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 M ⊙ . 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 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.

Merging neutron stars offer an excellent laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart (EM170817) with gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic data set, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultrarelativistic jets. Instead, we suggest that breakout of a wide-angle, mildly relativistic cocoon engulfing the jet explains the low-luminosity gamma rays, the high-luminosity ultraviolet-optical-infrared, and the delayed radio and x-ray emission. We posit that all neutron star mergers may lead to a wide-angle cocoon breakout, sometimes accompanied by a successful jet and sometimes by a choked jet.

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X-ray and Gamma-ray polarization measurements of the prompt emission of Gamma-ray bursts (GRBs) are believed to be an important tool to test the various models of GRBs. Although there are some reports of hard X-ray polarization measurements of the prompt emission of GRBs, the number of measurements are small to provide statistically significant inputs to the GRB models due to the extreme difficulty of measuring them and quantifying their significance. CZTI onboard AstroSat is primarily an X-ray spectroscopic instrument but works as a wide angle GRB monitor due to the increasing transparency of the CZTI support structure. It also has experimentally verified polarization measurement capability in the 100 − 300 keV energy range and thus provides a unique opportunity to attempt spectro-polarimetric studies of GRBs. Here we present the polarization data for the brightest 11 GRBs detected by CZTI during the first year of operation. Most of the GRBs show clear polarization signatures with ≥3σ detection significance for 4 GRBs and ∼2.5σ significance for another 3 GRBs. We could place meaningful upper limits for the remaining 4 GRBs. We provide the details of the various tests performed to validate the polarization measurements. While it is difficult to differentiate the various emission models with the current sample of polarization measurements, CZTI in its minimum lifetime of five years is expected to provide a large sample of polarization measurements which would lead to a better understanding of the prompt emission.

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In this paper we make a phase‐dependent study of the effect of the distortion of the local magnetic field due to confinement of the accreted matter in X‐ray pulsars on the cyclotron spectra emitted from the hotspot. We have numerically solved the Grad–Shafranov equation for axisymmetric static magnetohydrodynamic (MHD) equilibria of the matter confined at the polar cap of neutron stars. From our solution, we model the cyclotron spectra that will be emitted from the region, using a simple prescription and integrating over the entire mound. Radiative transfer through the accretion column overlying the mound may significantly modify the spectra in comparison to those presented here. However, we ignore this in the present paper in order to expose the effects directly attributable to the mound itself. We perform a spin phase‐dependent analysis of the spectra to study the effect of the viewing geometry.

Donors and other development partners commonly introduce innovative practices and technologies to improve health in low and middle income countries. Yet many innovations that are effective in improving health and survival are slow to be translated into policy and implemented at scale. Understanding the factors influencing scale-up is important. We conducted a qualitative study involving 150 semi-structured interviews with government, development partners, civil society organisations and externally funded implementers, professional associations and academic institutions in 2012/13 to explore scale-up of innovative interventions targeting mothers and newborns in Ethiopia, the Indian state of Uttar Pradesh and the six states of northeast Nigeria, which are settings with high burdens of maternal and neonatal mortality. Interviews were analysed using a common analytic framework developed for cross-country comparison and themes were coded using Nvivo. We found that programme implementers across the three settings require multiple steps to catalyse scale-up. Advocating for government to adopt and finance health innovations requires: designing scalable innovations; embedding scale-up in programme design and allocating time and resources; building implementer capacity to catalyse scale-up; adopting effective approaches to advocacy; presenting strong evidence to support government decision making; involving government in programme design; invoking policy champions and networks; strengthening harmonisation among external programmes; aligning innovations with health systems and priorities. Other steps include: supporting government to develop policies and programmes and strengthening health systems and staff; promoting community uptake by involving media, community leaders, mobilisation teams and role models. We conclude that scale-up has no magic bullet solution - implementers must embrace multiple activities, and require substantial support from donors and governments in doing so.