Mean Molecular Mass Research Articles

WISDOM project XX. – Strong shear tearing molecular clouds apart in NGC 524

ABSTRACT Early-type galaxies (ETGs) are known to harbour dense spheroids of stars but scarce star formation (SF). Approximately a quarter of these galaxies have rich molecular gas reservoirs yet do not form stars efficiently. We study here the ETG NGC 524, with strong shear suspected to result in a smooth molecular gas disc and low star-formation efficiency (SFE). We present new spatially resolved observations of the 12CO(2-1)-emitting cold molecular gas from the Atacama Large Millimeter/sub-millimeter Array (ALMA) and of the warm ionized-gas emission lines from SITELLE at the Canada–France–Hawaii Telescope. Although constrained by the resolution of the ALMA observations (≈37 pc), we identify only 52 GMCs with radii ranging from 30 to 140 pc, a low mean molecular gas mass surface density 〈Σgas〉 ≈ 125 M⊙ pc−2 and a high mean virial parameter 〈αobs, vir〉 ≈ 5.3. We measure spatially resolved molecular gas depletion times (τdep ≡ 1/SFE) with a spatial resolution of ≈100 pc within a galactocentric distance of 1.5 kpc. The global depletion time is ≈2.0 Gyr but τdep increases towards the galaxy centre, with a maximum τdep, max ≈ 5.2 Gyr. However, no pure H ii region is identified in NGC 524 using ionized-gas emission-line ratio diagnostics, so the τdep inferred are in fact lower limits. Measuring the GMC properties and dynamical states, we conclude that shear is the dominant mechanism shaping the molecular gas properties and regulating SF in NGC 524. This is supported by analogous analyses of the GMCs in a simulated ETG similar to NGC 524.

A3COSMOS: Dissecting the gas content of star-forming galaxies across the main sequence at 1.2 ≤ z < 1.6

Aims. We aim to understand the physical mechanisms that drive star formation in a sample of mass-complete (>109.5 M⊙) star-forming galaxies (SFGs) at 1.2 ≤ ɀ < 1.6. Methods. We selected SFGs from the COSMOS2020 catalog and applied a uυ-domain stacking analysis to their archival Atacama Large Millimeter/submillimeter Array (ALMA) data. Our stacking analysis provides precise measurements of the mean molecular gas mass and size of SFGs down to a stellar mass of M★ ~ 109.5 M⊙, even though at these stellar mass galaxies on the main sequence (MS) are no longer detected individually in the archival ALMA data. We also applied an image-domain stacking analysis on their HST i-band and UltraVISTA J - and Ks-band images. This allowed us to trace the distribution of their stellar component. Correcting these rest-frame optical sizes using the Rhalf–stellar–light-to-Rhalf–stellar–mass conversion at rest 5000 Å, we obtain the stellar mass size of MS galaxies and compare them to the sizes of their star-forming component obtained from our ALMA stacking analysis. Results. Across the MS (−0.2 < ∆MS = log(SFR/SFRMS) < 0.2), the mean molecular gas fraction of SFGs increases by a factor of ~1.4, while their mean molecular gas depletion time decreases by a factor of ~1.8. The scatter of the MS could thus be caused by variations in both the star formation efficiency and molecular gas fraction of galaxies. The mean molecular gas fraction of MS galaxies decreases by a factor of ~7 from M★~ 109.7 M⊙ to ~1011.3 M⊙, while their mean molecular gas depletion time remains roughly the same at all stellar masses. This finding could be a hint that the bending of the MS at ɀ ~1.4 is primarily driven by variations in cold gas accretion. The majority of the galaxies lying on the MS have RFIR ≈ Rstellar. Their central regions are subject to large dust attenuation. Starbursts (SBs, ∆MS > 0.7) have a mean molecular gas fraction ~2.1 times larger and mean molecular gas depletion time ~3.3 times shorter than MS galaxies. Additionally, they have more compact star-forming regions (~2.5 kpc for MS galaxies vs. ~1.4 kpc for SBs) and systematically disturbed rest-frame optical morphologies, which is consistent with their association with major-mergers. SBs and MS galaxies follow the same relation between their molecular gas mass and star formation rate surface densities with a slope of ~ 1.1–1.2, that is, the so-called Kennicutt-Schmidt relation.

