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.

Exoplanets hosting M dwarfs are the best targets to characterize Earth-like or super-Earth planetary atmospheres with the James Webb Space Telescope (JWST). We determine detailed stellar parameters ( Teff, log g, and ξ) and individual abundances of twelve elements for four cool M dwarfs hosting exoplanets TOI-1685, GJ 436, GJ 3470, and TOI-2445, scheduled for future observations by the JWST. The analysis utilizes high-resolution near-infrared spectra from the SDSS-IV APOGEE survey between 1.51-1.69 µm. Based on 1D-LTE plane-parallel models, we find that TOI-2445 is slightly metal-po or ([Fe/H1 =-0.16 ±0.09), while TOI-1685, GJ 436 and GJ 3470 are more metal-rich ([Fe/H1 = 0.06 ±0.18, 0.10 ±0.20 dex, 0.25 ±0.15). The derived C/O ratios for TOI-2445, TOI-1685, GJ 436, and GJ 3470 are 0.526 ±0.027, 0.558 ±0.097, 0.561 ±0.029, and 0.638 ±0.015, respectively. From results for 28 M dwarfs analyzed homogeneously from APOGEE spectra, we find exoplanet-hosting M dwarfs exhibit a C/O abundance ratio approximately 0.01 to 0.05 higher than those with non-detected exoplanets, at limits of a statistically significant offset. A linear regression of [Fe/H1 vs. C/O distribution reveals a noticeable difference in the angular coefficient between FGK dwarfs (0.27) and M dwarfs (0.13). Assuming our abundance ratios of Ca/Mg, Si/Mg, Al/Mg, and Fe/Mg, we determine a mass of 3.276−0.419 +0.448 M⊕ for TOI-2445 b, having density (6.793−0.099 +0.005 g.cm − 3 ) and core mass fraction (0.329−0.049 +0.028 ) very similar to Earth’s. We also present an atlas of 113 well-defined spectral lines to analyze M dwarfs in the Hband and a comprehensive evaluation of uncertainties from variations in the atmospheric parameters, signal-to-noise, and pseudo-continuum.

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.