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Atomic Hydrogen-21 cm transition (H  i) is an excellent tracer to study and understand the properties of the atomic gas in the Galaxy. Using the Westerbork Synthesis Radio Telescope, we observed 12 quasar sightlines to detect galactic H  i in absorption. We achieve an optical depth rms of ∼1−2 × 10−3, essential to detect the warm neutral medium (WNM). We detect H  i absorption in all our sightlines except along 1006+349, for which we set a strict upper limit on the spin temperature as 〈 T s〉 > 570 K. We find around 50 per cent of our sightlines have 〈 T s〉 > 500 K, indicating a WNM dominance. Further, we calculate an upper limit of the cold neutral medium (CNM) fraction along our sightlines and find a median CNM fraction of ∼0.12. With our observations, we reconfirm the existence of a threshold column density of ∼2 × 1020 |$\rm atoms \, cm^{-2}$| to form CNM in the interstellar medium (ISM). Using a two-temperature model of the H  i disc, we explore the distribution of spin temperature in the Galactic ISM. We find that a simple fixed axisymmetric two-temperature model could not produce either the observed column density or the integral optical depth. This indicates the existence of a more complex distribution of spin temperatures in the Galaxy. [ABSTRACT FROM AUTHOR]

Objectives Heparin-induced thrombocytopenia (HIT) is a rare but life-threatening condition that requires rapid diagnosis for proper management. Laboratory testing should only be performed on patients with intermediate- or high-risk pretest probability. The platelet factor 4 (PF4) enzyme-linked immunosorbent assay (ELISA) is the screening test that should be confirmed by higher specificity testing such as the heparin-induced platelet aggregation (HIPA) or the serotonin release assay (SRA). This study aims to evaluate the performance of the HIPA in comparison to the SRA, establish cutoffs of the PF4 ELISA to predict positivity for HIPA/SRA, and study the mortality rate between patients with suspected HIT confirmed as HIT positive vs negative. Methods All positive PF4 ELISA cases with confirmatory HIPA and SRA testing were included. As the SRA was considered the gold standard, the HIPA performance was evaluated in comparison to SRA before and after the implementation of a new standardized interpretation guide in 2022. The mortality of these cases was also documented by chart reviews. Results In total, 232 cases with positive or indeterminate anti-PF4 IgG ELISA had confirmatory testing with HIPA and SRA. The sensitivity of the HIPA improved from 55.4% in 2018 to 2021 to 73.8% in 2022. The specificity remained similarly high in 2018 to 2021 vs 2022 (94.9% vs 87.5%). The negative predictive value (NPV) improved in 2022. The PF4 optical density cutoff to predict the positivity of SRA was 0.85 vs 1.47 to predict the positivity of HIPA but decreased to 0.83 when combining HIPA and/or SRA. There was no significant difference in mortality between patients with suspected HIT confirmed positive vs negative. Conclusions Although the HIPA has a lower sensitivity than the SRA, the new standardized interpretation guide improved its sensitivity and NPV in 2022. Future improvements are needed to use the HIPA as a stand-alone confirmatory test with the goal to shorten hospital length of stay and expedite proper anticoagulation management. [ABSTRACT FROM AUTHOR]

Motivation When analyzing 1D time series, scientists are often interested in identifying regions where one variable depends linearly on the other. Typically, they use an ad hoc and therefore often subjective method to do so. Results Here, we develop a statistically rigorous, Bayesian approach to infer the optimal partitioning of a dataset not only into contiguous piece-wise linear segments, but also into contiguous segments described by linear combinations of arbitrary basis functions. We therefore present a general solution to the problem of identifying discontinuous change points. Focusing on microbial growth, we use the algorithm to find the range of optical density where this density is linearly proportional to the number of cells and to automatically find the regions of exponential growth for both Escherichia coli and Saccharomyces cerevisiae. For budding yeast, we consequently are able to infer the Monod constant for growth on fructose. Our algorithm lends itself to automation and high throughput studies, increases reproducibility, and should facilitate data analyses for a broad range of scientists. Availability and implementation The corresponding Python package, entitled Nunchaku, is available at PyPI: https://pypi.org/project/nunchaku. [ABSTRACT FROM AUTHOR]

This paper presents new optical and near-UV spectra of 11 extremely powerful jetted quasars, with radio to optical flux density ratio >103, which concomitantly cover the low-ionization emission of Mg  ii λ2800 and h β as well as the Fe  ii blends in the redshift range 0.35 ≲ z ≲ 1. We aim to quantify broad emission line differences between radio-loud (RL) and radio-quiet (RQ) quasars by using the 4D eigenvector 1 parameter space and its main sequence (MS) and to check the effect of powerful radio ejection on the low-ionization broad emission lines. The h β and Mg  ii λ2800 emission lines were measured by using non-linear multicomponent fittings as well as by analysing their full profile. We found that broad emission lines show large redward asymmetry both in h β and Mg  ii λ2800. The location of our RL sources in a UV plane looks similar to the optical one, with weak Fe  ii UV emission and broad Mg  ii λ2800. We supplement the 11 sources with large samples from previous work to gain some general inferences. We found that, compared to RQ, our extreme RL quasars show larger median h β full width at half maximum (FWHM), weaker Fe  ii emission, larger M BH, lower L bol/ L Edd, and a restricted bf space occupation in the optical and UV MS planes. The differences are more elusive when the comparison is carried out by restricting the RQ population to the region of the MS occupied by RL sources, albeit an unbiased comparison matching M BH and L bol/ L Edd suggests that the most powerful RL quasars show the highest redward asymmetries in h β. [ABSTRACT FROM AUTHOR]

The non-nitrogenous bisphosphonate clodronate disodium (CD) inhibits bone resorption and is approved for horses ≥ 4 yr of age. Extra-label use in juvenile exercising horses is a concern due to potential interference with normal bone growth and development. The objective was to determine the effects of single and repeated doses of CD on bone optical density (radiographic bone aluminum equivalence; RBAE) and lameness score (LS) in juvenile, exercising horses. Quarter Horses [n = 32 (16 geldings, 16 fillies); 500 ± 13 d of age; body weight (BW) = 336 ± 26 kg]) were used to test the hypothesis that horses receiving CD would have greater RBAE and reduced LS, and additional doses of CD would accentuate these effects. In a 168-d trial, horses were housed in individual stalls, and fed 1% BW/d concentrate and ad libitum Coastal bermudagrass hay. Horses were exercised 5 d/wk following a phase-based progressive workload using a free stall exerciser; Phase I (d 0 to 84) mimicked sales preparation whereas Phase II (d 85 to 168) simulated early training. Horses were stratified by age, BW, sex, and initial RBAE into control (CON; n = 8), single dose CD (1X; d 84; n = 8), 2-doses CD (2X; d 0 and d 84; n = 8), and four-doses CD (4X; d 0, d 42, d 84, d 126; n = 8). On injection d (0, 42, 84, and 126), horses were administered either 1.8 mg/kg BW CD (OSPHOS) or isovolumetric saline. On d 0, 84, and 168, dorsalpalmar and lateral-medial radiographs of the left third metacarpus and metatarsus were captured. An aluminum step wedge was included in each image and raw images were analyzed (Quantity One Basic, BioRad) to determine total bone RBAE at 1 cm distal to the nutrient foramen. On d 0 and d 168, horses were evaluated by a veterinarian unaware of treatment group and assigned a LS according to the American Association of Equine Practitioners Lameness Scale. The RBAE and LS data were analyzed via PROC MIXED and PROC GENMOD, respectively, in SAS. For each view, RBAE increased from d 0 to d 84 and remained increased to d 168 (P ≤ 0.02), regardless of treatment, likely due to progressing exercise protocol. On d 0, 29 horses were LS 0, 1 horse was LS 1, and 2 horses were LS 2; LS did not differ among treatment groups (P = 0.61). On d 168, 5 horses were LS 0, 13 horses were LS 2, 11 horses were LS 3, and 1 horse was LS 4; LS did not differ among treatments (P = 0.16). Based on these results, the hypothesis that single or repeated CD administration would increase RBAE and decrease lameness in juvenile, exercised Quarter Horses was rejected. [ABSTRACT FROM AUTHOR]