Phase equilibria of binary and ternary mixtures with poly(styrene-co-hexafluorobutyl methacrylate) and solvents at high pressure and temperature

This paper presents the synthesis of the fluoric copolymer poly(styrene-co-2,2,3,4,4,4-hexafluorobutyl methacrylate) [P(styrene-co-HFBMA)] through dispersed phase polymerization in a supercritical carbon dioxide (sc-CO2) medium. The physiochemical characteristics of P(styrene-co-HFBMA) were extensively studied by varying the styrene to HFBMA mole ratios (40:1, 25:1, and 20:1) and 2,2'-Azobisisobutyronitrile (AIBN) initiator at different mass percentages (mass%) from 1 to 4, along with the mean molecular mass (Mm). Phase transition data were reported for two-component and three-component P(styrene-co-HFBMA) in sc-C3H8, C3H6, C4H10, and C4H8, encompassing temperature “T” and pressure “P” limits (∼341 to ∼459) K, and (∼21 to ∼185) MPa, respectively. The phase behavior of the P(styrene-co-HFBMA) + solvent mixtures displayed an upper critical solution temperature (UCST) type behavior with a declining gradient. Equilibria curves were measured for the P(styrene-co-HFBMA) + (C3H10/C3H6) + CH3OCH3(i.e., DME) (25:1, AIBN mass%: 2.0) system in “P-T” phase diagram, spanning from the UCST region to LCST region at DME mass% ranging from 0.0 to 68.5. Additionally, solubility curves at “P”: up to ∼148 MPa and “T”: from ∼450 K to ∼350 K showed a shift from a declining slope to an inclined slope within the 0.0 to 60.3 mass% range for the P(styrene-co-HFBMA) (mole ratio:25:1; AIBN mass%: 2.0) + (C4H10/C4H8) + DME system. These findings provide valuable insights into the phase behavior and solubility characteristics of the P(styrene-co-HFBMA) copolymer in different sc-solvent mixtures.

Flame Characteristics and Abnormal Combustion of Methane Port Injection and Isooctane Direct Injection with Injection Timings Considered

Natural gas (NG) is a low-carbon fuel that can achieve low carbon emissions and high efficiencies. However, the low mean molecular mass and low energy density of methane result in low engine performance, and blending methane with gasoline is an effective way of improving the performance of NG engines. In this study, flame characteristics (including abnormal combustion) and engine performance are optically studied under methane port injection and isooctane direct injection conditions. The results indicate that the addition of isooctane can significantly increase the power output of NG engines. Under partial-load conditions, the minimum ignition advance for best IMEP is delayed with the addition of isooctane because of the higher flame speed of isooctane, and isooctane addition primarily improves the turbulent flame propagation rather than the initial flame formation. As for the isooctane injection timing, the indicated mean effective pressure (IMEP) first increases and then decreases with the delay in isooctane injection. The hot spots in the flame images confirm that late injection results in isooctane inhomogeneity, which reduces the engine’s thermal efficiency. At high loads, the low energy density of methane can lower the knocking intensity, even in the presence of auto-ignition at a speed of 120.7 m/s. The knocking pressure can lead to the ejection of oil droplets, which can increase the flame speed in the subsequent cycle.

Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d

Recent work on the characterization of small exoplanets has allowed us to accumulate growing evidence that sub-Neptunes with radii greater than ∼2.5 R ⊕ often host H2/He-dominated atmospheres both from measurements of their low bulk densities and from direct detections of their low mean molecular mass atmospheres. However, the smaller sub-Neptunes in the 1.5–2.2 R ⊕ size regime are much less understood and often have bulk densities that can be explained either by the H2/He-rich scenario or by a volatile-dominated composition known as the “water world” scenario. Here we report the detection of water vapor in the transmission spectrum of the 1.96 ± 0.08 R ⊕ sub-Neptune GJ 9827 d obtained with the Hubble Space Telescope (HST). We observe 11 HST Wide Field Camera 3 transits of GJ 9827 d and find an absorption feature at 1.4 μm in its transit spectrum, which is best explained (at 3.39σ) by the presence of water in GJ 9827 d’s atmosphere. We further show that this feature cannot be caused by unocculted starspots during the transits by combining an analysis of the K2 photometry and transit light source effect retrievals. We reveal that the water absorption feature can be similarly well explained by a small amount of water vapor in a cloudy H2/He atmosphere or a water vapor envelope on GJ 9827 d. Given that recent studies have inferred an important mass-loss rate (>0.5 M ⊕ Gyr−1) for GJ 9827 d, making it unlikely to retain a H-dominated envelope, our findings highlight GJ 9827 d as a promising water world candidate that could host a volatile-dominated atmosphere. This water detection also makes GJ 9827 d the smallest exoplanet with an atmospheric molecular detection to date.

Optimization of oil extraction from Carica papaya seedoil: A case of response surface methodology

The primary goal of this research is to determine the optimum value oil and to determine the effects of operational parameters on the physiochemical properties of the Carica papaya seed oil, such as Mean Molecular mass, viscosity, API, Acid value, Free Fatty Acid (%FFA), Peroxide value, Saponification value, Iodine value, moisture content, Specific gravity, Cetane number and Higher Heating value (HHV). Respond Surface Methodology (RSM) was used for regression analysis, ANOVA and to also predict the optimal value for the Carica papaya seed oil extracted. The model was created to be significant, according to the results, and a quadratic polynomial was achieved for forecasting the extraction procedure. The highest yield obtained was 23.67% (w/w) at the sample weight (55 g) the physicochemical properties of the extracted papaya seed oil, provided papaya seed oil with obviously reddish brown color, density 955kg/m3, specific gravity 0.9235, moisture content 0.004092% acid value 27.974 mg KOH/g, % FFA 13.99, saponification value 140.25 mg KOH/g oil, iodine value 93.70, peroxide value 56.00 meq O2/kg oil, viscosity 622.1 MPa.S at 29.6oC, Cetane number 82.88, diesel value 101.22, Higher Heating value, (HHV) 29.62325MJ/kg, Mean Molecular Mass 399.3, API 21.72, aniline point 466.03. The Carica papaya seed is rich in oil and gave a high quantity of oil, using Respond Surface Method it yielded 23.67% (w/w) archived at the following optimized conditions, sample weight (55 g), extraction time (50 min), and solvent volume of 250 ml, the values for coefficient of determination (R2) for RSM 0.9835, respectively. The research concluded that papaya seed oil is rich in oil which can be applied as a major feedstock in industries.

Interhemispheric Asymmetry of the Thermospheric Neutral Density Response to the 7–9 September 2017 Geomagnetic Storms

AbstractThe thermospheric neutral density response to the 7–9 September 2017 storms is investigated based on the Swarm satellite observations and the thermosphere‐ionosphere‐electrodynamic general circulation model (TIEGCM) simulation. The Swarm data depicted a prominent interhemispheric asymmetry (IHA) in the afternoon sector during the second storm, a feature that was yet explained. Driven by realistic high‐latitude electric potential and electron precipitation patterns, the TIEGCM is able to reproduce the observed storm‐time neutral density response. The TIEGCM simulation reveals that the differences in the traveling atmospheric disturbances (TADs) is largely responsible for the observed IHA in the neutral mass density response at low and middle latitudes, whereas the difference in mean molecular mass between the two hemispheres may contribute to the IHA in neutral density at higher latitudes. The IHAs in TADs and mean molecular mass are attributed to the IHA in Joule heating dissipation on the night and dawn sides.

