GW190412: The First Observation of an Unequal-Mass Black Hole Merger
Dated 20 April 2020. Read this summary in PDF format (in English) and in other languages: Bengali | Blackfoot | Chinese (traditional) | Dutch | French | German | Italian | Japanese | Korean | Marathi | Nepali | Polish | Spanish .
What did we find?
On April 12, 2019, the LIGO Scientific Collaboration and Virgo Collaboration observed gravitational waves produced by the inspiral and merger of two black holes. This event, dubbed GW190412, was observed with all three detectors operating in the network: both LIGO detectors (one in Hanford, Washington and one in Livingston, Louisiana) as well as the Virgo detector (located in Cascina, Italy). GW190412 was detected near the beginning of Advanced LIGO and Virgo's third observing run, known as O3, which started on April 1st 2019 and was suspended on March 27th 2020.
While the masses of the two black holes are consistent with those of previously observed black holes, GW190412 is unique in that it is the first black hole merger where the masses of the two black holes are definitively unequal — one black hole in the system is more than 3 times heavier than the other. This asymmetry in masses modifies the gravitational-wave signal in such a way that we can better measure other parameters, such as the distance and inclination of the system, the spin of the heavier black hole, and the amount that the system is precessing. In addition, the unequal masses of GW190412 enable us to verify a fundamental prediction of Albert Einstein's General relativity: that gravitational waves “ring” at more than one fundamental frequency, so-called higher multipoles.
How do we know GW190412 is a real gravitational-wave signal?
GW190412 is a loud event that was seen in all three detectors. Since the three detectors are all thousands of kilometers apart from one another, seeing this signal in all the detectors nearly simultaneously is a good sign that it is of astrophysical origin rather than due to noise.
The time-frequency representation of GW190412, known as a spectrogram, is shown in Figure 1. Though GW190412 is strong enough to be seen “by eye” in the data from the Hanford and Livingston detectors, we use a number of algorithms to systematically scan the data for gravitational-wave signals and determine their significance. Most techniques rely on matched filtering, which compares the observed data to simulated signals predicted from general relativity. We quantify the chance that a signal results from noise in the detectors as the false alarm rate. Using data from April 8 to April 18, we found a false alarm rate of one chance event per 30,000 years! This false alarm rate will become even more significant as more data from O3 are analyzed. We also performed checks for other types of instrumental and environmental sources of noise, and found nothing that could have significant impact on the detection or analysis of GW190412.
Properties of GW190412
The individual masses of the two black holes in GW190412 were consistent with what has been observed in prior observing runs — one black hole was about 30 times the mass of the Sun, and the other about 8 times the mass of the Sun. However, the mass ratio of GW190412, defined as the ratio of the lighter black hole mass and the heavier black hole mass, is unlike any of the other black hole mergers we have detected before. Whereas all 10 black hole mergers from the first two observing runs were consistent with both black holes in each system being equal in mass, the larger black hole in GW190412 was more than three times the mass of the smaller black hole.
The unequal masses of GW190412 lead to an asymmetry in the gravitational-wave emission that helps us to better infer particular parameters of the system. We find that the effective spin was positive, which tells us that at least one of the black holes was spinning in an orientation close to the orbit of the two black holes around each other. Notably, due to the unequal masses of GW190412 we can for the first time put strong constraints on the spin of the larger black hole, which we find to be spinning at about 40% of the maximal spin allowed by general relativity. The effective spin and mass ratio inferred for GW190412 are shown in Figure 2. We also see marginal signs that the system is precessing, though any effects of precession are not strong enough to be claimed definitively. In addition, the unequal masses also help to break an ambiguity between the distance and the inclination of the system, allowing for a better measurement of both parameters. GW190412 occurred almost 2.5 billion lightyears away from Earth!
Hearing the Hum of Higher Harmonics
The unique properties of GW190412 also allow for the observation of a fundamental property of gravitational waves. Starting with the pioneering work of Einstein, and later refined by Newman, Penrose, Thorne and many others, the gravitational radiation from compact binaries was shown to be predominantly quadrupolar. This quadrupolar radiation can be thought of like the main sound that is heard when plucking a string on a guitar. However, just like musical instruments, gravitational radiation is predicted to also ring at higher overtones. These higher harmonics or higher multipoles are exceptionally difficult to parse out of a signal when the black holes are near equal in mass. The asymmetric masses of GW190412 allows for these subtle signals to be better “heard” in the gravitational-wave emission. We find that the data support the hypothesis, by a factor of greater than 1000:1, that there are higher harmonics in the signal. In the future, the relative intensity of higher multipoles may help to better disentangle the properties of coalescing black holes.
