Massive Formation Research Articles

Insulin-like Growth Factor II mRNA-binding Protein 3 is a Highly Sensitive Marker for Intravascular Large B-cell Lymphoma: Immunohistochemical Analysis of 152 Pathology Specimens From 88 Patients.

Intravascular large B-cell lymphoma (IVLBCL) is a rare type of aggressive extranodal large B-cell lymphoma characterized by the selective growth of lymphoma cells within the lumina of blood vessels, particularly capillaries. IVLBCL lacks mass formation, and its diagnosis can be challenging. We analyzed the utility of insulin-like growth factor II mRNA-binding protein 3 (IMP3) immunohistochemistry for IVLBCL diagnosis in various organs. Double staining with paired box 5 (PAX5) was performed for validation. Overall, 152 pathological specimens (111 positive and 41 negative for IVLBCL) obtained from 88 patients with a diagnosis of IVLBCL were stained for IMP3 and IMP3/PAX5. As negative controls, 40 pathology specimens from 38 patients with no history of IVLBCL or other B-cell lymphomas were stained for IMP3, which comprised 31 benign pathological specimens from 29 patients in whom malignancy was suspected, 7 cases of appendicitis with intravascular and/or intralymphatic lymphoid proliferations, and 2 cases of intravascular natural killer/T-cell lymphoma. All mononuclear cells with cytoplasmic staining were considered positive for IMP3 expression, but expression restricted to germinal center B cells was excluded from evaluation. All 111 IVLBCL pathological specimens were positive for IMP3 and IMP3/PAX5. In addition, 11 of the 41 specimens originally diagnosed as IVLBCL-negative showed IMP3/PAX5 double-positive cells, raising the suspicion of IVLBCL. However, of the 40 negative control samples, IMP3-positive non-germinal center B cells were detected in only 2 samples ( P = 0.0131) and no intravascular IMP3-positive B cells suspicious for IVLBCL were identified. Altogether, IMP3 immunohistochemistry is a highly sensitive marker of IVLBCL and can be a helpful adjunct for IVLBCL diagnosis.

Constraining the Initial Mass Function in the Epoch of Reionization from Astrophysical and Cosmological Data

We aim to constrain the stellar initial mass function (IMF) during the epoch of reionization. To this purpose, we build up a semi-empirical model for the reionization history of the Universe based on various ingredients: the latest determination of the UV galaxy luminosity function from JWST out to redshift z≲12; data-inferred and simulation-driven assumptions on the redshift-dependent escape fraction of ionizing photons from primordial galaxies; a simple yet flexible parameterization of the IMF ϕ(m⋆)∼m⋆ξe−m⋆,c/m⋆ in terms of a high-mass end slope ξ<0 and a characteristic mass m⋆,c, below which a flattening or a bending sets in (allowing description of a variety of IMF shapes from the classic Salpeter to top-heavy ones); the PARSEC stellar evolution code to compute the UV and ionizing emission from different stars’ masses as a function of age and metallicity; and a few physical constraints related to stellar and galaxy formation in faint galaxies at the reionization redshifts. We then compare our model outcomes with the reionization observables from different astrophysical and cosmological probes and perform Bayesian inference on the IMF parameters via a standard MCMC technique. We find that the IMF slope ξ is within the range from −2.8 to −2.3, consistent with direct determination from star counts in the Milky Way, while appreciably flatter slopes are excluded at great significance. However, the bestfit value of the IMF characteristic mass m⋆,c∼a few M⊙ implies a suppression in the formation of small stellar masses at variance with the IMF in the local Universe. This may be induced by the thermal background of ∼20–30 K provided by CMB photons at the reionization redshifts. We check that our results are robust against different parameterizations for the redshift evolution of the escape fraction. Finally, we investigate the implications of our reconstructed IMF for the recent JWST detections of massive galaxies at and beyond the reionization epoch, showing that any putative tension with the standard cosmological framework is substantially alleviated.

