Stages Of Evolution Research Articles

Model-free detection and quantitative assessment of micro short circuits in lithium-ion battery packs based on incremental capacity and unsupervised clustering

Timely diagnosis of micro short circuit (MSC) faults is crucial for ensuring the safe operation of lithium-ion battery energy storage systems. Existing diagnostic methods face limitations such as high dependency on battery models, difficulty in determining accurate diagnostic thresholds, or low computational efficiency. This work presents a model-free approach for the detection and quantitative assessment of MSCs in lithium-ion battery packs, with incremental capacity (IC) and unsupervised clustering. First, the IC is extracted from charging voltage data to effectively characterize MSC faults in lithium-ion batteries. Next, principal component analysis is used to map the high-dimensional feature space onto a two-dimensional plane to facilitate fault detection and result visualization. Then, an unsupervised clustering algorithm is employed for anomaly detection to identify MSC cells within the battery pack. For the detected MSC cells, a method based on the maximum charging voltage difference between adjacent cycles is designed to estimate the MSC resistance, quantitatively assessing the severity and evolution stage of the MSC. Experimental results show that the accuracy of MSC detection is 99.17 % and the minimum relative error of short-circuit resistance estimation is 1.20 %, which demonstrates the effectiveness and feasibility of the proposed method.

Abstract IA-01: Targeting autophagy in pancreatic cancer

Abstract Pancreatic ductal adenocarcinoma (PDAC) is one of the most vexing problems in cancer with 5-year overall survival rates of 13%, thus there is a need for new therapeutic targets. PDAC have a distinct dependence on autophagy, a conserved eukaryotic catabolic pathway that serves to degrade proteins, other macromolecules, and organelles via the lysosome as part of a recycling process to maintain cellular homeostasis during basal and stress conditions. The unique importance of autophagy in PDAC suggests that there may be a subset of proteins that are specifically targeted by autophagy for degradation, which would promote proliferation and survival, and that these may represent new targets for therapy. Using a quantitative PDAC cellular autophagosomal proteomics approach, we identified NCOA4 as the autophagy receptor for ferritin, the cellular iron storage complex, and demonstrated that ferritin autophagy (ferritinophagy) is a highly regulated process and plays a central role in the larger context of cellular and organismal iron homeostasis. Given the reliance of PDAC, on both high levels of autophagy as well as iron, we studied the role of NCOA4 and ferritinophagy in PDAC thereby identifying NCOA4-mediated ferritinophagy and more broadly lysosomal iron metabolism as a PDAC dependency and therapeutic target. We recently determined the cryo-EM structure of the NCOA4-Ferritin complex for future drug design. To identify the role of autophagy and the lysosome in PDAC metastatic progression, we co-developed an in vivo capable lysosomal enrichment that enables capture and proteomic profiling of lysosomes at different stages of tumor evolution, including early stage, late stage, and metastatic disease. Employing this strategy, we successfully captured lysosomal proteins from primary tumors (pancreas), as well as lung and liver metastases. Our preliminary analysis revealed an enrichment of resident lysosomal membrane and luminal proteins in the datasets, confirming successful isolation of intact lysosomes from these complex tissues. Additionally, we identified non-resident lysosomal proteins (termed cargo) that are enriched and co-evolve with advancing tumor stages. Notably, our results reveal distinct differences in the lysosomal proteome of tumor cells across different tissues. These findings emphasize the critical role of lysosomal function in tumor progression and suggest that targeting lysosomal components could be a promising therapeutic strategy for treating metastatic PDAC. Finally, given the challenging pharmacokinetic and pharmacodynamic properties and limited clinical efficacy of hydroxychloroquine as an autophagy/lysosomal inhibition strategy, we are now exploring novel autophagy inhibition strategies in PDAC to effectively target this pathway for clinical benefit. Citation Format: Joseph D. Mancias. Targeting autophagy in pancreatic cancer [abstract]. In: Proceedings of the AACR Special Conference in Cancer Research: Advances in Pancreatic Cancer Research; 2024 Sep 15-18; Boston, MA. Philadelphia (PA): AACR; Cancer Res 2024;84(17 Suppl_2):Abstract nr IA-01.

