Ocorrência de Dioctophyma renale em Galictis cuja

A dioctofimose é uma parasitose causada pelo Dioctophyma renale (Goeze, 1782) de ocorrência mundial e acomete animais domésticos e silvestres. Em março de 2010, um exemplar adulto (macho) de Galictis cuja (Molina, 1782), encontrado morto por atropelamento no município de Guaíra, Paraná foi encaminhado ao laboratório de Patologia Veterinária de Universidade Federal do Paraná (UFPR), Campus Palotina, para a realização da necropsia. O cadáver apresentava bom estado nutricional e autólise moderada. Foram observados três exemplares de parasitos na cavidade abdominal, mas os rins encontravam-se preservados. Os parasitos foram fixados em formol acético e encaminhados ao laboratório de Parasitologia Veterinária da UFPR para identificação. Os exemplares coletados foram identificados como Dioctophyma renale, sendo duas fêmeas, uma com 39cm de comprimento por 4mm de largura e a outra com 16cm de comprimento por 4mm de largura e, um macho com 16cm de comprimento por 3mm de largura. O presente trabalho relata a ocorrência de parasitismo por D. renale em G. cuja na região oeste do estado do Paraná

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