We present extensive energy levels (1110 levels) and transition data for the Pr  iv. We also show the effect of such atomic data on opacity for neutron star (NS) merger. We performed energy spectra and transition data calculations using the GRASP2018 package, which is based on the multiconfiguration Dirac–Hartree–Fock and relativistic configuration interaction methods. Using the GRASP2018 data, the opacities in the NS merger ejecta containing pure Pr are calculated. Energy levels are compared with recommended values from the NIST Atomic Spectra Database and other available works. Furthermore, electric dipole (E1) transition data, line strengths, weighted oscillator strengths, and transition rates are computed between the above levels. We estimate the uncertainties of the computed line strengths giving the accuracy class. The computed line strengths are also compared with other theoretical computations. We proposed few ways to estimate the uncertainties of the line strengths of the E1 transitions. Our calculation for opacity for a typical condition of NS merger ejecta at t ∼ 1 d shows that the Planck mean opacity of Pr3 + reaches |$\sim 1\, \rm cm^{2}\, g^{-1}$| at |$T\, \sim \, 15000$| K. The opacity is higher than that by the previous studies, thanks to the higher completeness of the atomic data. We also highlight the importance of accurate atomic data for the opacity by comparing it with the opacity using the atomic calculation from HULLAC. Moreover, we identify the important configurations, especially for the transitions between the high-lying levels for the opacity of 3+ ionized lanthanides. [ABSTRACT FROM AUTHOR]

Giant radio galaxies (GRGs) are radio galaxies that have projected linear extents of more than 700 kpc or 1 Mpc, depending on definition. We have carried out a careful visual inspection in search of GRGs of the Boötes LOw-Frequency ARray Deep Field image at 150 MHz. We identified 74 GRGs with a projected size larger than 0.7 Mpc of which 38 are larger than 1 Mpc. The resulting GRG sky density is about 2.8 (1.43) GRGs per square degree for GRGs with linear size larger than 0.7 (1) Mpc. We studied their radio properties and the accretion state of the host galaxies using deep optical and infrared survey data and determined flux densities for these GRGs from available survey images at both 54 MHz and 1.4 GHz to obtain integrated radio spectral indices. We show the location of the GRGs in the P–D diagram. The accretion mode on to the central black holes of the GRG hosts is radiatively inefficient suggesting that the central engines are not undergoing massive accretion at the time of the emission. Interestingly, 14 out of 35 GRGs for which optical spectra are available show a moderate star-formation rate (10–100 |$\rm M_{\odot }\,yr^{-1}$|⁠). Based on the number density of optical galaxies taken from the Dark Energy Spectroscopic Instrument survey DR9 photometric redshift catalogue, we found no significant differences between the environments of GRGs and other radio galaxies, at least for redshift up to z = 0.7. [ABSTRACT FROM AUTHOR]

Aims: The purpose of this study was to compare the effect of hop extracts with diverse β‐acid concentrations on Streptococcus mutans biofilm formation. Methods and Results: Ten different hop extracts, with α‐acid concentrations similar to those found in commercial beer products and β‐acid concentrations ranging from 2.6 to 8.1%, were added to distilled water to make standardized concentrations. S. mutans isolates were treated with hop extract dilutions varying from 1:2 to 1:256. The minimum inhibitory, minimum bactericidal and minimum biofilm inhibitory concentrations were determined and the optical density was evaluated. Live/dead staining confirmed the bactericidal effects. Biofilm formation of several strains of S. mutans was significantly inhibited by hop extract dilutions of 1:2, 1:4, 1:8, 1:16 and 1:32. Strong negative correlations were observed between α‐ and β‐acid concentrations of the hop extracts and S. mutans total growth and biofilm formation. Conclusions: The use of hop extracts prepared similarly to commercial beer decreased S. mutans biofilm formation. Significance and Impact of the Study: The inclusion of hops in the commercial beer products may provide beneficial health effects. Further studies are warranted to determine an effect in vivo on the development of dental caries. [ABSTRACT FROM AUTHOR]

Some microalgal species can increase their collective size by forming colonies; notable examples are chained colonies in diatoms and Scenedesmus sp. and spherical colonies in Phaeocystis globosa. For a given cell-specific growth rate, chain formation increases collective length quickly to fend off ciliates, but not against tube- and pallium-feeding heterotrophic dinoflagellates or metazoan grazers with ability to manipulate chains to aid ingestion. Sphere increases in volume relatively slowly but would be difficult to manipulate even for metazoan grazers. Diffusive nutrient supply to a chained colony would be a fixed proportion of that to solitary cells, regardless of chain length, whereas cells within a spherical colony would experience increasing nutrient limitation with increasing colony size. One hemisphere of a spherical colony would inevitably receive less irradiance, creating an auto-light limitation. Experimental data showed that light decreased substantially as it passed through a P. globosa colony, and the optical density of the colony increased linearly with colony diameter. However, neither in situ nutrient nor light limitation alone can explain an order-of-magnitude difference in colony size between the European and the Asian P. globosa populations. Instead, some evidence of different expression of gene(s) involved in colony formation and enlargement suggests genomic variations among the different populations. [ABSTRACT FROM AUTHOR]

A new set of radiative parameters for spectral lines in La  v – x ions is reported in this paper. These data were determined through the use of a multiplatform approach involving three independent theoretical methods, i.e. the relativistic Hartree–Fock method including core-polarization corrections (HFR + CPOL), the multiconfiguration Dirac–Hartree–Fock (MCDHF) method, and the particle-hole configuration-interaction (PH-CI) method implemented in the AMBiT program. Based on cross-comparisons between the results obtained with these three methods, and from comparisons with the few previously published experimental and theoretical data, the most complete and reliable set of wavelengths, transition probabilities, and oscillator strengths was then used to determine the necessary opacities for the analysis of the spectra emitted in the early phases of kilonovae following neutron star mergers, i.e. for typical conditions corresponding to temperatures |$T \gt 20\,000 $|  K, a density ρ = 10−10 g cm−3, and a time after the merger t  = 0.1 d. [ABSTRACT FROM AUTHOR]

Background: Age-related hearing loss (ARHL) and retinal vessel changes have both been associated to neurodegeneration/dementia, suggesting a possible link between these 2 conditions in older age. We aimed to determine whether superficial and deep vascular density (SVD and DVD) of the capillary plexi of macular vasculature can be associated with peripheral ARHL and age-related central auditory central processing (CAPD).Method: We analyzed data on 886 older participants (65 years+, age range: 65-92 years) in the cross-sectional population-based Salus in Apulia Study. Optical coherence tomography angiography was used to measure SVD and DVD of the capillary plexi of the macula at the 3-mm circle area centered on the fovea (whole retina), the parafoveal quadrant, and foveal quadrant. Disabling peripheral ARHL was defined as >40 dB hearing level of pure tone average on the frequencies from 0.5, 1, 2, and 4 KHz in the better ear, and age-related CAPD as <50% at the Synthetic Sentence Identification with Ipsilateral Competitive Message test in at least one ear.Results: DVD at the whole retina and at the parafoveal quadrant were inversely associated only with age-related CAPD (odds ratio [OR]: 0.93, 95% confidence interval [CI]: 0.88-0.96 and OR: 0.94, 95 CI: 0.90-0.99, respectively). No further associations with peripheral ARHL were evident.Conclusions: Retinal vasculature is associated with central auditory processing pathology, possibly playing an important role in early detection and intervention. The association of retinal vascular density with age-related CAPD may bring us a further step forward in understanding the biological mechanisms underlying the links between neurodegeneration/dementia and ARHL. [ABSTRACT FROM AUTHOR]

