scholarly journals Application of the third RIT binary black hole simulations catalog to parameter estimation of gravitational-wave signals from the LIGO-Virgo O1 and O2 observational runs

2020 ◽  
Vol 102 (12) ◽  
Author(s):  
James Healy ◽  
Carlos O. Lousto ◽  
Jacob Lange ◽  
Richard O’Shaughnessy
Keyword(s):  
Black Hole ◽  
Parameter Estimation ◽  
Gravitational Wave ◽  
The Third ◽  
Binary Black Hole

scholarly journals Implications of recoil kicks for black hole mergers from LIGO/Virgo catalogs

2021 ◽  
Vol 502 (3) ◽  
pp. 3879-3884
Author(s):  
Giacomo Fragione ◽  
Abraham Loeb
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Globular Clusters ◽  
Star Clusters ◽  
Star Cluster ◽  
Effective Spin ◽  
The Third ◽  
Binary Black Hole ◽  
Super Star Clusters ◽  
Escape Speed

ABSTRACT The first and second Gravitational Wave Transient Catalogs by the LIGO/Virgo Collaboration include 50 confirmed merger events from the first, second, and first half of the third observational runs. We compute the distribution of recoil kicks imparted to the merger remnants and estimate their retention probability within various astrophysical environments as a function of the maximum progenitor spin (χmax), assuming that the LIGO/Virgo binary black hole (BBH) mergers were catalyzed by dynamical assembly in a dense star cluster. We find that the distributions of average recoil kicks are peaked at about $150\, \rm km\, s^{-1}$, $250\, \rm km\, s^{-1}$, $350\, \rm km\, s^{-1}$, $600\, \rm km\, s^{-1}$, for maximum progenitor spins of 0.1, 0.3, 0.5, 0.8, respectively. Only environments with escape speed ${\gtrsim}100\, \rm km\, s^{-1}$, as found in galactic nuclear star clusters as well as in the most massive globular clusters and super star clusters, could efficiently retain the merger remnants of the LIGO/Virgo BBH population even for low progenitor spins (χmax = 0.1). In the case of high progenitor spins (χmax ≳ 0.5), only the most massive nuclear star clusters can retain the merger products. We also show that the estimated values of the effective spin and of the remnant spin of GW170729, GW190412, GW190519_153544, and GW190620_030421 can be reproduced if their progenitors were moderately spinning (χmax ≳ 0.3), while for GW190517_055101 if the progenitors were rapidly spinning (χmax ≳ 0.8). Alternatively, some of these events could be explained if at least one of the progenitors is already a second-generation BH, originated from a previous merger.

scholarly journals Optimization of model independent gravitational wave search for binary black hole mergers using machine learning

2021 ◽  
Vol 104 (2) ◽  
Author(s):  
T. Mishra ◽  
B. O’Brien ◽  
V. Gayathri ◽  
M. Szczepańczyk ◽  
S. Bhaumik ◽  
...  
Keyword(s):  
Machine Learning ◽  
Black Hole ◽  
Gravitational Wave ◽  
Binary Black Hole ◽  
Model Independent

scholarly journals Biases in parameter estimation from overlapping gravitational-wave signals in the third-generation detector era

2021 ◽  
Vol 104 (4) ◽  
Author(s):  
Anuradha Samajdar ◽  
Justin Janquart ◽  
Chris Van Den Broeck ◽  
Tim Dietrich
Keyword(s):  
Parameter Estimation ◽  
Gravitational Wave ◽  
Third Generation ◽  
The Third

scholarly journals MAGIC electromagnetic follow-up of gravitational wave alerts

2016 ◽  
Vol 12 (S324) ◽  
pp. 287-290
Author(s):  
Barbara De Lotto ◽  
Stefano Ansoldi ◽  
Angelo Antonelli ◽  
Alessio Berti ◽  
Alessandro Carosi ◽  
...  
Keyword(s):  
Black Hole ◽  
Data Analysis ◽  
Gravitational Wave ◽  
Laser Interferometer ◽  
Cherenkov Telescopes ◽  
Direct Observations ◽  
Binary Black Hole ◽  
Set Up

AbstractThe year 2015 witnessed the first direct observations of a transient gravitational-wave (GW) signal from binary black hole mergers by the Advanced Laser Interferometer Gravitational-wave Observatory (aLIGO) Collaboration with the Virgo Collaboration. The MAGIC two 17m diameter Cherenkov telescopes system joined since 2014 the vast collaboration of electromagnetic facilities for follow-up of gravitational wave alerts. During the 2015 LIGO-Virgo science run we set up the procedure for GW alerts follow-up and took data following the last GW alert. MAGIC results on the data analysis and prospects for the forthcoming run are presented.