Isolated Abducens Nerve Palsy: A Case Report of Cerebral Pseudocyst of Dorello’s Canal

<p><strong>Background:</strong> Abducens nerve is the second longest intracranial path out of all of the cranial nerves. Abducens nerve pasly had a prevalence 11.3/100.000 and mostly seen in adults. Isolated abducens nerve palsy due to neoplastic lesion are rare and mostly related to skull base tumor.</p><p><strong>Case Presentation: </strong>We present a case of 57 years old woman with complaints of red right eye and worsening headache associates with diplopia on the right lateral gaze for three days prior admission. She was later diagnosed with isolated abducens nerve palsy associated to neoplasm cause in Dorello’s canal. Patient was then discharged with symptomatic therapy and educated for head posturing and avoid triggers.</p><p><strong>Conclusions:</strong> Abducens nerve palsy is the most common isolated ocular nerve palsy. The incidence of mass formation such as neoplastic lesion or cyst are rare.</p>

SARS-CoV-2 infection increases airway bleeding risk in patients after tracheostomies

BackgroundAirway bleeding events are a rare incident in SARS-CoV-2-infected patients after tracheostomies. We aimed to explore the correlation between airway bleeding and SARS-CoV-2 infection and evaluate the consistency of SARS-CoV-2 RNA test results in the upper and lower airway samples from patients after tracheostomies.MethodsForty-four patients after temporary or permanent tracheostomy were divided into a positive group (29 patients) and a negative group (15 patients) based on the SARS-CoV-2 RNA test results of their oropharyngeal swabs. The oropharyngeal and tracheal swabs of the positive group were re-collected for SARS-CoV-2 RNA detection. Demographic and clinical characteristics and airway bleeding events were recorded for all enrolled patients.ResultsAirway bleeding was reported in eleven patients of the positive group (11/29), with seven displaying bloody sputum or hemoptysis, and four featuring massive sputum crust formation in the trachea that resulted in dyspnea, and only one patient in the negative group (1/15), with a significant difference in the airway bleeding rate (37.9% vs. 6.7%, p < 0.05). The SARS-CoV-2 RNA test results showed a statistical difference in cycle threshold (Ct) values between oropharyngeal swabs and tracheal swabs (p < 0.05).ConclusionsAfter tracheostomies, patients are more susceptible to airway bleeding if they are infected with SARS-CoV-2. The findings signify that in addition to droplet transmission through tracheostoma, SARS-CoV-2 may infect the oropharynx by airborne and close contact transmission, and that given the higher viral load and longer infection time in the trachea, tracheal swabs are more reliable for SARS-CoV-2 detection in these patients.

Obscured star formation in clusters at z = 1.6–2.0: massive galaxy formation and the reversal of the star formation–density relation

ABSTRACT Clusters of galaxies at z $\mathrel {\gtrsim }$ 1 are expected to be increasingly active sites of star formation. To test this, an 850 $\mu$m survey was undertaken of eight clusters at z = 1.6–2.0 using SCUBA-2 on the James Clerk Maxwell Telescope. Mid-infrared properties were used to identify 53 probable counterparts to 45 SCUBA-2 sources with colours that suggested they were cluster members. This uncovered a modest overdensity of 850 $\mu$m sources, with far-infrared luminosities of LIR ≥ 1012 L⊙ (SFR $\mathrel {\gtrsim }$ 100 M⊙ yr−1) and colours consistent with being cluster members, of a factor of 4 ± 1 within the central 1 Mpc radius of the clusters. The submillimetre photometry of these galaxies was used to estimate the total cluster star formation rates. These showed that the mass-normalized rates in the clusters are two orders of magnitude higher than in local systems, evolving as (1 + z)5.5 ± 0.6. This rapid evolution means that the mass-normalized star formation rates in these clusters matched that of average haloes in the field at z ∼ 1.8 ± 0.2 marking the epoch where the local star formation–density relation reverses in massive haloes. The estimated stellar masses of the cluster submillimetre galaxies suggests that their descendants will be amongst the most massive galaxies in z ∼ 0 clusters. This reinforces the suggestion that the majority of the massive early-type galaxy population in z ∼ 0 clusters were likely to have formed at z $\mathrel {\gtrsim }$ 1.5–2 through very active, but dust-obscured, starburst events.

