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SO and SO2 are two potential candidates to trace the different evolutionary phases of the low-mass star-formation process. Here, we report observations of SO and SO2 along with their isotopologues, 34SO and 34SO2, respectively, in four distinct phases of the low-mass star-formation process (prestellar core, first hydrostatic core, Class 0, and Class I) with an unbiased survey carried out using the Institut de Radioastronomie Millimetrique (IRAM) 30 m telescope. Interestingly, the estimated abundances of SO and SO2 show an increasing trend from the prestellar phase to the Class 0 stage and then a decrease in the Class I phase. A similar trend is obtained for OCS and H2S. In contrast, the obtained SO/SO2 ratio decreases gradually from the prestellar core to the Class I stage. We have used the three-phase Rokko chemical code to explain our observations. The modeled abundances of SO and SO2 exhibit an increase within the inner region as the cold gas transforms into a hot gas. The modeled abundance ratio of SO to SO2 exhibits a notably high value in cold gas environments. This ratio decreases to less than 1 within the temperature range of 100-300 K and then increases to approximately 1 beyond 300 K. In the outer region, the simulated ratio consistently exceeds the value of 1. Our work is an observational testbed for modeling the chemistry of SO/SO2 during low-mass star formation. However, our findings may require more sample sources with higher resolution and a more robust model for validation. [ABSTRACT FROM AUTHOR]

To enable the long-term use of existing wooden structures, appropriately evaluating the extent of damage of the biodeterioration of structural performance, including members and joint systems, is necessary. To give one example, accurately estimating the single shear strength performance of nail and screw joints with decay is crucial. Therefore, this study proposes a method to model this by dividing wood into multiple layers with different strength performance, considering the grade of deterioration in a cross-section of decayed wood. The model was used to differentiate the sound layer and three decayed layers (multilayer) according to the extent of the damage. The estimated values, which were produced using the proposed model, were compared to the single shear strength of screw and nail joints with decay using two species of wood, namely Abies sachalinensis (Todomatsu) and Cryptomeria japonica (Sugi). The results point to a good fit between the average value of the experimental results and the estimated values of the proposed model. Compared with the existing (single-layer) model, the proposed model improved the accuracy of estimating the strength of wood undergoing early deterioration and therefore was considered usable. [ABSTRACT FROM AUTHOR]

Background: There is little available information regarding the difference in outcomes between severe hallux valgus (S-HV), defined as 40 degrees ≤ hallux valgus angle (HVA) < 50 degrees, and what we consider to be "super-severe HV" (SS-HV), defined as >50 degrees, following a proximal metatarsal osteotomy. We aimed to retrospectively compare the outcomes of a proximal metatarsal osteotomy in S- and SS-HV. Methods: The series consisted of 57 female patients (57 feet) treated with a proximal supination osteotomy for symptomatic S- and SS-HV (33 and 24 feet, respectively). The outcome measures included radiographic parameters and for 45 patients included the Self-Administered Foot Evaluation Questionnaire (SAFE-Q) score, and a visual analog scale pain score (VAS-PS) preoperatively and at a minimum follow-up of 12 months with a median of 26 months. No significant differences were found in age, body mass index, and the duration of follow-up between patients with S-HV and SS-HV (P >.10 for all comparisons) with the numbers available. Results: Preoperative HVA in patients with S- and SS-HV was significantly improved at the final follow-up (P <.0001 for both comparisons). No significant differences in postoperative HVA and IMA were observed between patients with S- and SS-HV (P =.51 and.50, respectively). All 5 preoperative subscale scores of SAFE-Q in patients with S- and SS-HV significantly improved postoperatively (P <.01 for all comparisons). Preoperative VAS-PS in patients with S- and SS-HV significantly improved postoperatively (P <.0001 and <.009, respectively). There were no significant differences in preoperative and postoperative scores of all the SAFE-Q subscales and VAS-PS between patients with S-HV and SS-HV (P >.10 for all) with the numbers available. Conclusion: We found for this patient group that a proximal supination osteotomy can achieve a large correction for SS-HV as well as S-HV and significantly improve radiologic and clinical outcomes in SS-HV. The outcomes between patients with S- and SS-HV were not different in this series. Level of Evidence: Level III, retrospective comparative study. [ABSTRACT FROM AUTHOR]

