Query : 2012A&A...542A.102M

2012A&A...542A.102M - Astronomy and Astrophysics, volume 542A, 102-102 (2012/6-1)

A cosmological view of extreme mass-ratio inspirals in nuclear star clusters.


Abstract (from CDS):

There is increasing evidence that many galaxies host both a nuclear star cluster (NC) and a super-massive black hole (SMBH). Their coexistence is particularly prevalent in spheroids with stellar mass 108-1010M. We study the possibility that a stellar-mass black hole (BH) hosted by a NC inspirals and merges with the central SMBH. Due to the high stellar density in NCs, extreme mass-ratio inspirals (EMRIs) of BHs onto SMBHs in NCs may be important sources of gravitational waves (GWs). We consider sensitivity curves for three different space-based GW laser interferometric mission concepts: the Laser Interferometer Space Antenna (LISA), the New Gravitational wave Observatory (NGO) and the DECi-hertz Interferometer Gravitational wave Observatory (DECIGO). We predict that, under the most optimistic assumptions, LISA and DECIGO will detect up to thousands of EMRIs in NCs per year, while NGO will observe up to tens of EMRIs per year. We explore how a number of factors may affect the predicted rates. In particular, if we assume that the mass of the SMBH scales with the square of the host spheroid mass in galaxies with NCs, rather than a linear scaling, then the event rates are more than a factor of 10 lower for both LISA and NGO, while they are almost unaffected in the case of DECIGO.

Abstract Copyright:

Journal keyword(s): gravitational waves - black hole physics - galaxies: nuclei - galaxies: star clusters: general - cosmology: theory

Simbad objects: 3

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Number of rows : 3
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
1 NGC 3384 GiG 10 48 16.8855574392 +12 37 45.371165844   10.0       ~ 590 1
2 NGC 4395 Sy2 12 25 48.8633109888 +33 32 48.700168152 10.84 10.54 10.11 9.98   ~ 1157 1
3 NGC 7457 AG? 23 00 59.9263288440 +30 08 41.764398792   11.04 11.87     ~ 436 0

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