Media contact

Dr. Elke Müller
Dr. Elke Müller
Press Officer AEI Potsdam
Phone:+49 331 567-7303Fax:+49 331 567-7298
Dr.  Benjamin  Knispel
Dr. Benjamin Knispel
Press Officer AEI Hannover
Phone:+49 511 762-19104Fax:+49 511 762-17182

Science contacts

Prof. Dr. Alessandra Buonanno
Prof. Dr. Alessandra Buonanno
Director
Phone:+49 331 567-7220Fax:+49 331 567-7298

LSC Principal Investigator

Homepage of Alessandra Buonanno

Prof. Dr. Karsten  Danzmann
Prof. Dr. Karsten Danzmann
Director
Phone:+49 511 762-2356Fax:+49 511 762-5861

LSC Principal Investigator

Karsten Danzmann's homepage

Dr. Frank Ohme
Dr. Frank Ohme
Research Group Leader
Phone:+49 511 762-17171Fax:+49 511 762-2784

LSC Principal Investigator

Frank Ohme's homepage

Publication

1.
The LIGO Scientific Collaboration and the Virgo Collaboration
GW190412: Observation of a Binary-Black-Hole Coalescence with Asymmetric Masses

Further information

Images and movies

Numerical simulation of a black-hole binary merger with asymmetric masses and orbital precession.

GW190412: Binary Black Hole Merger

Numerical simulation of a black-hole binary merger with asymmetric masses and orbital precession. [more]

A signal like none before

LIGO and Virgo detectors catch first gravitational wave from binary black hole merger with unequal masses

April 20, 2020

The expectations of the gravitational-wave research community have been fulfilled: gravitational-wave discoveries are now part of their daily work as they have identified in the past observing run, O3, new gravitational-wave candidates about once a week. But now, the researchers have published a remarkable signal unlike any of those seen before: GW190412 is the first observation of a binary black hole merger where the two black holes have distinctly different masses of about 8 and 30 times that of our Sun. This not only has allowed more precise measurements of the system’s astrophysical properties, but it has also enabled the LIGO/Virgo scientists to verify a so far untested prediction of Einstein’s theory of general relativity.
Binary black hole merger where the two black holes have distinctly different masses of about 8 and 30 times that of our Sun. Zoom Image
Binary black hole merger where the two black holes have distinctly different masses of about 8 and 30 times that of our Sun. [less]

“For the very first time we have ‘heard’ in GW190412 the unmistakable gravitational-wave hum of a higher harmonic, similar to overtones of musical instruments,” explains Frank Ohme, leader of the Independent Max Planck Research Group “Binary Merger Observations and Numerical Relativity” at the Max Planck Institute for Gravitational Physics (Albert Einstein Institute; AEI) in Hannover. “In systems with unequal masses like GW190412 – our first observation of this type – these overtones in the gravitational-wave signal are much louder than in our usual observations. This is why we couldn’t hear them before, but in GW190412, we finally can.” This observation once again confirms Einstein’s theory of general relativity, which predicts the existence of these higher harmonics, i.e. gravitational waves at two or three times the fundamental frequency observed so far.

“The black holes at the heart of GW190412 have 8 and 30 times the mass of our Sun, respectively. This is the first binary black-hole system we have observed for which the difference between the masses of the two black holes is so large!” says Roberto Cotesta, a PhD student in the “Astrophysical and Cosmological Relativity” division at the AEI in Potsdam. “This big mass difference means that we can more precisely measure several properties of the system: its distance to us, the angle we look at it, and how fast the heavy black hole spins around its axis.”

A signal like none before

GW190412: Binary black-hole merger with asymmetric masses and orbital precession

Numerical simulation of a black-hole binary merger with asymmetric masses and orbital precession (GW190412).

GW190412 was observed by both LIGO detectors and the Virgo detector on 12th of April 2019, early during the detectors’ third observation run O3. Analyses reveal that the merger happened at a distance of 1.9 to 2.9 billion light-years from Earth. The new unequal mass system is a unique discovery since all binaries observed previously by the LIGO and Virgo detectors consisted of two roughly similar masses.

Unequal masses imprint themselves on the observed gravitational-wave signal, which in turn allow scientists to more precisely measure certain astrophysical properties of the system. The presence of higher harmonics makes it possible to break an ambiguity between the distance to the system and the angle we look at its orbital plane; therefore these properties can be measured with higher precision than in equal-mass systems without higher harmonics.

