On August 17, 2017 at 12∶41:04 UTC the Advanced LIGO and Advanced Virgo gravitational-wave detectors made their first observation of a binary neutron star inspiral. The signal, GW170817, was detected with a combined signal-to-noise ratio of 32.4 and a false-alarm-rate estimate of less than one per 8.0×10^{4}  years. We infer the component masses of the binary to be between 0.86 and 2.26  M_{⊙}, in agreement with masses of known neutron stars. Restricting the component spins to the range inferred in binary neutron stars, we find the component masses to be in the range 1.17-1.60  M_{⊙}, with the total mass of the system 2.74_{-0.01}^{+0.04}M_{⊙}. The source was localized within a sky region of 28  deg^{2} (90% probability) and had a luminosity distance of 40_{-14}^{+8}  Mpc, the closest and most precisely localized gravitational-wave signal yet. The association with the γ-ray burst GRB 170817A, detected by Fermi-GBM 1.7 s after the coalescence, corroborates the hypothesis of a neutron star merger and provides the first direct evidence of a link between these mergers and short γ-ray bursts. Subsequent identification of transient counterparts across the electromagnetic spectrum in the same location further supports the interpretation of this event as a neutron star merger. This unprecedented joint gravitational and electromagnetic observation provides insight into astrophysics, dense matter, gravitation, and cosmology.

/pdf/gw170817-observation-of-gravitational-waves-from-a-binary-q2x9byg981.pdf

GW170817: observation of gravitational waves from a binary neutron star inspiral

The masses of supermassive black holes correlate almost perfectly with the velocity dispersions of their host bulges, Mbh ∝ σα, where α = 48 ± 05 The relation is much tighter than the relation between Mbh and bulge luminosity, with a scatter no larger than expected on the basis of measurement error alone Black hole masses recently estimated by Magorrian et al lie systematically above the Mbh-σ relation defined by more accurate mass estimates, some by as much as 2 orders of magnitude The tightness of the Mbh-σ relation implies a strong link between black hole formation and the properties of the stellar bulge

https://iopscience.iop.org/article/10.1086/312838/pdf

A Fundamental Relation Between Supermassive Black Holes and Their Host Galaxies

On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10(-21). It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410(-180)(+160)  Mpc corresponding to a redshift z=0.09(-0.04)(+0.03). In the source frame, the initial black hole masses are 36(-4)(+5)M⊙ and 29(-4)(+4)M⊙, and the final black hole mass is 62(-4)(+4)M⊙, with 3.0(-0.5)(+0.5)M⊙c(2) radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.

/pdf/the-observation-of-gravitational-waves-from-a-binary-black-58srpupgg9.pdf

The Observation of Gravitational Waves from a Binary Black Hole Merger

Many physically motivated extensions to general relativity (GR) predict significant deviations at energies present in massive neutron stars. We report the measurement of a 2.01 \(\pm \) 0.04 solar mass (M\(_\odot \)) pulsar in a 2.46-h orbit around a 0.172 \(\pm \) 0.003 M\(_\odot \) white dwarf. The high pulsar mass and the compact orbit make this system a sensitive laboratory of a previously untested strong-field gravity regime. Thus far, the observed orbital decay agrees with GR, supporting its validity even for the extreme conditions present in the system. The resulting constraints on deviations support the use of GR-based templates for ground-based gravitational wave detection experiments. Additionally, the system strengthens recent constraints on the properties of dense matter and provides novel insight to binary stellar astrophysics and pulsar recycling.

/pdf/a-massive-pulsar-in-a-compact-relativistic-binary-4fslj44n2n.pdf

A massive pulsar in a compact relativistic binary

We have compiled a new and complete catalog of the main properties of the 1509 pulsars for which published information currently exists. The catalog includes all spin-powered pulsars, as well as anomalous X-ray pulsars and soft gamma-ray repeaters showing coherent pulsed emission, but excludes accretion-powered systems. References are given for all data listed. We have also developed a new World Wide Web interface for accessing and displaying either tabular or plotted data with the option of selecting pulsars to be displayed via logical conditions on parameter expressions. The Web interface has an expert mode giving access to a wider range of parameters and allowing the use of custom databases. For users with locally installed software and database on Unix or Linux systems, the catalog may be accessed from a command-line interface. C-language functions to access specified parameters are also available. The catalog is updated from time to time to include new information.

https://iopscience.iop.org/article/10.1086/428488/pdf

The Australia Telescope National Facility Pulsar Catalogue

The Hipparcos distance determination of the Wolf-Rayet system gamma(2) Velorum (WC8+O) and its ramifications