We analyse spectra measured by the Jovian Infrared Auroral Mapper (JIRAM, a payload element of the NASA Juno mission) in the 3150–4910 cm−1 (2.0–3.2  μ m)  range during the perijiove passage of 2016 August. Despite modelling uncertainties, the quality and the relative uniformity of the data set allow us to determine several parameters characterizing the Jupiter's upper troposphere in the latitude range of 35°S–30°N. Ammonia relative humidity at 500 millibars varies between 5 per cent to supersaturation beyond 100 per cent for about 3 per cent of the processed spectra. Ammonia appears depleted over belts and relatively enhanced over zones. Local variations of ammonia, arguably associated with local dynamics, are found to occur in several locations on the planet (Oval BA, South Equatorial Belt). Cloud altitude, defined as the level where aerosol opacity reaches unit value at 3650 cm−1 (2.74  μ m), is maximum over the Great Red Spot (>20 km  above the 1 bar  level) and the zones (15 km),  while it decreases over the belts and towards higher latitudes. The aerosol opacity scale height suggests more compact clouds over zones and more diffuse clouds over belts. The integrated opacity of clouds above the 1.3-bar pressure level is found to be minimum in regions where thermal emission of the deeper atmosphere is maximum. The opacity of tropospheric haze above the 200-mbar level also increases over zones. Our results are consistent with a Hadley-type circulation scheme previously proposed in literature for belts and zones, with clear hemisphere asymmetries in cloud and haze. [ABSTRACT FROM AUTHOR]

Aims: Microbial induced calcium carbonate precipitation (MICP) is one of the bio‐cementation methods for improving granular soils. This study evaluate the feasibility of obtaining a bacterial solution with high optical density and urease activity by an inexpensive corn steep liquor (CSL) medium in non‐sterile conditions in order to achieve sand improvement. Methods and Results: Corn steep liquor media with different concentrations (different dilution rates) were prepared and, without any autoclaving (non‐sterile conditions), different percentage of the inoculum solutions were added to them and incubated. Effect of inoculum solution percentage and CSL dilution rates on specifications of bacterial solution was evaluated. Urease activity and scanning electron microscope (SEM) and X‐Ray Diffraction (XRD) were used to efficiency of CLS media in sand improvement. The considerable urease activity was measured as 5·7 mS cm−1 min−1 using nonsterile CLS. By using CYNU (CSL‐Yeast extract‐NH4Cl‐Urea) bacterial solution, the urease activity of 5·5 mS cm−1 min−1 for the OD600 (optical density at 600 nm) of 1·88 and, consequently, specific urease activity of 2·93 mS cm−1 min−1 OD600−1 was obtained. The highest unconfined compressive strength (811 kPa) was obtained for the CYNU. XRD revealed new calcite peaks next to the quartz peaks. Conclusions: Production of inexpensive bacterial solution using diluted CSL as the inexpensive, effective and powerful culture media for Sporosarcina pasteurii cultivation in nonsterile conditions, allows geotechnical and biotechnological engineers to use MICP technology more widely in land improvement and field‐scale bio‐cementation and bioremediation projects. Significance and Impact of the Study: Obtaining high urease activity of inexpensive microbial solution using diluted CSL as the culture medium in nonsterile conditions, as the unique results of this study, can be significant in the field of bioremediation studies using MICP. [ABSTRACT FROM AUTHOR]

Background Breastfeeding is associated with healthier weight and nutrient status in early life. However, the impact of breastfeeding on carotenoid status beyond infancy, and the influence of adiposity, are unknown. Objectives The aim of the study was to retrospectively investigate the relation between breastfeeding and carotenoid status, and the mediating effect of weight status and adiposity on this relation, among school-age children. Methods This was a secondary analysis of baseline data collected from a randomized-controlled clinical trial. Children 7–12 y old (n  = 81) were recruited from East-Central Illinois. DXA was used to assess visceral adipose tissue (VAT) and whole-body total fat percentage (%Fat; i.e. whole-body adiposity). Weight was obtained to calculate children's BMI percentiles. Skin carotenoids were assessed via reflection spectroscopy. Macular carotenoids were assessed as macular pigment optical density (MPOD). Dietary, birth, and breastfeeding information was self-reported by parents. Results Skin carotenoids were inversely related to %Fat (P < 0.01), VAT (P < 0.01), and BMI percentile (P < 0.01). VAT and BMI percentile significantly mediated this relation between exclusive breastfeeding duration and skin carotenoids, after adjustment for dietary carotenoids, energy intake, and mother education. Conclusions Weight status and adipose tissue distribution mediate the positive correlation between exclusive breastfeeding duration and skin carotenoids among children aged 7–12 y. The results indicate the need to support breastfeeding and healthy physical growth in childhood for optimal carotenoid status. This trial was registered at clinicaltrials.gov as NCT03521349. [ABSTRACT FROM AUTHOR]

Large-scale calculations of atomic structures and radiative properties have been carried out for singly, doubly, and trebly ionized cerium. For this purpose, the purely relativistic multiconfiguration Dirac–Hartree–Fock (MCDHF) method was used, taking into account the effects of valence–valence and core–valence electronic correlations in detail. The results obtained were then used to calculate the expansion opacities characterizing the kilonovae observed as a result of neutron star mergers. Comparisons with previously published experimental and theoretical studies have shown that the results presented in this work are the most complete currently available, in terms of quantity and quality, concerning the atomic data and monochromatic opacities for Ce  ii , Ce  iii , and Ce  iv ions. [ABSTRACT FROM AUTHOR]

Molecular hydrogen is the main constituent of dense molecular clouds, but is expected to also be a dominant constituent in many environments where CO can no longer be seen, the so-called 'CO-dark molecular gas'. Based on comparisons of ultraviolet spectroscopy of H2 and optical line observations (4300 Å), CH is a prime candidate to trace H2. Since the optical line (and the UV lines at 3143, 3890, and 3878 Å) require bright background sources (and the CH N  = 2←1 ground state rotation line at 149 µm requires space-based, or stratospheric, observations), the hyperfine structure transition at 3335 MHz is a potentially important tool for probing the CO-dark molecular gas. However, the excitation of this transition is complicated, and has often been found to be inverted, making column density determinations uncertain. To clarify the potential use of the 3.3-GHz line as a proxy for H2, we have observed the CH 3335-MHz line with the Arecibo 305-m radio telescope along 16 lines of sight towards stars with existing measurements of the 4300-Å line. By comparing the CH column densities from optical and UV absorption lines to the CH radio emission line, we can derive the excitation temperature (T ex) of the 3335-MHz transition. We obtain a wide range of excitation temperatures for nine lines of sight, including some with | T ex| < 5 K. The common assumption that T ex for the 3335-MHz line is always much larger than the background temperature (T bg) is not always warranted and can lead to significant errors in the value of N (CH). [ABSTRACT FROM AUTHOR]

