scholarly journals A hierarchical search for gravitational waves from supermassive black hole binary mergers

2008 ◽  
Vol 25 (18) ◽  
pp. 184027 ◽  
Author(s):  
I W Harry ◽  
S Fairhurst ◽  
B S Sathyaprakash
Keyword(s):  
Black Hole ◽  
Gravitational Waves ◽  
Supermassive Black Hole ◽  
Hierarchical Search ◽  
Binary Mergers ◽  
Black Hole Binary

scholarly journals THE SPIN-FLIP PHENOMENON IN SUPERMASSIVE BLACK HOLE BINARY MERGERS

2009 ◽  
Vol 697 (2) ◽  
pp. 1621-1633 ◽  
Author(s):  
László Árpád Gergely ◽  
Peter L. Biermann
Keyword(s):  
Black Hole ◽  
Supermassive Black Hole ◽  
Spin Flip ◽  
Binary Mergers ◽  
Black Hole Binary

scholarly journals Prospects of probing dark energy with eLISA: Standard versus null diagnostics

2020 ◽  
Vol 500 (3) ◽  
pp. 2896-2907
Author(s):  
Pratyusava Baral ◽  
Soumendra Kishore Roy ◽  
Supratik Pal
Keyword(s):  
Black Hole ◽  
Dark Energy ◽  
Cosmological Parameters ◽  
Supermassive Black Hole ◽  
Wide Range ◽  
Binary Mergers ◽  
Model Independent ◽  
Black Hole Binary ◽  
Intermediate Redshift ◽  
Shed Light

ABSTRACT Gravitational waves from supermassive black hole binary mergers along with an electromagnetic counterpart have the potential to shed ‘light’ on the nature of dark energy in the intermediate redshift regime. Accurate measurement of dark energy parameters at intermediate redshift is extremely essential to improve our understanding of dark energy, and to possibly resolve a couple of tensions involving cosmological parameters. We present a Fisher matrix forecast analysis in the context of eLISA to predict the errors for three different cases: the non-interacting dark energy with constant and evolving equation of state (EoS), and the interacting dark sectors with a generalized parametrization. In all three cases, we perform the analysis for two separate formalisms, namely, the standard EoS formalism and the Om parametrization which is a model-independent null diagnostic for a wide range of fiducial values in both phantom and non-phantom regions, to make a comparative analysis between the prospects of these two diagnostics in eLISA. Our analysis reveals that it is wiser and more effective to probe the null diagnostic instead of the standard EoS parameters for any possible signature of dark energy at intermediate redshift measurements like eLISA.

scholarly journals Constraining astrophysical observables of galaxy and supermassive black hole binary mergers using pulsar timing arrays

2019 ◽  
Vol 488 (1) ◽  
pp. 401-418 ◽  
Author(s):  
Siyuan Chen ◽  
Alberto Sesana ◽  
Christopher J Conselice
Keyword(s):  
Black Hole ◽  
Mass Function ◽  
Host Galaxy ◽  
Supermassive Black Hole ◽  
Pulsar Timing ◽  
Upper Limits ◽  
Binary Mergers ◽  
Black Hole Binary ◽  
Merger Rate ◽  
The Universe

ABSTRACT We present an analytic model to describe the supermassive black hole binary (SMBHB) merger rate in the Universe with astrophysical observables: galaxy stellar mass function, pair fraction, merger time-scale, and black hole–host galaxy relations. We construct observational priors and compute the allowed range of the characteristic spectrum hc of the gravitational wave background (GWB) to be 10−16 < hc < 10−15 at a frequency of f = 1 yr−1. We exploit our parametrization to tackle the problem of astrophysical inference from pulsar timing array (PTA) observations. We simulate a series of upper limits and detections and use a nested sampling algorithm to explore the parameter space. Corroborating previous results, we find that the current PTA non-detection does not place significant constraints on any observables; however, either future upper limits or detections will significantly enhance our knowledge of the SMBHB population. If a GWB is not detected at a level of hc(f = 1 yr−1) = 10−17, our current understanding of galaxy and SMBHB mergers is disfavoured at a 5σ level, indicating a combination of severe binary stalling, overestimating of the SMBH–host galaxy relations, and extreme dynamical properties of merging SMBHBs. Conversely, future detections of a Square Kilometre Array (SKA)-type instrument will allow to constrain the normalization of the SMBHB merger rate in the Universe, the time between galaxy pairing and SMBHB merging, the normalization of the SMBH–host galaxy relations and the dynamical binary properties, including their eccentricity and density of stellar environment.