Deformation mechanism and hardening behavior of gradient heterostructured magnesium alloys prepared by severe shear deformation

Lightweight equipment in aerospace and other fields urgently requires magnesium (Mg) alloys components with high-strength plasticity. For this reason, in this study, a gradient heterogeneous structure containing nanocrystallines was constructed successfully using a severe shear deformation process that combines severe plastic deformation techniques and torsional deformation characteristics. The evolution of the microstructure and hardness of Mg-12.12Gd-4.2Y-2.28Zn-0.36Zr (wt%) alloys prepared by severe shear deformation with changes in deformation temperature were investigated. The gradient heterogeneous structure of the alloys formed naturally under high hydrostatic pressure and severe shear stress, and its thickness increased with the deformation temperature. With the application of shear stress, a large amount of rotational dynamic recrystallization (RDRX) behavior occurs in the alloys, refining the coarse initial grains (∼126.3 µm) into fine grains (∼2.03 µm) or even ultrafine grains (∼1 µm). During the RDRX process, low angle grain boundaries (LAGBs) began to form at high distorted grain boundaries and unique lamellar structures, followed by a rapid expansion into the interior of the grains, which ultimately results in the grains being completely covered by subgrains. Meanwhile, the continuously broken long-period stacking-ordered (LPSO) phase and the precipitated bright rare earth rich (RE-rich) phase provide a large number of nucleation sites, further promoting the refinement process of the grains. Subsequently, the grains were further refined to nanocrystallines through the formation and rotation of subgrains under continuous loading of stress. The massive formation of nano-precipitated phases (β phases) along grain boundaries were accompanied by the complete disappearance of other types of second phases. The sources of β phases formation include the layer-by-layer decomposition of the cellular phases and the dissolution/re-precipitation of the LPSO phases. In addition, the introduction of shear stress promotes the random orientation of the DRXed grains through the extensive activation of pyramidal <a> and pyramidal <c+a> slip. The hardness of the alloys gradually decreased as the cumulative strain decreased at different deformation temperature conditions. When the deformation temperature was 440°C, the alloys reached a maximum hardness of 127.67 HV, which was nearly 43.5% higher than homogenized alloys. The ultra-high hardness of the alloys prepared by severe shear deformation is mainly attributed to grain boundary hardening, diffusion hardening and hetero-deformation induced (HDI) hardening.

Chitin-enriched insect frass fertilizer as a biorational alternative for root-knot nematode (Meloidogyne incognita) management.

Root-knot nematodes (Meloidogyne spp.) are serious pests of most food crops, causing up to 100% yield loss. Nevertheless, commercial nematicides are costly and harmful to the environment. While the nematicidal potential of crustacean and synthetic chitin has been demonstrated globally, research on the potential of insect-derived chitin for nematode control has received limited attention. Here, seven chitin-fortified black soldier fly frass fertilizer extracts (chFE) were assessed for their suppressiveness of Meloidogyne incognita and impacts on spinach growth in comparison with a commercial nematicide using in vitro and in vivo bioassays. The performance of chFE and control treatments was assessed by determining their effects on nematode egg hatchability; infective juvenile (J2) mortality and paralysis; number of galls, egg masses, and J2s per plant; and spinach root and shoot biomass. In vitro results showed that chFE and commercial nematicide suppressed nematode egg hatchability by 42% and 52%, respectively, relative to the control (sterile distilled water). Up to 100% paralysis was achieved when M. incognita J2s were exposed to either chFE or commercial nematicide. Further, the J2 mortality achieved using chFE (95%) was comparable to the value achieved using commercial nematicide (96%); in all treatments, mortality increased with exposure time. Similarly, up to 85% suppression of gall development was achieved when spinach plants were grown in soil drenched with chFE; up to 79% reduction in egg mass formation and 68% suppression of J2 development in the root system were achieved using chFE. Also, chFE application significantly increased spinach root and shoot biomass by 54%-74% and 39%-58%, respectively, compared to commercial nematicide. Our findings demonstrate the nematicidal potential of chFE and its benefits on crop production. Thus, chFE could be considered as a promising multipurpose, regenerative, and cost-effective input for sustainable management of plant-parasitic nematodes and enhancement of crop yield.

(026) Application of Gelatin Sponge as a Hemostatic Agent in Penile Prosthesis Implantation