scholarly journals Extraction of binary black hole gravitational wave signals from detector data using deep learning

2021 ◽  
Vol 104 (6) ◽  
Author(s):  
Chayan Chatterjee ◽  
Linqing Wen ◽  
Foivos Diakogiannis ◽  
Kevin Vinsen
Keyword(s):  
Black Hole ◽  
Deep Learning ◽  
Gravitational Wave ◽  
Binary Black Hole

scholarly journals Accuracy of Estimating Highly Eccentric Binary Black Hole Parameters with Gravitational-wave Detections

2018 ◽  
Vol 855 (1) ◽  
pp. 34 ◽  
Author(s):  
László Gondán ◽  
Bence Kocsis ◽  
Péter Raffai ◽  
Zsolt Frei
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Binary Black Hole

scholarly journals Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection

2020 ◽  
Vol 493 (3) ◽  
pp. 4333-4341 ◽  
Author(s):  
M Renzo ◽  
R J Farmer ◽  
S Justham ◽  
S E de Mink ◽  
Y Götberg ◽  
...  
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Time Scale ◽  
Turnover Time ◽  
Black Hole Mass ◽  
The Third ◽  
Mass Gap ◽  
Mixing Length Theory ◽  
State Assumption ◽  
Additional Equation

ABSTRACT Gravitational-wave detections are now probing the black hole (BH) mass distribution, including the predicted pair-instability mass gap. These data require robust quantitative predictions, which are challenging to obtain. The most massive BH progenitors experience episodic mass ejections on time-scales shorter than the convective turnover time-scale. This invalidates the steady-state assumption on which the classic mixing length theory relies. We compare the final BH masses computed with two different versions of the stellar evolutionary code $\tt{MESA}$: (i) using the default implementation of Paxton et al. (2018) and (ii) solving an additional equation accounting for the time-scale for convective deceleration. In the second grid, where stronger convection develops during the pulses and carries part of the energy, we find weaker pulses. This leads to lower amounts of mass being ejected and thus higher final BH masses of up to ∼$5\, \mathrm{M}_\odot$. The differences are much smaller for the progenitors that determine the maximum mass of BHs below the gap. This prediction is robust at $M_{\rm BH, max}\simeq 48\, \mathrm{M}_\odot$, at least within the idealized context of this study. This is an encouraging indication that current models are robust enough for comparison with the present-day gravitational-wave detections. However, the large differences between individual models emphasize the importance of improving the treatment of convection in stellar models, especially in the light of the data anticipated from the third generation of gravitational-wave detectors.

scholarly journals The astrophysical odds of GW151216

2020 ◽  
Vol 498 (2) ◽  
pp. 1905-1910 ◽  
Author(s):  
Gregory Ashton ◽  
Eric Thrane
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Wave ◽  
Bayesian Method ◽  
Massive Stars ◽  
Stellar Mass ◽  
Population Analyses ◽  
Wave Detection ◽  
Binary Black Hole ◽  
Bona Fide

ABSTRACT The gravitational-wave candidate GW151216 is a proposed binary black hole event from the first observing run of the Advanced LIGO detectors. Not identified as a bona fide signal by the LIGO–Virgo collaboration, there is disagreement as to its authenticity, which is quantified by pastro, the probability that the event is astrophysical in origin. Previous estimates of pastro from different groups range from 0.18 to 0.71, making it unclear whether this event should be included in population analyses, which typically require pastro > 0.5. Whether GW151216 is an astrophysical signal or not has implications for the population properties of stellar-mass black holes and hence the evolution of massive stars. Using the astrophysical odds, a Bayesian method that uses the signal coherence between detectors and a parametrized model of non-astrophysical detector noise, we find that pastro = 0.03, suggesting that GW151216 is unlikely to be a genuine signal. We also analyse GW150914 (the first gravitational-wave detection) and GW151012 (initially considered to be an ambiguous detection) and find pastro values of 1 and 0.997, respectively. We argue that the astrophysical odds presented here improve upon traditional methods for distinguishing signals from noise.

scholarly journals Impact of subdominant modes on the interpretation of gravitational-wave signals from heavy binary black hole systems

2020 ◽  
Vol 101 (12) ◽  
Author(s):  
Feroz H. Shaik ◽  
Jacob Lange ◽  
Scott E. Field ◽  
Richard O’Shaughnessy ◽  
Vijay Varma ◽  
...  
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Binary Black Hole
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