WVU scientists were members of the LIGO team that detected gravitational waves from merging pairs black holes approximately 29 to 36 times the mass of the sun, confirming that distortions in the fabric of space-time can be observed and measured.
WVU scientists are also continuing to make discoveries about the universe as members of North American Nanohertz Observatory for Gravitational Waves, or NANOGrav, which has spent the past decade searching for low-frequency gravitational waves emitted by pairs of black holes with masses many millions of times larger than those seen by LIGO.
Analysis of NANOGrav’s nine-year dataset provides very constraining limits – estimates of the largest possible signal that could be in the data – on the prevalence of such supermassive black hole binaries throughout the universe, as published yesterday in The Astrophysical Journal.
Given scientists’ current understanding of how often galaxies merge, these limits point to fewer detectable pairs of supermassive black holes, referred to as black hole binaries, than previously expected. This result has a significant impact on scientists’ understanding of how galaxies and their central black holes co-evolve.
Detecting a waveLow-frequency gravitational waves are extremely difficult to detect because their wavelengths span light-years and originate from black hole binaries in galaxies spread across the sky.
The combination of these giant binary black holes leads to a constant “hum” of gravitational waves that computer models predict should be detectable at Earth. Astrophysicists call this effect the “stochastic gravitational wave background,” and detecting it requires special analysis techniques, such as the use of pulsars.
Pulsars are the cores of massive stars left behind after the stars go supernova and explode, emitting pulses of radio waves as they spin. The fastest pulsars rotate hundreds of times each second and emit a pulse every few milliseconds.
These “millisecond pulsars” are considered nature’s most precise clocks and are ideal for detecting the small signal from gravitational waves.
“We have the ability to detect very tiny deviations in the arrival time of pulses from pulsars that might be due to gravitational waves,” says Maura McLaughlin, professor of physics and astronomy, and a co-author of the report.
Astrophysicists use computer models to predict how often galaxies merge and form supermassive black hole binaries. Those models use several assumptions about how pairs of black holes evolve by predicting the strength of the hum.
“By using information about galaxy mergers and constraints on the background, we can predict the properties of the sources we might detect and even use a non-detection to better understand the physics of black hole binary evolution,” says Sean McWilliams, assistant professor of physics and astronomy and also a co-author on the paper.
According to Sarah Burke-Spolaor, Jansky Fellow at the National Radio Astronomy Observatory in Soccoro, New Mexico, and a co-author on the paper, says there are two possible interpretations of this non-detection. She will join the physics and astronomy faculty at WVU as an assistant professor in January 2017.
“Some supermassive black hole binaries may not be in circular orbits or are significantly interacting with gas or stars,” Burke-Spolaor says. “This would drive them to merge faster than simple models have assumed in the past.”
An alternate explanation is that many of these binaries inspiral too slowly to ever emit detectable gravitational waves.
NANOGrav is currently monitoring 54 pulsars using the National Science Foundation’s Green Bank Telescope in West Virginia and Arecibo Radio Observatory in Puerto Rico, the two most sensitive radio telescopes in the world at these frequencies. Their array of pulsars is continually growing as new millisecond pulsars are discovered.
The group also collaborates with radio astronomers in Europe and Australia as part of the International Pulsar Timing Array, giving them access to many more pulsar observations. This increase in sensitivity could lead to a detection in as little as five years.
In addition, this measurement helps constrain the properties of cosmic strings, very dense and thin cosmological objects, which many theorists believe evolved when the universe was just a fraction of a second old. These strings can form loops, which then decay through gravitational wave emission.
The most conservative NANOGrav limit on cosmic string tension is the most stringent limit to date and will continue to improve as NANOGrav continues operating.
“These new limits have the most astrophysically relevant implications for the gravitational wave background at these frequencies yet,” says Duncan Lorimer, professor of physics and astronomy and a co-author on the paper. “If we can keep our access to the Green Bank Telescope and the Arecibo Observatory in Puerto Rico, a detection is easily within reach and we will soon have an entirely new way of understanding our universe and how galaxies form and evolve.”
NANOGrav is a collaboration of more than 60 scientists at more than a dozen institutions in the United States and Canada whose goal is detecting low-frequency gravitational waves to open a new window on the universe. The group uses radio pulsar timing observations to search for the ripples in the fabric of space-time.
In 2015, NANOGrav was awarded $14.5 million by the NSF to create and operate a Physics Frontiers Center. Three faculty members, one postdoctoral researcher, two graduate students and six undergraduate students in WVU’s Department of Physics and Astronomy participate in center-funded research.
“The Physics Frontiers Centers bring people together to address frontier science, and NANOGrav’s work in low-frequency gravitational wave physics is a great example,” says Jean Cottam Allen, the NSF program director who oversees the Physics Frontiers Center program. “We’re delighted with their progress thus far, and we’re excited to see where it will lead.”
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