A Late Devonian coelacanth reconfigures actinistian phylogeny, disparity, and evolutionary dynamics

The living coelacanth Latimeria (Sarcopterygii: Actinistia) is an iconic, so-called ‘living fossil’ within one of the most apparently morphologically conservative vertebrate groups. We describe a new, 3-D preserved coelacanth from the Late Devonian Gogo Formation in Western Australia. We assemble a comprehensive analysis of the group to assess the phylogeny, evolutionary rates, and morphological disparity of all coelacanths. We reveal a major shift in morphological disparity between Devonian and post-Devonian coelacanths. The newly described fossil fish fills a critical transitional stage in coelacanth disparity and evolution. Since the mid-Cretaceous, discrete character changes (representing major morphological innovations) have essentially ceased, while meristic and continuous characters have continued to evolve within coelacanths. Considering a range of putative environmental drivers, tectonic activity best explains variation in the rates of coelacanth evolution.

Evolving governance in the space sector: From Legacy Space to New Space models

The space sector is evolving from the “Legacy Space” to the “New Space”. Along with the space sector, space program governance is transitioning to support an environment where legacy and New Space actors co-exist. The aforementioned transitions and the entry of New Space players result in new governance models, as space agencies aim to exploit contributions from non-space sectors, leveraging on collaborative opportunities.Public-private partnerships (PPPs) become a new golden rule, disclosing unprecedented achievements.However, the existing body of knowledge lacks a framing of models of space program governance, covering both Legacy Space programs and New Space ones. It is not clear how the roles and responsibilities of stakeholders change from the Legacy Space to the New Space, alongside the related changes in contract structures and the practices space agencies favour in current space programs and projects. Therefore, our paper aims to investigate how space program governance evolved.We performed a single-case study on NASA-led space exploration programs to investigate the transition of space program governance and its actual state-of-the-art. We co-developed and validated three governance models for space programs through semi-structured interviews with senior experts. Furthermore, we present key drivers and barriers behind the evolution towards New Space governance models.We found and discussed three program governance models corresponding to the evolutionary stages of space exploration programs. In the Legacy Space model, the government owns space infrastructures to demonstrate technological supremacy. In the Transitional model, lumpsum contracts, transitioning between cost-plus and fixed-price, replace the legacy EPC (Engineering, Production, Construction) ones. In the New Space model, collaborative efforts and PPPs enable alignment between public and private expertise. Finally, we examine the factors that promote and impede the evolution of space governance, leading to the emergence of a polycentric governance structure observed in current space programs.The three models enable managers to visualize space programs from a governance perspective, where stakeholders’ roles and responsibilities in PPPs are clearly identified. Moreover, managers can leverage and innovate existing practices for transitioning across different models of governance in space programs and projects.We contribute to research by introducing a transitional governance model that enables the smooth transition between the Legacy Space and the New Space paradigms. We justify the concurrent adoption of multiple governance models within the same space program, as in the current Artemis program.

The Styrian Basin: an overview with new insights from seismic data

The Neogene Styrian Basin is the westernmost subbasin of the Pannonian Basin System. The last comprehensive studies on the basin were published in the last millennium. This overview of the current understanding of basin evolution is based on the re-interpretation of partly unpublished reflection seismic data and a wealth of sedimentological and stratigraphic studies performed during the last 25 years. Reflection seismic data indicate the presence of a major E to SE dipping detachment horizon within the pre-Neogene basement reflecting high-strain upper crustal extension during the early Miocene syn-rift stage of basin evolution. Fault block rotations caused subsidence in several subbasins, which developed often with marked asymmetric geometry. The maximum basin depth exceeds 4 km (Gnas Basin). Syn-rift deposits include thick alluvial fan and fan delta sediments overlain in the basin center by deeper marine pelitic rocks. Subduction-related magmatic activity commenced during the syn-rift stage and continued into the middle to late Miocene post-rift stage. Syn- and post-rift sediments are separated by the middle Miocene “Styrian Unconformity”. Shallow marine sedimentation, controlled by third- and fourth-order sea-level variations, prevailed during the early post-rift stage. The final stage of basin evolution was characterized by differential surface uplift, erosion, and Pliocene-Pleistocene basaltic magmatism.

