English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Gravitational waves provide direct information about the nature of spacetimeand the existence of black holes. The remnant of a binary black hole mergeremits gravitational waves in the form of quasinormal modes, whose spectrum isknown as the "fingerprints" of a black hole, as it depends only on theproperties of the remnant. The quasinormal modes can be used to test howclosely an astrophysical black hole matches the Kerr geometry. Each mode isparameterized by three indices: the harmonic numbers $(\ell, m)$ and theovertone index $n$, that labels the fundamental mode ($n = 0$) and theovertones ($n = 1,2,3,\ldots$). Black hole spectroscopy is the proposal to usethe detection of multiple quasinormal modes to test the no-hair theorem. Inthis work, we investigate the prospects for performing black hole spectroscopy.The $(2,2,0)$ is the dominant mode, and we analyze the contribution of the mostrelevant subdominant modes in numerical relativity simulations. We show thatthe overtone mode $(2,2,1)$ has an amplitude higher or comparable to theamplitude of the most relevant higher harmonic modes. For current and futuregravitational wave detectors, we compute the black hole spectroscopy horizon,which is the maximum distance of an event up to which two or more quasinormalmodes can be detected. For low mass ratio binaries, the secondary and tertiarymodes are the $(2,2,1)$ and $(3,3,0)$, respectively, and, for the large massratio case, the $(3,3,0)$ and $(4,4,0)$ are the most relevant subdominant modesfor detection. Our work indicates promising prospects for the detection ofsubdominant modes with future gravitational wave detectors. The event rate forLIGO is much smaller, but not prohibitively so.

Black hole spectroscopy: prospects for testing the nature of black holes with gravitational wave observations