Echinacea purpurea-derived homogeneous polysaccharide exerts anti-tumor efficacy via facilitating M1 macrophage polarization

Echinacea purpurea modulates tumor progression, but the underlying mechanismis poorly defined. We isolated and purified a novel homogeneous polysaccharide from E. purpurea (EPPA), which was shown to be an arabinogalactan with a mean molecular mass (Mr) of 3.8×104 Da and with α- (1 → 5) -L-Arabinan as the backbone and α-L-Araf-(1→, →6)-β-D-Galp-(1→, and →4)-α-D-GalpA-(1→ as the side chains. Interestingly, oral administration of EPPA suppresses tumor progression invivo and shapes the immune cell profile (e.g., facilitating M1 macrophages) in tumor microenvironment by single-cell RNA sequencing (scRNA-seq) analysis. More importantly, EPPA activates the inflammasome through a phagocytosis-dependent mechanism and rewires transcriptomic and metabolic profile, thereby potentiating M1 macrophage polarization. Collectively, we propose that EPPA supplementation could function as an adjuvant therapeutic strategy for tumor suppression.

A Novel Method to Derive Exospheric Temperatures from Swarm Thermospheric Densities during Quiet Times

One of the most important parameters in the atmosphere, the neutral temperature, becomes difficult to measure at high altitudes such as the exosphere. Therefore, based on the assumption of static equilibrium and isothermal atmosphere, a new method was developed to derive quiet-time exospheric temperatures using neutral atmospheric densities from 470 km to 550 km, which were obtained from the Swarm satellites. The derived neutral temperatures were obtained at an altitude of approximately 500 km in the low and middle latitudes from mid-April 2014 to early August 2014. The results were evaluated with nighttime temperatures from ground-based Fabry Perot Interferometers at 250 km. The mean deviation between the derived temperatures and FPI was 30.80 K and the standard deviation of the mean was 106.20 K. The diurnal variations of the exospheric temperatures, which tended to reach their maximum in the late afternoon, were in good consistency with the NRL-MSISE00 model simulations. This novel method performs well at low and middle latitudes. The greatest source of uncertainty is the mean molecular mass, which is also not well determined at these high altitudes. Hence, a measurement called “Satellite-tethered Mass Spectrometer Detection” was proposed to address this.

TRAPPIST-1h as an Exo-Titan. I. The Role of Assumptions about Atmospheric Parameters in Understanding an Exoplanet Atmosphere

The TRAPPIST-1 system is home to at least seven terrestrial planets and is a target of interest for future James Webb Space Telescope (JWST) observations. Additionally, these planets will be of interest to future missions making observations in the ultraviolet (UV). Although several of these planets are located in the traditional habitable zone, where liquid water could exist on the surface, TRAPPIST-1h is interesting to explore as a potentially habitable ocean world analog. In this study, we evaluate the observability of a Titan-like atmosphere on TRAPPIST-1h. The ability of the JWST or a future UV mission to detect specific species in the atmosphere at TRAPPIST-1h will depend on how far each species extends from the surface. In order to understand the conditions required for detection, we evaluate the input parameters used in one-dimensional models to simulate the structure of Titan-like atmospheres. These parameters include surface temperature and pressure, temperature profile as a function of distance from the surface, composition of the minor species relative to N2, and the eddy diffusion coefficient. We find that JWST simulated spectra for cloud- and haze-free atmospheres are most sensitive to surface temperature, temperature gradients with altitude, and surface pressure. The importance of temperature gradients in JWST observations shows that a simple isothermal scale height is not ideal for determining temperature or atmospheric mean molecular mass in transit spectra from exoplanet atmospheres. We demonstrate that UV transmission spectra are sensitive to the upper atmosphere, where the exobase can be used to approximate the vertical extent of the atmosphere.

