NASA / ESA - Hubble Space Telescope (HST) patch.
June 10, 2022
Artist’s Impression of an Isolated Black Hole
Astronomers estimate that 100 million black holes roam among the stars in our Milky Way galaxy, but they have never conclusively identified an isolated black hole. Following six years of meticulous observations, the NASA/ESA Hubble Space Telescope has, for the first time ever, provided direct evidence for a lone black hole drifting through interstellar space by a precise mass measurement of the phantom object. Until now, all black hole masses have been inferred statistically or through interactions in binary systems or in the cores of galaxies. Stellar-mass black holes are usually found with companion stars, making this one unusual.
The newly detected wandering black hole lies about 5,000 light-years away, in the Carina-Sagittarius spiral arm of our galaxy. However, its discovery allows astronomers to estimate that the nearest isolated stellar-mass black hole to Earth might be as close as 80 light-years away. The nearest star to our solar system, Proxima Centauri, is a little over 4 light-years away.
Microlensing Black Hole
Black holes roaming our galaxy are born from rare, monstrous stars (less than one-thousandth of the galaxy's stellar population) that are at least 20 times more massive than our Sun. These stars explode as supernovae, and the remnant core is crushed by gravity into a black hole. Because the self-detonation is not perfectly symmetrical, the black hole may get a kick, and go careening through our galaxy like a blasted cannonball.
Telescopes can't photograph a wayward black hole because it doesn't emit any light. However, a black hole warps space, which then deflects and amplifies starlight from anything that momentarily lines up exactly behind it.
Video above: Space Sparks Episode 16: Hubble Determines Mass of Isolated Black Hole Roaming Our Milky Way.
Ground-based telescopes, which monitor the brightness of millions of stars in the rich star fields toward the central bulge of our Milky Way, look for a tell-tale sudden brightening of one of them when a massive object passes between us and the star. Then Hubble follows up on the most interesting such events.
Two teams used Hubble data in their investigations — one led by Kailash Sahu of the Space Telescope Science Institute in Baltimore, Maryland; and the other by Casey Lam of the University of California, Berkeley. The teams' results differ slightly, but both suggest the presence of a compact object.
The warping of space due to the gravity of a foreground object passing in front of a star located far behind it will momentarily bend and amplify the light of the background star as it passes in front of it. Astronomers use the phenomenon, called gravitational microlensing, to study stars and exoplanets in the approximately 30,000 events seen so far inside our galaxy.
Artist’s Impression of a Black Hole (Animation)
The signature of a foreground black hole stands out as unique among other microlensing events. The very intense gravity of the black hole will stretch out the duration of the lensing event for over 200 days. Also, if the intervening object was instead a foreground star, it would cause a transient color change in the starlight as measured because the light from the foreground and background stars would momentarily be blended together. But no color change was seen in the black hole event.
Next, Hubble was used to measure the amount of deflection of the background star's image by the black hole. Hubble is capable of the extraordinary precision needed for such measurements. The star's image was offset from where it normally would be by about a milliarcsecond. That’s equivalent to measuring the height of an adult human lying on the surface of the moon from the Earth.
This astrometric microlensing technique provided information on the mass, distance, and velocity of the black hole. The amount of deflection by the black hole's intense warping of space allowed Sahu's team to estimate that it weighs seven solar masses.
Lam's team reports a slightly lower mass range, meaning that the object may be either a neutron star or a black hole. They estimate that the mass of the invisible compact object is between 1.6 and 4.4 times that of the Sun. At the high end of this range the object would be a black hole; at the low end, it would be a neutron star.
"As much as we would like to say it is definitively a black hole, we must report all allowed solutions. This includes both lower mass black holes and possibly even a neutron star," said Jessica Lu of the Berkeley team.
"Whatever it is, the object is the first dark stellar remnant discovered wandering through the galaxy, unacompanied by another star" Lam added.
