Multi-messenger observations of a binary neutron star merger

On 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 ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 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 Mo. 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 ~40 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 ~9 and ~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 NGC4993 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

Fast and not-so-furious: Case study of the fast and faint Type IIb SN 2021bxu

We present photometric and spectroscopic observations and analysis of SN 2021bxu (ATLAS21dov), a low-luminosity, fast-evolving Type IIb supernova (SN). SN 2021bxu is unique, showing a large initial decline in brightness followed by a short plateau phase. With during the plateau, it is at the lower end of the luminosity distribution of stripped-envelope supernovae (SE-SNe) and shows a distinct ∼10 d plateau not caused by H- or He-recombination. SN 2021bxu shows line velocities which are at least slower than typical SE-SNe. It is photometrically and spectroscopically similar to Type IIb SNe during the photospheric phases of evolution, with similarities to Ca-rich IIb SNe. We find that the bolometric light curve is best described by a composite model of shock interaction between the ejecta and an envelope of extended material, combined with a typical SN IIb powered by the radioactive decay of 56Ni. The best-fitting parameters for SN 2021bxu include a 56Ni mass of, an ejecta mass of, and an ejecta kinetic energy of. From the fits to the properties of the extended material of Ca-rich IIb SNe we find a trend of decreasing envelope radius with increasing envelope mass. SN 2021bxu has MNi on the low end compared to SE-SNe and Ca-rich SNe in the literature, demonstrating that SN 2021bxu-like events are rare explosions in extreme areas of parameter space. The progenitor of SN 2021bxu is likely a low-mass He star with an extended envelope

The Wide-field Spectroscopic Telescope (WST) Science White Paper

The Wide-field Spectroscopic Telescope (WST) is proposed as a new facility dedicated to the efficient delivery of spectroscopic surveys. This white paper summarises the initial concept as well as the corresponding science cases. WST will feature simultaneous operation of a large field-of-view (3 sq. degree), a high multiplex (20,000) multi-object spectrograph (MOS) and a giant 3x3 sq. arcmin integral field spectrograph (IFS). In scientific capability these requirements place WST far ahead of existing and planned facilities. Given the current investment in deep imaging surveys and noting the diagnostic power of spectroscopy, WST will fill a crucial gap in astronomical capability and work synergistically with future ground and space-based facilities. This white paper shows that WST can address outstanding scientific questions in the areas of cosmology; galaxy assembly, evolution, and enrichment, including our own Milky Way; origin of stars and planets; time domain and multi-messenger astrophysics. WST's uniquely rich dataset will deliver unforeseen discoveries in many of these areas. The WST Science Team (already including more than 500 scientists worldwide) is open to the all astronomical community. To register in the WST Science Team please visit https://www.wstelescope.com/for-scientists/participat

Localization and broadband follow-up of the gravitational-wave transient GW150914

A gravitational-wave transient was identified in data recorded by the Advanced LIGO detectors on 2015 September 14. The event candidate, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the gravitational wave data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network Circulars, giving an overview of the participating facilities, the gravitational wave sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the electromagnetic data and results of the electromagnetic follow-up campaign will be disseminated in the papers of the individual teams

Cardiovascular toxicity and distribution kinetics of intravenous chloroquine.

Chloroquine diphosphate (3 mg base kg-1) was given by constant rate intravenous injection over 10 min to 12 healthy adult male volunteers. Plasma concentrations of chloroquine and the principal metabolite desethylchloroquine, electrocardiograph intervals, and arterial blood pressure were measured at frequent intervals to determine the relationship between cardiovascular effects and plasma concentrations. Peak plasma concentrations ranged between 784 and 6649 (mean 2913) ng ml-1. The decline in plasma concentrations was multiexponential with an initial rapid distribution phase; mean (+/- s.d.) first order rate constant 0.65 +/- 0.14 min-1, and an estimated apparent volume of the central compartment of 0.18 +/- 0.15 l kg-1. There was no serious toxicity, but subjective side effects were reported in all patients and there was a significant fall in systolic blood pressure (110 +/- 9.5 to 101 +/- 12.5 mm Hg; P = 0.03) and rise in heart rate which paralleled the change in plasma chloroquine concentrations. Coincident with changes in blood pressure, there was a significant prolongation of the electrocardiograph QRS interval; 81 +/- 15 to 92 +/- 13 ms (P less than 0.01) but no change in the QTc interval. These findings suggest that the cardiovascular toxicity of parenteral chloroquine is related to transiently high plasma concentrations occurring early in the distribution phase. This results from incomplete distribution from a central compartment that is approximately one thousand times smaller than the eventual total apparent volume of distribution at steady state. Rate of administration is therefore a major determinant of toxicity

Pharmacokinetics of intravenous amodiaquine.

Amodiaquine hydrochloride (3 mg base kg-1) was given by constant rate intravenous injection over 10 min to seven healthy adult male volunteers, and by constant rate infusion (10 mg base kg-1) over 4 h to 10 adult patients admitted to hospital with falciparum malaria. After intravenous injection in volunteers there was considerable variation in plasma concentration profiles between subjects; peak plasma concentrations ranged between 65 and 1921 ng ml-1. A biexponential equation was fitted to the plasma concentration time data and the following estimated pharmacokinetic parameters (geometric mean; range) were derived; lambda 1 = 24.4 (7.6-95.0) h-1, lambda 2 = 0.33 (0.12-0.79) h-1, V1:1.1 (0.3-3.6) 1 kg-1, Vss: 17.4 (2.3-95.9) 1 kg-1 and systemic clearance 13.0 (4.7-56.6) 1 kg-1 h-1. After intravenous infusion there was also considerable variability between patients with post-infusion plasma concentrations ranging between 82 and 836 ng ml-1. The plasma concentration-time profiles were biphasic with the following estimated pharmacokinetic parameters (geometric mean; range) alpha = 1.87 (0.60-8.52) h-1, beta = 0.069 (0.021-0.265) h-1, V1: 4.6 (0.5-29.3) 1 kg-1, Vss: 38.3 (3.7-127.9) 1 kg-1 and systemic clearance CL (1.6-17.3) 1 kg-1 h-1. There was no measurable long terminal elimination phase, and the principal metabolite desethyl amodiaquine was not detected in the plasma samples. There was no serious toxicity in either group. During intravenous injection there was a significant fall in systolic blood pressure in four subjects (mean fall 16 mm Hg) but there was no significant change in heart rate.(ABSTRACT TRUNCATED AT 250 WORDS