We present the results of flux density, spectral index, and polarization intra-night monitoring studies of a sample of eight optically bright blazars, carried out by employing several small to moderate aperture (0.4 to 1.5 m diameter) telescopes fitted with CCDs and polarimeters located in Europe, India, and Japan. The duty cycle of flux variability for the targets is found to be ∼45 per cent, similar to that reported in earlier studies. The computed two-point spectral indices are found to be between 0.65 to 1.87 for our sample, comprised of low- and intermediate-frequency peaked blazars, with one exception: they are also found to be statistically variable for about half the instances where 'confirmed' variability is detected in flux density. In the analysis of the spectral evolution of the targets on hourly time-scale, a counterclockwise loop (soft-lagging) is noted in the flux–spectral index plane on two occasions, and in one case a clear spectral flattening with the decreasing flux is observed. In our data set, we also observe a variety of flux–polarization degree variability patterns, including instances with a relatively straightforward anticorrelation, correlation, or counterclockwise looping. These changes are typically reflected in the flux–polarization angle plane: the anticorrelation between the flux and polarization degree is accompanied by an anticorrelation between the polarization angle and flux, while the counterclockwise flux–PD looping behaviour is accompanied by a clockwise looping in the flux–polarization angle representation. We discuss our findings in the framework of the internal shock scenario for blazar sources. [ABSTRACT FROM AUTHOR]

The economic viability of the biorefinery concept is limited by the valorization of lignin. One possible method of lignin valorization is biological upgrading with aromatic-catabolic microbes. In conjunction, lignin monomers can be produced by fast pyrolysis and fractionation. However, biological upgrading of these lignin monomers is limited by low water solubility. Here, we address the problem of low water solubility with an emulsifier blend containing approximately 70 wt% Tween® 20 and 30 wt% Span® 80. Pseudomonas putida KT2440 grew to an optical density (OD600) of 1.0 ± 0.2 when supplied with 1.6 wt% emulsified phenolic monomer-rich product produced by fast pyrolysis of red oak using an emulsifier dose of 0.076 ± 0.002 g emulsifier blend per g of phenolic monomer-rich product. This approach partially mitigated the toxicity of the model phenolic monomer p-coumarate to the microbe, but not benzoate or vanillin. This study provides a proof of concept that processing of biomass-derived phenolics to increase aqueous availability can enhance microbial utilization. [ABSTRACT FROM AUTHOR]

Current observational data of exoplanets are providing increasing detail of their 3D atmospheric structures. As characterization efforts expand in scope, the need to develop consistent 3D radiative-transfer methods becomes more pertinent as the complex atmospheric properties of exoplanets are required to be modelled together consistently. We aim to compare the transmission and emission spectra results of a 3D Monte Carlo radiative transfer (MCRT) model to contemporary radiative-transfer suites. We perform several benchmarking tests of an MCRT code, Cloudy Monte Carlo Radiative Transfer (cmcrt), to transmission and emission spectra model output. We add flexibility to the model through the use of k -distribution tables as input opacities. We present a hybrid MCRT and ray tracing methodology for the calculation of transmission spectra with a multiple scattering component. cmcrt compares well to the transmission spectra benchmarks at the 10s of ppm level. Emission spectra benchmarks are consistent to within 10 per cent of the 1D models. We suggest that differences in the benchmark results are likely caused by geometric effects between plane-parallel and spherical models. In a practical application, we post-process a cloudy 3D HD 189733b GCM model and compare to available observational data. Our results suggest the core methodology and algorithms of cmcrt produce consistent results to contemporary radiative transfer suites. 3D MCRT methods are highly suitable for detailed post-processing of cloudy and non-cloudy 1D and 3D exoplanet atmosphere simulations in instances where atmospheric inhomogeneities, significant limb effects/geometry or multiple scattering components are important considerations. [ABSTRACT FROM AUTHOR]

The galaxy cluster Abell 3733 (A3733) is a very suitable candidate in addressing dynamical processes throughout galaxy cluster mergers. This study shows structural analysis results of A3733 (z  = 0.038) based on X-ray and optical data. According to X-ray luminosity map, A3733 hosts two sub-structures separated in the sky by 0.25 Mpc, and the two distinct clumps are located in the East (A3733E) and the West (A3733W) directions. Both sub-structures are centred on two different brightest cluster galaxies (BCGs), and the X-ray and optical centroids of both BCGs substantially coincide with each other. The intracluster medium (ICM) temperatures of the sub-structures are estimated to be 2.79 keV for A3733E and 3.28 keV for A3733W. Both sub-structures are found to be hosting cool central gas (kT ∼ 1.5–2.5 keV) surrounded by hotter gas (kT ∼ 3.0–3.5 keV). Besides, the X-ray concentration parameters are found to be c ∼ 0.3 for each sub-structure. These results indicate the existence of cool centres for both sub-structures. The optical density map reveals a crowded galaxy population within the vicinity of A3733W. The high probable (per cent 88.2) dynamical binding model of A3733 suggests that the cores of sub-structures have a 3D separation of 0.27 Mpc and will collide in 0.14 Gyr with the relative in-falling velocity of 1936 km s−1. As a conclusion, this study demonstrates some evidence suggesting that the A3733 system is in the pre-merger state. [ABSTRACT FROM AUTHOR]

While the width–luminosity relation (WLR) among type Ia supernovae (slower is brighter) is one of the best-studied properties of this type of events, its physical basis has not been identified convincingly. The 'luminosity' is known to be related to a clear physical quantity – the amount of 56Ni synthesized, but the 'width' has not been quantitatively linked yet to a physical time-scale. We show that the recombination time of 56Fe and 56Co from doubly to singly ionized states causes the typical observed break in the colour curve B–V due to a cliff in the mean opacities and is a robust width measure of the light curve, which is insensitive to radiation transfer uncertainties. A simple photospheric model is shown to predict the recombination time to an accuracy of ∼5 d, allowing a quantitative understanding of the colour WLR. Two physical time-scales of the WLR are shown to be set by two column densities– the total column density that sets the gamma-ray escape time t 0 (previous Paper I) and the 56Ni column density that sets the recombination time (this Paper II). Central detonations of sub- |$\rm M_{ch}$| WDs and direct WD collision models have gamma-ray escape times and recombination times that are consistent with observations across the luminosity range of type Ia's. Delayed detonation Chandrasekhar mass models have recombination times that are broadly consistent with observations, with tension at the bright end of the luminosity range and inconsistent gamma-ray escape times at the faint end. [ABSTRACT FROM AUTHOR]

We present new Herschel -derived images of warm dust in the Andromeda galaxy, M31, with unprecedented spatial resolution (∼30 pc), column density accuracy, and constraints on the three-dimensional distributions of dust temperature and dust opacity index (hence grain size and composition), based on the new ppmap Bayesian analysis procedure. We confirm the overall radial variation of dust opacity index reported by other recent studies, including the central decrease within ∼3 kpc of the nucleus. We also investigate the detailed distribution of dust in the nuclear region, a prominent feature of which is an ∼500 pc bar-like structure seen previously in H α. The nature of this feature has been the subject of some debate. Our maps show it to be the site of the warmest dust, with a mean line-of-sight temperature ∼30 K. A comparison with the stellar distribution, based on 2MASS data, provides strong evidence that it is a gravitationally induced bar. A comparison with radial velocity maps suggests the presence of an inflow towards the nucleus from opposite directions along this bar, fed presumably by the nuclear spiral with which it appears to connect. Such behaviour is common in large-scale bars in spiral galaxies, as is the phenomenon of nested bars whereby a subkiloparsec nuclear bar exists within a large-scale primary bar. We suggest that M31 represents an example of such nesting. [ABSTRACT FROM AUTHOR]