Abstract Introduction Gelfoam® Sterile Compressed Sponge is a hemostatic that is directly applied to bleeding surfaces. This cost-effective hemostatic agent is prepared from purified porcine skin, Gelatin granules and Water for Injection. It is water insoluble, however is completely absorbed within 4–6 weeks with minimal scar formation. Gelfoam is available sterile for intra-operative use, and is applied in a multitude of surgical specialties. Objective In this work, we demonstrate for the first time the of Gelfoam to minimize the risk of bleeding in penile prosthesis implantation. Methods Eight cases received a three-piece inflatable implant (Rigicon Infla10®) through a peno-scrotal incision. Following cylinder insertion, corporotomies were closed by tying the stay sutures rather than water-tight sewing. Gelfoam was soaked in antibiotic-supplemented saline. Air bubbles were squeezed out followed by soaking. Gelfoam was then applied to the corporotomies, pump space and entry rout to the reservoir space. It was secured over the corporotomies by closing a pre-fashioned layer of Buck’s fascia. A suction drain was inserted. Mummy wrap was not used. Drain output was monitored and complications recorded. Results In two cases, drain output was an average of 80 cc’s in the first 24 hours, then 20 cc’s in the following 24 hours. However, in 6 cases, drain output was an average of 18 cc’s in the first 24 hours, mostly sero-sanguinous, then none in the following 24 hours. No cases of hematoma formation, infection, foreign body reaction, mass formation or hypersensitivity reaction were encountered. Conclusions The initial results of the current small case series demonstrate that Gelfoam is well-tolerated in penile surgeries, with possible value at minimizing post-operative bleeding, encouraging a multi-center larger study. Disclosure No.

Tumor growth for remodeling process: A 2D approach

This paper aims to present a comprehensive framework for coupling tumor-bone remodeling processes in a 2-dimensional geometry. This is achieved by introducing a bio-inspired damage that represents the growing tumor, which subsequently affects the main populations involved in the remodeling process, namely, osteoclasts, osteoblasts, and bone tissue. The model is constructed using a set of differential equations based on the Komarova’s and Ayati’s models, modified to incorporate the bio-inspired damage that may result in tumor mass formation. Three distinct models were developed. The first two models are based on the Komarova’s governing equations, with one demonstrating an osteolytic behavior and the second one an osteoblastic model. The third model is a variation of Ayati’s model, where the bio-inspired damage is induced through the paracrine and autocrine parameters, exhibiting an osteolytic behavior. The obtained results are consistent with existing literature, leading us to believe that our in-silico experiments will serve as a cornerstone for paving the way towards targeted interventions and personalized treatment strategies, ultimately improving the quality of life for those affected by these conditions.

ALMA-LEGUS. II. The Influence of Subgalactic Environments on Molecular Cloud Properties

We compare the molecular cloud properties in subgalactic regions of two galaxies, barred spiral NGC 1313, which is forming many massive clusters, and flocculent spiral NGC 7793, which is forming significantly fewer massive clusters despite having a similar star formation rate to NGC 1313. We find that there are larger variations in cloud properties between different regions within each galaxy than there are between the galaxies on a global scale, especially for NGC 1313. There are higher masses, line widths, pressures, and virial parameters in the arms of NGC 1313 and the center of NGC 7793 than in the interarm and outer regions of the galaxies. The massive cluster formation of NGC 1313 may be driven by its greater variation in environment, allowing more clouds with the necessary conditions to emerge, although no one parameter seems primarily responsible for the difference in star formation. Meanwhile NGC 7793 has clouds that are as massive and have as much kinetic energy as the clouds in the arms of NGC 1313, but have densities and pressures more similar to those in the interarm regions and so are less inclined to collapse and form stars. The cloud properties in NGC 1313 and NGC 7793 suggest that spiral arms, bars, interarm regions, and flocculent spirals each represent distinct environments with regard to molecular cloud populations. We see surprisingly little difference in surface density between the regions, suggesting that the differences in surface densities frequently seen between arm and interarm regions in lower-resolution studies are indicative of the sparsity of molecular clouds, rather than differences in their true surface density.

ALMA-LEGUS. I. The Influence of Galaxy Morphology on Molecular Cloud Properties

We present a comparative study of the molecular gas in two galaxies from the Legacy ExtraGalactic UV Survey (LEGUS) sample: barred spiral NGC 1313 and flocculent spiral NGC 7793. These two galaxies have similar masses, metallicities, and star formation rates, but NGC 1313 is forming significantly more massive star clusters than NGC 7793, especially young massive clusters (<10 Myr, >104 M ⊙). Using Atacama Large Millimeter/submillimeter Array (ALMA) CO(2–1) observations of the two galaxies with the same sensitivity and resolution (13 pc), we directly compare the molecular gas in these two similar galaxies to determine the physical conditions responsible for their large disparity in cluster formation. By fitting size–line width relations for the clouds in each galaxy, we find that NGC 1313 has a higher intercept than NGC 7793, implying that its clouds have higher kinetic energies at a given size scale. NGC 1313 also has more clouds near virial equilibrium than NGC 7793, which may be connected to its higher rate of massive cluster formation. However, these virially bound clouds do not show a stronger correlation with young clusters than with the general cloud population. We find surprisingly small differences between the distributions of molecular cloud populations in the two galaxies, though the largest of those differences is that NGC 1313 has higher surface densities and lower freefall times.

