those in UC. Conclusions: The quantitative immunohistochemical analysis shows an altered protein expression of chromatin remodeler DAXX in UC and in its preinvasive phases, when compared to NU. DAXX evaluation, if associated with markers related to global DNA methylation and histone acetylation, could be used in clinical practice as a marker of aggressiveness. Virtual slides: The virtual slides for this article can be found here: http://www.diagnosticpathology.diagnomx.eu/vs/139845729710237

X-ray Observations of a [C II]-bright, z=6.59 Quasar/Companion System

We present deep Chandra observations of PSO J231.6576$-$20.8335, a quasar at redshift z=6.59 with a nearby (${\sim}8$ proper kpc) companion galaxy. ALMA observed both the quasar and companion to be bright in [C II], and the system has significant extended Ly$\alpha$ emission around the quasar, suggesting that a galaxy merger is ongoing. Unlike previous studies of two similar systems, and despite observing the system with Chandra for 140 ks, we do not detect the companion in X-rays. The quasar itself is detected, but only $13.3^{+4.8}_{-3.7}$ net counts are observed. From a basic spectral analysis, the X-ray spectrum of the quasar is soft (hardness ratio of $\mathcal{HR} = -0.60_{-0.27}^{+0.17}$, power-law index of $\Gamma=2.6^{+1.0}_{-0.9}$), which results in a rest-frame X-ray luminosity comparable to other bright quasars ($L_{2-10} = 1.09^{+2.20}_{-0.70}\times 10^{45}\ \textrm{erg}\ \textrm{s}^{-1}$) despite the faint observed X-ray flux. We highlight two possible interpretations of this result: the quasar has a steep value of$\Gamma$-- potentially related to observed ongoing Eddington accretion -- thereby pushing much of the emission out of our observed band, or the quasar has a more normal spectrum ($\Gamma{\sim}2$) but is therefore less X-ray luminous ($L_{2-10} \sim 0.6 \times 10^{45}\ \textrm{ erg}\ \textrm{ s}^{-1}$).Comment: 11 pages, 4 figures. Accepted for publication in Ap

X-Ray Observations of a z ∼ 6.2 Quasar/Galaxy Merger

Quasars at early redshifts (z > 6) with companion galaxies offer unique insights into the growth and evolution of the first supermassive black holes. Here, we report on a 150 ks Chandra observation of PSO.J308.0416-21.2339, a z = 6.23 quasar with a merging companion galaxy identified in [C II] and rest-frame UV emission. With 72.3(-8.6)(+9.6) net counts, we find that PSO.J308.0416-21.2339 is powerful (L-X = 2.31(-0.76)(+1.14) x 10(45) erg s(-1) cm(-2) in rest-frame 2.0-10.0 keV) yet soft (spectral power-law index Gamma = 2.39(-0.36)(+0.37) and optical-to-X-ray slope alpha(OX) = -1.41 +/- 0.11). In addition, we detect three hard-energy photons 2 ''.0 to the west of the main quasar, cospatial with the brightest UV emission of the merging companion. As no soft-energy photons are detected in the same area, this is potentially indicative of a highly obscured source. With conservative assumptions, and accounting for both background fluctuations and the extended wings of the quasar's emission, these photons only have a probability P = 0.021 of happening by chance. If confirmed by deeper observations, this system is the first high-redshift quasar and companion individually detected in X-rays and is likely a dual active galactic nucleus.STSCI/NASAThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]

The Decoupled Kinematics of High- z QSO Host Galaxies and Their Ly α Halos

© 2022. The Author(s). Published by the American Astronomical Society. This is an open access article distributed under the Creative Commons Attribution License, to view a copy of the license, see: https://creativecommons.org/licenses/by/4.0/We present a comparison of the interstellar medium traced by [C ii] (Atacama Large Millimeter/submillimeter Array), and ionized halo gas traced by Lyα (Multi Unit Spectroscopic Explorer), in and around QSO host galaxies at z ∼ 6. To date, 18 QSOs at this redshift have been studied with both MUSE and high-resolution ALMA imaging; of these, 8 objects display a Lyα halo. Using data cubes matched in velocity resolution, we compare and contrast the spatial and kinematic information of the Lyα halos and the host galaxies’ [C ii] (and dust-continuum) emission. We find that the Lyα halos extend typically 3−30 times beyond the interstellar medium of the host galaxies. The majority of the Lyα halos do not show ordered motion in their velocity fields, whereas most of the [C ii] velocity fields do. In those cases where a velocity gradient can be measured in Lyα, the kinematics do not align with those derived from the [C ii] emission. This implies that the Lyα emission is not tracing the outskirts of a large rotating disk, which is a simple extension of the central galaxy seen in [C ii] emission. It rather suggests that the kinematics of the halo gas are decoupled from those of the central galaxy. Given the scattering nature of Lyα, these results need to be confirmed with James Webb Space Telescope Integral Field Unit observations that can constrain the halo kinematics further using the nonresonant Hα line.Peer reviewe

