Radial velocity (RV) surveys have discovered giant exoplanets on au-scale orbits with a broad distribution of eccentricities. Those with the most eccentric orbits are valuable laboratories for testing theories of high-eccentricity migration. However, few such exoplanets transit their host stars, thus removing the ability to apply constraints on formation from their bulk internal compositions. We report the discovery of Kepler-1704 b, a transiting 4.15 M J giant planet on a 988.88 day orbit with an extreme eccentricity of -+ 0.921 0.015 0.010 . Our decade-long RV baseline from the Keck I telescope allows us to measure the orbit and bulk heavy-element composition of Kepler-1704 b and place limits on the existence of undiscovered companions. A failed hot Jupiter, Kepler-1704 b was likely excited to high eccentricity by scattering events that possibly began during its gas accretion phase. Its final periastron distance was too large to allow for tidal circularization, so now it orbits its host from distances spanning 0.16-3.9 au. The maximum difference in planetary equilibrium temperature resulting from this elongated orbit is over 700 K. A simulation of the thermal phase curve of Kepler-1704 b during periastron passage demonstrates that it is a remarkable target for atmospheric characterization from the James Webb Space Telescope, which could potentially also measure the planet's rotational period as the hot spot from periastron rotates in and out of view. Continued characterization of the Kepler-1704 system promises to refine theories explaining the formation of hot Jupiters and cool giant planets like those in the solar system.

We have examined the abilities of three complementary γ-peptide nucleic acid (γPNA) oligomers to invade an RNA G-quadruplex and potently inhibit translation of a luciferase reporter transcript containing the quadruplex-forming sequence (QFS) within its 5'-untranslated region. All three γPNA oligomers bind with low nanomolar affinities to an RNA oligonucleotide containing the QFS. However, while all probes inhibit translation with low to midnanomolar IC50 values, the γPNA designed to hybridize to the first two G-tracts of the QFS and adjacent 5'-overhanging nucleotides was 5-6 times more potent than probes directed to either the 3'-end or internal regions of the target at 37 °C. This position-dependent effect was eliminated after the probes and target were preincubated at an elevated temperature prior to translation, demonstrating that kinetic effects exert significant control over quadruplex invasion and translation inhibition. We also found that antisense γPNAs exhibited similarly potent effects against luciferase reporter transcripts bearing QFS motifs having G2, G3, or G4 tracts. Finally, our results indicate that γPNA oligomers exhibit selectivity and/or potency higher than those of other antisense molecules such as standard PNA and 2'-OMe RNA previously reported to target G-quadruplexes in RNA.

Characterizing the bulk compositions of transiting exoplanets within the M dwarf radius valley offers a unique means to establish whether the radius valley emerges from an atmospheric mass-loss process or is imprinted by planet formation itself. We present the confirmation of such a planet orbiting an early-M dwarf (T mag = 11.0294 ± 0.0074, M s = 0.513 ± 0.012 M ⊙, R s = 0.515 ± 0.015 R ⊙, and T eff = 3690 ± 50 K): TOI-1695 b (P = 3.13 days and R p = 1.90 − 0.14 + 0.16 R ⊕ ). TOI-1695 b’s radius and orbital period situate the planet between model predictions from thermally driven mass loss versus gas depleted formation, offering an important test case for radius valley emergence models around early-M dwarfs. We confirm the planetary nature of TOI-1695 b based on five sectors of TESS data and a suite of follow-up observations including 49 precise radial velocity measurements taken with the HARPS-N spectrograph. We measure a planetary mass of 6.36 ± 1.00 M ⊕, which reveals that TOI-1695 b is inconsistent with a purely terrestrial composition of iron and magnesium silicate, and instead is likely a water-rich planet. Our finding that TOI-1695 b is not terrestrial is inconsistent with the planetary system being sculpted by thermally driven mass loss. We present a statistical analysis of seven well-characterized planets within the M dwarf radius valley demonstrating that a thermally driven mass-loss scenario is unlikely to explain this population.