bluuebunny/crossref_metadata_2025_split huggingface dataset:
Occupational health staff’s involvement contributes to supervisor’s perceived organizational support in Japanese workforce: a prospective cohort study
Authors: Mori Takahiro , Nagata Tomohisa , Odagami Kiminori , Adi Nuri Purwito , Mori Koji ,   for the W2S-Ohpm II study
Published: July 2024

Abstract

Objectives
Enhancing employees’ perceived organizational support (POS) is crucial for organizations, and one effective approach is enhancing supervisors’ POS. However, there is limited research focusing specifically on enhancing supervisors’ POS. We aimed to investigate the influence of occupational health staff’s involvement for supervisors on their POS.

Methods
A prospective cohort study was conducted using an online survey targeting supervisors in various industries across Japan. We assessed supervisors’ POS using 8 effective items of the Japanese version of the Survey of Perceived Organizational Support. Data were collected on the involvement of occupational health staff in providing supervisors with training on workplace health management and guidance on addressing specific subordinates with health concerns. The association between this involvement and POS was assessed through multiple regression analyses.

Results
The study involved 541 supervisors with occupational health staff at their workplace in the final analysis. Training from occupational health staff was significantly associated with an increase in POS at follow-up after adjustment for potential confounders, including demographic variables and POS at baseline. Similarly, guidance from occupational health staff was also significantly associated with increased POS. This effect was particularly notable in small workplaces.

Conclusions
Our study indicates that occupational health staff’s involvement in supporting supervisors can contribute to enhancing supervisors’ POS, especially in small workplaces. These findings suggest that by developing structured systems and establishing specific roles for occupational health staff, organizations may effectively enhance supervisors’ POS.
Hepatitis B infection and immunity in migrant children and pregnant persons in Europe: a systematic review and meta-analysis
Authors: Hobart Carla , Pescarini Julia M , Evans Laith , Adil Haleema S , Adil Shehzhore T , Deal Anna , Carter Jessica , Matthews Philippa C , Hargreaves Sally , Sanchez Clemente Nuria 
Published: July 2024

Abstract

Background
The WHO’s global hepatitis strategy aims to achieve viral hepatitis elimination by 2030. Migrant children and pregnant persons represent an important target group for prevention strategies. However, evidence on the burden of chronic hepatitis B (CHB) infection and the factors affecting its incidence is lacking.

Methods
EMBASE, Global Health, Global Index Medicus, Web of Science and Medline were searched for articles in any language from 1 January 2012 to 8 June 2022. Studies reporting CHB prevalence, disease severity, complications and/or prevention strategies, including vaccination, prevention of vertical transmission and access to care/treatment for migrant children and pregnant migrants, were included. Pooled estimates of CHB prevalence and hepatitis B vaccination (HBV) coverage among migrant children were calculated using random effects meta-analysis.

Findings
42 studies were included, 27 relating to migrant children and 15 to pregnant migrants across 12 European countries, involving data from 64 773 migrants. Migrants had a higher incidence of CHB than host populations. Among children, the pooled prevalence of CHB was higher for unaccompanied minors (UAM) (5%, [95% CI: 3–7%]) compared to other child migrants, including internationally adopted children (IAC) and refugees (1%, [95% CI: 1–2%]). Region of origin was identified as a risk factor for CHB, with children from Africa and pregnant migrants from Africa, Eastern Europe and China at the highest risk. Pooled estimates of HBV vaccine coverage were lower among UAM (12%, [95% CI: 3–21%]) compared to other child migrants (50%, [95% CI: 37–63%]).

Conclusion
A range of modifiable determinants of HBV prevalence in migrant children and pregnant persons were identified, including sub-optimal screening, prevention and continuum of care. There is a need to develop evidence-based approaches in hepatitis care for these groups, thereby contributing towards global viral hepatitis elimination goals.
The role of chloroplast SRP54 domains and its C-terminal tail region in post- and co-translational protein transport in vivo
Authors: Bischoff Annika , Ortelt Jennifer , Dünschede Beatrix , Zegarra Victor , Bedrunka Patricia , Bange Gert , Schünemann Danja 
Published: July 2024

