The plant life cycle is characterized by the alternation of generations between genetically active diploid sporophytes and haploid gametophytes. The gametophytes of flowering plants are sexually dimorphic. While the male gametophyte consists of only three cells (two sperm and a vegetative cell) and is released by the parent sporophyte, the female gametophyte (or embryo sac) is more complex and remains imbedded within diploid sporophyte tissues. In maize, the female gametophyte is embedded in a large ovule surrounded with multiple nucellar cell layers impeding live-cell imaging approaches to study embryo sac functions. Here, we describe a simple protocol to visualize embryo sacs with hormonal fluorescent reporters by increasing accessibility of the female gametophyte. The method described is applicable for visualization of any fluorescent embryo sac reporter. The embryo sacs visualization method developed for maize could be extended to facilitate visualization of embryos sac in other important cereals like wheat, rice, and oats.

Post-transcriptional gene regulation is robustly regulated by RNA-binding proteins (RBPs). Here we describe the collection of RNAs regulated by AUF1 (AU-binding factor 1), an RBP linked to cancer, inflammation and aging. Photoactivatable ribonucleoside-enhanced crosslinking and immunoprecipitation (PAR-CLIP) analysis reveals that AUF1 primarily recognizes U-/GU-rich sequences in mRNAs and noncoding RNAs and influences target transcript fate in three main directions. First, AUF1 lowers the steady-state levels of numerous target RNAs, including long noncoding RNA NEAT1, in turn affecting the organization of nuclear paraspeckles. Second, AUF1 does not change the abundance of many target RNAs, but ribosome profiling reveals that AUF1 promotes the translation of numerous mRNAs in this group. Third, AUF1 unexpectedly enhances the steady-state levels of several target mRNAs encoding DNA-maintenance proteins. Through its actions on target RNAs, AUF1 preserves genomic integrity, in agreement with the AUF1-elicited prevention of premature cellular senescence.

The explosion of RNA-Seq data has enabled the identification of expressed genes without relying on gene models with biases toward open reading frames, allowing the identification of many more long noncoding RNAs (lncRNAs) in eukaryotes. Various tissue enrichment strategies and deep sequencing have also enabled the identification of an extensive list of genes expressed in maize gametophytes, tissues that are intractable to both traditional genetic and gene expression analyses. However, the function of very few genes from the lncRNA and gametophyte sets (or from their intersection) has been tested. Methods for isolating and identifying lncRNAs from gametophyte samples of maize are described here. This method is transferable to any maize gametophyte mutant enabling the development of gene networks involving both protein-coding genes and lncRNAs. Additionally, these methods can be adapted to apply to other grass model systems to test for evolutionary conservation of lncRNA expression patterns.

Author summary

The recent detection of a repeating fast radio burst (FRB) in an old globular cluster in M81 challenges traditional FRB formation mechanisms based on the magnetic activity of young neutron stars formed in core-collapse supernovae. Furthermore, the detection of this repeater in such a nearby galaxy implies a high local universe rate of similar events in globular clusters. Building off the properties inferred from the M81 FRB, we predict the number of FRB sources in nearby (d? 20 Mpc) galaxies with large globular cluster systems known. Incorporating the uncertain burst energy distribution, we estimate the rate of bursts detectable in these galaxies by radio instruments such as FAST and MeerKat. Of all local galaxies, we find M87 is the best candidate for FRB detections. We predict that M87's globular cluster system contains 0(10) FRB sources at present and that a dedicated radio survey (by either FAST or MeerKat) of 0(10) hr has a 90% probability of detecting a globular cluster FRB in M87. The detection of even a handful of additional globular cluster FRBs would provide invaluable constraints on FRB mechanisms and population properties. Previous studies have demonstrated young neutron stars formed following the collapse of dynamically formed massive white dwarf binary mergers may provide the most natural mechanism for these bursts. We explore the white dwarf merger scenario using a suite of N-body cluster models, focusing in particular on such mergers in M87's clusters. We describe a number of outstanding features of this scenario that in principle may be testable with an ensemble of observed FRBs in nearby globular clusters.