This was a particularly difficult measurement for the team because there is another bright star that is extremely close in angular separation to the source star. “So it’s like trying to measure the tiny motion of a firefly next to a bright light bulb,” said Sahu. “We had to meticulously subtract the light of the nearby bright star to precisely measure the deflection of the faint source.”
Sahu's team estimates the isolated black hole is traveling across the galaxy at 160,000 kilometres per hour (fast enough to travel from Earth to the Moon in less than three hours). That's faster than most of the other neighbouring stars in that region of our galaxy.
“Astrometric microlensing is conceptually simple but observationally very tough,” said Sahu. “Microlensing is the only technique available for identifying isolated black holes.” When the black hole passed in front of a background star located 19,000 light-years away in the galactic bulge, the starlight coming toward Earth was amplified for a duration of 270 days as the black hole passed by. However, it took several years of Hubble observations to follow how the background star's position appeared to be deflected by the bending of light by the foreground black hole.
Hubble Space Telescope (HST)
The existence of stellar-mass black holes has been known since the early 1970s, but all of their mass measurements—until now—have been in binary star systems. Gas from the companion star falls into the black hole and is heated to such high temperatures that it emits X-rays. About two dozen black holes have had their masses measured in X-ray binaries through their gravitational effect on their companions. Mass estimates range from 5 to 20 solar masses. Black holes detected in other galaxies by gravitational waves from mergers between black holes and companion objects have been as high as 90 solar masses.
“Detections of isolated black holes will provide new insights into the population of these objects in the Milky Way,” said Sahu. He expects that his programme will uncover more free-roaming black holes inside our galaxy. But it is a needle-in-a-haystack search. The prediction is that only one in a few hundred microlensing events are caused by isolated black holes.
In his 1916 paper on general relativity, Albert Einstein predicted that his theory could be tested by observing the offset in the apparent position of a background star caused by the Sun’s gravity. This was tested by a collaboration led by astronomers Arthur Eddington and Frank Dyson during a solar eclipse on 29 May 1919. Eddington and his colleagues measured a background star being offset by 2 arc seconds, validating Einstein’s theories. These scientists could hardly have imagined that over a century later this same technique would be used — with a then-unimaginable thousandfold improvement in precision — to look for black holes across our galaxy.
More information:
The Hubble Space Telescope is a project of international cooperation between ESA and NASA.
The international team of astronomers in Sahu's study consists of K. C. Sahu (Space Telescope Science Institute, USA), J. Anderson (Space Telescope Science Institute, USA), S. Casertano (Space Telescope Science Institute, USA), H. E. Bond (Space Telescope Science Institute, USA; University of Pennsylvania, USA), A. Udalski (University of Warsaw, Poland), M. Dominik (University of St. Andrews, UK), A. Calamida (Space Telescope Science Institute, USA), A. Bellini (Space Telescope Science Institute, USA), T. M. Brown (Space Telescope Science Institute, USA), M. Rejkuba (European Southern Observatory, Germany), V. Bajaj (Space Telescope Science Institute, USA), N. Kains (Columbia University, USA), H. C. Ferguson (Space Telescope Science Institute, USA), C. L. Fryer (Los Alamos National Laboratory, USA), and P. Yock (University of Auckland, New Zealand), together with the other members of the following teams: the OGLE Collaboration consisting of P. Mroz (University of Warsaw, Poland), S. Kozlowski (University of Warsaw, Poland), P. Pietrukowicz (University of Warsaw, Poland), R. Poleski (University of Warsaw, Poland), J. Skowron (University of Warsaw, Poland), I. Soszynski (University of Warsaw, Poland), M. K. Szymanski (University of Warsaw, Poland), K. Ulaczyk (University of Warsaw, Poland; University of Warwick, UK), and L. Wyrzykowski (University of Warsaw, Poland); the MOA Collaboration consisting of R. Barry (NASA Goddard Space Flight Centre, USA), D. P. Bennett (NASA Goddard Space Flight Centre, USA; University of Maryland, USA), I. A. Bond (Massey University, New Zealand), Y. Hirao (Osaka University, Japan), S. I. Silva (NASA Goddard Space Flight Centre, USA; Catholic University of America, USA), I. Kondo (Osaka University, Japan), N. Koshimoto (NASA Goddard Space Flight Centre, USA), C. Ranc (Heidelberg University, Germany), N. J. Rattenbury (University of Auckland, New Zealand), T. Sumi (Osaka University, Japan), D. Suzuki (Osaka University, Japan), P. J. Tristram (University of Canterbury, New Zealand), and A. Vandorou (NASA Goddard Space Flight Centre, USA; University of Maryland, USA); the PLANET Collaboration consisting of J. Beaulieu (University of Tasmania, Australia; Sorbonne University, France), J. Marquette (University of Bordeaux, France), A. Cole (University of Tasmania, Australia), P. Fouque (University of Toulouse, France), K. Hill (University of Tasmania, Australia), S. Dieters (University of Tasmania, Australia), C. Coutures (Sorbonne University, France), D. Dominis-Prester (National Astronomical Observatory of Japan, Japan), C. Bennett (Massachussets Institute of Technology, USA), E. Bachelet (Las Cumbres Observatory, USA), J. Menzies (South African Astronomical Observatory, South Africa), M. Alb-row (University of Canterbury, New Zealand), and K. Pollard (University of Canterbury, New Zealand); the µFUN Collaboration consisting of A. Gould (Max Planck Institute for Astronomy, Germany; Ohio State University, USA), J. C. Yee (Center for Astrophysics | Harvard & Smithsonian, USA), W. Allen (Vintage Lane Observatory, New Zealand), L. A. de Almeida (Federal University of Rio Grande do Norte, Brazil; State University of Rio Grande do Norte, Brazil), G. Christie (Auckland Observatory, New Zealand), J. Drummond (Possum Observatory, New Zealand; University of Southern Queensland, Australia), A. Gal-Yam (Weizmann Institute of Science, Israel), E. Gorbikov (Tel Aviv University, Israel), F. Jablonski (Natonal Institute for Space Research, Brazil), C. Lee (Korea Astronomy and Space Science Institute, Republic of Korea), D. Maoz (Tel Aviv University, Israel), I. Manulis (Weizmann Institute of Science, Israel), J. McCormick (Centre for Backyard Astrophysics, New Zealand), T. Natusch (Auckland Observatory, New Zealand; Auckland University of Technology, New Zealand), R. W. Pogge (Ohio State University, USA), and Y. Shvartzvald (Weizmann Institute of Science, Israel); the MiNDSTEp Collaboration consisting of U. G. Jorgensen (University of Copenhagen, Denmark), K. A. Alsubai (Hamad Bin Khalifa University, Qatar), M. I. Andersen (University of Copenhagen, Denmark), V. Bozza (University of Salerno, Italy), S. C. Novati (California Institute of Technology, USA), M. Burgdorf (Hamburg, Germany), T. C. Hinse (Nicolaus Copernicus University, Poland; Chungnam National University, Republic of Korea), M. Hundertmark (Heidelberg University, Germany), T. Husser (University of Göttingen, Germany), E. Kerins (University of Manchester, UK), P. Longa-Pena (University of Antofagasta, Chile), L. Mancini (Tor Vergata University of Rome, Italy; Max Planck Institute for Astronomy, Germany; Astrophysical Observatory of Turin, Italy), M. Penny (Louisiana State University, USA), S. Rahvar (Sharif University of Technology, Iran), D. Ricci (Padova Astronomical Observatory, Italy), S. Sajadian (Isfahan University of Technology, Iran), J. Skottfelt (The Open University, UK), C. Snodgrass (University of Edinburgh, UK), J. Southworth (Keele University, UK), J. Tregloan-Reed (University of Atacama, Chile), J. Wambsganss (Heidelberg University, Germany), and O. Wertz (University of Liège, Belgium); and the RoboNet Collaboration consisting of Y. Tsapras (Heidelberg University, Germany), R. A. Street (Las Cumbres Observatory, USA), D. M. Bramich (New York University Abu Dhabi, United Arab Emirates), K. Horne (University of St. Andrews, UK), and I. A. Steele (Liverpool John Moores University, UK).