A suite of tests were also performed to determine if GW190412 is consistent with general relativity. We found no inconsistencies with general relativity, adding another point of support for Einstein's theory of gravity.
Forming an Unequal-Mass Binary Black Hole
Each observing run of the Advanced LIGO and Virgo network has brought new and exciting insights into the zoo of compact binaries. As the first binary black hole system with definitively unequal masses, GW190412 provides an important datapoint in our understanding of binary black hole population properties. The observation of this single event tells us that black hole systems with unequal masses are relatively common, and that we should expect to observe many more such systems in the future.
Based on the detailed physics of stellar evolution, astronomers have built models of how binary black holes form in the universe, and of their expected masses and other properties. Though most models predict that binaries with near-equal masses should be more common, many also predict an appreciable number of systems like GW190412 with clearly unequal masses. Such systems are typically predicted to form at least ten times less often than their equal-mass counterparts. However, the observation of GW190412 with its apparently extreme mass-ratio is not unexpected, given that we have now detected well over 10 events. As we continue to increase our sensitivity to the gravitational-wave universe and build a quickly growing catalog of compact binary mergers, we expect to observe many more systems that better enlighten our view of stellar evolution, compact binary formation, and fundamental physics.
FIND OUT MORE:
- Visit our websites: www.ligo.org, www.virgo-gw.eu
- You can read a free preprint of the full scientific article here or on arXiv.org.
- There is also an infographic and a fact sheet for GW190412.
- Black Hole: An object so compact that not even light can escape its gravitational pull.
- Compact Binary: A system made of two compact stellar remnants, e.g. neutron stars or black holes.
- Effective Spin: The best-measured parameter encoding spin information in a gravitational-wave signal. Formally, it is a mass-weighted projection of the individual black hole spins in the direction of the orbit of the two black holes.
- General Relativity: The theory of gravity proposed by Albert Einstein in 1915. In this theory, space is like malleable fabric that bends in the presence of matter and energy, and objects follow trajectories through this curved space.
- Higher Multipoles: Emission from gravitational waves can be described as an expansion of “spherical harmonics”. Higher multipoles are terms in this expansion beyond the dominant, quadrupolar term.
- Inclination: The tilt of the orbiting black holes with respect to Earth.
- Matched Filtering: A technnique to detect signals buried within noisy data. Templates of gravitational waveforms calculated from general relativity are scanned across the data, and ring off when matching patterns are found in the data.
- Precession: Due to conservation of angular momentum, when black holes are spinning in a direction different than the orbit of the binary, the plane of the orbit will rotate (“precess”) around the direction of the total angular momentum.
- Quadrupole: The strongest of the multipoles for gravitational-wave emission from a compact binary. Thinking of these waves as the “sounds of spacetime”, the quadrupole emission is the fundamental tone. The name refers to the emission pattern in different directions: for comparison, a simple radio antenna sends out a dipole as its strongest emission.
- Spectrogram: A time-frequency-energy representation of time-series data. The strength of individual frequencies are shown as colors.
- Waveform: A theoretical gravitational-wave signal produced using approximations of Einstein's general relativity.
Figures from the Publication
For more information on these figures, see the full publication here.
Figure 1: The spectrogram of GW190412 in the three gravitational-wave detectors. The horizontal axis represents time, and the vertical axis shows the frequency of the signal. Color represents the amount of energy in a certain frequency at a certain time. The familiar “chirp” can be seen from this signal as an increase in frequency and energy over time, resulting from the increased power of gravitational-wave emission as the two black holes orbit closer and closer (the “inspiral”) and subsequently merge.
Figure 2: The inferred mass ratio (q) and effective spin (χeff) of GW190412. The orange and blue contours show the distributions on the parameters recovered using two different waveform models, which make slightly different approximations for modeling the true general-relativistic signal.