A new line list for ethylene, 12C21H4, is presented. The line list is based on high-level ab initio potential energy and dipole moment surfaces. The potential energy surface is refined by fitting to experimental energies. The line list covers the range up to 7000 cm−1 (1.43 μm) with all ro-vibrational transitions (50 billion) with the lower state below 5000 cm−1 included and thus should be applicable for temperatures up to 700 K. A technique for computing molecular opacities from vibrational band intensities is proposed and used to provide temperature-dependent cross-sections of ethylene for shorter wavelength and higher temperatures. When combined with realistic band profiles (such as the proposed three-band model), the vibrational intensity technique offers a cheap but reasonably accurate alternative to the full ro-vibrational calculations at high temperatures and should be reliable for representing molecular opacities. The C2H4 line list, which is called MaYTY, is made available in electronic form from the CDS (http://cdsarc.u-strasbg.fr) and ExoMol (www.exomol.com) databases. [ABSTRACT FROM AUTHOR]

The thermal state of the post-reionization IGM is sensitive to the timing of reionization and the nature of the ionizing sources. We have modelled here the thermal state of the IGM in cosmological radiative transfer simulations of a realistic, extended, spatially inhomogeneous hydrogen reionization process, carefully calibrated with Ly α forest data. We compare these with cosmological simulations run using a spatially homogeneous ionizing background. The simulations with a realistic growth of ionized regions and a realistic spread in reionization redshifts show, as expected, significant spatial fluctuations in the temperature--density relation (TDR) of the post-reionization IGM. The most recently ionized regions are hottest and exhibit a flatter TDR. In simulations consistent with the average TDR inferred from Ly α forest data, these spatial fluctuations have a moderate but noticeable effect on the statistical properties of the Ly α opacity of the IGM at z ~ 4-6. This should be taken into account in accurate measurements of the thermal properties of the IGM and the free-streaming of dark matter from Ly α forest data in this redshift range. The spatial variations of the TDR predicted by our simulations are, however, smaller by about a factor of 2 than would be necessary to explain the observed large spatial opacity fluctuations on large (≥50 h-1 comoving Mpc) scales at z ... 5.5. [ABSTRACT FROM AUTHOR]

Clues to the physical conditions in radio cores of blazars come from measurements of brightness temperatures as well as effects produced by intrinsic opacity. We study the properties of the ultra-compact blazar AO0235+164 with RadioAstron ground-space radio interferometer, multifrequency VLBA, EVN, and single-dish radio observations. We employ visibility modelling and image stacking for deriving structure and kinematics of the source, and use Gaussian process regression to find the relative multiband time delays of the flares. The multifrequency core size and time lags support prevailing synchrotron self-absorption. The intrinsic brightness temperature of the core derived from ground-based very long baseline interferometry (VLBI) is close to the equipartition regime value. In the same time, there is evidence for ultra-compact features of the size of less than 10 μas in the source, which might be responsible for the extreme apparent brightness temperatures of up to 1014 K as measured by RadioAstron. In 2007-2016 the VLBI components in the source at 43 GHz are found predominantly in two directions, suggesting a bend of the outflow from southern to northern direction. The apparent opening angle of the jet seen in the stacked image at 43 GHz is two times wider than that at 15 GHz, indicating a collimation of the flow within the central 1.5 mas. We estimate the Lorentz factor Γ = 14, the Doppler factor δ = 21, and the viewing angle θ = 1.7° of the apparent jet base, derive the gradients of magnetic field strength and electron density in the outflow, and the distance between jet apex and the core at each frequency. [ABSTRACT FROM AUTHOR]

Stark width regularities within spectral series of the lithium isoelectronic sequence have been studied in an approach that includes both neutrals and ions. The influence of environmental conditions and certain atomic parameters on the Stark widths of spectral lines has been investigated. This study gives a simple model for the calculation of Stark broadening data for spectral lines within the lithium isoelectronic sequence. The proposed model requires fewer parameters than any other model. The obtained relations were used for predictions of Stark widths for transitions that have not yet been measured or calculated. In the framework of the present research, three algorithms for fast data processing have been made and they enable quality control and provide verification of the theoretically calculated results. [ABSTRACT FROM AUTHOR]

We are entering the era of high-precision and high-resolution spectroscopy of exoplanets. Such observations herald the need for robust self-consistent spectral models of exoplanetary atmospheres to investigate intricate atmospheric processes and to make observable predictions. Spectral models of plane-parallel exoplanetary atmospheres exist, mostly adapted from other astrophysical applications, with different levels of sophistication and accuracy. There is a growing need for a new generation of models custom-built for exoplanets and incorporating state-of-the-art numerical methods and opacities. The present work is a step in this direction. Here we introduce GENESIS, a plane-parallel, self-consistent, line-by-line exoplanetary atmospheric modelling code that includes (a) formal solution of radiative transfer using the Feautrier method, (b) radiative-convective equilibrium with temperature correction based on the Rybicki linearization scheme, (c) latest absorption cross-sections, and (d) internal flux and external irradiation, under the assumptions of hydrostatic equilibrium, local thermodynamic equilibrium and thermochemical equilibrium. We demonstrate the code here with cloud-free models of giant exoplanetary atmospheres over a range of equilibrium temperatures, metallicities, C/O ratios and spanning non-irradiated and irradiated planets, with and without thermal inversions. We provide the community with theoretical emergent spectra and pressure-temperature profiles over this range, along with those for several known hot Jupiters. The code can generate self-consistent spectra at high resolution and has the potential to be integrated into general circulation and non-equilibrium chemistry models as it is optimized for efficiency and convergence. GENESIS paves the way for high-fidelity remote sensing of exoplanetary atmospheres at high resolution with current and upcoming observations. [ABSTRACT FROM AUTHOR]

The highly luminous and variable prompt emission in Gamma-Ray Bursts (GRBs) arises in an ultra-relativistic outflow. The exact underlying radiative mechanism shaping its non-thermal spectrum is still uncertain, making it hard to determine the outflow's bulk Lorentz factor Γ. GRBs with spectral cutoff due to pair production (γγ → e+e-) at energies Ec ≳ 10MeV are extremely useful for inferring Γ. We find that when the emission region has a high enough compactness, then as it becomes optically thick to scattering, Compton downscattering by non-relativistic e±-pairs can shift the spectral cutoff energy well below the self-annihilation threshold, Esa = Γmec²/(1+z). We treat this effect numerically and show that Γ obtained assuming Ec = Esa can under-predict its true value by as much as an order of magnitude. [ABSTRACT FROM AUTHOR]

I examine a possible spectral distortion of the Cosmic Microwave Background (CMB) due to its absorption by galactic and intergalactic dust. I show that even subtle intergalactic opacity of 1 x 10-7 mag h Gpc-1 at the CMB wavelengths in the local Universe causes non-negligible CMB absorption and decline of the CMB intensity because the opacity steeply increases with redshift. The CMB should be distorted even during the epoch of the Universe defined by redshifts z < 10. For this epoch, the maximum spectral distortion of the CMB is at least 20 x 10-22 Wm-2 Hz-1 sr-1 at 300 GHz being well above the sensitivity of the COBE/FIRAS, WMAP or Planck flux measurements. If dust mass is considered to be redshift dependent with noticeable dust abundance at redshifts 2-4, the predicted CMB distortion is even higher. The CMB would be distorted also in a perfectly transparent universe due to dust in galaxies but this effect is lower by one order than that due to intergalactic opacity. The missing dust signature in the CMB measurements is intriguing and questions either opacity and extinction law measurements or validity of the current model of the Universe. [ABSTRACT FROM AUTHOR]

