The dark side of nature: The crime was almost perfect

December 20, 2006

Nature has again thrown astronomers for a loop. Just when they thought they understood how gamma-ray bursts formed, they have uncovered what appears to be evidence for a new kind of cosmic explosion. These seem to arise when a newly born black hole swallows most of the matter from its doomed parent star.

Gamma-ray bursts (GRBs), the most powerful explosions in the Universe, signal the formation of a new black hole and come in two flavours, long and short ones. In recent years, international efforts have shown that long gamma-ray bursts are linked with the explosive deaths of massive stars (hypernovae; see e.g. ESO PR 16/03).

Last year, observations by different teams - including the GRACE and MISTICI collaborations that use ESO's telescopes - of the afterglows of two short gamma-ray bursts provided the first conclusive evidence that this class of objects most likely originates from the collision of compact objects: neutron stars or black holes (see ESO PR 26/05 and ESO PR 32/05).

The newly found gamma-ray bursts, however, do not fit the picture. They instead seem to share the properties of both the long and short classes.

"Some unknown process must be at play, about which we have presently no clue," said Massimo Della Valle of the Osservatorio Astrofisico di Arcetri in Firenze, Italy, lead author of one of the reports published in this week's issue of the journal Nature. "Either it is a new kind of merger which is able to produce long bursts, or a new kind of stellar explosion in which matter can't escape the black hole."

One of the mysterious events went bang on 14 June 2006, hence its name, GRB 060614. The gamma-ray burst lasted 102 seconds and belongs clearly to the category of long GRBs. As it happened in a relatively close-by galaxy, located only 1.6 billion light-years away in the constellation Indus, astronomers worldwide eagerly pointed their telescopes toward it to capture the supernova, watching and waiting as if for a jack-in-the-box to spring open.

The MISTICI collaboration used ESO's Very Large Telescope to follow the burst for 50 days. "Despite our deep monitoring, no rebrightening due to a supernova was seen," said Gianpiero Tagliaferri from the Observatory of Brera, Italy and member of the team. "If a supernova is present, if should at least be 100 times fainter than any other supernova usually associated with a long burst."

The burst exploded in a dwarf galaxy that shows moderate signs of star formation. Thus young, massive stars are present and, at the end of its life one of them could have uttered this long, agonising cry before vanishing into a black hole. "Why did it do so in a dark way, with no sign of a supernova"" asked Guido Chincarini, from the University of Milano-Bicocca, Italy, also member of the team. "A possibility is that a massive black hole formed that did not allow any matter to escape. All the material that is usually ejected in a supernova explosion would then fall back and be swallowed."

The same conclusion was previously reached by another team, who monitored both GRB 060614 and another burst, GRB 060505 (5 May 2006) for 5 and 12 weeks, respectively. For this, they used the ESO VLT and the 1.54-m Danish telescope at La Silla.

GRB 060505 was a faint burst with a duration of 4 seconds, and as such also belongs to the category of long bursts.

For GRB 060505, the astronomers could only see the burst in visible light for one night and then it faded away, while for GRB 060614, they could only follow it for four nights after the burst. Thus, if supernovae were associated with these long-bursts, as one would have expected, they must have been about a hundred times fainter than a normal supernova.

"Although both bursts are long, the remarkable conclusion from our monitoring is that there were no supernovae associated with them," said Johan Fynbo from the DARK Cosmology Centre at the Niels Bohr Institute of the Copenhagen University in Denmark, who led the study. "It is a bit like not hearing the thunder from a nearby storm when one could see a very long lasting flash."

For the May burst, the team has obtained deep images in very good observing conditions allowing the exact localisation of the burst in its host galaxy. The host galaxy turns out to be a small spiral galaxy, and the burst occurred in a compact star-forming region in one of the spiral arms of the galaxy. This is strong evidence that the star that made the GRB was massive.

"For the 5 May event, we have evidence that it was due to a massive star that died without making a supernova," said Fynbo. "We now have to find out what is the fraction of massive stars that die without us noticing, that is, without producing either a gamma-ray burst or a supernova."

"Whatever the solution to the problem is, it is clear that these new results challenge the commonly accepted scenario, in which long bursts are associated with a bright supernova," said Daniele Malesani, from the International School for Advanced Studies in Trieste, and now also at the DARK Cosmology Centre. "Our hope is to be able to find more of these unconventional bursts. The chase is on!"
More Information

The two gamma-ray bursts were discovered with the NASA/ASI/PPARC Swift satellite, which is dedicated to the discovery of these powerful explosions.

The work presented here is published in the 21 December 2006 issue of the journal Nature: "No supernovae associated with two long-duration gamma-ray bursts", by Johan P. U. Fynbo et al., and "An enigmatic long-lasting gamma-ray burst not accompanied by a bright supernova", by Massimo Della Valle et al. Two other reports about the same events are published in the same issue of Nature.

The Italian-led team - the MISTICI collaboration - is composed of Massimo Della Valle (INAF, Osservatorio Astrofisico di Arcetri, Italy), Guido Chincarini (INAF, Osservatorio Astronomico di Brera & Università degli Studi di Milano-Bicocca, Italy), Nino Panagia (Space Telescope Science Institute, USA), Gianpiero Tagliaferri, Dino Fugazza, Sergio Campana, Stefano Covino, Paolo D'Avanzo, and Paolo D'Avanzo (INAF, Osservatorio Astronomico di Brera, Italy), Daniele Malesani (SISSA/ISAS, Italy and Dark Cosmology Centre, Copenhagen), Vincenzo Testa, L. Angelo Antonelli, Silvia Piranomonte, and Luigi Stella (INAF, Osservatorio Astronomico di Roma, Italy), Vanessa Mangano (INAF/IASF Palermo, Italy), K. Hurley (University of California, Berkeley, USA), I. Felix Mirabel (ESO), and Leonardo J. Pellizza (Instituto de Astronomia y Fisica del Espacio).

The Danish-led team is composed of Johan P. U. Fynbo, Darach Watson, Christina C. Thöne, Tamara M. Davis, Jens Hjorth, José Mar"á Castro Cerón, Brian L. Jensen, Maximilian D. Stritzinger, and Dong Xu (Dark Cosmology Centre, University of Copenhagen, Denmark), Jesper Sollerman (Dark Cosmology Centre and Department of Astronomy, Stockholm University, Sweden), Uffe G. Jørgensen, Tobias C. Hinse, and Kristian G. Woller (Niels Bohr Institute, University of Copenhagen), Joshua S. Bloom, Daniel Kocevski, Daniel Perley (Department of Astronomy, University of California at Berkeley, USA), Páll Jakobsson (Centre for Astrophysics Research, University of Hertfordshire, UK), John F. Graham and Andrew S. Fruchter (Space Telescope Science Institute, Baltimore, USA), David Bersier (Astrophysics Research Institute, Liverpool John Moores University, UK), Lisa Kewley (University of Hawaii, Institute of Astronomy, USA), Arnaud Cassan and Marta Zub (Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Germany), Suzanne Foley (School of Physics, University College Dublin, Ireland), Javier Gorosabel (Instituto de Astrofisica de Andalucia, Granada, Spain), Keith D. Horne (12SUPA Physics/Astronomy, University of St Andrews, Scotland, UK), