Constrains on the electric charges of the binary black holes with GWTC-1 events

AbstractTesting black hole’s charged property is a fascinating topic in modified gravity and black hole astrophysics. In the first Gravitational-Wave Transient Catalog (GWTC-1), ten binary black hole merger events have been formally reported, and these gravitational wave signals have significantly enhanced our understanding of the black hole. In this paper, we try to constrain the amount of electric charge with the parameterized post-Einsteinian framework by treating the electric charge as a small perturbation in a Bayesian way. We find that the current limits in our work are consistent with the result of Fisher information matrix method in previous works. We also develop a waveform model considering a leading order charge effect for binary black hole inspiral.

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The Eccentric and Accelerating Stellar Binary Black Hole Mergers in Galactic Nuclei: Observing in Ground and Space Gravitational-wave Observatories

The Astrophysical Journal ◽

10.3847/1538-4357/ac2c07 ◽

2021 ◽

Vol 923 (2) ◽

pp. 139

Author(s):

Fupeng Zhang ◽

Xian Chen ◽

Lijing Shao ◽

Kohei Inayoshi

Keyword(s):

Black Hole ◽

Gravitational Wave ◽

Signal To Noise Ratio ◽

Galactic Nuclei ◽

Signal To Noise ◽

High Eccentricity ◽

Massive Black Hole ◽

Binary Black Holes ◽

Binary Black Hole ◽

Space Observatories

Abstract We study the stellar binary black holes (BBHs) inspiraling/merging in galactic nuclei based on our numerical method GNC. We find that 3%–40% of all newborn BBHs will finally merge due to various dynamical effects. In a five-year mission, up to 104, 105, and ∼100 of BBHs inspiraling/merging in galactic nuclei can be detected with signal-to-noise ration >8 in Advanced LIGO (aLIGO), Einstein/DECIGO, and TianQin/LISA/TaiJi, respectively. Roughly tens are detectable in both LISA/TaiJi/TianQin and aLIGO. These BBHs have two unique characteristics. (1) Significant eccentricities: 1%–3%, 2%–7%, or 30%–90% of them have e i > 0.1 when they enter into aLIGO, Einstein, or space observatories, respectively. Such high eccentricities provide a possible explanation for that of GW190521. Most highly eccentric BBHs are not detectable in LISA/Tianqin/TaiJi before entering into aLIGO/Einstein, as their strain becomes significant only at f GW ≳ 0.1 Hz. DECIGO becomes an ideal observatory to detect those events, as it can fully cover the rising phase. (2) Up to 2% of BBHs can inspiral/merge at distances ≲103 r SW from the massive black hole, with significant accelerations, such that the Doppler phase drift of ∼10–105 of them can be detected with signal-to-noise ratio >8 in space observatories. The energy density of the gravitational-wave backgrounds (GWBs) contributed by these BBHs deviates from the power-law slope of 2/3 at f GW ≲ 1 mHz. The high eccentricity, significant accelerations, and the different profile of the GWB of these sources make them distinguishable, and thus interesting for future gravitational-wave detections and tests of relativities.

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Searching for eccentricity: signatures of dynamical formation in the first gravitational-wave transient catalogue of LIGO and Virgo

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2996 ◽

2019 ◽

Vol 490 (4) ◽

pp. 5210-5216 ◽

Cited By ~ 19

Author(s):

Isobel M Romero-Shaw ◽

Paul D Lasky ◽

Eric Thrane

Keyword(s):

