Unlike Hollywood stars who are wanting to be discovered, this hot blue star has been elusive and is the most distant star ever discovered. The Hubble Space Telescope has made quite an impressive find … a star that existed 4.4 billion years after the Earth began.
Astronomers using the NASA/ESA Hubble Space Telescope have found the most distant star ever discovered. The hot blue star existed only 4.4 billion years after the Big Bang. This discovery provides new insight into the formation and evolution of stars in the early Universe, the constituents of galaxy clusters and also on the nature of dark matter.
The international team, led by Patrick Kelly (University of Minnesota, USA), Jose Diego (Instituto de Física de Cantabria, Spain) and Steven Rodney (University of South Carolina, USA), discovered the distant star in the galaxy cluster MACS J1149-2223 in April 2016. The observations with Hubble were actually performed in order to detect and follow the latest appearance of the gravitationally lensed supernova explosion nicknamed “Refsdal” (heic1525)[1], when an unexpected point source brightened in the same galaxy that hosted the supernova.
“Like the Refsdal supernova explosion the light of this distant star got magnified, making it visible for Hubble,” says Patrick Kelly. “This star is at least 100 times farther away than the next individual star we can study, except for supernova explosions.”
This shows the discovery of the most distant known star using the NASA/ESA Hubble Space Telescope. The image shows a part of the the deep-field observation of the galaxy cluster MACS J1149.5+2223 from the Frontier Fields program gathered in 2014. The square indicates the position of the star in May 2016 magnified by gravitational microlensing. This also shows the four images of the Refsdal supernova, arranged in an Einstein cross. All photos: NASA & ESA and P. Kelly (University of California, Berkeley)
The observed light from the newly discovered star, called Lensed Star 1 (LS1) was emitted when the Universe was only about 30 percent of its current age — about 4.4 billion years after the Big Bang. The detection of the star through Hubble was only possible because the light from the star was magnified 2000 times.
“The star became bright enough to be visible for Hubble thanks to a process called gravitational lensing,” explains Jose Diego. The light from LS1 was magnified not only by the huge total mass of the galaxy cluster, but also by another compact object of about three times the mass of the Sun within the galaxy cluster itself; an effect known as gravitational microlensing [2].
“The discovery of LS1 allows us to gather new insights into the constituents of the galaxy cluster. We know that the microlensing was caused by either a star, a neutron star, or a stellar-mass black hole,” explains Steven Rodney. LS1 therefore allows astronomers to study neutron stars and black holes, which are otherwise invisible and they can estimate how many of these dark objects exist within this galaxy cluster.
As galaxy clusters are among the largest and most massive structures in the Universe, learning about their constituents also increases our knowledge about the composition of the Universe overall. This includes additional information about the mysterious dark matter.
“If dark matter is at least partially made up of comparatively low-mass black holes, as it was recently proposed, we should be able to see this in the light curve of LS1. Our observations do not favour the possibility that a high fraction of dark matter is made of these primordial black holes with about 30 times the mass of the Sun”, highlights Kelly.
After the discovery the researchers used Hubble again to measure a spectrum of LS1. Based on their analysis, the astronomers think that LS1 is a B-type supergiant star. These stars are extremely luminous and blue in color, with a surface temperature between 11 000 and 14 000 degrees Celsius; making them more than twice as hot as the Sun.
The upper image pinpoints the position of the star, observed in 2011. The lower image shows where the star was undergoing the microlensing event in late May 2016.But this was not the end of the story. Observations made in October 2016 suddenly showed a second image of the star. “We were actually surprised to not have seen this second image in earlier observations, as also the galaxy the star is located in can be seen twice,” comments Diego. “We assume that the light from the second image has been deflected by another moving massive object for a long time — basically hiding the image from us. And only when the massive object moved out of the line of sight the second image of the star became visible.” This second image and the blocking object add another piece of the puzzle to reveal the makeup of galaxy clusters.