Unveiling Luminous Lyα Emitters at z ≈ 6 through JWST/NIRCam Imaging in the COSMOS Field

We study a sample of 14 spectroscopically confirmed Lyα emitters (LAEs) in the late era of reionization (at redshift z ≈ 6) based on the JWST/NIRCam imaging data set. These LAEs with high Lyα luminosity of L(Lyα) ∼1042.4–1043.4 erg s−1 have been covered by the (ongoing) COSMOS-Web survey over 0.28 deg2 in four NIRCam bands (F115W, F150W, F277W, and F444W). With JWST/NIRCam imaging, we determine the UV continua with M UV ranging from −20.5 to −18.5 mag. The UV slopes have a median value of β ≈ −2.35, and the steepest slopes can reach β < −3. Under the excellent spatial resolution of JWST, we identify three objects in the sample as potential merging/interacting systems. The 14 LAEs (and their components) are compact in morphology, residing substantially below the mass–size relation of high-z galaxies. We further investigate their physical properties, including the stellar mass (M *) and star formation rates (SFRs). Most of the LAEs lie on the SFR–M * main-sequence relation, while two of them, featured as “little red dots,” likely host active galactic nuclei (AGNs), implying a ∼10% AGN fraction. Moreover, we reveal that a new correlation may exist between Lyα equivalent width and the offset between Lyα and UV emission (Δd Lyα ), with a median Δd Lyα ∼ 1 kpc. This could be explained by the Lyα radiative transfer process in both the interstellar medium and circumgalactic medium. The results usher in a new era of detailed analysis on high-z LAEs with the JWST capability.

A comparative study of the fundamental metallicity relation

Aims. We aim to investigate the influences on the evolution of the fundamental metallicity relation of different selection criteria. Methods. We used 5 487 star-forming galaxies at a median redshift of z ≈ 0.63 extracted from the VIMOS Public Extragalactic Redshift Survey (VIPERS) and 143 774 comparison galaxies in the local Universe from the GALEX-SDSS-WISE Legacy Catalog. We employed two families of methods: parametric and nonparametric. In the parametric approaches, we compared the fundamental metallicity relation projections plagued by observational biases on differently constructed control samples at various redshifts. Then, we compare the metallicity difference between different redshifts in stellar mass-star formation rate bins. In the nonparametric approach, we related the metallicity and the normalized specific star formation rate (sSFR). To compare galaxies with the same physical properties, we normalized the sSFR of our samples according to the median value at median redshift z ≈ 0.09. Then, the galaxies with the same distance from the star-forming main sequence at their respective redshifts were compared when the sSFR is normalized according to the expected values from their respective star-forming main sequences. Results. The methodologies implemented to construct fair, complete samples for studying the mass-metallicity relation and the fundamental metallicity relation produced consistent results showing a small but still statistically significant evolution of both relations up to z ≈ 0.63. In particular, we observed a systematic trend where the median metallicity of the sample at z = 0.63 is lower than that of the local sample at the same stellar mass and star formation rate. The average difference in the metallicity of the low and intermediate redshifts is approximately 1.8 times the metallicity standard deviation of the median of the intermediate redshift sample in stellar mass-star formation rate bins. We confirmed this result using the Kolmogorov-Smirnov test. When we applied the stellar mass-completeness criterion to catalogs, the metallicity difference in redshifts decreased to approximately 0.96 times the metallicity standard deviation of the median, and thus it was not statistically significant. The limited area of the FMR surface explored once the stellar mass-completeness criterion is applied might dominate this difference reduction, leaving out the area where the difference between the two samples is the highest. A careful reading of the results and their underlying selection criteria is crucial in studies of the mass-metallicity and fundamental metallicity relations. Conclusions. When studying the mass-metallicity and fundamental metallicity relations, we recommend using the nonparametric approach, which provides similar results compared to parametric prescriptions, is easier to use, and is clear to interpret. The nonparametric methodology provides a convenient way to compare physical properties, with a smaller impact on observational selection biases.

