Micronuclei and other nuclear anomalies in exfoliated buccal mucosa cells of Mexican women with breast cancer

Purpose: Breast cancer (BC) is the most frequently diagnosed form of cancer and the leading cause of cancer-related deaths among females in the world. Results of several studies showed that the genome of primary cancer patients (naive for any treatment) is unstable. The purpose of the present study was to evaluate the genomic instability in BC patients by means of buccal cells micronucleus (MN) cytome assay Methods: The frequencies of nuclear anomalies including MN, binucleates (BN), broken eggs (BE), condensed chromatin (CC), karyorrhexis (KR) and karyolysis (KL) were evaluated in exfoliated buccal mucosa cells of Mexican women with primary BC and healthy women. Buccal cells were collected from 21 BC patients (9 with stage I and 12 with stage II) and from 20 healthy females used as control group. Results: The results of the evaluation of cells showed that the frequencies of MN, BN, BE, KR and KL were significantly increased in the pooled group of BC patients compared with the control group. However, no one parameter of buccal MN-cytome assay in patients with stage I BC was significant compared with controls and BC patients with stage II. Conclusion: Application of the buccal MN-cytome assay for the study of genomic instability in primary BC patients showed that both genotoxic and cytotoxic effects can be evaluated in such patients

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