Photographic scale for the characterization of actinic keratosis through reflectance confocal microscopy: a quantitative approach to cellular transformation.

Actinic keratosis (AK) is a highly prevalent pre-cancerous skin lesion that often leads to cutaneous squamous cell carcinoma. There are different stages of evolution of the disease and several features that characterize keratosis. This study aimed to develop a qualitative and quantitative visual diagnostic tool to facilitate the identification of the characteristics and severity of the main cellular attributes of AK and to show its applicability in evaluating the evolution or treatment through image analysis. Literature research on the main scientific databases and in the institute's database was carried out to gather all the different levels of cellular transformation. To validate the scale, a preliminary characterization study was carried out with 21 subjects who had clinically diagnosed AK lesions to classify the attributes in each skin layer and test the accuracy of the diagnosis of the scale. Afterward, and to show the possibility of a follow-up with a topical treatment, the subjects were divided into two treatment groups, receiving either a cream formulation containing retinoic acid, or a placebo formula. The evaluation was carried out through confocal reflectance microscopy and a digital camera with dermoscopic quality before and after 90 days of treatment. A table detailing the 18 attributes of AK, and a photographic scale containing RCM images graded by scores established for each characteristic and the frequency of spreading were developed. The results of the validation presented good repeatability, correlation with clinical evaluation, and capacity for differentiating treatments demonstrated by the significant improvement after topical treatment by the reduction of the score for 10 out of the 18 attributes. The preliminary study, evaluated by the detailed transformation scale highlights important differences in the subclinical approach that allows a deeper evaluation of the aspects of the lesion's re-incidence even after fully treated skin sites. This study brings an innovative method based on RCM, to assist in the quantification of cell transformation level, provide early diagnosis, and deliver a powerful treatment evaluation tool to provide smoother treatment, as well as prevent re-incidence in the cases.

A dual-adaptive directed genetic algorithm for construction scheduling

The precise and efficient generation of construction sequences is a crucial concern within the engineering field. However, the formulation of construction schedules heavily depends on the expertise and proficiency of project planners, leading to significant potential for inefficiencies and instability in project management. To deal with this challenge, this study automatically extracts constructability constraints from 3D models and proposes a dual-adaptive directed genetic algorithm (DADGA) to generate a structurally stable installation sequence. The proposed algorithm adaptively changes both the crossover and mutation probabilities based on the quality of individuals and evolutionary stages. In addition, the idea of directionality and the chief strategy artificially controls the direction of evolution, which greatly improves the efficiency and robustness of local search. The results of comparison experiments demonstrate that the DADGA outperforms the traditional genetic algorithm in terms of both efficiency and accuracy, and a practical example is also presented to showcase the capability of the DADGA in solving ultra-complicated construction scheduling problems.

Breaching of sand dikes: assessment of 1D and 2D numerical models against laboratory experiments

Dike failures often induce highly damaging floods. Improved understanding of the inherent mechanisms is important to predict and prevent dike failures. This research focuses on sand dike failure by overtopping. During the experiments, the evolution of nine sections was monitored using laser-sheet while the water level in the upstream reservoir was captured using ultrasonic gauges. The impact of the grain size was studied by comparing a fine and a coarser sand. Even though the failure mechanisms look similar in both cases, some differences could be observed in the evolution of the geometry of the dike. Finally, the failure was simulated with 1D and 2D models. The 1D model shows good results for the initial stage of the dike evolution and in predicting the evolution of the width of the breach. The 2D model predicts the morphological evolution of the dike more accurately but slightly overestimates the widening of the breach.