Cosmic Vine: A z = 3.44 large-scale structure hosting massive quiescent galaxies

We report the discovery of a large-scale structure at z = 3.44 revealed by JWST data in the Extended Groth Strip (EGS) field. This structure, called the Cosmic Vine, consists of 20 galaxies with spectroscopic redshifts at 3.43 &lt; z &lt; 3.45 and six galaxy overdensities (4 − 7σ) with consistent photometric redshifts, making up a vine-like structure extending over a ∼4 × 0.2 pMpc2 area. The two most massive galaxies (M* ≈ 1010.9 M⊙) of the Cosmic Vine are found to be quiescent with bulge-dominated morphologies (B/T &gt; 70%). Comparisons with simulations suggest that the Cosmic Vine would form a cluster with halo mass Mhalo &gt; 1014 M⊙ at z = 0, and the two massive galaxies are likely forming the brightest cluster galaxies (BCGs). The results unambiguously reveal that massive quiescent galaxies can form in growing large-scale structures at z &gt; 3, thus disfavoring the environmental quenching mechanisms that require a virialized cluster core. Instead, as suggested by the interacting and bulge-dominated morphologies, the two galaxies are likely quenched by merger-triggered starburst or active galactic nucleus (AGN) feedback before falling into a cluster core. Moreover, we found that the observed specific star formation rates of massive quiescent galaxies in z &gt; 3 dense environments are one to two orders of magnitude lower than that of the BCGs in the TNG300 simulation. This discrepancy potentially poses a challenge to the models of massive cluster galaxy formation. Future studies comparing a large sample with dedicated cluster simulations are required to solve the problem.

Antimatter Enigma Solved: Astronomical Data Allows Identification of 77 Supermassive Antimatter Black Holes and 23 Antimatter Galaxies.

Initial results from the Alpha-CERN antihydrogen experiment indicate no discernible difference in the gravitational behavior between matter and antimatter, challenging CP violation models. Given that antimatter exhibits the same gravitational behavior as matter, distinguishing between a supermassive black hole (SMBH) composed of matter and an antimatter supermassive black hole (ASMBH) becomes challenging, as their gravitational effects are indistinguishable. This raises the question: Could the SMBH in the Milky Way, and all observed spiral galaxies, potentially be an ASMBH, with its event horizon concealing the equivalent number of antimatter particles, thereby preventing matter-antimatter destruction within a matter galaxy? This article assesses astronomical data comparing the mass of 100 SMBHs with their host galaxies. A theoretical value for the logarithmic mass relationship Log( MStellar /MSMBH ) is presented: 2.963 for ASMBHs situated in matter galaxies, and 2.285 for MSBHs in antimatter galaxies. This relationship, derived from the Ulianov Theory, is based on the premise of matter galaxy formation from protons and electrons expelled by ASMBHs during cosmic inflation. The same theory also posits antimatter galaxy formation from antiprotons and positrons released by matter SMBHs during this period. The database analysis (of 100 galaxies and their respective SMBHs) revealed that 77% of the SMBHs are composed of antimatter, resulting in a logarithmic relationship value of (2.945 ± 0.018) for the Log(MStellar/MASMBH ), while 23% are composed of matter, resulting in a value of (2.267 ± 0.036) for the Log( MAStellar/MSMBH). The congruence between these values and the theoretical prediction is likely not mere coincidence. A thorough examination of the results confirms the model's validity and underscores the precision of astronomers' mass measurements, with only 3 cases showing actual measurement errors beyond the predicted range. This discovery is pivotal, as it suggests the Ulianov Theory's potential to produce novel predictions, such as this model. Originating from a cold and empty universe, this model outlines the galaxy mass formation process, in which ASMBHs harness energy from cosmic inflation, converting it into matter and antimatter particles. This process is termed the "Small Bang" model by the author, reflecting its cold and gradual nature, contrasting the explosive nature of the "Big Bang".

