Gauge-Invariant Initial Conditions and Early Time Perturbations in Quintessence Universes

We present a systematic treatment of the initial conditions and evolution of cosmological perturbations in a universe containing photons, baryons, neutrinos, cold dark matter, and a scalar quintessence field. By formulating the evolution in terms of a differential equation involving a matrix acting on a vector comprised of the perturbation variables, we can use the familiar language of eigenvalues and eigenvectors. As the largest eigenvalue of the evolution matrix is fourfold degenerate, it follows that there are four dominant modes with non-diverging gravitational potential at early times, corresponding to adiabatic, cold dark matter isocurvature, baryon isocurvature and neutrino isocurvature perturbations. We conclude that quintessence does not lead to an additional independent mode.Comment: Replaced with published version, 12 pages, 2 figure

Determinação do valor nutritivo de alimentos energéticos e protéicos utilizados em rações para cães adultos Evaluation of nutritive value of energy and protein feeds in adult dogs diets

Dois experimentos foram realizados para avaliar a digestibilidade aparente da EB, MS e PB em alimentos energéticos e protéicos utilizados para cães adultos. Foram utilizados quatro cães adultos (13,1 &plusmn; 2,0 kg), dois machos e duas fêmeas, sem raça definida, na avaliação de cada alimento. Os animais receberam a mesma quantidade de ração por unidade de peso metabólico. No experimento 1, foi determinado o valor nutritivo dos alimentos energéticos e, no experimento 2, os coeficientes de digestibilidade dos alimentos protéicos. Os coeficientes de digestibilidade da EB do milho extrusado (ME), do milho gelatinizado (MG), da gordura de coco e do óleo de soja, em dois níveis de inclusão (OS1 e OS2), e da gordura suína foram, respectivamente, 85,1; 84,4; 92,5; 92,1; 96,2 e 98,6%. Os coeficientes de digestibilidade da MS e PB do ME e MG foram, respectivamente, 84,2 e 65,3 e 84,5 e 65,0%. Na soja integral extrusada e nas farinhas de carne, de carne extrusada, de vísceras, de vísceras extrusada, de peixe extrusada e de pena extrusada, foram obtidos, respectivamente, os seguintes coeficientes de digestibilidade: 80,0; 73,3; 80,7; 87,6; 91,2; 91,1 e 79,8% da EB; 80,0; 68,4; 87,8; 86,7; 88,1; 85,2 e 76,0% da MS; e 83,7; 74,7; 82,3; 88,0; 88,9; 91,9 e 82,3% da PB.<br>Two trials were conducted to evaluate the apparent digestibility of GE, DM and CP in energy and high protein feedstuffs for adult dogs. Four adult mongrel dogs (two males and two females) averaging of 13.1 &plusmn; 2.0 kg were used in both trials, to evaluate each feedstuff. The animals were fed the same amount of food per metabolic weight. The nutritive value of energy feedstuffs was evaluated in the trial 1. In the trial 2, the digestibility coefficients of protein feedstuffs were evaluated. The digestibility coefficients of GE in extruded corn (EC), gelatinized corn (GC), coconut oil, and soybean oil, in two levels of inclusion (5%-OS1 and 12%-OS2) and swine fat were respectively of 85.1, 84.4, 92.5, 92.1, 96.2, and 98.6%. The digestibility coefficients of DM and CP of EC and GC were, respectively, of 84.2 and 65.3 and 84.5 and 65.0%. The digestibility coefficients of extruded whole soybean, meat meal, extruded meat meal, poultry by-product meal, extruded poultry by-product meal, extruded fish meal, and extruded feather meal were, respectively, of 80.0, 73.3, 80.7, 87.6, 91.2, 91.1, and 79.8% for GE, of 80.0, 68.4, 87.8, 86.7, 88.1, 85.2, and 76.0 for DM and of 83.7, 74.7, 82.3, 88.0, 88.9, 91.9, and 82.3% for CP

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