With more research and the arrival of new, more powerful telescopes like the NASA/ESA/CSA James Webb Space Telescope, the astronomers suggest that with microlensing, it will be possible to study the evolution of the earliest stars in the Universe in greater detail than ever expected.
Notes
[1] Observations of this supernova, nicknamed Refsdal in honour of the Norwegian astronomer Sjur Refsdal, were made as part of Hubble’s Frontier Fields project.
[2] Gravitational lensing magnifies the light from fainter, background objects, allowing Hubble to see objects it would otherwise not be able to detect. The process was first predicted by Albert Einstein and is now used to find some of the most distant objects in the Universe. Usually the lensing object is a galaxy or a galaxy cluster, but in some cases it can also be a star or even a planet. When it involves these smaller objects the process is called microlensing.
More information
The Hubble Space Telescope is a project of international cooperation between ESA and NASA.
The results were released in the paper Extreme magnification of an individual star at redshift 1.5 by a galaxy-cluster lens to be published in Nature Astronomy.
The international team of astronomers in this study consists of P. Kelly (University of Minnesota, USA); J. Diego (IFAC, Instituto de F ísica de Cantabria, Spain); S. Rodney (University of South Carolina, USA); N. Kaiser (Institute for Astronomy, University of Hawaii, USA); T. Broadhurst (University of Basque Country, Spain and IKERBASQUE of the Basque Foundation for Science, Spain); A. Zitrin (Ben Gurion University of the Negev, Israel); T. Treu (University of California, Los Angeles, USA); P. Pérez-González (Universidad Complutense de Madrid, Spain); T. Morishita (University of California, Los Angeles, USA; Tohoku University, Japan) M. Jauzac (Durham University, U.K.; University of KwaZulu-Natal, South Africa); J. Selsing (University of Copenhagen, Denmark); M. Oguri (University of Tokyo, Japan); L. Pueyo (Space Telescope Science Institute, USA); T. W. Ross (University of California, Berkeley, USA); A. V. Filippenko (University of California, Berkeley, USA); N. Smith (University of Arizona, USA); J. Hjorth (University of Copenhagen, Denmark); S. B. Cenko (Goddard Space Flight Center, USA; University of Maryland, USA); Xin Wang (University of California, Los Angeles, USA); D. A. Howell (Las Cumbres Observatory, USA; University of California, Santa Barbara, USA); J. Richard (Université Claude Bernard Lyon 1, France); B. L. Frye (University of Arizona, USA); S. W. Jha (The State University of New Jersey, USA); R.J. Foley (University of California, Santa Cruz); C. Norman (the Johns Hopkins University, USA); M. Bradac (University of California, Davis, USA); WeiKang Zheng (University of California, Berkeley, USA); G. Brammer (Space Telescope Science Institute, USA); A. M. Benito (Universidade de São Paulo); A. Cava (University of Geneva, Switzerland); L. Christensen (University of Copenhagen, Denmark); S. D de Mink (University of Amsterdam, the Netherlands); Or Gaur (Harvard-Smithsonian Center for Astrophysics, USA; American Museum of Natural History, USA; NSF Astronomy and Astrophysics Postdoctoral Fellow); C. Grillo (Universitá degli Studi di Milano, Italy); R. Kawamata (University of Tokyo, Japan); J. Kneib (Observatoire de Sauverny, Switzerland); T. Matheson (National Optical Astronomical Observatory, USA); C. McCully (Las Cubres Observatory, USA; University of California, Santa Barbara); M. Nonino (Osservatorio Astronomico di Trieste, Italy); I. Perez-Fournon (Instituto de Astrofísica de Canarias, Spain; Universidad de La Laguna, Spain); A. G. Reiss (The Johns Hopkins University, USA; Space Telescope Science Institute, USA); P. Rosati (Universitá degli Studi di Ferrara, Italy); K. Borello Schmidt (Leibniz-Institut für Astrophysik Potsdam, Germany); K. Sharon (University of Michigan, USA); and B. J. Weiner (University of Arizona, USA)
