Joint Gemini Observatory And Institute for Astronomy (IfA) Press Release
For Immediate Release Thursday August 30th, 2012
Harvard-Smithsonian Center for Astrophysics
Email: eberger "at" cfa.harvard.edu
Phone: (617) 335-7963
Institute for Astronomy
University of Hawai'i – Manoa, Hawai‘i
Email: jt "at" ifa.hawaii.edu
Phone: (808) 956-8701
Gemini Observatory, Hilo Hawai‘i
Email: pmichaud "at" gemini.edu
Desk: (808) 974-2510
Cell: (808) 936-6643
Roy R. Gal
Institute for Astronomy
University of Hawai'i – Manoa, Hawai‘i
Email: rgal "at" ifa.hawaii.edu
Cell: (301) 728-8637
Desk: (808) 956-6235
Nature hath no fury like a dying star – and astronomers couldn’t be happier…
An international research team, led by Edo Berger of Harvard University, made the most of a dying star’s fury to probe a distant galaxy some 9.5 billion light-years distant. The dying star, which lit the galactic scene, is the most distant stellar explosion of its kind ever studied. According to Berger, “It’s like someone turned on a flashlight in a dark room and suddenly allowed us to see, for a short time, what this far-off galaxy looks like, what it is composed of.”
The study, published recently in The Astrophysical Journal, describes how the researchers used the exploding star’s light (called an ultra-luminous core-collapse supernova) as a probe to study the gas conditions in the space between the host galaxy’s stars. Berger says the findings reveal that the distant galaxy‘s interstellar conditions appear “reassuringly normal” when compared to those seen in the galaxies of our local universe. “This shows the enormous potential of using the most luminous supernovae to study the early universe,” he says. “Ultimately it will help us understand how galaxies like our Milky Way came to be.”
The discovery of the dying star in this distant galaxy was made using images from the Pan-STARRS1 survey telescope on Haleakala in Maui, Hawai‘i. “These are the types of exciting and unexpected applications that appear when a new capability comes on line,” said John Tonry, one of the study's co-authors and supernovae researcher at the University of Hawai‘i at Manoa's Institute for Astronomy. Tonry adds, “Pan-STARRS is pioneering a new era in deep, wide-field, time-critical astronomy – and this is just the beginning.” After the Pan-STARRS discovery, spectroscopic follow-up studies using the Multiple Mirror Telescope in Arizona and the 8-meter Gemini North telescope on Mauna Kea, Hawai‘i provided the data used by the team to probe the gas of the distant galaxy’s interstellar environment.
The spectra revealed the signatures of a distant ultra-luminous supernova, and equally important, the unique fingerprints of iron and magnesium within the distant galaxy that hosted the explosion. The galaxy itself contains a very young population of stars (~15 to 45 million years old) with a mass totaling some 2 billon Suns.
Left: Portion of the Gemini spectrum of PS1-11bam from December 5 containing several interstellar absorption features of Fe II and Mg II at z = 1.566 (black). The error spectrum is shown in blue. For comparison we plot the GRB composite spectrum of Christensen et al. (2011). Right: A zoom-in on the relevant Fe II and Mg II lines demonstrates the similarity to GRB absorption spectra. Also shown is the [O II]3727 emission line at z = 1.567 from the January 1 Gemini spectrum.
The ultra-luminous supernova explosion belongs to a relatively recently-identified and special breed of exploding stars. They are some 10-100 times more luminous than their ordinary less-energetic cousins and unusually blue in color. While the process leading to their demise is still being explored, evidence points to the central core-collapse of a star having as much as 100 times the mass of our Sun. The collapse triggers an enormous explosion that blasts prodigious amounts of heavier elements through the star’s enormous outer layers before expanding into space.
Traditionally, astronomers have used two techniques to study distant galaxies: They would either; 1) look directly for chemical elements leaving bright imprints on the galaxy’s spectrum of light; or 2) search indirectly for dark signatures in the spectrum of an even more distant quasar, which reveals chemical elements in an intervening system that have absorbed light along our line of sight.
Recently, astronomers have supplanted these methods with another: seeking dark absorption imprints in the afterglows of “gamma-ray bursts” (GRBs); these brief flashes are the brightest and most energetic explosions in the universe, but they fade away within hours. The method is also limited by the need for expensive Earth-orbiting satellites to first detect and pinpoint a burst’s location with precision before astronomers can make ground-based studies.
“The beauty of studying distant galaxies using ultra-luminous supernovae as a tool is that it eliminates the need for satellites and offers more time for study,” says Alicia Soderberg of Harvard University. “A typical ultra-luminous supernova can take several weeks to fade away.”
The study by Berger and his team provides the ﬁrst direct demonstration that ultra-luminous supernovae can serve as probes of distant galaxies. Their results suggest that with the future combination of large survey and spectroscopic telescopes ultra-luminous supernovae could be used to probe galaxies 90 percent of the way back to the Big Bang.
The Pan-STARRS Project is being led by the University of Hawai‘i Institute for Astronomy, and exploits the unique combination of superb observing sites and technical and scientific expertise available in Hawai‘i. Funding for the development of the observing system has been provided by the United States Air Force Research Laboratory. The PS1 Surveys have been made possible through contributions by the Institute for Astronomy, the University of Hawai‘i, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching. The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. Any opinions, findings, and conclusions or recommendations expressed in this article are those of the author(s), and do not necessarily reflect the views of the National Aeronautics and Space Administration.