Abstract
In the chloroplast, the 54 kDa subunit of the signal recognition particle (cpSRP54) is involved in the post-translational transport of the light-harvesting chlorophyll a/b-binding proteins (LHCPs) and the co-translational transport of plastid-encoded subunits of the photosynthetic complexes to the thylakoid membrane. It forms a high-affinity complex with plastid-specific cpSRP43 for post-translational transport, while a ribosome-associated pool coordinates its co-translational function. CpSRP54 constitutes a conserved multidomain protein, comprising a GTPase (NG) and a methionine-rich (M) domain linked by a flexible region. It is further characterized by a plastid-specific C-terminal tail region containing the cpSRP43-binding motif. To characterize the physiological role of the various regions of cpSRP54 in thylakoid membrane protein transport, we generated Arabidopsis cpSRP54 knockout (ffc1-2) lines producing truncated cpSRP54 variants or a GTPase point mutation variant. Phenotypic characterization of the complementation lines demonstrated that the C-terminal tail region of cpSRP54 plays an important role exclusively in post-translational LHCP transport. Furthermore, we show that the GTPase activity of cpSRP54 plays an essential role in the transport pathways for both nuclear as well as plastid-encoded proteins. In addition, our data revealed that plants expressing cpSRP54 without the C-terminal region exhibit a strongly increased accumulation of a photosystem I assembly intermediate.
The mean longitudinal magnetic field and its uses in radial-velocity surveys
Authors: Rescigno F , Mortier A , Dumusque X , Lakeland B S , Haywood R , Piskunov N , Nicholson B A , López-Morales M , Dalal S , Cretignier M , Klein B , Cameron A Collier , Ghedina A , Gonzalez M , Cosentino R , Sozzetti A , Saar S H 
Published: July 2024

ABSTRACT
This work focuses on the analysis of the mean longitudinal magnetic field as a stellar activity tracer in the context of small exoplanet detection and characterization in radial-velocity (RV) surveys. We use Solar Dynamics Observatory/Helioseismic and Magnetic Imager filtergrams to derive Sun-as-a-star magnetic field measurements, and show that the mean longitudinal magnetic field is an excellent rotational period detector and a useful tracer of the solar magnetic cycle. To put these results into context, we compare the mean longitudinal magnetic field to three common activity proxies derived from HARPS-N Sun-as-a-star data: the full width at half-maximum, the bisector span, and the S-index. The mean longitudinal magnetic field does not correlate with the RVs and therefore cannot be used as a one-to-one proxy. However, with high cadence and a long baseline, the mean longitudinal magnetic field outperforms all other considered proxies as a solar rotational period detector, and can be used to inform our understanding of the physical processes happening on the surface of the Sun. We also test the mean longitudinal magnetic field as a ‘stellar proxy’ on a reduced solar data set to simulate stellar-like observational sampling. With a Gaussian Process regression analysis, we confirm that the solar mean longitudinal magnetic field is the most effective of the considered indicators, and is the most efficient rotational period indicator over different levels of stellar activity. This work highlights the need for polarimetric time series observations of stars.
High-priority targets for transient gravitational waves from glitching pulsars
Authors: Yim Garvin , Shao Lijing , Xu Renxin 
Published: July 2024

ABSTRACT
Glitching pulsars are expected to be important sources of gravitational waves (GWs). In this paper, we explore six different models that propose the emission of transient continuous waves, lasting days to months, coincident with glitches. The maximal GW energy is calculated for each model, which is then used to determine whether associated GWs could be detectable with LIGO-Virgo-KAGRA’s O4 detectors. We provide an analytical approximation to calculate the signal-to-noise ratio (SNR) which includes information about the source’s sky position, improving on previous estimates that assume isotropic or sky and orientation averaged sensitivities. By analysing the entire glitching population, we find that certain models predict detectable signals in O4, whereas others do not. We also rank glitching pulsars by SNR, based on archival data, and we find that for all models, the Vela pulsar (PSR J0835$-$4510) would provide the strongest signal. Moreover, PSR J0537$-$6910 is not expected to yield a detectable signal in O4, but will start becoming relevant for next-generation detectors. Our analysis also extends to the entire pulsar population, regardless of whether they have glitched, and we provide a list of pulsars that would present a significant signal, if they were to glitch. Finally, we apply our analysis to the 2024 April Vela glitch and find that a signal should be detectable under certain models. The non-detection of a supposedly detectable signal would provide an efficiency factor that quantifies a model’s contribution to GW emission, eventually leading to a differentiation of models and independent constraints on physical parameters.
Astrophysical calibration of the oscillator strengths of YJ-band absorption lines in classical Cepheids
Authors: Elgueta S S , Matsunaga N , Jian M , Taniguchi D , Kobayashi N , Fukue K , Hamano S , Sameshima H , Kondo S , Arai A , Ikeda Y , Kawakita H , Otsubo S , Yasui C , Tsujimoto T 
Published: July 2024

ABSTRACT
Newly-developed spectrographs with increased resolving powers, particularly those covering the near-IR range, allow the characterization of more and more absorption lines in stellar spectra. This includes the identification and confirmation of absorption lines and the calibration of oscillator strengths. In this study, we provide empirical values of ${{\rm log} gf}$ based on the abundances of classical Cepheids obtained with optical spectra to establish the consistency between optical and infrared abundance results. Using time series spectra of classical Cepheids obtained with WINERED spectrograph (0.97–1.35 $\mu$m, R$\sim$ 28000), we demonstrate that we can determine the stellar parameters of the observed Cepheids, including effective temperature (${T_\mathrm{eff}}$), surface gravity (${{\rm log} g}$), microturbulence ($\xi$), and metallicity (${\rm {[{\mathrm{ M}}/\mathrm{ H}]}}$). With the newly calibrated relations of line-depth ratios, we can achieve accuracy and precision comparable to optical studies, with uncertainties of $\sim$90 K and 0.108 dex for ${T_\mathrm{eff}}$, and ${{\rm log} g}$, respectively. Finally, we created a new atlas of absorption lines, featuring precise abundance measurements of various elements found in the atmosphere of Cepheids, including neutron-capture elements whose ${{\rm log} gf}$ values have been astrophysically calibrated.
Black hole spin estimation of XTE J2012+381 using simultaneous observations of Swift/XRT and NuSTAR
Authors: Kumar Raj 
Published: July 2024

ABSTRACT
A sufficiently precise measurement of black hole spin is required to carry out quantitative tests of the Kerr metric and to understand several phenomena related to astrophysical black holes. After 24 yr, XTE J2012+381 again underwent an outburst in 2022 December. In this work, we focused on the measurement of the spin and mass of the black hole candidate XTE J2012+381 using broad-band spectral analysis of X-ray data from Swift/XRT and NuSTAR. Using the relxillCp model, the spin and inclination of the source were found to be $0.883_{-0.061}^{+0.033}$ and $46.2_{-2.0}^{+3.7}$ deg, respectively, for high disc density ($i.e.\,\,10^{20}\,\,\mathrm{cm}^{-3}$). We further test our results for lamp-post geometry using the relxilllpCp model. The spin and inclination of the source were found to be $0.892_{-0.044}^{+0.020}$ and $43.1_{-1.2}^{+1.4}$ deg, respectively. Then ‘continuum-fitting’ method was used for the soft state to estimate the mass of BH and found to be $7.95_{-3.25}^{+7.65}\,\,\mathrm{M}_{\odot }$ and $7.48_{-2.75}^{+5.80}\,\,\mathrm{M}_{\odot }$ for the spin and inclination estimated from the relxillCp and relxilllpCp model, respectively. We used a distance of 5.4 kpc as measured by Gaia using the parallax method. This study also addresses the issue of supersolar iron abundance in XTE J2012+381 using reflionx-based reflection model and found high disc density for the source.
Automating galaxy morphology classification using k-nearest neighbours and non-parametric statistics
Authors: Mukundan Kavya , Nair Preethi , Bailin Jeremy , Li Wenhao 
Published: July 2024