Young massive clusters (YMCs) are the most massive star clusters forming in nearby galaxies and are thought to be a young analogue to the globular clusters. Understanding the formation process of YMCs leads to looking into very efficient star formation in high-redshift galaxies suggested by recent JWST observations. We investigate possible observational signatures of their formation stage, particularly when the mass of a cluster is increasing via accretion from a natal molecular cloud. To this end, we study the broad-band continuum emission from ionized gas and dust enshrouding YMCs, whose formation is followed by recent radiation hydrodynamics simulations. We perform post-process radiative transfer calculations using simulation snapshots and find characteristic spectral features at radio and far-infrared frequencies. We show that a striking feature is long-lasting, strong free–free emission from a ∼10-pc-scale H  ii region with a large emission measure of ≳107 cm−6 pc, corresponding to the mean electron density of ≳103 cm−3. There is a turnover feature below ∼10 GHz, a signature of the optically thick free–free emission, often found in Galactic ultracompact H  ii regions. These features come from the peculiar YMC formation process, where the cluster's gravity effectively traps photoionized gas for a long duration and enables continuous star formation within the cluster. Such large and dense H  ii regions show distinct distribution on the density–size diagram, apart from the standard sequence of Galactic H  ii regions. This is consistent with the observational trend inferred for extragalactic H  ii regions associated with YMCs. [ABSTRACT FROM AUTHOR]

We report the first extragalactic detection of the higher-order millimeter hydrogen recombination lines (Δ n > 2). The γ -, ϵ -, and η -transitions have been detected toward the millimeter continuum source N 105–1 A in the star-forming region N 105 in the Large Magellanic Cloud with the Atacama Large Millimeter/submillimeter Array. We use the H40 α line, the brightest of the detected recombination lines (H40 α, H36 β, H50 β, H41 γ, H57 γ, H49 ϵ, H53 η, and H54 η), to determine the electron temperature and study ionized gas kinematics in the region, and the 3 mm free–free continuum emission to determine the physical parameters: the size, emission measure, and electron density. We compare the physical properties of N 105–1 A to a large sample of Galactic compact and ultracompact (UC) H ii regions and conclude that N 105–1 A is similar to the most luminous (L > 105 L ⊙) UC H ii regions in the Galaxy. N 105–1 A is ionized by an O5.5 V star; it is deeply embedded in its natal molecular clump, and likely associated with a (proto)cluster. We incorporate high-resolution molecular line data including CS, SO, SO2, and CH3OH (∼0.12 pc), and HCO+ and CO (∼0.087 pc) to explore the molecular environment of N 105–1 A. Based on the CO data, we find evidence for a cloud–cloud collision that likely triggered star formation in the region. We find no clear outflow signatures, but the presence of filaments and streamers indicates ongoing accretion onto the clump hosting the UC H ii region. Sulfur chemistry in N 105–1 A is consistent with the accretion shock model predictions. [ABSTRACT FROM AUTHOR]

The destiny of complex organic molecules (COMs) in star-forming regions is interlinked with various evolutionary phases. Therefore, identifying these species in diversified environments of identical star-forming regions would help to understand their physical and chemical heritage. We identified multiple COMs utilizing the Large Program Astrochemical Surveys At Institut de Radio Astronomie Millimétrique (IRAM) data, dedicated to chemical surveys in Sun-like star-forming regions with the IRAM 30 m telescope. It was an unbiased survey in the millimeter regime, covering the prestellar core, protostar, outflow region, and protoplanetary disk phase. Here, we report the transitions of seven COMs, namely, methanol (CH3OH), acetaldehyde (CH3CHO), methyl formate (CH3OCHO), ethanol (C2H5OH), propynal (HCCCHO), dimethyl ether (CH3OCH3), and methyl cyanide (CH3CN) in sources L1544, B1-b, IRAS4A, and SVS13A. We found a trend among these species from the derived abundances using the rotational diagram method and Monte Carlo Markov chain fitting. We have found that the abundances of all of the COMs, except for HCCCHO, increase from the L1544 (prestellar core) and peaks at IRAS16293-2422 (class 0 phase). It is noticed that the abundance of these molecules correlates with the luminosity of the sources. The obtained trend is also visible from the previous interferometric observations and considering the beam dilution effect. [ABSTRACT FROM AUTHOR]

In this study, numerical simulations of HE-E experiment in Mont Terri rock laboratory were performed with Thermo–Hydro–Mechanical (THM) coupled processes. The aim of this study is to validate modelling, understand THM coupled behaviour and verify applicability of material parameters obtained by a column test to the full-scale model. The results of THM and TH coupled analysis are compared, and the influence of fluid and thermal terms/factors on mechanical behaviour is discussed. The analysis code used for THM and TH coupled analysis was CODE_BRIGHT. An axisymmetric analytical model, which allowed modelling of two heaters, was used for the THM and TH coupled model, and their results were compared. As a result, a better reproducibility of relative humidity in the Engineered Barrier System (EBS) and pore water pressure of the bedrock was achieved by performing mechanical coupling. Furthermore, experimental conditions were simulated more realistically, since two heathers and different backfill materials were also modelled in the analysis.