COOL-LAMPS. VI. Lens Model and New Constraints on the Properties of COOL J1241+2219, a Bright z = 5 Lyman Break Galaxy and its z = 1 Cluster Lens

We present a strong lensing analysis of COOL J1241+2219, the brightest known gravitationally lensed galaxy at z ≥ 5, based on new multiband Hubble Space Telescope (HST) imaging data. The lensed galaxy has a redshift of z = 5.043, placing it shortly after the end of the “Epoch of Reionization,” and an AB magnitude z AB = 20.47 mag (Khullar et al.). As such, it serves as a touchstone for future research of that epoch. The high spatial resolution of HST reveals internal structure in the giant arc, from which we identify 15 constraints and construct a robust lens model. We use the lens model to extract the cluster mass and lensing magnification. We find that the mass enclosed within the Einstein radius of the z = 1.001 cluster lens is M(<5.″77)=1.079−0.007+0.023×1013M☉ , significantly lower than other known strong lensing clusters at its redshift. The average magnification of the giant arc is 〈μ arc〉 = 76−20+40 , a factor of 2.4−0.7+1.4 greater than previously estimated from ground-based data; the flux-weighted average magnification is 〈μ arc〉 = 92−31+37 . We update the current measurements of the stellar mass and star formation rate (SFR) of the source for the revised magnification to log(M⋆/M⊙)= 9.7 ± 0.3 and SFR = 10.3−4.4+7.0 M ⊙ yr−1, respectively. The powerful lensing magnification acting upon COOL J1241+2219 resolves the source and enables future studies of the properties of its star formation on a clump-by-clump basis. The lensing analysis presented here will support upcoming multiwavelength characterization with HST and JWST data of the stellar mass assembly and physical properties of this high-redshift lensed galaxy.

A post-merger enhancement only in star-forming Type 2 Seyfert galaxies: the deep learning view

ABSTRACT Supermassive black holes require a reservoir of cold gas at the centre of their host galaxy in order to accrete and shine as active galactic nuclei (AGN). Major mergers have the ability to drive gas rapidly inwards, but observations trying to link mergers with AGN have found mixed results due to the difficulty of consistently identifying galaxy mergers in surveys. This study applies deep learning to this problem, using convolutional neural networks trained to identify simulated post-merger galaxies from survey-realistic imaging. This provides a fast and repeatable alternative to human visual inspection. Using this tool, we examine a sample of ∼8500 Seyfert 2 galaxies ($L[\mathrm{O\, {\small III}}] \sim 10^{38.5 - 42}$ erg s−1) at z &amp;lt; 0.3 in the Sloan Digital Sky Survey and find a merger fraction of $2.19_{-0.17}^{+0.21}$ per cent compared with inactive control galaxies, in which we find a merger fraction of $2.96_{-0.20}^{+0.26}$ per cent, indicating an overall lack of mergers among AGN hosts compared with controls. However, matching the controls to the AGN hosts in stellar mass and star formation rate reveals that AGN hosts in the star-forming blue cloud exhibit a ∼2 × merger enhancement over controls, while those in the quiescent red sequence have significantly lower relative merger fractions, leading to the observed overall deficit due to the differing M*–SFR distributions. We conclude that while mergers are not the dominant trigger of all low-luminosity, obscured AGN activity in the nearby Universe, they are more important to AGN fuelling in galaxies with higher cold gas mass fractions as traced through star formation.

Cold quasar investigation: comparing star formation rates to black hole growth

ABSTRACT Cold quasars are a rare population of luminous, unobscured quasars associated with host galaxies that have a high star formation rate. We aimed to study the host galaxies of 64 of these cold quasars in order to probe how the supermassive black holes and host galaxies were co-evolving. We compiled data from the XMM-XXL survey and cross-matched with the VHS, WISE, and HerMES surveys to obtain multiwavelength photometry spanning the X-ray to the infrared and including optical spectroscopy. From the data, we calculated the supermassive black hole’s mass using broad emission from the Mg ii and Hbeta lines. We compared this with the stellar mass of the entire galaxy and found that the black holes are significantly more massive than would be predicted by local relations, indicating that the majority of black hole growth precedes the bulk of the the stellar mass formation. In addition to this, we created a spectral energy distribution for each galaxy to calculate the star formation rate. We compared the star formation rate with the black hole accretion rate and find that the stellar mass is rapidly increasing at a relative rate faster than the black hole growth, supporting the picture where the black hole grows first.

Brain-Decellularized ECM-Based 3D Myeloid Sarcoma Platform: Mimicking Adaptive Phenotypic Alterations in the Brain.