The true nature of HE 0057-5959, the most metal-poor, Li-rich star

The Li-rich stars are a class of rare objects with a surface lithium abundance, A(Li), that exceeds that of other stars in the same evolutionary stage. The origin of these stars is still debated, and valuable routes to look at include the Cameron-Fowler mechanism, a mass-transfer process in a binary system, or the engulfment of rocky planets or brown dwarfs. Metal-poor ([Fe/H]<−1 dex) stars are only a small fraction of the entire population of Li-rich stars. We observed the metal-poor ([Fe/H]=−3.95±0.11 dex) giant star HE 0057–5959 with MIKE at the Magellan Telescope, deriving A(Li)NLTE=+2.09±0.07 dex. Such an Li abundance is significantly higher, by about 1 dex, than that of other stars at the same evolutionary stage. A previous analysis of the same target suggested that its high A(Li) reflects an ongoing first-dredge-up process. We revised the nature of HE 0057-5959 by comparing its stellar parameters and A(Li) with appropriate stellar evolution models describing Li depletion due to the deepening of the convective envelope. This comparison rules out that HE 0057-5959 is caught during its first dredge-up, the latter having already ended according to the parameters of this star. Its A(Li), remarkably higher than the typical lithium plateau drawn by similar giant stars, demonstrates that HE 0057-5959 joins the class of the rare metal-poor, Li-rich stars. HE 0057-5959 is the most metal-poor, Li-rich star discovered so far. We considered different scenarios to explain this star also comparing it with the other metal-poor, Li-rich stars. No internal mixing able to activate the Cameron-Fowler mechanism is known for metal-poor stars at this evolutionary stage. The engulfment of planets is also disfavoured because such metal-poor stars should not host planets. Finally, HE 0057-5959 is one of the most Na-rich among the Li-rich stars, and we found that a strong excess of Na abundance is common to all three Li-rich stars with [Fe/H]<–3 dex. This finding could support the scenario of mass transfer from a massive companion star (able to simultaneously produce large amounts of both elements) in a binary system, even if we found no evidence of radial velocity variations.

Magnetic properties of the umbral boundary during sunspot decay

Context. In recent years, the magnetic properties of the umbra-penumbra boundary of sunspots and the boundary of pores at various evolutionary stages have been characterised using datasets from different instruments. Aims. We aim to study the intrinsic differences between the intensity and vector magnetic field properties derived from Hinode/SP and SDO/HMI observations of a decaying sunspot. Methods. We analysed the sunspot embedded in active region NOAA 12797 during six days in 30 SP/Hinode scans and 704 HMI/SDO for both regular maps and maps corrected for scattered light, HMIdcon. We studied the correlation of the magnetic properties and continuum intensity in the datasets within the spot, and we investigated the differences at the umbra-penumbra boundary. We examined the decaying process in detail using the full temporal resolution of the HMIdcon maps. Results. We find a good one-to-one correspondence between the magnetic properties in the SP and HMIdcon maps, but the continuum intensity of the spots in the SP maps is found to be 0.04 IQS brighter than in the HMIdcon maps. The considerable influence of scattered light in the HMI maps makes it the least ideal dataset for studying the boundary of spots without a penumbra. The properties at the umbra-penumbra boundary evolve slowly during the sunspot decay stage, while the penumbra still provides some stability. In contrast, they respond more abruptly to areal changes in the naked-spot stage. During the sunspot decay, we find linear decay in the area and in the magnetic flux. Moreover, the umbra shows two characteristic decaying processes: a slow decay during the first three days, and a sudden fast decay during the final dissipation of the penumbra. We find indications of a 3.5 h lag between the dissipation of the vertical fields in the umbral region and the photometric decay of the umbral area. Conclusions. The differences found in the continuum intensity and in the vertical component of the magnetic field, Bver, between the analysed datasets explain the discrepancies among the Bver values found at the boundaries of umbrae in previous studies.