The international team of astronomers in Lam's study consists of C. Y. Lam (University of California, Berkeley, USA), J. R. Lu (University of California, Berkeley, USA), A. Udalski (University of Warsaw, Poland), I. Bond (Massey University, New Zealand), D. P. Bennett (NASA Goddard Space Flight Center, USA; University of Maryland, USA), J. Skowron (University of Warsaw, Poland), P. Mroz (University of Warsaw, Poland), R. Polski (University of Warsaw, Poland), T. Sumi (Osaka University, Japan), M. Szmanski (University of Warsaw, Poland), S. Kozlowski (University of Warsaw, Poland), P. Pietrukowicz (University of Warsaw, Poland), I. Soszynski (University of Warsaw, Poland), K. Ulaczyk (University of Warsaw, Poland; University of Warwick, UK), L. Wyrzykowski (University of Warsaw, Poland), S. Miyazaki (Osaka University, Japan), D. Suzuki (Osaka University, Japan), N. Koshimoto (NASA Goddard Space Flight Center, USA; University of Maryland, USA; The University of Tokyo, Japan), N. J. Rattenbury (University of Auckland, New Zealand), M. W. Josek, Jr. (University of California, Los Angeles, USA), F. Abe (Nagoya University, Japan), R. Barry (NASA Goddard Space Flight Center), A. Bhattacharya (NASA Goddard Space Flight Center; University of Maryland, USA), A. Fukui (The University of Tokyo, Japan; Instituto de Astrofisica de Canarias, Spain), H. Fuji (Nagoya University, Japan), Y. Hirao (Osaka University, Japan), Y. Itow (Nagoya University, Japan), R. Kirikawa (Osaka University, Japan), I. Kondo (Osaka University, Japan), Y. Matsubara (Nagoya University, Japan), S. Matsumoto (Osaka University, Japan), Y. Muraki (Nagoya University, Japan), G. Olmschenk (NASA Goddard Space Flight Center), C. Ranc (Universitat Heidelberg, Germany), A. Okamura (Osaka University, Japan), Y. Satoh (Osaka University, Japan), S. I. Silva (The Catholic University of America, DC, USA; NASA Goddard Space Flight Center, USA), T. Toda (Osaka University, Japan), T. Toda (Osaka University, Japan), P. J. Tristram (University of Canterbury, New Zealand), A. Vandorou (NASA Goddard Space Flight Center, USA; University of Maryland, USA), H. Yama (Osaka University, Japan), N. S. Abrams (University of California, Berkeley, USA), S. Agarwal (University of California, Berkeley, USA), S. Rose (University of California, Berkeley, USA), S. K. Terry (University of California, Berkeley, USA).
Links:
Images of Hubble: https://esahubble.org/images/archive/category/spacecraft/
Hubblesite release: https://hubblesite.org/contents/news-releases/2022/news-2022-001
Sahu et al. science paper: https://arxiv.org/abs/2201.13296
Lam et al. science paper: https://arxiv.org/abs/2202.01903v2
ESA's Hubble: https://esahubble.org/
Images, Animation Credits: ESA/Hubble, Digitized Sky Survey, Nick Risinger (skysurvey.org), N. Bartmann/NASA, ESA, K. Sahu (STScI), J. DePasquale (STScI)/Videos Credits: ESA/Hubble, Digitized Sky Survey, Nick Risinger (skysurvey.org), N. Bartmann/Text Credits: ESA/Hubble/Bethany Downer/STSi/Kailash Sahu.
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