Age of a millisecond binary pulsar

We find that the orbital period (2.4 h), eccentricity (0.09), dipole magnetic field strength (6.9 x 10 9 G) and spin period (22 ms) of the new highly relativistic double neutron star system PSR J0737 - 3039 can all be consistently explained if this system originated from a close helium star plus neutron star (HeS-NS) binary in which at the onset of the evolution the helium star had a mass in the range 4.0-6.5 M ○. and an orbital period in the range 0.1-0.2 d. Such systems are the post-common-envelope remnants of wide Be/X-ray binaries (orbital period ∼100 to 1000 d) which consist of a normal hydrogen-rich star with a mass in the range 10-20 M ○. and a neutron star. The close HeS-NS progenitor system went through a phase of mass transfer by Roche-lobe overflow at a high rate lasting a few times 10 4 yr; assuming Eddington-limited disc accretion on to the neutron star, this star was spun up to its present rapid spin rate. At the moment of the second supernova explosion the He star had a mass in the range 2.3-3.3 M ○. , and in order to obtain the present orbital parameters of PSR J0737 - 3039 a kick velocity in the range 70-230 km s -1 must have been imparted to the second neutron star at its birth.

The formation of the double neutron star pulsar J0737 − 3039

Preface. List of Participants. 1: Radio Pulsars and Neutron Stars. Radio Pulsars - an Observer's Perspective D.R. Lorimer. Neutron Star Birth Rates D.R. Lorimer. Kinematics of Radio Pulsars R. Ramachandran. Superfluid Dynamics and Energy Dissipation in Neutron Stars M.A. Alpar. Magnetic Fields of Neutron Stars S. Konar, D. Bhattacharya. 2: The Neutron Star - Black Hole Connection. Neutron Star and Black Hole Formation C.L. Fryer. Coalescence Rates of Compact Objects V. Kalogera. The Final Fate of Coalescing Compact Binaries: From Black Hole to Planet Formation F.A. Rasio. 3: Accretion Discs. Accretion Discs H.C. Spruit. Radiatively Inefficient Accretion Discs H.C. Spruit. Inner Region of Accretion Flows onto Black Holes M. Kafatos, P. Subramanian. 4: Neutron stars and Black Holes in Binaries. Neutron Stars and Black Holes in Binaries E.P.J. van den Heuvel. Formation and Evolution of Neutron Stars and Black Holes in Binary Systems E.P.J. van den Heuvel. Transient Low-Mass X-Ray Binaries in Quiescence L. Bildsten, R.E. Rutledge. A Comparison of Radio Emission from Neutron Star and Black Hole X-ray Binaries R.P. Fender. Black Hole and Neutron Star Jet Sources I.F. Mirabel. Bulk-Flow Comptonization and Time Lags due to Comptonization N.D. Kylafis, P. Reig. GRS 1915+105 as a Black Hole Accretion Disk Laboratory T. Belloni. Weighing Black Holes with the Largest Optical Telescopes E.T. Harlaftis, A.V. Filippenko. Physics of Plasma Outflows S.V. Bogovalov, K. Tsinganos. Timing the Kilohertz Quasi-periodic Oscillations in Low-Mass Binaries M. Mendez. Modeling the Time Variability of Black Hole Candidates D.Kazanas. Relativistic Models of kHz QPOs W. Kluzniak. Phenomenology of the 35-day Cycle of Hercules X-1 N.I. Shakura, et al. Spin-Orbit Couplings in X-ray Binaries T.M. Tauris, G.J. Savonije. High Mass Black Holes in Soft X-ray Transients G.E. Brown, et al. 5: Magnetars. The Anomalous X-ray Pulsars S. Mereghetti. Astrophysics of the Soft Gamma Repeaters and the Anomalous X-ray Pulsars C. Thompson. Neutron Star Envelopes and Thermal Radiation from the Magnetic Surface J. Ventura, and A.Y. Potekhin. 6: Gamma-ray Bursts. Gamma-ray Bursts: History and Observations G.J. Fishman. The Afterglow of Gamma-ray Bursts: Light on the Mystery L. Piro. Gamma-ray Bursts and Afterglows: The Fireball Shock Model P. Meszaros. Gamma-ray Bursts from Neutron Stars Spun up in X-ray Binaries H.C. Spruit. 7: New Experiments. The Candra X-ray Observatory (CXO) M.C. Weisskopf.

The Neutron Star-Black Hole Connection

BeppoSAX. Proceedings of the BeppoSAX Conference ``The Restless High-Energy Universe''

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