Double periodic variable V4142 Sgr: A key to approaching the stellar dynamo

Aims. In this work we focus on the double periodic variable (DPV) star V4142 Sgr, aiming to provide a deeper understanding of its evolution, the formation of its accretion disk, and the operation of magnetic dynamos within the donor star. We analyze its characteristics in detail as well as the phenomena associated with DPV stars more generally. Methods. The model was implemented using the stellar evolution code MESA r22.11.1. The modeling process starts from the zero age main sequence and incorporates differential rotation to facilitate the creation of a stellar dynamo in the donor star. We adjusted the model by employing a chi-square algorithm, minimizing the deviation between theoretical and observed values based on previously published fundamental parameters for this system. Our analysis includes an evaluation of various parameters, such as initial masses, orbital periods, mixing parameters, the thermohaline parameter, and metallicities. We assessed the algorithm convergence and set the stopping criterion at 20% helium core depletion in the donor star. A comprehensive analysis was conducted at each evolutionary stage, utilizing the Tayler–Spruit formalism to understand the mechanism of magnetic dynamos. Results. The model begins by adjusting fundamental parameters published for this system through a chi-squared optimization algorithm, adopting an initial orbital period of 15.0 days and initial masses for the donor and gainer star of Mi, d = 3.50 M⊙ and Mi, g = 1.50 M⊙, with a metallicity associated with this type of DPV of Z = 0.02. It successfully converges with six degrees of freedom and 5% confidence, resulting in a chi-squared value of 0.007. In addition, the best-fit model for V4142 Sgr shows it is in thermal-timescale mass transfer. Our analysis provides insights into the role of differential rotation in facilitating the formation of a stellar dynamo. Additionally, we have determined that our type-B gainer star is located in a region similar to other type-B DPVs that have undergone rejuvenation due to the transfer of matter. The size of the gainer star shrinks considerably, but it rejuvenates thanks to the material acquired from its donor companion. As for the donor star, the creation and amplification of magnetic fields are influenced by the mixing diffusivity, DST, which is activated by advection outside the overshooting zone.

SO2 and OCS toward high-mass protostars

Context. OCS and SO2 are both major carriers of gaseous sulfur and are the only sulfurated molecules detected in interstellar ices to date. They are thus the ideal candidates for exploring the evolution of the volatile sulfur content throughout the different stages of star formation. Aims. We aim to investigate the chemical history of interstellar OCS and SO2 by deriving a statistically significant sample of gas-phase column densities toward massive protostars and comparing them to observations of gas and ices toward other sources, from dark clouds to comets. Methods. We analyzed a subset of 26 line-rich massive protostars observed by ALMA in Band 6 as part of the High Mass Protocluster Formation in the Galaxy (ALMAGAL) survey. Column densities were derived for OCS and SO2 from their rare isotopologs O13CS and 34SO2 toward the compact gas around the hot cores. We compared the abundance ratios of gaseous OCS, SO2, and CH3OH with ice detections toward both high- and low-mass sources as well as dark clouds and comets. Results. We find that gas-phase column density ratios of OCS and SO2 with respect to methanol remain fairly constant as a function of luminosity between low- and high-mass sources, despite their very different physical conditions. In our dataset, OCS and SO2 are weakly correlated. The derived gaseous OCS and SO2 abundances relative to CH3OH are overall similar to protostellar ice values, with a significantly larger scatter for SO2 than for OCS. Cometary and dark-cloud ice values agree well with protostellar gas-phase ratios for OCS, whereas higher abundances of SO2 are generally seen in comets compared to the other sources. Gaseous SO2/OCS ratios are consistent with ices toward dark clouds, protostars, and comets, albeit with some scatter. Conclusions. The constant gas-phase column density ratios throughout low- and high-mass sources indicate an early-stage formation before intense environmental differentiation begins. Icy protostellar values are similar to the gas-phase medians and are compatible with an icy origin for these species followed by thermal sublimation. The larger spread in SO2 compared to OCS ratios with respect to CH3OH is likely due to a more water-rich chemical environment associated with the former, as opposed to a CO-rich origin for the latter. Post-sublimation gas-phase processing of SO2 can also contribute to the large spread. Comparisons to ices in dark clouds and comets point to a significant inheritance of OCS from earlier to later evolutionary stages.