A3COSMOS: A census on the molecular gas mass and extent of main-sequence galaxies across cosmic time

Aims. We aim to constrain for the first time the mean mass and extent of the molecular gas of a mass-complete sample of normal > 1010 M⊙ star-forming galaxies at 0.4 < z < 3.6. Methods. We apply an innovative uv-based stacking analysis to a large set of archival Atacama Large Millimeter/submillimeter Array (ALMA) observations using a mass-complete sample of main-sequence (MS) galaxies. This stacking analysis, performed on the Rayleigh-Jeans dust continuum emission, provides accurate measurements of the mean mass and extent of the molecular gas of galaxy populations, which are otherwise individually undetected. Results. The molecular gas mass of MS galaxies evolves with redshift and stellar mass. At all stellar masses, the molecular gas fraction decreases by a factor of ∼24 from z ∼ 3.2 to z ∼ 0. At a given redshift, the molecular gas fraction of MS galaxies decreases with stellar mass at roughly the same rate that their specific star-formation rate (SFR/M⋆) decreases. The molecular gas depletion time of MS galaxies remains roughly constant at z > 0.5 with a value of 300–500 Myr, but increases by a factor of ∼3 from z ∼ 0.5 to z ∼ 0. This evolution of the molecular gas depletion time of MS galaxies can be predicted from the evolution of their molecular gas surface density and a seemingly universal MS-only ΣMmol − ΣSFR relation with an inferred slope of ∼1.13, the so-called Kennicutt–Schmidt (KS) relation. The far-infrared size of MS galaxies shows no significant evolution with redshift or stellar mass, with a mean circularized half-light radius of ∼2.2 kpc. Finally, our mean molecular gas masses are generally lower than previous estimates, likely due to the fact that literature studies were largely biased toward individually detected MS galaxies with massive gas reservoirs. Conclusions. To first order, the molecular gas content of MS galaxies regulates their star formation across cosmic time, while variation in their star-formation efficiency plays a secondary role. Despite a large evolution of their gas content and star-formation rates, MS galaxies have evolved along a seemingly universal MS-only KS relation.

Modelling the He I triplet absorption at 10 830 Å in the atmospheres of HD 189733 b and GJ 3470 b

Characterising the atmospheres of exoplanets is key to understanding their nature and provides hints about their formation and evolution. High resolution measurements of the helium triplet absorption of highly irradiated planets have been recently reported, which provide a new means of studying their atmospheric escape. In this work we study the escape of the upper atmospheres of HD 189733 b and GJ 3470 b by analysing high resolution He I triplet absorption measurements and using a 1D hydrodynamic spherically symmetric model coupled with a non-local thermodynamic model for the He I triplet state. We also use the H density derived from Lyα observations to further constrain their temperatures, mass-loss rates, and H/He ratios. We have significantly improved our knowledge of the upper atmospheres of these planets. While HD 189733 b has a rather compressed atmosphere and small gas radial velocities, GJ 3470 b, on the other hand with a gravitational potential ten times smaller, exhibits a very extended atmosphere and large radial outflow velocities. Hence, although GJ 3470 b is much less irradiated in the X-ray and extreme ultraviolet radiation, and its upper atmosphere is much cooler, it evaporates at a comparable rate. In particular, we find that the upper atmosphere of HD 189733 b is compact and hot, with a maximum temperature of 12 400−300+400 K, with a very low mean molecular mass (H/He = (99.2/0.8) ± 0.1), which is almost fully ionised above 1.1 RP, and with a mass-loss rate of (1.1 ± 0.1) × 1011 g s−1. In contrast, the upper atmosphere of GJ 3470 b is highly extended and relatively cold, with a maximum temperature of 5100 ± 900 K, also with a very low mean molecular mass (H/He = (98.5/1.5)−1.5+1.0), which is not strongly ionised, and with a mass-loss rate of (1.9 ± 1.1) × 1011 g s−1. Furthermore, our results suggest that upper atmospheres of giant planets undergoing hydrodynamic escape tend to have a very low mean molecular mass (H/He ≳ 97/3).

