scholarly journals Gravitational waveforms for neutron star binaries from binary black hole simulations

2016 ◽  
Vol 93 (4) ◽  
Author(s):  
Kevin Barkett ◽  
Mark A. Scheel ◽  
Roland Haas ◽  
Christian D. Ott ◽  
Sebastiano Bernuzzi ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Binary Black Hole

scholarly journals Recent searches for continuous gravitational waves

2017 ◽  
Vol 32 (39) ◽  
pp. 1730035 ◽  
Author(s):  
Keith Riles
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Star ◽  
Gravitational Waves ◽  
Gamma Ray ◽  
Continuous Wave ◽  
New Era ◽  
Binary Neutron Star ◽  
Binary Black Hole ◽  
Bose Einstein

Gravitational wave astronomy opened dramatically in September 2015 with the LIGO discovery of a distant and massive binary black hole coalescence. The more recent discovery of a binary neutron star merger, followed by a gamma ray burst (GRB) and a kilonova, reinforces the excitement of this new era, in which we may soon see other sources of gravitational waves, including continuous, nearly monochromatic signals. Potential continuous wave (CW) sources include rapidly spinning galactic neutron stars and more exotic possibilities, such as emission from axion Bose Einstein “clouds” surrounding black holes. Recent searches in Advanced LIGO data are presented, and prospects for more sensitive future searches are discussed.

scholarly journals DESGW Optical Follow-up of BBH LIGO-Virgo Events with DECam

2017 ◽  
Vol 13 (S338) ◽  
pp. 61-64
Author(s):  
Robert E. Butler ◽  
M. Soares-Santos ◽  
J. Annis ◽  
K. Herner ◽  
Keyword(s):  
Black Hole ◽  
Dark Energy ◽  
Neutron Star ◽  
Optical Emission ◽  
Binary Neutron Star ◽  
Dark Energy Survey ◽  
Binary Black Hole ◽  
The Status ◽  
Energy Survey

AbstractThe DESGW program is a collaboration between members of the Dark Energy Survey, the wider astronomical community, and the LIGO-Virgo Collaboration to search for optical counterparts of gravitational wave events, such as those expected from binary neutron star mergers or neutron star-black hole mergers. While binary black hole (BBH) events are not expected to produce an electromagnetic (EM) signature, emission is certainly not impossible. The DESGW program has performed follow-up observations of four BBH events detected by LIGO in order to search for any possible EM counterpart. Failure to find such counterparts is still relevant in that it produces limits on optical emission from such events. This is a review of follow-up results from O1 BBH events and a discussion of the status of ongoing uniform re-analysis of all BBH events that DESGW has followed up to date.

scholarly journals Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

2020 ◽  
Vol 23 (1) ◽  
Author(s):  
B. P. Abbott ◽  
◽  
R. Abbott ◽  
T. D. Abbott ◽  
S. Abraham ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Binary Systems ◽  
Compact Objects ◽  
Binary Neutron Star ◽  
Binary Black Hole ◽  
Credible Region ◽  
Binary Mergers ◽  
Black Hole Binary

AbstractWe present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is binary neutron star, neutron star–black hole, and binary black hole systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. During O3, the median localization volume (90% credible region) is expected to be on the order of $$10^{5}, 10^{6}, 10^{7}\mathrm {\ Mpc}^3$$ 10 5 , 10 6 , 10 7 Mpc 3 for binary neutron star, neutron star–black hole, and binary black hole systems, respectively. The localization volume in O4 is expected to be about a factor two smaller than in O3. We predict a detection count of $$1^{+12}_{-1}$$ 1 - 1 + 12 ($$10^{+52}_{-10}$$ 10 - 10 + 52 ) for binary neutron star mergers, of $$0^{+19}_{-0}$$ 0 - 0 + 19 ($$1^{+91}_{-1}$$ 1 - 1 + 91 ) for neutron star–black hole mergers, and $$17^{+22}_{-11}$$ 17 - 11 + 22 ($$79^{+89}_{-44}$$ 79 - 44 + 89 ) for binary black hole mergers in a one-calendar-year observing run of the HLV network during O3 (HLVK network during O4). We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers.

scholarly journals Could GRB170817A be really correlated to an NS–NS merging?

2018 ◽  
Vol 27 (06) ◽  
pp. 1841001 ◽  
Author(s):  
D. Fargion ◽  
M. Yu. Khlopov ◽  
P. Oliva
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gamma Ray ◽  
Solid Angle ◽  
Open Disk ◽  
Binary Neutron Star ◽  
Binary Black Hole ◽  
Exciting Development ◽  
Soft Disk ◽  
Optical Transient

The exciting development of gravitational wave (GW) astronomy in the correlation of LIGO and VIRGO detection of GW signals makes possible to expect registration of effects of not only binary black hole (BH) coalescence but also binary neutron star (NS) merging accompanied by electromagnetic (gamma ray burst; GRB) signal. Here we consider the possibility that an NS, merging in an NS–NS or NS–BH system might be (soon) observed in correlation with any LIGO–VIRGO GWs detection. We analyze as an example the recent case of the short GRB170817A observed by Fermi and integral. The associated optical transient (OT) source in NGC4993 implies a rare near source, a consequent averaged large rate of such events (almost) compatible with expected NS–NS merging rate. However the expected beamed GRB (or short GRB) may be mostly aligned to a different direction than ours. Therefore, even soft GRB photons, spread more than hard ones, might be hardly able to shower to us. Nevertheless, a prompt spiraling electron turbine jet in largest magnetic fields, at the base of the NS–NS collapse, might shine by its tangential synchrotron radiation in spread way with its skimming photons shining in large open disk. The consequent solid angle for such soft disk gamma radiation may be large enough to be nevertheless often observed.

scholarly journals First direct comparison of nondisrupting neutron star-black hole and binary black hole merger simulations

2013 ◽  
Vol 88 (6) ◽  
Author(s):  
Francois Foucart ◽  
Luisa Buchman ◽  
Matthew D. Duez ◽  
Michael Grudich ◽  
Lawrence E. Kidder ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Binary Black Hole

scholarly journals 3-OGC: Catalog of Gravitational Waves from Compact-binary Mergers

2021 ◽  
Vol 922 (1) ◽  
pp. 76
Author(s):  
Alexander H. Nitz ◽  
Collin D. Capano ◽  
Sumit Kumar ◽  
Yi-Fan Wang ◽  
Shilpa Kastha ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Parameter Estimates ◽  
The Public ◽  
Binary Neutron Star ◽  
The Third ◽  
Compact Binary ◽  
Binary Black Hole ◽  
Binary Mergers

Abstract We present the third open gravitational-wave catalog (3-OGC) of compact-binary coalescences, based on the analysis of the public LIGO and Virgo data from 2015 through 2019 (O1, O2, O3a). Our updated catalog includes a population of 57 observations, including 4 binary black hole mergers that had not been previously reported. This consists of 55 binary black hole mergers and the 2 binary neutron star mergers, GW170817 and GW190425. We find no additional significant binary neutron star or neutron star–black hole merger events. The most confident new detection is the binary black hole merger GW190925_232845, which was observed by the LIGO–Hanford and Virgo observatories with  astro > 0.99 ; its primary and secondary component masses are 20.2 − 2.5 + 3.9 M ⊙ and 15.6 − 2.6 + 2.1 M ⊙ , respectively. We estimate the parameters of all binary black hole events using an up-to-date waveform model that includes both subdominant harmonics and precession effects. To enable deep follow up as our understanding of the underlying populations evolves, we make available our comprehensive catalog of events, including the subthreshold population of candidates, and the posterior samples of our source parameter estimates.

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