Protostellar Disk Formation Regimes: Angular Momentum Conservation versus Magnetic Braking

Protostellar disks around young protostars exhibit diverse properties, with their radii ranging from less than ten to several hundred astronomical units. To investigate the mechanisms shaping this disk radius distribution, we compiled a sample of 27 Class 0 and I single protostars with resolved disks and dynamically determined protostellar masses from the literature. Additionally, we derived the radial profile of the rotational-to-gravitational-energy ratio in dense cores from the observed specific angular momentum profiles in the literature. Using these observed protostellar masses and rotational energy profile, we computed theoretical disk radii from the hydrodynamic and nonideal magnetohydrodynamic (MHD) models in Y.-N. Lee et al. and generated synthetic samples to compare with the observations. In our theoretical model, the disk radii are determined by hydrodynamics when the central protostar+disk mass is low. After the protostars and disks grow and exceed certain masses, the disk radii become regulated by magnetic braking and nonideal MHD effects. The synthetic disk radius distribution from this model matches well with the observations. This result suggests that hydrodynamics and nonideal MHD can be dominant in different mass regimes (or evolutionary stages), depending on the rotational energy and protostar+disk mass. This model naturally explains the rarity of large (>100 au) disks and the presence of very small (<10 au) disks. It also predicts that the majority of protostellar disks have radii of a few tens of astronomical units, as observed.

Discs are born eccentric

Context. Recent observations have begun probing the early phases of disc formation, but little data yet exists on disc structure and morphology of Class 0 objects. Using simulations, we are able to lay out predictions of disc morphologies expected in future surveys of young discs. Based on detailed simulations of ab initio star formation by core collapse, we predict that early discs must be eccentric. Aims. In this Letter, we study the morphology and, in particular, the eccentricity of discs formed in non-ideal magnetohydrodynamic (MHD) collapse simulations. We attempt to show that discs formed by cloud collapse are likely to be eccentric. Methods. We ran non-ideal MHD collapse simulations in the adaptive mesh refinement code RAMSES with radiative transfer. We used state-of-the-art analysis methods to measure the disc eccentricity. Results. We find that despite no asymmetry in the initial conditions, the discs formed are eccentric, with eccentricities on the order of 0.1. Conclusions. These results may have important implications for protoplanetary disc dynamics and planet formation. The presence of eccentricity in young discs that is not seen at later stages of disc evolution is in tension with current viscous eccentricity damping models. This implies that there may be an as-yet undiscovered circularisation mechanism in circumstellar discs.

Cultural Moral Evolution: A Proposed Model and Application in a Review and Analysis of the Evolutionary Stages of Diverse Cultures and the Impact on the Emergence and Identification of LGBTQA+ Communities

Abstract The authors present a five-part initial examination of cultural moral evolution in several diverse cultures, looking specifically at attitudes towards LGBTQA+ communities and scrutinizing how societal attitudes shift from fear, animus, tolerance, and acceptance to integration. This evolution is gauged through various societal lenses, including laws, religion, human rights, and educational practices. In Part One, the authors discuss the concept of cultural moral evolution and how it differs from and shares some of the same traits as cultural anthropology. Part Two explores cultural moral evolution towards LGBTQA+ communities in three countries: Malaysia, the Netherlands, and Saudi Arabia. Part Three extends this analysis to four US states – Florida, Alaska, Hawaii, and Colorado. Part Four focuses on the US military, particularly the US Navy, analysing its cultural moral evolution towards the LGBTQA+ community. Finally, these observations are synthesized, with a summary of how the cultural moral evolution model is applied across different societal segments.