Investigation of Glass Transition Process in Narrow Oil Fractions in a Wide Temperature Range

The results of a study of the phase behavior of six narrow oil fractions in the 150-350 K temperature range at atmospheric pressure using scanning calorimetry are presented. It is shown that there is a correlation between glass transition of the studied oil fractions and their mean boiloff temperature, molecular mass, and initial oil viscosity.

Change in Molecular Mass of Pitch on Thermodestructive Polycondensation of Heavy Pyrolysis Tar

By determining the molecular mass of pitch from heavy pirolysis tar, additional information may be obtained regarding the thermal polycondensation and quality of pitch. The weighted mean molecular mass of toluene-soluble components of the pirolysis pitch is determined by gel-permeation chromatography. The molecular mass of the components in specific petroleum-pitch fractions is studied as a function of the time and temperature employed in isothermal holding of the heavy pirolysis tar. The weighted mean molecular mass of toluene-soluble components depends on the heat treatment of the pirolysis tar and the softening temperature of the petroleum pitch.

Extracción y caracterización de quitina de escamas de tilapia roja (oreochromis sp.) del Huila mediante métodos químicos

La quitina es el segundo biopolímero lineal más importante en el mundo. Avances recientes sugieren que la quitina se puede obtener de las escamas de peces. Para este artículo, se utilizaron tres tratamientos diferentes para obtener quitina de las escamas de tilapia roja (Orechromis sp.). Todas las muestras fueron insolubles en los solventes y ácidos usados; también presentaron diferentes porcentajes de carbono (3,27-55,80 %), oxígeno (22,09-42,51 %), nitrógeno (11,61-11,81 %), P (1,08-22,2 %), Ca (1,26-26,11 %), Na (0,53-1,02 %) y Mg (0,26-0,91 %). Las bandas de 3.340 cm-1 presentes en el espectro de infrarrojo corresponden al grupo hidroxilo de las bases de glucosamina poliméricas y los picos 1.415-1.456 cm-1 están relacionados con la banda N-H característica del grupo funcional amida. Las imágenes (SE) muestran diferentes dimensiones de partículas (0,1-30 μm) y las masas moleculares promedio, Mw, para Ch1, Ch2 y Ch3 fueron 1.064,28; 1.064,56; y 823,428, respectivamente, con una polidispersidad de 1,0074.

Apparatus for Rapid Measurement of Oil Density and Molecular Mass Using Proton Magnetic Resonance

Methods for calculating the mean molecular mass (MM) from the density are analyzed. The density ρ of crude oils was determined experimentally as a function of proton spin–lattice (T1H) and spin–spin relaxation times (T2H). The dependences of MMs on times T1,2H were calculated from the obtained correlations. A comparison of the experimental and theoretical functions MM(T2H) showed that the relaxation times allowed rapid determination of the MM.

A Novel Mass Spectrometry Method to Identify the Serum Monoclonal Light Chain Component and Infer Organ Involvement in Systemic Light Chain Amyloidosis