We present the first results from applying the spectral inversion technique in the cloudy L dwarf regime. Our newframework provides a flexible approach to modelling cloud opacity which can be built incrementally as the data require and improves upon previous retrieval experiments in the brown dwarf regime by allowing for scattering in two-stream radiative transfer. Our first application of the tool to two mid-L dwarfs is able to reproduce their near-infrared spectra far more closely than grid models. Our retrieved thermal, chemical and cloud profiles allow us to estimate Teff = 1796+23-25 K and log g = 5.21+0.05-0.08 for 2MASS J05002100+0330501, and for 2MASSW J2224438-015852 we find Teff = 1723+18-19 K and log g = 5.31+0.04-0.08, in close agreement with previous empirical estimates. Our best model for both objects includes an optically thick cloud deck which passes τ cloud ≥ 1 (looking down) at a pressure of around 5 bar. The temperature at this pressure is too high for silicate species to condense, and we argue that corundum and/or iron clouds are responsible for this cloud opacity. Our retrieved profiles are cooler at depth and warmer at altitude than the forward grid models that we compare, and we argue that some form of heating mechanism may be at work in the upper atmospheres of these L dwarfs. We also identify anomalously high CO abundance in both targets, which does not correlate with the warmth of our upper atmospheres or our choice of cloud model, and find similarly anomalous alkali abundance for one of our targets. These anomalies may reflect unrecognized shortcomings in our retrieval model or inaccuracies in our gas phase opacities. [ABSTRACT FROM AUTHOR]

An accurate line list of spectroscopic transitions is presented for the hot ZrS molecule. The lowest-lying 11 singlet and triplet states are considered by using the methods of complete active-space self-consistent field (CASSCF) and the multireference single and double configuration interaction method (MRSDCI). Potential energy curves are constructed by using large basis sets aug-cc-pVQZ-PP with relativistic effective core potentials at the spin-free level. Dipole moments curves, used to obtain transition intensities, are computed using high levels of theory (MRSDCI). Several spectroscopic constants were calculated for the investigated states (Te, ωe, re, Be and De). This absorption line list contains over 2 million transitions between almost 14 900 energy levels. It covers the frequency range between 0 and 20 000 cm−1 and includes all transitions from energy levels within the lowest six singlet electronic states. The effect of temperature on the spectra of hot ZrS was investigated with a partition function calculated between 298 K and 2000 K. The present work should help in identifying the singlet state spectrum of hot ZrS. [ABSTRACT FROM AUTHOR]

We investigate the dust distribution in the crescent disk around HD 142527 based on the continuum emission at 890μm obtained by ALMA Cycle 0. The map is divided into 18 azimuthal sectors, and the radial intensity profile in each sector is reproduced with a two-dimensional diskmodel. Ourmodel takes account of scattering and inclination of the disk as well as the azimuthal dependence in intensity. When the dust is assumed to have the conventional composition and a maximum size of 1mm, the northwestern region (PA = 291°-351°) cannot be reproduced. This is because the model intensity becomes insensitive to the increase in surface density due to heavy self-scattering, reaching its ceilingmuch lower than the observed intensity. The ceiling depends on the position angle, PA. When the scattering opacity is reduced by a factor of 10, the intensity distribution is reproduced successfully in all the sectors, including those in the northwestern region. The best-fitting model parameters depend little on the scattering opacity in the southern region where the disk is optically thin. The contrast ratio of dust surface densities along PA is derived to be about 40, much smaller than the value in the case of conventional opacities (70-130). These results strongly suggest that the albedo is lower than that considered for some reason, at least in the northwestern region. [ABSTRACT FROM AUTHOR]

The observed extragalactic background light (EBL) is affected by light attenuation due to absorption of light by galactic and intergalactic dust in the Universe. Even galactic opacity of 10-20 per cent and minute universe intergalactic opacity of 0.01 mag h Gpc-1 at the local Universe have a significant impact on the EBL because obscuration of galaxies and density of intergalactic dust increase with redshift as (1 + z)³. Consequently, intergalactic opacity increases and the Universe becomes considerably opaque at z > 3. Adopting realistic values for galactic and intergalactic opacity, the estimates of the EBL for the expanding dusty universe are close to observations. The luminosity density evolution fits well measurements. The model reproduces a steep increase of the luminosity density at z < 2, its maximum at z = 2-3, and its decrease at higher redshifts. The increase of the luminosity density at low z is not produced by the evolution of the star formation rate but by the fact that the Universe occupied a smaller volume in previous epochs. The decline of the luminosity density at high z originates in the opacity of the Universe. The calculated bolometric EBL ranges from 100 to 200 nWm-2 sr-1 and is within the limits of 40 and 200 nWm-2 sr-1 of current EBL observations. The model predicts 98 per cent of the EBL coming from radiation of galaxies at z < 3.5. Accounting for light extinction by intergalactic dust implies that the Universe was probably more opaque than dark for z > 3.5. [ABSTRACT FROM AUTHOR]

The GeV-range spectra of blazars are shaped not only by non-thermal emission processes internal to the relativistic jet but also by external pair-production absorption on the thermal emission of the accretion disc and the broad-line region (BLR). For the first time, we compute here the pair-production opacities in the GeV range produced by a realistic BLR accounting for the radial stratification and radiation anisotropy. Using photoionization modelling with the CLOUDY code, we calculate a series of BLR models of different sizes, geometries, cloud densities, column densities and metallicities. The strongest emission features in the model BLR are Ly α and He II Ly α. Contribution of recombination continua is smaller, especially for hydrogen, because Ly continuum is efficiently trapped inside the large optical depth BLR clouds and converted to Lyman emission lines and higher order recombination continua. The largest effects on the gamma-ray opacity are produced by the BLR geometry and localization of the gamma-ray source. We show that when the gamma-ray source moves further from the central source, all the absorption details move to higher energies and the overall level of absorption drops because of decreasing incidence angles between the gamma-rays and BLR photons. The observed positions of the spectral breaks can be used to measure the geometry and the location of the gamma-ray emitting region relative to the BLR. Strong dependence on geometry means that the soft photons dominating the pair-production opacity may be actually produced by a different population of BLR clouds than the bulk of the observed broad line emission. [ABSTRACT FROM AUTHOR]

We have measured the transmission spectrum of the extremely inflated hot Jupiter WASP-52b using simultaneous photometric observations in SDSS u′, g′ and a filter centred on the sodium doublet (NaI) with the ULTRACAM instrument mounted on the 4.2m William Herschel Telescope. We find that Rayleigh scattering is not the dominant source of opacity within the planetary atmosphere and find a transmission spectrum more consistent with wavelength-independent opacity such as from clouds. We detect an in-transit anomaly that we attribute to the presence of stellar activity and find that this feature can be more simply modelled as a bright region on the stellar surface akin to Solar faculae rather than spots. A spot model requires a significantly larger planet/star radius ratio than that found in previous studies. Our results highlight the precision that can be achieved by ground-based photometry with errors in the scaled planetary radii of less than one atmospheric scale height, comparable to HST observations [ABSTRACT FROM AUTHOR]

The performance of recently developed polydimethylsiloxane (PDMS)-based optical system was tested for measuring optical density of microbial culture. The data showed that PDMS-based spectrometer is superior to “one drop” spectrometers in the accuracy, and has an advantage over conventional spectrometers in measuring dense culture without dilution. [ABSTRACT FROM PUBLISHER]

OBJECTIVES: To identify epidermal growth factor receptor (EGFR) mutation status between different lesions in lung adenocarcinoma presenting as multiple ground-glass opacity (GGO) lesions and analyse its association with clinical characteristics. METHODS: Seventy-eight patients with lung adenocarcinoma presenting as multiple GGO lesions were identified to investigate EGFR mutation in exon 18-21. Lesions with the largest size in diameter were defined as the primary lesions; the others were defined as the secondary lesions. One hundred and fifty-nine lesions of these patients were classified into pure GGO and mixed GGO by computed tomography scan images. RESULTS: The EGFR mutation rate in the patients was 48.7% (38 of 78). Patients with high frequency of EGFR mutation were females and non-smokers. The EGFR mutation rate of invasive adenocarcinoma was higher than that of atypical adenomatous hyperplasia/adenocarcinoma in situ and minimally invasive adenocarcinoma (P = 0.001). Although 19-deletion and L858R were the most common EGFR mutations, there was no difference of EGFR mutation in pathological subtypes of adenocarcinoma. Of the 38 paired lesions in patients harbouring EGFR mutation, the discordance rate of EGFR mutation was 92.1%. CONCLUSIONS: The study showed different EGFR mutational profiles in multiple GGO lesions, suggesting that lesions seem to arise as independent events. It would offer useful information for determining the appropriate treatment strategy for lung adenocarcinoma presenting as multiple GGO lesions. [ABSTRACT FROM AUTHOR]