ABSTRACT
Morphology is a fundamental property of any galaxy population. It is a major indicator of the physical processes that drive galaxy evolution and in turn the evolution of the entire Universe. Historically, galaxy images were visually classified by trained experts. However, in the era of big data, more efficient techniques are required. In this work, we present a k-nearest neighbours based approach that utilizes non-parametric morphological quantities to classify galaxy morphology in Sloan Digital Sky Survey images. Most previous studies used only a handful of morphological parameters to identify galaxy types. In contrast, we explore 1023 morphological spaces (defined by up to 10 non-parametric statistics) to find the best combination of morphological parameters. Additionally, while most previous studies broadly classified galaxies into early types and late types or ellipticals, spirals, and irregular galaxies, we classify galaxies into 11 morphological types with an average accuracy of ${\sim} 80\!-\!90 \, {{\rm per\, cent}}$ per T-type. Our method is simple, easy to implement, and is robust to varying sizes and compositions of the training and test samples. Preliminary results on the performance of our technique on deeper images from the Hyper Suprime-Cam Subaru Strategic Survey reveal that an extension of our method to modern surveys with better imaging capabilities might be possible.
Mapping the oxygen abundance in Red Geysers and its relation with the gas kinematics using megacubes
Authors: Ilha Gabriele S , Krabbe Angela C , Riffel Rogemar A , Dors Oli L , Riffel Rogério , Rembold Sandro B , Storchi-Bergmann Thaisa , Mallmann Nicolas D 
Published: July 2024

ABSTRACT
Red Geysers are galaxies with low-star formation rates and galactic scale ionized outflows likely driven by low-luminosity active galactic nuclei (AGN). We investigated the impact of AGN winds on the oxygen abundance using integral field spectroscopic data from Mapping Nearby Galaxies for Red Geysers, control galaxies (quiescent galaxies without outflows), and AGN hosts within the inner 1.5 kpc radius. Red Geyser galaxies have higher W$_{80}$ values compared to those of AGN and controls, with 64 per cent showing W$_{80}\gt 500$ km s$^{-1}$ that is indicative of outflow. Only 40 per cent of controls and 31 per cent of AGNs reach this value. We found a small tendency of the oxygen abundance distribution of controls to be biased towards higher values than those of Red Geysers. However, Red Geysers do not show a correlation between H$\alpha$ width (parametrized by the W$_{\rm 80}$) and oxygen abundance, which indicates that AGN winds are not significantly impacting the chemical abundance of the nuclear region of these galaxies. The oxygen abundance distribution mean value for the tree samples is $\rm 12+log(O/H)\sim$8.7 ($\mathit{Z}\sim \rm Z_{\odot })$. On the other hand, AGN hosts show a positive correlation between W$_{80}$ and O/H which could be due to star formation that outflows from the active nuclei could induce; or to the reservoir of gas that makes the nucleus active, and its is also used in the star formation.
A comprehensive analysis towards the Fermi-LAT source 4FGL J1846.9–0227: jets of a protoplanetary nebula producing γ-rays?
Authors: Ortega M E , Petriella A , Paron S 
Published: July 2024

ABSTRACT
Most of the $\gamma$-ray sources in the Fermi-LAT 14-yr source catalogue are associated with pulsars and blazars. However, unveiling the nature of the still unassociated $\gamma$-ray sources is important for the understanding of high energy emission mechanisms in astrophysical objects. This work presents a comprehensive study towards the region covered by the Fermi source 4FGL J1846.9$-$0227, previously suggested to be a blazar and a massive protostar. Using multiwavelength observations, we analysed several astrophysical objects in the region as possible counterparts of the Fermi-LAT source. Having discarded most of them after a detailed and comprehensive analysis, we suggest that the most likely candidate to be such a counterpart is IRAS 18443$-$0231, a likely protoplanetary nebula. We found that the radio continuum emission at 3 GHz of IRAS 18443$-$0231 shows a compact source related to faint emission with jet-like morphology. Additionally, we identified an associated redshifted CO molecular outflow. Using data from several catalogues, we obtained radio spectral index values ranging from $-$0.57 to $-$0.39 for IRAS 18443$-$0231, indicating synchrotron emission due to particles accelerated by the jets. We point out that these jets could explain the $\gamma$-ray emission through mechanisms such as proton–proton collisions and relativistic bremsstrahlung. IRAS 18443$-$0231, lying almost at the centre of the Fermi confidence ellipse and related to the hard X-ray source 4XMM J184700.4$-$022752, would be the first association between a protoplanetary nebula and $\gamma$-ray emission.
Unprecedented extreme high-frequency radio variability in early-stage active galactic nuclei
Authors: Järvelä E , Savolainen T , Berton M , Lähteenmäki A , Kiehlmann S , Hovatta T , Varglund I , Readhead A C S , Tornikoski M , Max-Moerbeck W , Reeves R A , Suutarinen S 
Published: July 2024

