Tests of general relativity using multiband observations of intermediate mass binary black hole mergers

Sayantani Datta, Anuradha Gupta, Shilpa Kastha, K. G. Arun, B. S. Sathyaprakash

Research output: Contribution to journalArticlepeer-review

17 Scopus citations


Observation of gravitational waves (GWs) in two different frequency bands is referred to as multiband GW astronomy. With the planned Laser Interferometric Space Antenna (LISA) operating in the 10-4-0.1 Hz range, and third-generation (3G) ground-based detectors such as the Cosmic Explorer (CE) and Einstein Telescope (ET) operating in the 1-104 Hz range, multiband GW astronomy could be a reality in the coming decades. In this paper, we present the potential of multiband observations of intermediate-mass binary black holes (IMBBHs) of component masses ∼102-103 M to test general relativity (GR). We show that mutiband observations of IMBBHs would permit multiparameter tests of GR - tests where more than one post-Newtonian (PN) coefficient is simultaneously measured - yielding more rigorous constraints on possible modifications to GR. We also find that the improvement due to multibanding can often be much larger than the best of the bounds from either of the two observatories. The origin of this result, as we shall demonstrate, can be traced to the lifting of degeneracies among the various parameters when the information from LISA and 3G is taken together. A binary of redshifted total mass of 200 M gives the best bounds. Such a system at 1 Gpc and mass ratio m1/m2=2 would bound the deviations on all the PN coefficients to below 10% when they are measured individually, and additionally place simultaneous bounds on the first seven PN coefficients to below 50%.

Original languageEnglish (US)
Article number024036
JournalPhysical Review D
Issue number2
StatePublished - Jan 20 2021

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy (miscellaneous)


Dive into the research topics of 'Tests of general relativity using multiband observations of intermediate mass binary black hole mergers'. Together they form a unique fingerprint.

Cite this