Resolving Twin Jets and Twin Disks with JWST and ALMA: The Young WL 20 Multiple System

We report the discovery of jets emanating from pre-main-sequence objects exclusively at mid-infrared wavelengths, enabled by the superb sensitivity of JWST’s Mid-Infrared Instrument Medium-Resolution Spectrometer. These jets are observed only in lines of [Ni ii], [Fe ii], [Ar ii], and [Ne ii]. The H2 emission, imaged in eight distinct transitions, has a completely different morphology, exhibiting a wide-angled, biconical shape, symmetrically distributed about the jet axes. Synergistic high-resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations resolve a pair of side-by-side edge-on accretion disks lying at the origin of the twin mid-infrared jets. Assuming coevality of the components of the young multiple system under investigation, the system age is at least (2–2.5) × 106 yr, despite the discrepantly younger age inferred from the spectral energy distribution of the combined edge-on disk sources. The later system evolutionary stage is corroborated by ALMA observations of CO(2−1), 13CO(2−1), and C18O(2−1), which show no traces of molecular outflows or remnant cavity walls. Consequently, the observed H2 structures must have their origins in wide-angled disk winds, in the absence of any ambient, swept-up gas. In the context of recent studies of protostars, we propose an outflow evolutionary scenario in which the molecular gas component dominates in the youngest sources, whereas the fast, ionized jets dominate in the oldest sources, as is the case for the twin jets discovered in the WL 20 system.

Revisiting the massive star-forming complex RCW 122: New millimeter and submillimeter study

In this paper, we present a new multifrequency study of the giant star-forming complex RCW 122. We used molecular data obtained with the ASTE 10 m and the APEX 12 m telescopes, along with infrared observations spanning from 3.6 µm to 870 µm, obtained from available databases. We also incorporated a range of public datasets, including the radio continuum at 3 GHz, narrowband Ha images, and deep JHK photometry. Our analysis focuses mostly on cataloged ATLASGAL sources, showcasing a spectrum of evolutionary stages from infrared dark cloud (IRDC)/high-mass protostellar object (HMPO) to ultra-compact HII region (UCHII), as inferred from preliminary inspections of the public dataset. Based on ASTE HCO+(4−3) and CO(3−2) data, we identified five molecular clumps, designated A, B, C, D, and E, as molecular counterparts of the ATLASGAL sources. These clumps have radial velocities ranging from ~−15 km s−1 to −10 km s−1, confirming their association with RCW 122. In addition, we report the detection of 20 transitions from 11 distinct molecules in the APEX spectra in the frequency ranges from 258.38 GHz to 262.38 GHz, 228.538 GHz to 232.538 GHz, and 218.3 GHz to 222.3 GHz, unveiling a diverse chemical complexity among the clumps. Utilizing CO(2−1) and C18O(2−1) data taken from the observations with the APEX telescope, we estimated the total LTE molecular mass, ranging from 200 M⊙ (clump A) to 4400 M⊙ (clump B). Our mid- to far-infrared (MIR-FIR) flux density analysis yielded minimum dust temperatures of 23.7 K (clump A) to maximum temperatures of 33.9 K (clump B), indicating varying degrees of internal heating among the clumps. The bolometric luminosities span 1.7×103 L⊙ (clump A) to 2.4×105 L⊙ (clump B), while the total (dust+gas) mass ranges from 350 M⊙ (clump A) to 3800 M⊙ (clump B). Our analysis of the molecular line richness, L/M ratios, and CH3CCH and dust temperatures reveals an evolutionary sequence of A/E→C→D/B, consistent with preliminary inferences of the ATLASGAL sources. In this context, clumps A and E exhibit early stages of collapse, with clump A likely in an early HMPO phase, which is supported by identifying a candidate molecular outflow. Clump E appears to be in an intermediate stage between IRDC and HMPO. Clumps D and B show evidence of being in the UCHII phase, with clump B likely more advanced. Clump C likely represents an intermediate stage between HMPO and HMC. Our findings suggest clump B is undergoing ionization and heating by multiple stellar and protostellar members of the stellar cluster DBS 119. Meanwhile, other cluster members may be responsible for ionizing other regions of RCW 122 that have evolved into fully developed HII regions, beyond the molecular dissociation stage.