ABSTRACT
We report on the discovery of one of the most extreme cases of high-frequency radio variability ever measured in active galactic nuclei (AGNs), observed on time-scales of days and exhibiting variability amplitudes of 3–4 orders of magnitude. These sources, all radio-weak narrow-line Seyfert 1 (NLS1) galaxies, were discovered some years ago at Aalto University Metsähovi Radio Observatory (MRO) based on recurring flaring at 37 GHz, strongly indicating the presence of relativistic jets. In subsequent observations with the Karl G. Jansky Very Large Array (JVLA) at 1.6, 5.2, and 9.0 GHz no signs of jets were seen. To determine the cause of their extraordinary behaviour, we observed them with the JVLA at 10, 15, 22, 33, and 45 GHz, and with the Very Long Baseline Array (VLBA) at 15 GHz. These observations were complemented with single-dish monitoring at 37 GHz at MRO, and at 15 GHz at Owens Valley Radio Observatory (OVRO). Intriguingly, all but one source either have a steep radio spectrum up to 45 GHz, or were not detected at all. Based on the 37 GHz data, the time-scales of the radio flares are a few days, and the derived variability brightness temperatures and variability Doppler factors are comparable to those seen in blazars. We discuss alternative explanations for their extreme behaviour, but so far no definite conclusions can be made. These sources exhibit radio variability at a level rarely, if ever, seen in AGN. They might represent a new type of jetted AGN, or a new variability phenomenon, and thus deserve our continued attention.
Optimal patient selection for yttrium-90 glass plus chemotherapy in the treatment of colorectal liver metastases: additional quality of life, efficacy, and safety analyses from the EPOCH study
Authors: Salem Riad , Garin Etienne , Boucher Eveline , Fowers Kirk , Lam Marnix , Padia Siddharth , Harris William 
Published: July 2024

Abstract

Background
Evaluating transarterial radioembolization (TARE) in patients with metastatic colorectal carcinoma of the liver who have progressed on first-line chemotherapy (EPOCH) demonstrated superior outcomes using yttrium-90 glass microspheres plus chemotherapy (TARE/Chemo) vs chemotherapy (Chemo) to treat colorectal liver metastases. Additional exploratory analyses were undertaken to assess the impact of TARE/Chemo on efficacy, safety, time to subsequent therapy, time to deterioration in quality of life (QoL), and identify criteria for improved patient selection.

Methods
Time to deterioration in QoL was analyzed for the primary study population. Subsequently, a post hoc analysis was undertaken to identify subgroups for which time to deterioration in QoL was improved with TARE/Chemo vs Chemo. Progression-free survival (PFS), hepatic (h)PFS, time to subsequent therapy, and safety outcomes were compared between treatments.

Results
The primary population showed no significant difference in time to deterioration in QoL between treatment arms; however, significance was seen in 2 identified subgroups, namely: Subgroup A (N = 303) which excluded patients with both Eastern Cooperative Oncology Group (ECOG) 1 and baseline CEA ≥ 35 ng/mL from both treatment arms; subgroup B (N = 168) additionally excluded patients with KRAS (Kirsten rat sarcoma) mutation. In subgroup A, TARE/Chemo patients (N = 143) demonstrated superior outcomes vs Chemo (N = 160): PFS (9.4 vs. 7.6 months, hazard ratio (HR): 0.64; 1-sided P = .0020), hPFS (10.8 vs. 7.6 months, HR: 0.53; 1-sided P &lt; .0001), time to deterioration in QoL (5.7 vs. 3.9 months, HR: 0.65; 1-sided P = .0063), and time to subsequent therapy (21.2 vs. 10.5 months, HR: 0.52; 1-sided P &lt; .0001). Subgroup B patients showed similar but larger significant differences between treatment arms. Median PFS, hPFS, and time to deterioration in QoL were numerically greater for TARE/Chemo in both subgroups vs the primary population, with the greatest magnitude of difference in subgroup B. Both subgroups exhibited higher percentage of CEA responders and improved ORR with TARE/Chemo vs chemo alone. Safety (reported as event rate/100 patient-years) was higher with Chemo in all populations. Additional efficacy analyses in the primary population are also reported.

Conclusions
Careful patient selection, including consideration of the prognostic factors ECOG, baseline CEA, and KRAS status, sets outcome expectations in patients with colorectal liver metastases suitable for TARE/Chemo as second-line treatment (Trial Registry Number: NCT01483027).