Simple Summary: The present study aims to establish a method of whole mitochondrial DNA (mtDNA) sequencing for domestic dogs. Prior to proceeding with the experiment, the collection of relevant DNA samples was essential. Therefore, we decided to use oral mucosa DNA, which can be collected non-invasively. A polymerase chain reaction (PCR) was performed using the DNA collected from six dogs raised in Japan and four primer pairs as specific to the mtDNA, after which the amplified products were sequenced using next-generation sequencing. As a result, the whole mtDNA obtained from all dogs was correctly sequenced. Thus, we determined that the method we used in our study may be useful for future research on dog-related medical care and welfare. In human beings, whole mitochondrial DNA (mtDNA) sequencing has been widely used in many research fields, including medicine, forensics, and genetics. With respect to the domestic dog (Canis lupus familiaris), which is commonly recognized as being an additional member of the traditional human family structure, research studies on mtDNA should be developed to expand and improve our collective knowledge of dog medicine and welfare as it seems that there is still room for further development in these areas. Moreover, a simple and robust method for sequencing whole mtDNA that can be applied to various dog breeds has not yet been described in the literature. In the present study, we aim to establish such a method for the whole mtDNA sequencing of the domestic dog. In the experiments we conducted, oral mucosa DNA samples obtained from six Japanese domestic dogs were used as a template. We designed four primer pairs that could amplify approximately 5 kbp from each region of the mtDNA and validated several PCR conditions. Subsequently, the PCR amplicons were pooled and subjected to library preparation. The sequencing of the libraries was performed using next-generation sequencing (NGS), followed by bioinformatics analysis. Our results demonstrate that the proposed method can be used to perform highly accurate resequencing. We believe that this method may be useful for future research conducted to better understand dog medicine and welfare. [ABSTRACT FROM AUTHOR]

We present ∼10–40 μ m SOFIA-FORCAST images of 11 isolated protostars as part of the SOFIA Massive (SOMA) Star Formation Survey, with this morphological classification based on 37 μ m imaging. We develop an automated method to define source aperture size using the gradient of its background-subtracted enclosed flux and apply this to build spectral energy distributions (SEDs). We fit the SEDs with radiative transfer models, developed within the framework of turbulent core accretion (TCA) theory, to estimate key protostellar properties. Here, we release the sedcreator python package that carries out these methods. The SEDs are generally well fitted by the TCA models, from which we infer initial core masses M c ranging from 20–430 M ⊙, clump mass surface densities Σcl ∼ 0.3–1.7 g cm−2, and current protostellar masses m * ∼ 3–50 M ⊙. From a uniform analysis of the 40 sources in the full SOMA survey to date, we find that massive protostars form across a wide range of clump mass surface density environments, placing constraints on theories that predict a minimum threshold Σcl for massive star formation. However, the upper end of the m *−Σcl distribution follows trends predicted by models of internal protostellar feedback that find greater star formation efficiency in higher Σcl conditions. We also investigate protostellar far-IR variability by comparison with IRAS data, finding no significant variation over an ∼40 yr baseline. [ABSTRACT FROM AUTHOR]

We report on a direct comparison of VLBI maser data and ALMA thermal-emission data for the high-mass protostar G353.273+0.641. We detected a gravitationally-unstable disk by dust and a high-velocity jet traced by a thermal CO line by ALMA long-baselines (LB). 6.7 GHz CH3OH masers trace infalling streamlines inside the disk. The innermost maser ring indicates another compact accretion disk of 30 au. Such a nested system could be caused by angular momentum transfer by the spiral arms. 22 GHz H2O masers trace the jet-accelerating region, which are directly connecting the CO jet and the protostar. The recurrent maser flares imply episodic jet ejections per 1–2 yr, while typical separation of CO knots indicates a variation of outflow rate per 100 yr. Our study demonstrates that VLBI maser observations are still a powerful tool to explore detailed structures nearby high-mass protostars by combining ALMA LB. [ABSTRACT FROM AUTHOR]

