Non-concerted evolution of the RET76 satellite DNA family in Reticulitermes taxa (Insecta, Isoptera).

The evolutionary dynamics of satellite DNA is most often studied in canonical mating systems, where bisexuality and panmixis are the rule. In eusocial termites, the limited number of reproducers starting a new colony and the maintenance of the colony through few neotenics act as bottle-necks both in space and time. No data on repetitive DNA are available for Isoptera and for their peculiar reproductive strategy. Here we present the first satellite DNA family isolated in European Reticulitermes. RET76 is a G+C rich satellite embodying two sub-families with a 76 bp monomer. RET76 sequences are highly variable (sequence homology is lower than 80% within sub-families and lower than 68% in the entire family) and this variability is equally distributed among the eight analysed taxa, thus depicting a pattern of non-concerted evolution. The absence of variant fixation – together with the strict monomer length conservation – may be explained at the molecular level as due to functional constraints acting on these sequences, and/or at the organismic level by considering the involvement of eusociality in preventing or greatly reducing variant fixation, somehow mimicking an unisexual strategy

Multi-messenger Observations of a Binary Neutron Star Merger

International audienceOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta