Fluids and melts in planetary interiors significantly influence geodynamic processes from volcanism to global-scale differentiation. The roles of these geofluids depend on their viscosities (eta). Constraining geofluid eta at relevant pressures and temperatures relies on laboratory-based measurements and is most widely done using Stokes' Law viscometry with falling spheres. Yet small sample chambers required by high-pressure experiments introduce significant drag on the spheres. Several correction schemes are available for Stokes' Law but there is no consensus on the best scheme(s) for high-pressure experiments. We completed high-pressure experiments to test the effects of (a) the relative size of the sphere diameter to the chamber diameter and (b) the top and bottom of the chamber, that is, the ends, on the sphere velocities. We examined the influence of current correction schemes on the estimated viscosity using Monte Carlo simulations. We also compared previous viscometry work on various geofluids in different experimental setups/geometries. We find the common schemes for Stokes' Law produce statistically distinct values of eta. When inertia of the sphere is negligible, the most appropriate scheme may be the Fax & eacute;n correction for the chamber walls. Correction for drag due to the chamber ends depends on the precision in the sinking distance and may be ineffective with decreasing sphere size. Combining the wall and end corrections may overcorrect eta. We also suggest the uncertainty in eta is best captured by the correction rather than propagated errors from experimental parameters. We develop an overlying view of Stokes' Law viscometry at high pressures.

We present SN 2023zaw-a subluminous (M-r = -16.7 mag) and rapidly evolving supernova (t(1/2,r) = 4.9 days), with the lowest nickel mass (approximate to 0.002 M-circle dot) measured among all stripped-envelope supernovae discovered to date. The photospheric spectra are dominated by broad He I and Ca near-infrared emission lines with velocities of similar to 10,000-12,000 km s(-1). The late-time spectra show prominent narrow He I emission lines at similar to 1000 km s(-1), indicative of interaction with He-rich circumstellar material. SN 2023zaw is located in the spiral arm of a star-forming galaxy. We perform radiation-hydrodynamical and analytical modeling of the lightcurve by fitting with a combination of shock-cooling emission and nickel decay. The progenitor has a best-fit envelope mass of approximate to 0.2 M-circle dot and an envelope radius of approximate to 50 R-circle dot. The extremely low nickel mass and low ejecta mass (approximate to 0.5 M-circle dot) suggest an ultrastripped SN, which originates from a mass-losing low-mass He-star (zero-age main-sequence mass < 10 M-circle dot) in a close binary system. This is a channel to form double neutron star systems, whose merger is detectable with LIGO. SN 2023zaw underscores the existence of a previously undiscovered population of extremely low nickel mass (<0.005 M-circle dot) stripped-envelope supernovae, which can be explored with deep and high-cadence transient surveys.

We report a new, rare detection of H I 21 cm absorption associated with a quasar (only six quasars are known at 1 < z < 2) toward J2339-5523 at z(em) = 1.3531, discovered through the MeerKAT Absorption Line Survey (MALS). The absorption profile is broad (similar to 400 km s(-1) ), and the peak is redshifted by similar to 200 km s(-1) from z(em). Interestingly, optical/far-UV spectra of the quasar from the Magellan-MIKE/HST-COS spectrographs do not show any absorption features associated with the 21 cm absorption, despite the coincident presence of the optical quasar and the radio core inferred from a flat-spectrum component with a flux density of similar to 65 mJy at high frequencies (> 5 GHz). The simplest explanation would be that no large H I column (N(H I) > 10(17) cm(-2)) is present toward the radio core and the optical active galactic nucleus. Based on the joint optical and radio analysis of a heterogeneous sample of 16 quasars (z(median) = 0.7) and 19 radio galaxies (z(median) = 0.4) with H I 21 cm absorption detection and matched in 1.4 GHz luminosity (L-1.4 GHz), a consistent picture emerges according to which quasars primarily trace the gas in the inner circumnuclear disk and cocoon created by the interaction of the jet with interstellar medium. They (i.e., quasars) exhibit a L-1.4 GHz - Delta V-null correlation and a frequent mismatch of the radio and optical spectral lines. The radio galaxies show no such correlation and likely trace the gas from the cocoon and the galaxy-wide interstellar medium outside the photoionization cone. The analysis presented here demonstrates the potential of radio spectroscopic observations to reveal the origin of the absorbing gas associated with active galactic nuclei that may be missed in optical observations.

For more than a decade, the CheMin X-ray diffraction instrument on the Mars Science Laboratory rover, Curiosity, has been returning definitive and quantitative mineralogical and mineral-chemistry data from similar to 3.5-billion-year-old (Ga) sediments in Gale crater, Mars. To date, 40 drilled rock samples and three scooped soil samples have been analyzed during the rover's 30+ km transit. These samples document the mineralogy of over 800 m of flat-lying fluvial, lacustrine, and aeolian sedimentary rocks that comprise the lower strata of the central mound of Gale crater (Aeolis Mons, informally known as Mt. Sharp) and the surrounding plains (Aeolis Palus, informally known as the Bradbury Rise). The principal mineralogy of the sedimentary rocks is of basaltic composition, with evidence of post-depositional diagenetic overprinting. The rocks in many cases preserve much of their primary mineralogy and sedimentary features, suggesting that they were never strongly heated or deformed. Using aeolian soil composition as a proxy for the composition of the deposited and lithified sediment, it appears that, in many cases, the diagenetic changes observed are principally isochemical. Exceptions to this trend include secondary nodules, calcium sulfate veining, and rare Si-rich alteration halos. A surprising and yet poorly understood observation is that nearly all of the similar to 3.5 Ga sedimentary rocks analyzed to date contain 15-70 wt.% of X-ray amorphous material. Overall, this >800 m section of sedimentary rock explored in lower Mt. Sharp documents a perennial shallow lake environment grading upward into alternating lacustrine/fluvial and aeolian environments, many of which would have been habitable to microbial life.

HZ610x Genomics HZ810x Genomics HZ910x Genomics Crop_R1Illumina RiboZero TruSeq Crop_R2Illumina RiboZero TruSeq Crop_R3Illumina RiboZero TruSeq SG_R1Illumina PolyA TruSeq SG_R2Illumina PolyA TruSeq SG_R3Illumina PolyA TruSeq PV_GF_R1Illumina RiboZero TruSeq PV_GF_R2Illumina RiboZero TruSeq PV_GF_R3Illumina RiboZero TruSeq PV_GF_R4Illumina RiboZero TruSeq PV_GF_R5Illumina RiboZero TruSeq PV_LpWF_R1Illumina RiboZero TruSeq PV_LpWF_R2Illumina RiboZero TruSeq PV_LpWF_R3Illumina RiboZero TruSeq PV_LpWF_R4Illumina RiboZero TruSeq PV_LpWF_R5Illumina RiboZero TruSeq Adult Drosophila foregut contains a diverse set of tissue and cell types. We applied single cell RnA sequencing (scRnA-seq) and bulk RnA sequencing (bulk RnA-seq) to delineate the cellular composition and molecular profile of the foregut and its associated physiological functions.