On the modeling of Intermediate- and Extreme-Mass-Ratio Inspirals
On the modeling of Intermediate- and Extreme-Mass-Ratio Inspirals
On the modeling of Intermediate- and Extreme-Mass-Ratio Inspirals
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Introduction to IMRIs <strong>and</strong> EMRIs<br />
After many years <strong>of</strong> observations <strong>the</strong> existence <strong>of</strong> stellarmass<br />
black holes (~4-50 solar masses) <strong>and</strong> (super)massive<br />
black holes (~100000 to billion solar masses ) has been<br />
established with a high degree <strong>of</strong> confidence.<br />
There is a gap in <strong>the</strong> BH mass range, between ~100 to several<br />
10000 solar masses, where <strong>the</strong>re is not yet a strong<br />
observational evidence. The BHs in this mass range cannot<br />
have nei<strong>the</strong>r stellar origin nor primordial (early universe).<br />
These are <strong>the</strong> <strong>Intermediate</strong>-<strong>Mass</strong> BHs (IMBHs).<br />
Therefore, <strong>the</strong>re is no observational evidence that supports <strong>the</strong><br />
existence <strong>of</strong> IMRIs, whereas <strong>the</strong> possible existence <strong>of</strong> EMRIs is<br />
sound <strong>and</strong> <strong>the</strong> uncertainties are related to formation<br />
mechanisms <strong>and</strong> <strong>the</strong>ir associated event rates.<br />
2nd Iberian Gravitational Wave Meeting [February 16th, 2012] 5
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