▪IntroductionLight chain (AL) amyloidosis is caused by progressive organ dysfunction due to the deposition of structurally abnormal monoclonal light chains (LC) as amyloid fibrils. Serial free light chain measurement is the cornerstone of AL diagnosis but is limited by current methods which measure normal polyclonal and abnormal monoclonal LCs. Since each individual monoclonal LC has a unique amino acid sequence, mass spectrometry (MS) has the ability to detect serum monoclonal LCs.We report a novel MS method for monoclonal LC detection in AL amyloidosis.MethodsTwenty patients with systemic AL amyloidosis, diagnosed and treated at the UK National Amyloidosis Centre (UK-NAC), were randomly selected. This included 16 newly diagnosed patients, 2 patients in a complete haematological remission (CR) post-treatment and 2 patients with no amyloidosis (acting as negative controls). All patients had detailed baseline assessments of organ function and serum FLC measurements. Organ involvement was defined according to the international amyloidosis consensus criteria. Magnetic microparticles were covalently coated with modified polyclonal sheep antibodies monospecific for free kappa light chains (anti-free k) and free lambda light chains (anti-free l). The microparticles were incubated with patient sera, washed and treated with acetic acid (5% v/v) containing TCEP (20 mM) in order to elute free light chains in monomeric form. Mass spectra were acquired on a Microflex LT/SH smart matrix-assisted laser desorption ionization time-of-flight mass spectrometer (MALDI-TOF-MS; Bruker, GmbH).ResultsThe median number of organs involved was 2 (range 1-4); cardiac involvement was most common in 70% (14/20) patients, followed by renal 40% (8/20), autonomic and soft tissue in 15% (3/20) and peripheral nerve involvement in 5% (1/20). No patients had liver involvement. The median N-terminal pro b-type natriuretic peptide (NT-proBNP) and cardiac troponin T were 3761.5 (range 245-25348 ng/L) and 35.5 (8-170 ng/L) respectively. The median presenting serum albumin was 37 (19-45 g/L) and eGFR 62 (10-100 mls/min). The amyloid deposits were typed as AL lambda in 14(70%), kappa in 2(10%) patients and amyloid of uncertain type in two cases (10%). The median involved FLC was kappa 76 mg/L (range 71-440) and lambda 185 mg/L (44-1023), with difference involved to uninvolved (dFLC) 118 mg/L (33-1015). An intact monoclonal protein was present in 70% (14/20).In all cases, MS correctly identified the presence and type of monoclonal LC, identifying a monoclonal lambda in 14/14 (100%) and a monoclonal kappa in 2/2 (100%); the two patients where a clear monoclonal component could not be identified were patients whose amyloid fibrils failed to be typed by immunohistochemistry or MS. The assay also confirmed normal polyclonal expression of both kappa and lambda LCs in the two control samples. In the two lambda patients in a CR, the MS method identified monoclonal lambda LC expression; in one of these patients next-generation sequencing (NGS) confirmed minimal residual disease (MRD). A clear shift in the LC mass spectra was seen relating to the specific pattern of organ involvement: in patients with renal amyloid the monoclonal LC predominantly displayed a “heavy” molecular mass, (with a mean molecular mass of 11596+/- 436 daltons), whereas in patients with cardiac involvement the monoclonal LC mainly exhibited a “light” mass (with a mean molecular mass of 11443 +/- 102 daltons).ConclusionThis small study shows that monoclonal light chains can be accurately detected by MS and be concordant to the tissue amyloid type. A monoclonal LC was detected in 2 patients in serological “CR” - in one case presence of persistent disease was demonstrated by NGS-MRD. Even in this small sample size, there appears to be a marked difference in LC mass for patients with cardiac (“light” LC) vs. renal (“heavy” LC) involvement, raising the interesting possibility that “heavy” LC are trapped by the glomerulus causing renal AL but are unable to penetrate the tight cardiac capillary gap junctions, and vice versa. The unique molecular location of LC on MS offers the possibility of exploiting this technique as a tool to detect amyloidogenic FLC and potentially predict organ involvement in patients with gammopathies. We plan to expand this study to a large cohort of patients to confirm these findings and assess the impact on survival and organ response outcomes. [Display omitted] DisclosuresWechalekar:Janssen: Honoraria.

