On Oct. 20, 2004, Japanese amateur astronomer Koichi Itagaki saw the star let loose an outburst so bright that it was initially mistaken for a supernova. The star survived, but for only two years. On Oct. 11, 2006, professional and amateur astronomers witnessed the star actually blowing itself to smithereens as Supernova 2006jc.

“We have never observed a stellar outburst and then later seen the star explode,” says University of California, Berkeley, astronomer Ryan Foley. His group studied the event with ground-based telescopes, including the 10-meter (32.8-foot) W. M. Keck telescopes in Hawaii. Narrow helium spectral lines showed that the supernova’s blast wave ran into a slow-moving shell of material, presumably the progenitor’s outer layers ejected just two years earlier. If the spectral lines had been caused by the supernova’s fast-moving blast wave, the lines would have been much broader.

Another group, led by Stefan Immler of NASA’s Goddard Space Flight Center, Greenbelt, Md., monitored SN 2006jc with NASA’s Swift satellite and Chandra X-ray Observatory. By observing how the supernova brightened in X-rays, a result of the blast wave slamming into the outburst ejecta, they could measure the amount of gas blown off in the 2004 outburst: about 0.01 solar mass, the equivalent of about 10 Jupiters.

“The beautiful aspect of our SN 2006jc observations is that although they were obtained in different parts of the electromagnetic spectrum, in the optical and in X-rays, they lead to the same conclusions,” says Immler.

“This event was a complete surprise,” added Alex Filippenko, leader of the UC Berkeley/Keck supernova group and a member of NASA’S Swift team. “It opens up a fascinating new window on how some kinds of stars die.”

All the observations suggest that the supernova’s blast wave took only a few weeks to reach the shell of material ejected two years earlier, which did not have time to drift very far from the star. As the wave smashed into the ejecta, it heated the gas to millions of degrees, hot enough to emit copious X-rays. The Swift satellite saw the supernova continue to brighten in X-rays for 100 days, something that has never been seen before in a supernova. All supernovae previously observed in X-rays have started off bright and then quickly faded to invisibility.

“You don’t need a lot of mass in the ejecta to produce a lot of X-rays,” notes Immler. Swift’s ability to monitor the supernova’s X-ray rise and decline over six months was crucial to his team’s mass determination. But he adds that Chandra’s sharp resolution enabled his group to resolve the supernova from a bright X-ray source that appears in the field of view of Swift’s X-ray Telescope.

“We could not have made this measurement without Chandra,” says Immler, who will submit his team’s paper next week to the Astrophysical Journal. “The synergy between Swift’s fast response and its ability to observe a supernova every day for a long period, and Chandra’s high spatial resolution, is leading to a lot of interesting results.”

Foley and his colleagues, whose paper appears in the March 10 Astrophysical Journal Letters, propose that the star recently transitioned from a Luminous Blue Variable (LBV) star to a Wolf-Rayet star. An LBV is a massive star in a brief but unstable phase of stellar evolution. Similar to the 2004 eruption, LBVs are prone to blow off large amounts of mass in outbursts so extreme that they are frequently mistaken for supernovae, events dubbed “supernova impostors.” Wolf-Rayet stars are hot, highly evolved stars that have shed their outer envelopes.

Most astronomers did not expect that a massive star would explode so soon after a major outburst, or that a Wolf-Rayet star would produce such a luminous eruption, so SN 2006jc represents a puzzle for theorists.

“It challenges some aspects of our current model of stellar evolution,” says Foley. “We really don’t know what caused this star to have such a large eruption so soon before it went supernova.”

“SN 2006jc provides us with an important clue that LBV-style eruptions may be related to the deaths of massive stars, perhaps more closely than we used to think,” adds coauthor and UC Berkeley astronomer Nathan Smith. “The fact that we have no well-established theory for what actually causes these outbursts is the elephant in the living room that nobody is talking about.”

SN 2006jc occurred in galaxy UGC 4904, located 77 million light years from Earth in the constellation Lynx. The supernova explosion, a peculiar variant of a Type Ib, was first sighted by Itagaki, American amateur astronomer Tim Puckett and Italian amateur astronomer Roberto Gorelli.

NOTE: Ryan Foley may be reached at 1-510-643-8593 (office); 1-510-388-3364 (cell); or rfoley@astro.berkeley.edu. Stefan Immler is at 1-301-286-0072 (office); 1-240-281-6208 (cell); or immler@milkyway.gsfc.nasa.gov. Alex Filippenko can be reached at 1-510-642-1813 (office); 1-510-852-4829 (cell); or alex@astro.berkeley.edu. Nathan Smith is at 1-510-642-6931 or nathans@astro.berkeley.edu.


A Lick Observatory image of the supernova and a graphic explaining the double whammy are at: http://www.berkeley.edu/news/media/download/

Caption for SN2006jc_Lick.jpg: A color image of SN2006jc (center) taken by the Katzman Automatic Imaging Telescope (KAIT) at Lick Observatory on Oct. 13, 2006. The smudge to the upper left of the supernova is the visible part of the galaxy in which it occurred, UGC 4904, located 77 million light years from Earth. Credit: Mohan Ganeshalingam, Alex Filippenko & Weidong Li/UC Berkeley/KAIT/Lick Observatory

Caption for sn2006jcstrip.jpg: This artistic rendering depicts two years in the life of a massive blue supergiant star, which burped and spewed a shell of gas, then, two years later, exploded. When the supernova slammed into the shell of gas, X-rays were produced.

Credit: Aurore Simonnet/Sonoma State University, NASA Education & Public Outreach

Chandra and Swift images are at:

http://lheawww.gsfc.nasa.gov/users/immler/SN2006jc/SN2006jc_UVOT_scalebar.jpg Caption for SN2006jc_UVOT_scalebar.jpg: The Ultraviolet/Optical Telescope aboard NASA’s Swift satellite monitored the brightening and fading of SN 2006jc, a very peculiar supernova whose original star had a large outburst just two years before it met its explosive end. Credit: NASA/Swift/Stefan Immler (NASA/GSFC)

http://lheawww.gsfc.nasa.gov/users/immler/SN2006jc/SN2006jc_XRT_scalebar.jpg Caption for SN2006jc_XRT_scalebar.jpg: The X-ray Telescope aboard NASA’s Swift satellite captured SN 2006jc as it brightened over a period of 100 days. The brightening was due to the supernova’s blast wave plowing through gas ejected by the original star two years before it exploded. Credit: NASA/Swift/Stefan Immler (NASA/GSFC)

http://lheawww.gsfc.nasa.gov/users/immler/SN2006jc/SN2006jc_Chandra_scalebar.jpg Caption for SN2006jc_Chandra_scalebar.jpg: NASA’s Chandra X-ray Observatory pinpointed SN2006jc’s location (lower right) near three other bright X-ray sources, all of them apparently within the same galaxy, UGC 4904, that hosted SN2006jc. The image gives the same field as the Swift UVOT and Swift XRT images.

Credit: NASA/CXC/Stefan Immler (NASA/GSFC)

See NASA Goddard press release at http://www.nasa.gov/centers/goddard/news/topstory/2007/supernova_imposter.html

For more information about NASA’s Swift satellite, please visit on the Web: http://www.nasa.gov/mission_pages/swift/main/index.html

Fore more information about the Chandra X-ray Observatory, please visit on the Web: http://chandra.harvard.edu/