Artist’s impression of g objects, with the reddish centers, orbiting the supermassive black hole at the center of our galaxy. the black hole is represented as a dark sphere inside a white ring (above the middle of the rendering).
Credit: Jack Ciurlo
Maunakea, Hawaii – Astronomers from UCLA and W. M.
Keck Observatory have discovered four more bizarre objects at the center
of our galaxy, not far from the supermassive black hole called
Sagittarius A*, that are now forming a class of their own.
The study, which is part of UCLA’s Galactic Center Orbits Initiative,
consists of 13 years of data taken from Keck Observatory on Maunakea in
Hawaii; the results published online today in the journal Nature.
“These objects look like gas but behave like stars,” said co-author
Andrea Ghez, UCLA’s Lauren B. Leichtman and Arthur E. Levine Professor
of Astrophysics and director of the UCLA Galactic Center Group.
This new class of objects, called G objects, look compact most of the
time and stretch out when their orbits bring them closest to the black
hole. Their orbits range from about 100 to 1,000 years, said lead author
Anna Ciurlo, a UCLA postdoctoral researcher.
Ciurlo led the study while participating in Keck Observatory’s Visiting Scholars Program
and labeled the four new objects G3, G4, G5 and G6. This set is in
addition to the first pair of G objects found near the Galactic Center;
G1 was discovered by Ghez’s research group in 2005, followed by G2, which was discovered by astronomers in Germany in 2012.
“The fact that there now several of these objects observed near the black hole means that they are, most likely, part of a common
population,” said co-author Randy Campbell, science operations lead at
Keck Observatory.
The researchers have determined orbits for each of the newly
discovered G objects. While G1 and G2 have similar orbits, G3, G4, G5,
and G6 all have very different orbits.
Ghez and her research team believe that G2 is most likely two stars
that had been orbiting the black hole in tandem and merged into an
extremely large star, cloaked in unusually thick gas and dust.
“At the time of closest approach, G2 had a really strange signature,”
Ghez said. “We had seen it before, but it didn’t look too peculiar
until it got close to the black hole and became elongated, and much of
its gas was torn apart. It went from being a pretty innocuous object
when it was far from the black hole to one that was really stretched out
and distorted at its closest approach and lost its outer shell, and now
it’s getting more compact again.”
Orbits of the G objects at the center of our galaxy, with the supermassive black hole marked with a white cross. Stars, gas, and dust are in the background. Credit: Anna Ciurlo, Tuan Do/UCLA Galactic Center Group
“One of the things that has gotten everyone excited about the G
objects is that the stuff that gets pulled off of them by tidal forces
as they sweep by the central black hole must inevitably fall into the
black hole,” said co-author Mark Morris, UCLA professor of physics and
astronomy. “When that happens, it might be able to produce an impressive
fireworks show since the material eaten by the black hole will heat up
and emit copious radiation before it disappears across the event
horizon.”
Ghez believes all six objects were binary stars — a system of two
stars orbiting each other — that merged because of the strong
gravitational force of the supermassive black hole. The merging of two
stars takes more than 1 million years to complete, Ghez said.
“Mergers of stars may be happening in the universe more often than we
thought, and likely are quite common,” Ghez said. “Black holes may be
driving binary stars to merge. It’s possible that many of the stars
we’ve been watching and not understanding may be the end product of
mergers that are calm now. We are learning how galaxies and black holes
evolve. The way binary stars interact with each other and with the black
hole is very different from how single stars interact with other single
stars and with the black hole.”
Ciurlo noted that while the gas from G2’s outer shell got stretched
dramatically, its dust inside the gas did not get stretched much.
“Something must have kept it compact and enabled it to survive its
encounter with the black hole,” Ciurlo said. “This is evidence for a
stellar object inside G2.”
“The unique dataset that Professor Ghez’s group has gathered during
more than 20 years is what allowed us to make this discovery,” Ciurlo
said. “We now have a population of ‘G’ objects, so it is not a matter of
explaining a ‘one-time event’ like G2.”
The researchers made the observations using powerful technology that
Ghez helped pioneer at Keck Observatory called adaptive optics (AO),
which corrects the distorting effects of the Earth’s atmosphere in real
time. AO, combined with Keck Observatory’s OH-Suppressing Infrared
Imaging Spectrograph (OSIRIS), allowed the team to obtain spectroscopic
measurements of the Galactic Center’s gas dynamics.
“The challenge was trying distinguish G objects from a crowded
cluster of stars,” said Campbell. “Because their spectra are different
from standard stars, we were able to separate them using a tool called
the OSIRIS-Volume Display, or OsrsVol.”
The OsrsVol software Campbell developed produces a 3-D spectral data
cube that consists of two spatial dimensions plus a wavelength dimension
that contains velocity information. This allowed the team to clearly
isolate the G-objects and track their movement to see how they behaved
around the Milky Way’s supermassive black hole.
In September 2019, Ghez’s team reported that the black hole is getting hungrier and
it is unclear why. The stretching of G2 in 2014 appeared to pull off
gas that may recently have been swallowed by the black hole, said
co-author Tuan Do, a UCLA research scientist and deputy director of the
Galactic Center Group.
The research is funded by the National Science Foundation, W. M. Keck
Foundation, Keck Visiting Scholars Program, the Gordon and Betty Moore
Foundation, the Heising-Simons Foundation, Lauren Leichtman and Arthur
Levine, Jim and Lori Keir, and Howard and Astrid Preston.
About Adaptive Optics
W. M. Keck Observatory is a distinguished leader in the field of adaptive optics (AO), a breakthrough technology that removes the distortions caused by the turbulence in the Earth’s atmosphere. Keck Observatory pioneered the astronomical use of both natural guide star (NGS) and laser guide star adaptive optics (LGS AO) and current systems now deliver images three to four times sharper than the Hubble Space Telescope at near-infrared wavelengths. AO has imaged the four massive planets orbiting the star HR8799, measured the mass of the giant black hole at the center of our Milky Way Galaxy, discovered new supernovae in distant galaxies, and identified the specific stars that were their progenitors. Support for this technology was generously provided by the Bob and Renee Parsons Foundation, Change Happens Foundation, Gordon and Betty Moore Foundation, Mt. Cuba Astronomical Foundation, NASA, NSF, and W. M. Keck Foundation.
About OSIRIS
The OH-Suppressing Infrared Imaging Spectrograph (OSIRIS) is one of W. M. Keck Observatory’s “integral field spectrographs.” The instrument works behind the adaptive optics system, and uses an array of lenslets to sample a small rectangular patch of the sky at resolutions approaching the diffraction limit of the 10-meter Keck Telescope. OSIRIS records an infrared spectrum at each point within the patch in a single exposure, greatly enhancing its efficiency and precision when observing small objects such as distant galaxies. It is used to characterize the dynamics and composition of early stages of galaxy formation. Support for this technology was generously provided by the Heising-Simons Foundation and the National Science Foundation.
About W. M. Keck Observatory
The W. M. Keck Observatory telescopes are among the most scientifically productive on Earth. The two, 10-meter optical/infrared telescopes on the summit of Maunakea on the Island of Hawaii feature a suite of advanced instruments including imagers, multi-object spectrographs, high-resolution spectrographs, integral-field spectrometers, and world-leading laser guide star adaptive optics systems.
Some of the data presented herein were obtained at Keck Observatory, which is a private 501(c) 3 non-profit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