Black Holes ◽

Black Hole ◽

Bayesian Inference ◽

Gravitational Wave ◽

Globular Clusters ◽

Reference Frequency ◽

Binary Black Holes ◽

Binary Black Hole ◽

Upper Limits ◽

Formation History

ABSTRACT Binary black holes are thought to form primarily via two channels: isolated evolution and dynamical formation. The component masses, spins, and eccentricity of a binary black hole system provide clues to its formation history. We focus on eccentricity, which can be a signature of dynamical formation. Employing the spin-aligned eccentric waveform model seobnre, we perform Bayesian inference to measure the eccentricity of binary black hole merger events in the first gravitational-wave transient catalogue of LIGO and Virgo. We find that all of these events are consistent with zero eccentricity. We set upper limits on eccentricity ranging from 0.02 to 0.05 with 90 per cent confidence at a reference frequency of $10\, {\rm Hz}$. These upper limits do not significantly constrain the fraction of LIGO–Virgo events formed dynamically in globular clusters, because only $\sim 5{{\ \rm per\ cent}}$ are expected to merge with measurable eccentricity. However, with the gravitational-wave transient catalogue set to expand dramatically over the coming months, it may soon be possible to significantly constrain the fraction of mergers taking place in globular clusters using eccentricity measurements.

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Implications of Eccentric Observations on Binary Black Hole Formation Channels

The Astrophysical Journal ◽

10.3847/2041-8213/ac32dc ◽

2021 ◽

Vol 921 (2) ◽

pp. L43

Author(s):

Michael Zevin ◽

Isobel M. Romero-Shaw ◽

Kyle Kremer ◽

Eric Thrane ◽

Paul D. Lasky

Keyword(s):

Black Hole ◽

Gravitational Wave ◽

State Of The Art ◽

Star Clusters ◽

Selection Effects ◽

Orbital Eccentricity ◽

Hole Formation ◽

Local Universe ◽

Binary Black Holes ◽

Binary Black Hole

Abstract Orbital eccentricity is one of the most robust discriminators for distinguishing between dynamical and isolated formation scenarios of binary black hole mergers using gravitational-wave observatories such as LIGO and Virgo. Using state-of-the-art cluster models, we show how selection effects impact the detectable distribution of eccentric mergers from clusters. We show that the observation (or lack thereof) of eccentric binary black hole mergers can significantly constrain the fraction of detectable systems that originate from dynamical environments, such as dense star clusters. After roughly 150 observations, observing no eccentric binary signals would indicate that clusters cannot make up the majority of the merging binary black hole population in the local universe (95% credibility). However, if dense star clusters dominate the rate of eccentric mergers and a single system is confirmed to be measurably eccentric in the first and second gravitational-wave transient catalogs, clusters must account for at least 14% of detectable binary black hole mergers. The constraints on the fraction of detectable systems from dense star clusters become significantly tighter as the number of eccentric observations grows and will be constrained to within 0.5 dex once 10 eccentric binary black holes are observed.

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

Physical Review D ◽

10.1103/physrevd.104.023014 ◽

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

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MAGIC electromagnetic follow-up of gravitational wave alerts

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317001430 ◽

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.

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

Physical Review D ◽

10.1103/physrevd.104.064046 ◽

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

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Searching for Near-Horizon Quantum Structures in the Binary Black-Hole Stochastic Gravitational-Wave Background

Physical Review Letters ◽

10.1103/physrevlett.121.051105 ◽

2018 ◽

Vol 121 (5) ◽

Cited By ~ 8

Author(s):

Song Ming Du ◽

Yanbei Chen

Keyword(s):

Black Hole ◽

Gravitational Wave ◽

Quantum Structures ◽

Binary Black Hole ◽

Gravitational Wave Background

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

The Astrophysical Journal ◽

10.3847/1538-4357/aaad0e ◽

2018 ◽

Vol 855 (1) ◽

pp. 34 ◽

Cited By ~ 27

Author(s):

László Gondán ◽

Bence Kocsis ◽

Péter Raffai ◽

Zsolt Frei

Keyword(s):

Black Hole ◽

Gravitational Wave ◽

Binary Black Hole

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The astrophysical odds of GW151216

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2332 ◽

2020 ◽

Vol 498 (2) ◽

pp. 1905-1910 ◽

Cited By ~ 1

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.

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