Cosmic metallicity evolution possibly creates the diversity of star formation modes at different epochs. Gravitational fragmentation of circumstellar discs provides an important formation channel of multiple star systems, including close binaries. We here study the nature of disc fragmentation, systematically performing a suite of 2D radiation-hydrodynamic simulations, in a broad range of metallicities, from the primordial to the solar values. In particular, we follow relatively long-term disc evolution over 15 kyr after the disc formation, incorporating the effect of heating by the protostellar irradiation. Our results show that the disc fragmentation occurs at all metallicities 1– |$0 \, \rm {Z}_{\odot }$|⁠ , yielding self-gravitating clumps. Physical properties of the clumps, such as their number and mass distributions, change with the metallicity due to different gas thermal evolution. For instance, the number of clumps is the largest for the intermediate metallicity range of 10−2– |$10^{-5} \, \rm {Z}_{\odot }$|⁠ , where the dust cooling is effective exclusively in a dense part of the disc and causes the fragmentation of spiral arms, although the disc might fragment at a similar rate, also at lower metallicities 10−6– |$0 \, \rm {Z}_{\odot }$| with higher spatial resolution. The disc fragmentation is more modest for 1– |$0.1 \, \rm {Z}_{\odot }$|⁠ , thanks to the disc stabilization by the stellar irradiation. Such metallicity dependence agrees with the observed trend that the close binary fraction increases with decreasing metallicity in the range of 1– |$10^{-3} \, \rm {Z}_{\odot }$|⁠. [ABSTRACT FROM AUTHOR]

We present a detailed study of the massive star-forming region G35.2-0.74N with Atacama Large Millimeter/submillimeter Array (ALMA) 1.3 mm multi-configuration observations. At 0.″2 (440 au) resolution, the continuum emission reveals several dense cores along a filamentary structure, consistent with previous ALMA 0.85 mm observations. At 0.″03 (66 au) resolution, we detect 22 compact sources, most of which are associated with the filament. Four of the sources are associated with compact centimeter continuum emission, and two of these are associated with H30 α recombination line emission. The H30 α line kinematics shows the ordered motion of the ionized gas, consistent with disk rotation and/or outflow expansion. We construct models of photoionized regions to simultaneously fit the multiwavelength freeâ€"free fluxes and the H30 α total fluxes. The derived properties suggest the presence of at least three massive young stars with nascent hypercompact H ii regions. Two of these ionized regions are surrounded by a large rotating structure that feeds two individual disks, revealed by dense gas tracers, such as SO2, H2CO, and CH3OH. In particular, the SO2 emission highlights two spiral structures in one of the disks and probes the faster-rotating inner disks. The 12CO emission from the general region reveals a complex outflow structure, with at least four outflows identified. The remaining 18 compact sources are expected to be associated with lower-mass protostars forming in the vicinity of the massive stars. We find potential evidence for disk disruption due to dynamic interactions in the inner region of this protocluster. The spatial distribution of the sources suggests a smooth overall radial density gradient without subclustering, but with tentative evidence of primordial mass segregation. [ABSTRACT FROM AUTHOR]

Massive dense clumps in the Large Magellanic Cloud can be an important laboratory to explore the formation of populous clusters. We report multiscale ALMA observations of the N159W-North clump, which is the most CO-intense region in the galaxy. High-resolution CO isotope and 1.3 mm continuum observations with an angular resolution of ∼0.″25 (∼0.07 pc) revealed more than five protostellar sources with CO outflows within the main ridge clump. One of the thermal continuum sources, MMS-2, shows an especially massive/dense nature whose total H2 mass and peak column density are ∼104 M ⊙ and ∼1024 cmâˆ'2, respectively, and harbors massive (∼100 M ⊙) starless core candidates identified as its internal substructures. The main ridge containing this source can be categorized as one of the most massive protocluster systems in the Local Group. The CO high-resolution observations found several distinct filamentary clouds extending southward from the star-forming spots. The CO (1â€"0) data set with a larger field of view reveals a conical, ∼30 pc long complex extending toward the northern direction. These features indicate that a large-scale gas compression event may have produced the massive star-forming complex. Based on the striking similarity between the N159W-North complex and the other two previously reported high-mass star-forming clouds in the nearby regions, we propose a “teardrops inflow model” that explains the synchronized, extreme star formation across >50 pc, including one of the most massive protocluster clumps in the Local Group. [ABSTRACT FROM AUTHOR]