scholarly journals A reduced orbital period for the supermassive black hole binary candidate in the quasar PG 1302-102?

2015 ◽  
Vol 452 (3) ◽  
pp. 2540-2545 ◽  
Author(s):  
D. J. D'Orazio ◽  
Z. Haiman ◽  
P. Duffell ◽  
B. D. Farris ◽  
A. I. MacFadyen
Keyword(s):  
Black Hole ◽  
Orbital Period ◽  
Supermassive Black Hole ◽  
Black Hole Binary

scholarly journals Constraints on ultra-low-frequency gravitational waves with statistics of pulsar spin-down rates

2019 ◽  
Vol 489 (3) ◽  
pp. 3547-3552
Author(s):  
Hiroki Kumamoto ◽  
Yuya Imasato ◽  
Naoyuki Yonemaru ◽  
Sachiko Kuroyanagi ◽  
Keitaro Takahashi
Keyword(s):  
Black Hole ◽  
Gravitational Waves ◽  
Time Derivative ◽  
Low Frequency ◽  
Upper Bounds ◽  
Galactic Centre ◽  
Frequency Range ◽  
Rate Distribution ◽  
Black Hole Binaries ◽  
Supermassive Black Hole

Abstract We probe ultra-low-frequency gravitational waves (GWs) with statistics of spin-down rates of millisecond pulsars (thereafter MSPs) by a method proposed in our previous work. The considered frequency range is 10−12 Hz ≲ fGW ≲ 10−10  Hz . The effect of such low-frequency GWs appears as a bias to spin-down rates that has a quadrupole pattern in the sky. We use the skewness of the spin-down rate distribution and the number of MSPs with negative spin-down rates to search for the bias induced by GWs. Applying this method to 149 MSPs selected from the ATNF pulsar catalogue, we derive upper bounds on the time derivative of the GW amplitudes of $\dot{h} \lt 6.2 \times 10^{-18}~{\rm s}^{-1}$ and $\dot{h} \lt 8.1 \times 10^{-18}~{\rm s}^{-1}$ in the directions of the Galactic Centre and M87, respectively. Approximating the GW amplitude as $\dot{h} \sim 2 \pi f_{\rm GW} h$, the bounds translate into h < 3 × 10−8 and h < 4 × 10−8, respectively, for fGW = 1/(1000 yr). Finally, we give the implications to possible supermassive black hole binaries at these sites.

scholarly journals Stellar black hole binary mergers in open clusters

2018 ◽  
Vol 483 (1) ◽  
pp. 1233-1246 ◽  
Author(s):  
S Rastello ◽  
P Amaro-Seoane ◽  
M Arca-Sedda ◽  
R Capuzzo-Dolcetta ◽  
G Fragione ◽  
...  
Keyword(s):  
Black Hole ◽  
Open Clusters ◽  
Binary Mergers ◽  
Black Hole Binary

scholarly journals ALIGNMENT OF SUPERMASSIVE BLACK HOLE BINARY ORBITS AND SPINS

2013 ◽  
Vol 774 (1) ◽  
pp. 43 ◽  
Author(s):  
M. Coleman Miller ◽  
Julian H. Krolik
Keyword(s):  
Black Hole ◽  
Supermassive Black Hole ◽  
Black Hole Binary
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