Numerical simulation of a black-hole binary merger with asymmetric masses and orbital precession (GW190412) Zoom Image
Numerical simulation of a black-hole binary merger with asymmetric masses and orbital precession (GW190412)

“During O1 and O2, we have observed the tip of the iceberg of the binary population composed of stellar-mass black holes,” says Alessandra Buonanno, director of the “Astrophysical and Cosmological Relativity” division at the AEI in Potsdam and College Park professor at the University of Maryland. “Thanks to the improved sensitivity, GW190412 has begun to reveal us a more diverse, submerged population, characterized by mass asymmetry as large as 4 and black holes spinning at about 40% the possible maximum value allowed by general relativity,” she adds.

AEI researchers contributed to detecting and analyzing GW190412. They have provided accurate models of the gravitational waves from coalescing black holes that included, for the first time, both the precession of the black-holes’ spins and multipole moments beyond the dominant quadrupole. Those features imprinted in the waveform were crucial to extract unique information about the source’s properties and carry out tests of general relativity. The high-performance computer clusters “Minerva” and “Hypatia” at AEI Potsdam and “Holodeck” at AEI Hannover contributed significantly to the analysis of the signal.

Testing Einstein’s theory

LIGO/Virgo scientists also used GW190412 to look for deviations of the signals from what Einstein’s general theory of relativity predicts. Even though the signal has properties unlike all others found so far, the researchers could find no significant departure from the general-relativistic predictions.

An improved international network of detectors using squeezed light

This discovery is the second reported from the third observation run (O3) of the international gravitational-wave detector network. Scientists at the three large detectors have made several technological upgrades to the detectors.

“During O3, squeezed light was used to enhance the sensitivity of LIGO and Virgo. This technique of carefully tuning the quantum-mechanical properties of the laser light was pioneered at the German-British detector GEO600,” explains Karsten Danzmann, director at the AEI Hannover and director of the Institute for Gravitational Physics at Leibniz University Hannover. “The AEI is leading the world-wide efforts to maximize the degree of squeezing, which has already improved the sensitivity of the GEO600 detector by a factor of two. Our advances in this technology will benefit all future gravitational-wave detectors.”

2 done, 54 on the to-do list

The detector network has issued alerts for 56 possible gravitational-wave events (candidates) in O3 (April 1, 2019 to March 27, 2020 with an interruption for upgrades and commissioning in October 2019). Out of these 56, one other confirmed signal, GW190425, has already been published. LIGO and Virgo scientists are examining all remaining 54 candidates and will publish all those for which detailed follow-up analyses confirm their astrophysical origin.

The observation of GW190412 means that similar systems are probably not as rare as predicted by some models. Therefore, with additional gravitational-wave observations and growing event catalogues in the future, more such signals are to be expected. Each of them could help astronomers better understand how black holes and their binary systems are formed, and shed new light on the fundamental physics of space-time.


LIGO Scientific and Virgo Collaborations

LIGO is funded by the National Science Foundation (NSF) and operated by Caltech and MIT, which conceived of LIGO and lead the project. Financial support for the Advanced LIGO project was led by the NSF with Germany (Max Planck Society), the U.K. (Science and Technology Facilities Council) and Australia (Australian Research Council-OzGrav) making significant commitments and contributions to the project. Approximately 1,300 scientists from around the world participate in the effort through the LIGO Scientific Collaboration, which includes the GEO Collaboration. A list of additional partners is available at https://my.ligo.org/census.php.

The Virgo Collaboration is currently composed of more than 500 scientists, engineers, and technicians from 99 institutes from Belgium, France, Germany, Hungary, Italy, the Netherlands, Poland, and Spain. The European Gravitational Observatory (EGO) hosts the Virgo detector near Pisa in Italy, and is funded by Centre National de la Recherche Scientifique (CNRS) in France, the Istituto Nazionale di Fisica Nucleare (INFN) in Italy, and Nikhef in the Netherlands. A list of the Virgo Collaboration members can be found at http://public.virgo-gw.eu/the-virgo-collaboration/. More information is available on the Virgo website at http://www.virgo-gw.eu.

 
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