Properties of a recombinant GH49 family dextranase heterologously expressed in two recipient strains of Penicillium species

The dexA gene encoding Penicillium funiculosum dextranase (GenBank accession MH581385) belonging to family 49 of glycoside hydrolases (GH49) was cloned and heterologously expressed in two recipient strains, P. canescens RN3-11-7 and P. verruculosum B1-537. Crude enzyme preparations with the recombinant dextranase content of 8–36% of the total secreted protein were obtained on the basis of new Penicillium strains. Both recombinant forms of the dextranase were isolated in a homogeneous state using chromatographic techniques. The purified enzymes displayed very similar properties, that is, pI 4.55, activity optima at pH 4.5–5.0 and 55–60 °C and a melting temperature of 60.7–60.9 °C. They were characterized by similar specific activities (1020–1340 U/mg) against dextrans with a mean molecular mass of 20, 70 and 500 kDa, as well as similar kinetic parameters in the hydrolysis of 70 kDa dextran (Km = 1.10–1.11 g/L, kcat = 640–680 s−1). However, the recombinant dextranases expressed in P. canescens and P. verruculosum had different molecular masses according to the data of SDS-PAGE (∼63 and ∼60 kDa, respectively); this was the result of different N-glycosylation patterns as MALDI-TOF mass spectrometry analysis showed. The main products of dextran hydrolysis at its initial phase were isomaltooligosaccharides, while after the prolonged time (24 h) the reaction system contained isomaltose and glucose as the major products and minor amounts of other oligosaccharides.

Herschel and ALMA Observations of Massive SZE-selected Clusters

Abstract We present new Herschel observations of four massive, Sunyaev–Zel’dovich effect–selected clusters at , two of which have also been observed with the Atacama Large Millimeter/submillimeter Array (ALMA). We detect 19 Herschel/Photoconductor Array Camera and Spectrometer (PACS) counterparts to spectroscopically confirmed cluster members, five of which have redshifts determined via CO (4–3) and [C i] ( ) lines. The mean [C i]/CO line ratio is 0.19 ± 0.07 in brightness temperature units, consistent with previous results for field samples. We do not detect significant stacked ALMA dust continuum or spectral-line emission, implying upper limits on mean interstellar medium (H2 + H i) and molecular gas masses. An apparent anticorrelation of with clustercentric radius is driven by the tight relation between star formation rate and stellar mass. We find an average specific star formation rate of log(sSFR/yr−1) = −10.36, which is below the correlation measured for field galaxies at similar redshifts. The fraction of infrared-bright galaxies (IRBGs; ) per cluster and average sSFR rise significantly with redshift. For CO detections, we find , comparable to those of field galaxies, and gas depletion timescales of about 2 Gyr. We use radio observations to distinguish active galactic nuclei (AGNs) from star-forming galaxies. At least four of our 19 Herschel cluster members have , implying an AGN fraction for our PACS-selected sample.

Development and Validation of the Whole Atmosphere Community Climate Model With Thermosphere and Ionosphere Extension (WACCM‐X 2.0)

AbstractKey developments have been made to the NCAR Whole Atmosphere Community Climate Model with thermosphere and ionosphere extension (WACCM‐X). Among them, the most important are the self‐consistent solution of global electrodynamics, and transport of O+ in the F‐region. Other ionosphere developments include time‐dependent solution of electron/ion temperatures, metastable O+ chemistry, and high‐cadence solar EUV capability. Additional developments of the thermospheric components are improvements to the momentum and energy equation solvers to account for variable mean molecular mass and specific heat, a new divergence damping scheme, and cooling by O(3P) fine structure. Simulations using this new version of WACCM‐X (2.0) have been carried out for solar maximum and minimum conditions. Thermospheric composition, density, and temperatures are in general agreement with measurements and empirical models, including the equatorial mass density anomaly and the midnight density maximum. The amplitudes and seasonal variations of atmospheric tides in the mesosphere and lower thermosphere are in good agreement with observations. Although global mean thermospheric densities are comparable with observations of the annual variation, they lack a clear semiannual variation. In the ionosphere, the low‐latitude E × B drifts agree well with observations in their magnitudes, local time dependence, seasonal, and solar activity variations. The prereversal enhancement in the equatorial region, which is associated with ionospheric irregularities, displays patterns of longitudinal and seasonal variation that are similar to observations. Ionospheric density from the model simulations reproduces the equatorial ionosphere anomaly structures and is in general agreement with observations. The model simulations also capture important ionospheric features during storms.