We present an up-to-date, comprehensive summary of the rates for all types of compact binary coalescence sources detectable by the initial and advanced versions of the ground-based gravitational-wave detectors LIGO and Virgo. Astrophysical estimates for compact-binary coalescence rates depend on a number of assumptions and unknown model parameters and are still uncertain. The most confident among these estimates are the rate predictions for coalescing binary neutron stars which are based on extrapolations from observed binary pulsars in our galaxy. These yield a likely coalescence rate of 100 Myr−1 per Milky Way Equivalent Galaxy (MWEG), although the rate could plausibly range from 1 Myr−1 MWEG−1 to 1000 Myr−1 MWEG−1 (Kalogera et al 2004 Astrophys. J. 601 L179; Kalogera et al 2004 Astrophys. J. 614 L137 (erratum)). We convert coalescence rates into detection rates based on data from the LIGO S5 and Virgo VSR2 science runs and projected sensitivities for our advanced detectors. Using the detector sensitivities derived from these data, we find a likely detection rate of 0.02 per year for Initial LIGO–Virgo interferometers, with a plausible range between 2 × 10−4 and 0.2 per year. The likely binary neutron–star detection rate for the Advanced LIGO–Virgo network increases to 40 events per year, with a range between 0.4 and 400 per year.

Abstract. We describe the PyCBC search for gravitational waves from compactobject binary coalescences in advanced gravitational-wave detector data. The search was used in the first Advanced LIGO observing run and unambiguously identified two black hole binary mergers, GW150914 and GW151226. At its core, the PyCBC search performs a matched-filter search for binary merger signals using a bank of gravitational-wave template waveforms. We provide a complete description of the search pipeline including the steps used to mitigate the effects of noise transients in the data, identify candidate events and measure their statistical significance. The analysis is able to measure false-alarm rates as low as one per million years, required for confident detection of signals. Using data from initial LIGO's sixth science run, we show that the new analysis reduces the background noise in the search, giving a 30% increase in sensitive volume for binary neutron star systems over previous searches.

In 2009-2010, the Laser Interferometer Gravitational-wave Observatory (LIGO) operated together with international partners Virgo and GEO600 as a network to search for gravitational waves of astrophysical origin. The sensitivity of these detectors was limited by a combination of noise sources inherent to the instrumental design and its environment, often localized in time or frequency, that couple into the gravitational-wave readout. Here we review the performance of the LIGO instruments during this epoch, the work done to characterize the detectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of LIGO to a variety of astrophysical sources.

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1. INTRODUCTION 1.1 Generalities and Context 1.2 C-N Bond Formation via Cross-Coupling Reactions 1.3 C-N Bond Formation via Nucleophile-Electrophile Cross-Coupling 1.4 C-N Bond Formation via Nucleophile-Nucleophile Cross-Coupling 2. DISCUSSION 2.1 Discovery 2.2 Development of Reaction Conditions 2.3 A General Mechanistic Description of the Chan-Lam Reaction 2.4 Reactions Variables and Selection of Reaction Conditions 3. SCOPE OF THE CHAN-LAM AMINATION 3.1 Organoboron Variation 3.2 Aryl Amines (Anilines) 3.3 Heteroaryl Amines (Heterocyclic Anilines) 3.4 Alkyl Amines 3.5 Amides 3.6 NH-Heterocycles 3.7 C-N Bond Formation to non-NH-Nucleophiles 3.8 Sulfonamides and Sulfoximes 3.9 Sequential Processes 3.10 C-N Bond Formation on Nucleobases and Peptides 4. MECHANISM 4.1 Historical Context 4.2 Mechanistic Investigations in the Etherification Reaction 4.3 Mechanistic Investigations in the Amination Reaction 4.4 Mechanistic Investigations in the Amination Reaction: Ligand-based Systems 4.5 Mechanism Summary