The red cell distribution width (RDW): value and role in preterm, IUGR (intrauterine growth restricted), full-term infants.

To measure the red cell distribution width (RDW) ranges at birth and to evaluate potential association with typical neonatal diseases: patent of the ductus arteriousus (PDA), bronchopulmonary dysplasia (BPD), and late-onset sepsis (LOS) mortality.Forty-six full-term, 41 preterm, and 35 intrauterine growth restricted (IUGR) infants participated in this retrospective, observational study. RDW was measured before 3 days of life (T0) in all infants, and at first month of life (T1) in preterm/IURG patients.RDW% mean (standard deviation) at T0 was: 15.65 (1.18) in full-term newborns; 17.7 (2.06) in preterm; 17.45 (1.81) in IUGR. A negative correlation (r = -0.51; P0.001) between RDW and gestational age was found. RDW at T1 was: 17.25 (2.19) in the preterm group; 17.37 (2.56) in IUGR group. Fourteen preterm infants reported: 12 PDA, 5 LOS, 4 BPD, and 3 died; 10 IUGR infants had: 4 PDA, 6 LOS, 3 BPD, and 1 died. RDW of IUGR infants suffering from those pathologies was not statistically different compared with unaffected infants, while preterm newborns with pathologies reported higher RDW: PDA vs. PDA absent: P = 0.008 at T0; P0.002 at T1. BPD vs. BPD absent: P0.005 at T1. LOS vs. LOS absent: P0.005 at T0. RDW in preterm/IUGR population was associated with early mortality, T0: dead 21.2 (2.7) vs. alive 16.7 (1.7), P0.0001.RDW and gestational age at birth were negatively correlated. High RDW resulted to be an indication of risk for critical newborns. This parameter can be inexpensively and routinely verified and further studies are required to confirm its prognostic role in neonatal pathologies

Enhanced X-ray Emission from the Most Radio-Powerful Quasar in the Universe's First Billion Years

We present deep (265 ks) Chandra X-ray observations of PSO J352.4034$-$15.3373, a quasar at z=5.831 that, with a radio-to-optical flux ratio of R>1000, is one of the radio-loudest quasars in the early universe and is the only quasar with observed extended radio jets of kpc-scale at $z \gtrsim 6$. Modeling the X-ray spectrum of the quasar with a power law, we find a best fit of $\Gamma = 1.99^{+0.29}_{-0.28}$, leading to an X-ray luminosity of $L_{2-10} = 1.26^{+0.45}_{-0.33} \times 10^{45}\ {\rm erg}\ {\rm s}^{-1}$ and an X-ray to UV brightness ratio of $\alpha_{\rm OX} = -1.36 \pm 0.11$. We identify a diffuse structure 50 kpc (${\sim}8^{\prime\prime}$) to the NW of the quasar along the jet axis that corresponds to a $3\sigma$ enhancement in the angular density of emission and can be ruled out as a background fluctuation with a probability of P=0.9985. While with few detected photons the spectral fit of the structure is uncertain, we find that it has a luminosity of $L_{2-10}\sim10^{44}\ {\rm erg}\ {\rm s}^{-1}$. These observations therefore potentially represent the most distant quasar jet yet seen in X-rays. We find no evidence for excess X-ray emission where the previously-reported radio jets are seen (which have an overall linear extent of $0.^{\prime\prime}28$), and a bright X-ray point source located along the jet axis to the SE is revealed by optical and NIR imaging to not be associated with the quasar.Comment: 16 pages, 7 Figures. Accepted for publication the Astrophysical Journa