Leukemia circulates in the bloodstream and induces various symptoms and complications. Occasionally, these cells accumulate in non-marrow tissues, forming a tumor-like myeloid sarcoma (MS). When the blast-stage leukemia cells invade the brain parenchyma, intracranial MS occurs, leading to a challenging prognosis owing to the limited penetration of cytostatic drugs into the brain and the development of drug resistance. The scarcity of tissue samples from MS makes understanding the phenotypic changes occurring in leukemia cells within the brain environment challenging, thereby hindering development of effective treatment strategies for intracranial MS. This study presents a novel 3D in vitro model mimicking intracranial MS, employing a hydrogel scaffold derived from the brain-decellularized extracellular matrix in which suspended leukemia cells are embedded, simulating the formation of tumor masses in the brain parenchyma. This model reveals marked phenotypic changes in leukemia cells, including altered survival, proliferation, differentiation, and cell cycle regulation. Notably, proportion of dormant leukemia stem cells increases and expression of multidrug resistance genes is upregulated, leading to imatinib resistance, mirroring the pathological features of in vivo MS tissue. Furthermore, suppression of ferroptosis is identified as an important characteristic of intracranial MS, providing valuable insights for the development of targeted therapeutic strategies.

(217) Revitalizing Penile Health: Advanced Surgical Approach for Treating Penile Mass Formation Resulting from Neglected Fractures, Enhanced with Pericardial Graft Reinforcement

Abstract Introduction Penile fractures are rare but serious emergencies caused by the rupture of the tunica albuginea during sexual activity. Prompt medical attention is crucial to prevent complications like erectile dysfunction, penile curvature, and hematoma. Delayed reporting due to embarrassment or fear can lead to further complications. Diagnosing penile fractures primarily relies on clinical examination, and treatment options depend on the timing of presentation. Seeking immediate medical help is vital to prevent long-term complications and ensure proper management. Objective To emphasize the importance of early medical attention and surgical intervention in the context of penile fractures, with the aim of preventing or reducing the occurrence of long-term complications. Methods This case report involves a 55-year-old male who experienced a penile fracture during intercourse. Initially, he had no hematoma, bruising, pain, or loss of erection. Two weeks later, he sought medical advice due to a penile bump and slightly painful erections. He was managed conservatively with ice, nonsteroidal anti-inflammatory medications, and abstinence from intercourse. Two months later, he presented to our clinic with complaints of a penile mass and curvature, affecting his erections and penetration. A penile Doppler ultrasound revealed a fibrotic hematoma with a complex cystic lesion measuring 23.1 mm × 18.1 mm × 28.3 mm on the right lateral mid-penile shaft. The patient underwent complex penile mass excision, tunica albuginea plication, and pericardium graft reinforcement. During the surgery, scar tissue and underlying fibrotic hematoma were removed (Figure 1). A complex cystic lesion on the right lateral mid-penile shaft was also excised (Figure 2). A tunica albuginea plication corrected the 30° left dorsal curvature. A pericardium graft (Tutoplast®, IOP Ophthalmics, Costa Mesa, CA, USA) reinforced the weakened tunica albuginea and covered the defect (Figure 3). Histopathology of the mass reported “a penile fibrotic mass, measuring 2 cm × 1.8 cm × 2.6 cm with an irregular dark brown firm cystic structure filled with yellow-tan necrotic tissue.” Microscopic description showed “a fibrous capsule with central hemorrhage and fibrin.” Results The patient had a successful procedure and smooth recovery. At 6- and 9-month follow-up, he expressed satisfaction with no complications or long-term side effects. Erectile function was restored, and penile curvature resolved, enabling satisfactory penetrative intercourse. Surgical treatment is recommended for achieving satisfactory results and restoring sexual function in penile fractures. Various graft materials can be used to reinforce penile defects. Tutoplast® (processed allograft tissue from cadaveric pericardium) has shown excellent results in Peyronie's curvature repair, but the efficacy of bovine pericardium remains uncertain. In this case, Tutoplast® was chosen for its accessibility and the surgeons' expertise in Peyronie's repair and penile prosthesis implantation, ensuring the best possible outcome. Conclusions This case report highlights fibrotic hematoma due to delayed penile fracture presentation, managed through mass excision and curvature correction. Currently, there is no literature available that discusses fibrotic hematoma formation from delayed penile fractures. Prompt medical attention crucial to avoid long-term complications. Early surgical management prevents erection loss, curvature, hematoma, or mass formation, improving quality of life for patients with penile fractures. Disclosure No.