We compare mid-infrared (mid-IR), extinction-corrected H alpha, and CO (2-1) emission at 70-160 pc resolution in the first four PHANGS-JWST targets. We report correlation strengths, intensity ratios, and power-law fits relating emission in JWST's F770W, F1000W, F1130W, and F2100W bands to CO and H alpha. At these scales, CO and H alpha each correlate strongly with mid-IR emission, and these correlations are each stronger than the one relating CO to H alpha emission. This reflects that mid-IR emission simultaneously acts as a dust column density tracer, leading to a good match with the molecular-gas-tracing CO, and as a heating tracer, leading to a good match with the H alpha. By combining mid-IR, CO, and H alpha at scales where the overall correlation between cold gas and star formation begins to break down, we are able to separate these two effects. We model the mid-IR above I ( nu ) = 0.5 MJy sr(-1) at F770W, a cut designed to select regions where the molecular gas dominates the interstellar medium (ISM) mass. This bright emission can be described to first order by a model that combines a CO-tracing component and an H alpha-tracing component. The best-fitting models imply that similar to 50% of the mid-IR flux arises from molecular gas heated by the diffuse interstellar radiation field, with the remaining similar to 50% associated with bright, dusty star-forming regions. We discuss differences between the F770W, F1000W, and F1130W bands and the continuum-dominated F2100W band and suggest next steps for using the mid-IR as an ISM tracer.

JWST/Mid-Infrared Instrument imaging of the nearby galaxies IC 5332, NGC 628, NGC 1365, and NGC 7496 from PHANGS reveals a richness of gas structures that in each case form a quasi-regular network of interconnected filaments, shells, and voids. We examine whether this multiscale network of structure is consistent with the fragmentation of the gas disk through gravitational instability. We use FilFinder to detect the web of filamentary features in each galaxy and determine their characteristic radial and azimuthal spacings. These spacings are then compared to estimates of the most Toomre-unstable length (a few kiloparsecs), the turbulent Jeans length (a few hundred parsecs), and the disk scale height (tens of parsecs) reconstructed using PHANGS-Atacama Large Millimeter/submillimeter Array observations of the molecular gas as a dynamical tracer. Our analysis of the four galaxies targeted in this work indicates that Jeans-scale structure is pervasive. Future work will be essential for determining how the structure observed in gas disks impacts not only the rate and location of star formation but also how stellar feedback interacts positively or negatively with the surrounding multiphase gas reservoir.

We present a high-resolution view of bubbles within the Phantom Galaxy (NGC 628), a nearby (similar to 10 Mpc), star-forming (similar to 2 M (circle dot) yr(-1)), face-on (i similar to 9 degrees) grand-design spiral galaxy. With new data obtained as part of the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-JWST treasury program, we perform a detailed case study of two regions of interest, one of which contains the largest and most prominent bubble in the galaxy (the Phantom Void, over 1 kpc in diameter), and the other being a smaller region that may be the precursor to such a large bubble (the Precursor Phantom Void). When comparing to matched-resolution H alpha observations from the Hubble Space Telescope, we see that the ionized gas is brightest in the shells of both bubbles, and is coincident with the youngest (similar to 1 Myr) and most massive (similar to 10(5) M (circle dot)) stellar associations. We also find an older generation (similar to 20 Myr) of stellar associations is present within the bubble of the Phantom Void. From our kinematic analysis of the H I, H-2 (CO), and H ii gas across the Phantom Void, we infer a high expansion speed of around 15 to 50 km s(-1). The large size and high expansion speed of the Phantom Void suggest that the driving mechanism is sustained stellar feedback due to multiple mechanisms, where early feedback first cleared a bubble (as we observe now in the Precursor Phantom Void), and since then supernovae have been exploding within the cavity and have accelerated the shell. Finally, comparison to simulations shows a striking resemblance to our JWST observations, and suggests that such large-scale, stellar-feedback-driven bubbles should be common within other galaxies.

We combine archival Hubble Space Telescope and new James Webb Space Telescope imaging data covering the ultraviolet to mid-infrared regime to morphologically analyze the nuclear star cluster (NSC) of NGC 628, a grand-design spiral galaxy. The cluster is located in a 200 pc x 400 pc cavity lacking both dust and gas. We find roughly constant values for the effective radius (r(eff) similar to 5 pc) and ellipticity (is an element of similar to 0.05), while the Sersic index (n) and position angle (PA) drop from n similar to 3 to similar to 2 and PA similar to 130 degrees to 90 degrees, respectively. In the mid-infrared, r(eff)similar to 12 pc, is an element of similar to 0.4, and n similar to 1-1.5, with the same PA similar to 90 degrees. The NSC has a stellar mass of log(10) (M(sic)(nsc) /M-circle dot)= 7.06 +/- 0.31, as derived through B -V, confirmed when using multiwavelength data, and in agreement with the literature value. Fitting the spectral energy distribution (SED), excluding the mid-infrared data, yields a main stellar population age of (8 +/- 3) Gyr with a metallicity of Z= 0.012 +/- 0.006. There is no indication of any significant star formation over the last few gigayears. Whether gas and dust were dynamically kept out or evacuated from the central cavity remains unclear. The best fit suggests an excess of flux in the mid-infrared bands, with further indications that the center of the mid-infrared structure is displaced with respect to the optical center of the NSC. We discuss five potential scenarios, none of them fully explaining both the observed photometry and structure.