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The Leonard E Parker Center for Gravitation, Cosmology and Astrophysics is supported by NASA, the National Science Foundation, UW-Milwaukee College of Letters and Science, and UW-Milwaukee Graduate School. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of these organizations.
The LIGO and Virgo ground-based interferometric gravitational wave detectors are capable of detecting broad-band gravitational wave (GW) signals with frequencies from tens to thousands of cycles per second. Many violent astrophysical events, such as exploding supernovae or colliding neutron stars and black holes, produce a unique GW signature with frequencies in this range. Interestingly, black holes with masses that are tens to thousands of times the mass of our Sun vibrate when disturbed by an infalling object or a collision, sending out GWs within this frequency range that propagate through spacetime. The GW signature of a perturbed black hole is known as a damped sinusoid GW that we call a "ringdown".
This is due to the fact that the oscillation properties of a perturbed black hole are surprisingly similar to those of a ringing bell or tuning fork. Just as a bell has a unique tone and timbre determined by its size and composition, each black hole rings with a unique fundamental pitch and duration that depends on its mass and rate of spin. These properties were described in 1973 by Saul Teukolsky who studied what would happen to a spinning black hole if it was perturbed from its stable configuration. He found that the black hole would oscillate with a collection of quasinormal modes, or characteristic frequencies, before eventually returning to a stable configuration.
The masses of perturbed black holes that are detectable by LIGO and Virgo fall within the regime of intermediate mass black holes (IMBH), an elusive class of objects that have masses up to 100,000 times the mass of our Sun. We have strong evidence for stellar mass black holes and supermassive black holes but no conclusive evidence for the existence of IMBHs with masses that lie between the ranges of the other two types of black hole. Some models and observations suggest that IMBHs could be the source of ultra-luminous X-rays or that they could exist in the centers of globular clusters where two IMBHs could possibly form a binary system. Two IMBHs that inspiral and merge into one perturbed black hole could be a strong source of GWs detectable by LIGO and Virgo, particularly from the perturbed black hole ringdown. Detection of GWs from these objects may be the only way that we can find them. Additionally, the GWs would allow us to infer information about how the perturbed black hole was created and give us an opportunity to test the accuracy of General Relativity, Einstein's theory of gravity.
Since we can model the signature waveform, we can utilize a signal-processing technique known as matched filtering to search noisy detector data for a weak hidden signal. The hidden signal should reveal itself by "standing out" from the background, which we measure as a large signal-to-noise ratio, when the most similar model waveform matches the signal. In practice, detector data can be very noisy and we must utilize others tools such as multi-detector coincidence and signal consistency to determine how significant a potential GW signal really is.
We performed a matched filter search for ringdown GWs over LIGO-Virgo data from 2005-2010. Our search targeted damped sinusoid signals with masses in the range 10 to 600 solar masses and spins in the range 0 to 0.99. The strongest source of gravitational waves in this regime would be from merging IMBHs. The figures shown below report our sensitivity to this particular type of source. Additionally, we could also detect ringdown GWs from other types of perturbed black holes such as the stellar mass black holes resulting from the collapse of very massive stars. However, our sensitivity to these is significantly less than that reported in the figures.
After searching the data for GWs and carefully classifying the candidates using a multivariate statistical classifier, we found no signals from perturbed IMBHs. This non-detection was used to place an upper limit on the rate of IMBH mergers in the universe for different possible mass ranges. Based on our best upper limit, we found that the rate of such mergers with a total mass between 100 and 150 solar masses is very likely less than one per year within a distance of 490 million light years. This result is consistent with the rate upper limit reported for an 'unmodeled' search for IMBH mergers . Our results tell us that these astrophysical events are exceedingly rare!
Additionally, we explored the improvement in sensitivity over the first search for ringdown GWs from IMBH mergers performed on LIGO data collected between February and March of 2005 . Due to a huge increase in analysis time, an improvement in detector performance, and more sophisticated search techniques, we found a rate upper limit that is nearly three orders of magnitude more stringent than our previous results.
With the improved low frequency performance of the Advanced LIGO and Virgo detectors, which are expected to begin operation in 2015, we will have sensitivity to IMBH mergers with masses up to ~1000 to 2000 solar masses. At peak sensitivity, the horizon distance for the perturbed black holes shown in Fig. (1) and (2) will approach cosmological distances. For the first time, we will have the chance to detect ringdown gravitational waves from IMBH mergers and begin to understand the extreme nature of these mysterious objects.
Figure 1 and 2: We analyzed data from LIGO's fifth and sixth science runs (S5 and S6) and Virgo's science runs 2 and 3 (VSR2/3). In order to gauge the sensitivity of our search to GWs from perturbed IMBHs, we can plot the ringdown horizon distance as a function of black hole mass for the LIGO detectors (H1, H2, and L1) during S5 and the LIGO and Virgo detectors (H1, L1, and V1) during S6-VSR2/3 as shown above. The horizon distance shown here is the maximum distance to which we could see a perturbed black hole with a signal-to-noise ratio of 8. We assume that the source is optimally located and oriented to provide the strongest signal to our detectors, that the black hole is radiating ~1% of its mass in GWs, and that it is spinning very quickly. In reality, it is unlikely for a source to be perfectly oriented, to emit a significant portion of its mass as GWs, and to have very high spin; thus, we expect the actual sensitivity of the search to be less. For example, during S5, we could detect a ~200 solar mass black hole at a distance of ~530 Megaparsecs (1.7 billion light years) with a signal-to-noise ratio of 8. This distance encompasses all of the Virgo Supercluster and extends out to include other local galaxy superclusters. Credit: S. Caudill