While narrow absorption lines (NALs) are relatively stable, broad absorption lines (BALs) and mini-BAL systems usually show violent time variability within a few years via a mechanism that is not yet understood. In this study, we examine the variable ionization state (VIS) scenario as a plausible mechanism, as previously suspected. Over three years, we performed photometric monitoring observations of four mini-BAL and five NAL quasars at zem ~ 2.0-3.1 using the 105cm Kiso Schmidt Telescope in u, g, and i bands. We also performed spectroscopic monitoring observation of one of our mini-BAL quasars (HS1603+3820) using the 188 cm Okayama Telescope over the same period as the photometric observations. Our main results are as follows: (1) Structure function (SF) analysis revealed that the quasar UV flux variability over three years was not large enough to support the VIS scenario, unless the ionization condition of outflow gas is very low. (2) There was no crucial difference between the SFs of mini-BAL and NAL quasars. (3) The variability of the mini-BAL and quasar light curves was weakly synchronized with a small time delay for HS1603+3820. These results suggest that the VIS scenario may need additional mechanisms such as variable shielding by X-ray warm absorbers. [ABSTRACT FROM AUTHOR]

Objective: To develop an alpha dosimetry technique for activity calibration of alpha-emitting radiopharmaceuticals using the Gafchromic EBT3 (Gaf-EBT3) radio chromic film (International Speciality product, Wayne, NJ). Methods: The Gaf-EBT3 has a tissue equivalent radiosensitive layer (approximately 28p,m) sandwiched between two 100-μm thick polyester sheaths, thereby making it insensitive to alpha particles. We have split a Gaf-EBT3 sheet using a surgical scalpel to remove one of the polyester protective layers and covered the radiosensitive layer with thin Mylar* foil (Goodfellow Cambridge Limited, Huntingdon, UK) (2.5μm). Small pieces of modified film were exposed at contact with a 560-Bq thin 241Am source for 5, 10, 24 and 94 h. The optical density of the films was evaluated using an optical densitometer. The alpha energy spectra of the 241Am source were recorded using a Si(Li) surface barrier detector. Results: Time-integrated specific alpha surface activity ( kBq cm-2h) was represented as a function of optical density. Conclusion: By removing one of the 100 μm thick polyester protective layers, the authors have modified the Gaf- EBT3 film to a sensitive alpha dosemeter. The calibration function relevant to a 241,Am reference source was evaluated from the optical densities of the dosemeter foils. Furthermore, calibration functions for important alpha emitters such as 223Ra, 225Ac or 210Bi were parameterized from the 241Am reference data. Advances in knowledge: The authors have developed and tested the principle of a clinical alpha dosemeter using Gaf-EBT3 radiochromic films originally developed for photon dosimetry. This novel, user-friendly technique could be implemented in quality assurance and calibration procedures of important alpha-emitting radiopharmaceuticals prior to their clinical applications. [ABSTRACT FROM AUTHOR]

We examine the apparent photosphere, thermalization surface and expected spectrum of a black hole wind, which is an optically thick, spherically symmetric outflow blown off from the very center of a black hole, taking into account the frequency dependence of opacities. In the case of the optically thick spherical wind, the apparent photosphere is generally aspherical, since the wind density gradually decreases with radius. In addition, if electron scattering is important, the thermalization surface decouples with the apparent photosphere, and is located deep inside it. Furthermore, since the free-free opacity depends on frequency, the location of the thermalization surface also depends on frequency. We find that the shape of the apparent photosphere is aspherical, but does not depend on frequency so much. On the other hand, in the low-frequency regime the thermalization surface is located somewhat closely to the apparent photosphere, and its shape is aspherical, since the free-free opacity dominates the electron scattering one at low frequencies. In the high-frequency regime, however, the thermalization surface is located deep inside the flow, and its shape is nearly spherical, since the electronscattering opacity dominates the free-free one at high frequencies. As a result, the expected spectrum becomes a multi-temperature blackbody one; the spectrum has a Wien peak, but the spectral slope below the peak is shallower than the Rayleigh-Jeans slope. This is partly due to the non-spherical shapes of the apparent photosphere and thermalization surface in some cases, but mainly because we observe a different part for different frequencies; i.e., low-frequency photons come from larger thermalization radii with lower temperatures, while high-frequency ones come from smaller thermalization radii with higher temperatures. [ABSTRACT FROM AUTHOR]

There has been growing observational evidence for the presence of condensates in the atmospheres and/or comet-like tails of extrasolar planets. As a result, systematic and homogeneous tables of dust properties are useful in order to facilitate further observational and theoretical studies. In this paper we present calculations and analysis of non-isotropic phase functions, asymmetry parameter (mean cosine of the scattering angle), absorption and scattering opacities, single scattering albedos, equilibrium temperatures, and radiative accelerations of dust grains relevant for extrasolar planets. Our assumptions include spherical grain shape, Deirmendjian particle size distribution, and Mie theory. We consider several species: corundum/alumina, perovskite, olivines with 0 and 50 per cent iron content, pyroxenes with 0, 20, and 60 per cent iron content, pure iron, carbon at two different temperatures, water ice, liquid water, and ammonia. The presented tables cover the wavelength range of 0.2-500 μm and modal particle radii from 0.01 to 100 μm. Equilibrium temperatures and radiative accelerations assume irradiation by a non-blackbody source of light with temperatures from 7000 to 700 K seen at solid angles from 2π to 10-6 sr. The tables are provided to the community together with a simple code which allows for an optional, finite, angular dimension of the source of light (star) in the phase function. [ABSTRACT FROM AUTHOR]

Staphylococci are important mastiticpathogens of humans and livestock. Chlorate is reported to be a potent inhibitor against staphylococci but adaptation by the microbes can occur. Presently, we cultured multi-drug resistant Staphylococcus aureus strain ATCC 12600 anaerobically at 39oC in nitratesupplemented (5 mM) Tryptic Soy broth. The broth was treated without (control) or alone with 5 mM sodium chlorate (ClO3) or 9 mM of either 2-nitro-1-propanol (NPOH), ethyl nitroacetate (ENA) or ethyl 2-nitropropionate (E2NPA) or with combinations of CLO3 and respective nitrocompound. Control and treated cultures were incubated in triplicate and growth was measured via absorbance (600 nm) at during 9 h. An analysis of variance revealed an inhibitory effect of treatments (P < 0.05; SEM = 0.078) on mean specific growth rates of S. aureus, with rates during logarithmic growth being most rapid in controls and cultures treated with ENA or EN2PA (1.45, 1.23 and 1.21 h-1, respectively) and more than 92% slower in NPOH and NPOH+CLO3-treated cultures (0.09 and 0.03 h-1, respectively). Growth rates of cultures treated solely with CLO3 (0.66 h-1) were more than 50% slower than controls and were decreased further in cultures treated with combinations of CLO3 plus E2NPA or ENA (0.39 and 0.45 h-1). After 9 h of growth, maximum optical densities (maxOD) were highest for controls and cultures treated with ENA or EN2PA (0.52, 0.52 and 0.50 maxOD, respectively), intermediate in cultures treated with CLO3 alone (0.21 maxOD) and lower yet in cultures treated with CLO3 plus ENA, E2NPA or NPOH (0.15, 0.11 and 0.02 maxOD, respectively). The maxOD for cultures treated with NPOH alone was 0.02 and did not differ from cultures treated with the combination of CLO3+NPOH. Results demonstrate marked synergistic and prolonging effects of combing ENA and E2NPA with CLO3 but no additional effect of the potent anti-staphylococcal activity of NPOH. [ABSTRACT FROM AUTHOR]