Simple Summary: Although serum DJ-1 has been evaluated in some types of cancer, it has not been analyzed in detail in bladder cancer (BC). Furthermore, DJ-1 expression patterns in BC and their clinicopathologic significance and relationship with prognosis are unclear. In the present study, we evaluated serum DJ-1 levels in BC and the localization of DJ-1 expression in BC tissues. Our research showed that serum DJ-1 was significantly higher in 172 patients with BC who underwent the transurethral resection of bladder tumors (TURBT) than in those with urolithiasis or in healthy participants. Immunohistochemically, a DJ-1 cytoplasm-positive (Cy+) and nucleus-negative (N−) pattern in 92 archived radical cystectomy BC specimens was associated with a significantly increased risk for lower overall, recurrence-free and cancer-specific survival. Our findings suggest that DJ-1 might be a new biomarker for diagnosing BC and predicting biologically aggressive cancers so as to determine the appropriate treatment modality after radical cystectomy. The overexpression of DJ-1 protein and its secretion into the bloodstream has been reported in various neoplasms. However, serum levels and the subcellular localization of DJ-1 have not been analyzed in detail in bladder cancer (BC). Our comprehensive analysis of these variables started with the measurement of DJ-1 in serum from 172 patients with BC, 20 patients with urolithiasis and 100 healthy participants. Next, an immunohistochemical study of DJ-1 expression and localization was conducted in 92 patients with BC, and associations with clinicopathologic factors and patient outcomes were evaluated. Serum DJ-1 was significantly higher in patients with BC than in those with urolithiasis or in healthy participants. Immunohistochemically, a cytoplasm-positive (Cy+) and nucleus-negative (N−) DJ-1 pattern was associated with age and pathologic stage. Log-rank tests indicated that the Cy+, N− pattern was significantly associated with overall survival (OS), recurrence-free survival (RFS), and cancer specific survival (CSS). In addition, the Cy+, N− pattern was an independent prognostic factor in the multivariate analysis adjusted for the effects of the clinicopathologic outcomes. The investigation of DJ-1 expression might help physicians to make decisions regarding further follow-up and additional treatments. [ABSTRACT FROM AUTHOR]

Background: Helicobacter pylori infection is a well‐established risk factor for gastric cancer and has been linked to other gastrointestinal diseases, including pancreatic and biliary tract cancers; however, the relevance of enterohepatic non‐H. pylori helicobacters to the pathophysiology of these diseases remains unclear. Materials and Methods: We estimated the prevalence of two enterohepatic non‐H. pylori helicobacters (Helicobacter hepaticus and Helicobacter bilis) in the framework of a hospital‐based case‐control study involving 121 patients with biliary tract cancer, pancreatic cancer, or other gastrointestinal diseases. Bile and blood samples were collected from the patients undergoing endoscopic retrograde cholangiopancreatography. The presence of H. bilis, H. hepaticus, and other Helicobacter spp. was examined using bacterial culture, PCR‐based detection, and serological tests. Results: Culture of Helicobacter spp. from biliary brush samples was unsuccessful. Approximately 13.0% (15/115) of the bile samples collected from patients with a variety of gastrointestinal cancers, including pancreatic and biliary tract cancers, tested positive for one of the enterohepatic non‐H. pylori helicobacter species as determined by PCR. Specifically, H. bilis and H. hepaticus DNA were detected in 11 and 4 bile samples, respectively. Approximately 20%–40% of the patients tested positive for serum non‐H. pylori helicobacter IgG antibodies. The seroprevalence of H. bilis and H. hepaticus in the patients without evidence of H. pylori infection appeared to be higher in the pancreatic cancer group than in the control group. Conclusion: Our findings suggest a role for Helicobacter spp., especially H. bilis and H. hepaticus, in the etiology of pancreatic and biliary tract cancers. [ABSTRACT FROM AUTHOR]

Multi-epoch narrowband Hubble Space Telescope images of the bipolar H ii region Sh2-106 reveal highly supersonic nebular proper motions that increase with projected distance from the massive young stellar object S106 IR, reaching over ∼30 mas yrâˆ'1 (∼150 km sâˆ'1 at D = 1.09 kpc) at a projected separation of ∼1.′4 (0.44 pc) from S106 IR. We propose that S106 IR experienced a ∼1047 erg explosion ∼3500 yr ago. The explosion may be the result of a major accretion burst or a recent encounter with another star, or a consequence of the interaction of a companion with the bloated photosphere of S106 IR as it grew from ∼10 through ∼15 M ⊙ at a high accretion rate. Near-IR images reveal fingers of H2 emission pointing away from S106 IR and an asymmetric photon-dominated region surrounding the ionized nebula. Radio continuum and Br Îł emission reveal a C-shaped bend in the plasma, indicating either the motion of S106 IR toward the east, or the deflection of plasma toward the west by the surrounding cloud. The H ii region bends around a ∼1′ diameter dark bay west of S106 IR that may be shielded from direct illumination by a dense molecular clump. Herbigâ€"Haro and Molecular Hydrogen Objects tracing outflows powered by stars in the Sh2-106 protocluster such as the Class 0 source S106 FIR are discussed. [ABSTRACT FROM AUTHOR]