The Limits of Archaeology and Cultural Anthropology: Archaeological Witnesses and Ethnographical Data Among the Bakola-Bagyeli “Pygmies” (South Cameroon)

The reading of the transformations recorded in the material equipment of disappeared societies still remains largely inspired by the dogma of materialism. This inclines inferences, in archaeology, to systematically deduce evolutionary stages on a double level, chronological and economic, from the material remains of technological changes only. However, the unpredictable experience of human societies can often reveal situations that contradict the established inferential model. Such a reality therefore poses the problem of searching for an approach capable of achieving balance in the possible equation between the experience of human societies and the methodological means implemented to account for it. The question therefore remains to know whether data collected and explained in a methodological approach specific to a discipline always reproduce the improbable nature of the reality of human societies, both living and extinct? Thus, ethnographic, qualitative data and archaeological facts are do they still agree regarding the current experience of life of the Bakola-Bayéli “Pygmies” of South Cameroon, since the 1990s? The hypothesis supports: data collected according to the orthodoxy of techniques specific to dissociated disciplinary fields, in a conventional manner, can contradict each other on the same fact. The complexity of the reality of human societies escapes the specific filter of conceptual and methodological practices characteristic of the disciplines that separate techniques specific to each method. The archaeological witnesses, taken from surveys carried out on the sites where the Bakola-Bagyéli “Pygmies” live, contradict the oral testimonies, given by these same populations through interviews, directive and semi-directive, guided by a questionnaire. A comparative study of qualitative and quantitative data makes it possible to verify the hypotheses put forward. The theoretical approach acquired to the cause of disorganization and opposed to the terminism of ends makes it possible to discuss the a priori organization of cultural facts and the accomplishment of reserved goals.

Convergent alterations in the tumor microenvironment of MYC-driven human and murine prostate cancer

How prostate cancer cells and their precursors mediate changes in the tumor microenvironment (TME) to drive prostate cancer progression is unclear, in part due to the inability to longitudinally study the disease evolution in human tissues. To overcome this limitation, we perform extensive single-cell RNA-sequencing (scRNA-seq) and molecular pathology of the comparative biology between human prostate cancer and key stages in the disease evolution of a genetically engineered mouse model (GEMM) of prostate cancer. Our studies of human tissues reveal that cancer cell-intrinsic activation of MYC signaling is a common denominator across the well-known molecular and pathological heterogeneity of human prostate cancer. Cell communication network and pathway analyses in GEMMs show that MYC oncogene-expressing neoplastic cells, directly and indirectly, reprogram the TME during carcinogenesis, leading to a convergence of cell state alterations in neighboring epithelial, immune, and fibroblast cell types that parallel key findings in human prostate cancer.

Standardization of robot-assisted radical nephroureterectomy via intraperitoneal approach: insights from a high-volume Japanese Center.

We present the trial-and-error process of standardizing robot-assisted radical nephroureterectomy (RANU) at a high-volume center in Japan. Our urology team performed 53 RANU cases using the Da Vinci Xi system, undergoing five major evolutionary stages. We performed RANU via transperitoneal approach in all cases and lymph-node dissection in selected cases. During the evolution, we adopted a lithotomy position and significantly modified port placement to facilitate lower ureter management. However, we ultimately arrived at a method that minimizes port and patient repositioning during lower ureter processing. By strategically placing ProGrasp™ forceps in the most caudal port, we effectively retracted the bladder and grasped the opened bladder wall during lower ureter manipulation. This approach also allowed us to perform pelvic, para-aortic, and renal portal lymph-node dissection without major changes in patient positioning or port placement. Nevertheless, we acknowledge that some variations in positioning and techniques may be necessary depending on specific case requirements.