Frequency-dependent photon absorption and scattering transport cross-sections for iron-group elements were generated using a revised version of the OPAL opacity code. The calculations take advantage of advances in computers to generate improved atomic data as well as several fast algorithms developed for the computational demanding bound-bound spectrum. The new iron group calculations are combined with the existing OPAL data for lighter elements to generate astrophysical opacities at matter conditions applicable to B stars. The results are slightly reduced Rosseland mean opacities of Population I stars at the peak of the Z-bump. The analysis explores several uncertainties related to the iron group opacities and includes comparisons with existing OPAL and OP results. [ABSTRACT FROM AUTHOR]

Direct measurements of solar ultraviolet radiations (UVRs) have an important role in the protection of humans against UVR hazard. This work presents simple technique based on the application of EBT2 GAFCHROMIC® film for direct solar UVA dose assessment. It demonstrates the effects of different parts of the solar spectrum (UVB, visible and infrared) on performed UVA field measurements and presents the measurement uncertainty budget. The gradient of sunlight exposure level permitted the authors to establish the mathematical relationships between the measured solar UVA dose and two measured quantities: the first was the changes in spectral absorbance at the wavelength 633 nm (A633) and the second was the optical density (OD). The established standard relations were also applied to calculate the solar UVA dose variations during the whole day; 15 min of exposure each hour between 8:00 and 17:00 was recorded. Results show that both applied experimental methods, spectrophotometer absorbance and densitometer OD, deliver comparable figures for EBT2 solar UVA dose assessment with relative uncertainty of 11 % for spectral absorbance measurements and 15 % for OD measurements. [ABSTRACT FROM AUTHOR]

Aims To explore the predictions of a novel rearrangement of the Baranyi-Roberts model ( BRM) with time to detection data obtained from optical density data of microbial growth. Methods and Results Growth of Escherichia coli and Salmonella Typhimurium under mild conditions of temperature (25-37°C), salt (0·086, 0·51 and 1·03 mol l−1) and pH (6·85-4·5) was examined using optical density. Time to detection (TTD) data were fitted to a model based on a rearrangement of the BRM. Observations showed compatibility with standard viable count studies and produced highly accurate specific growth rates and lag phase durations. At high salt and low pH, however, there was a substantial dependency on the initial inoculum for the observation of visible growth. At 30 and 37°C, with 1·03 mol l−1 salt, and at pH <5·75, no visible growth was recorded for E. coli at initial inoculum levels below 107 CFU ml−1. Conclusions The rearranged BRM can be used directly with TTD data obtained from optical density measurements. Significance and Impact of the Study A distinct advantage of the rearranged model is that it allows for a very simple interpretation of easily obtainable data using standard nonlinear regression. The rearranged model gives to TTD data the same modelling capability that the BRM gives to plate count data. [ABSTRACT FROM AUTHOR]

Accurate and rapid Voigt function evaluations are an essential component of synthetic stellar spectrum calculations and the development of improved algorithms continues to be a priority. Multiprecision arithmetic was applied to obtain Voigt functions evaluated to 56 digits, which could be extended to arbitrarily high precision if required. While the technique cannot be used in practical applications, it provides results against which fast routines may be benchmarked for accuracy. [ABSTRACT FROM AUTHOR]

Objective: This meta-analysis is to determine the overall diagnostic yield of CT-guided transthoracic needle biopsy (TNB) of ground-glass opacity (GGO) lesions. Methods: A PubMed search was performed using "ground-glass opacity" crossed with "core biopsy" and " needle biopsy" . Test performance characteristics with the use of forest plots, summary receiver operating characteristic curves and bivariate random effects models were summarized. Adverse events, if reported, were recorded. Results: Our search identified 52 citations, of which 6 diagnostic studies evaluated 341 patients. Pooled specificity estimates were 0.94 [95% confidence interval (Cl), 0.84-0.98 ] and sensitivity estimates were 0.92 (95% Cl, 0.88-0.95), respectively. The positive likelihood ratio was 11.27 (95% Cl, 4.2-30.6), the negative likelihood ratio was 0.1 (95% Cl, 0.06-0.19), the diagnostic odds ratio was 131.38 (95% Cl, 39.6-436.0) and the area under the curve was 0.97. Conclusion: Our data suggest that the CT-guided TNB is likely to be a useful tool for tissue diagnosis and may serve as an alternative for further patient management with GGO lesions. However, considering the limited studies and patients included, large scale studies are needed to verify these findings. Advances in knowledge: Some studies about CT-guided TNB of GGO lesions have been published, most have been small, single-institution case series. To our knowledge, our study is the first systematic analysis about CT-guided TNB of GGO lesions. [ABSTRACT FROM AUTHOR]

We report the statistical properties of stars and brown dwarfs obtained from four radiation hydrodynamical simulations of star cluster formation that resolve masses down to the opacity limit for fragmentation. The calculations are identical except for their dust and gas opacities. Assuming dust opacity is proportional to metallicity, the calculations span a range of metallicities from 1/100 to 3 times solar, although we emphasize that changing the metallicity has other thermodynamic effects that the calculations do not capture (e.g. on the thermal coupling between gas and dust). All four calculations produce stellar populations whose statistical properties are difficult to distinguish from observed stellar systems, and we find no significant dependence of stellar properties on opacity. The mass functions and properties of multiple stellar systems are consistent with each other. However, we find that protostellar mergers are more common with lower opacities. Combining the results from the three calculations with the highest opacities, we obtain a stellar population consisting of more than 500 stars and brown dwarfs. Many of the statistical properties of this population are in good agreement with those observed in our Galaxy, implying that gravity, hydrodynamics, and radiative feedback may be the primary ingredients for determining the statistical properties of low-mass stars. However, we do find indications that the calculations may be slightly too dissipative. Although further calculations will be required to understand all of the effects of metallicity on stellar properties, we conclude that stellar properties are surprisingly resilient to variations of the dust and gas opacities. [ABSTRACT FROM AUTHOR]

We use MERLIN, VLA and VLBA observations of Galactic H i absorption towards 3C 138 to estimate the structure function of the H i opacity fluctuations at au scales. Using Monte Carlo simulations, we show that there is likely to be a significant bias in the estimated structure function at signal-to-noise ratios characteristic of our observations, if the structure function is constructed in the manner most commonly used in the literature. We develop a new estimator that is free from this bias and use it to estimate the true underlying structure function slope on length-scales ranging from 5 to 40 au. From a power-law fit to the structure function, we derive a slope of $0.81^{+0.14}_{-0.13}$, i.e. similar to the value observed at parsec scales. The estimated upper limit for the amplitude of the structure function is also consistent with the measurements carried out at parsec scales. Our measurements are hence consistent with the H i opacity fluctuation in the Galaxy being characterized by a power-law structure function over length-scales that span six orders of magnitude. This result implies that the dissipation scale has to be smaller than a few au if the fluctuations are produced by turbulence. This inferred smaller dissipation scale implies that the dissipation occurs either in (i) regions with densities ≳ 103cm−3 (i.e. similar to that inferred for ‘tiny scale’ atomic clouds or (ii) regions with a mix of ionized and atomic gas (i.e. the observed structure in the atomic gas has a magnetohydrodynamic origin). [ABSTRACT FROM AUTHOR]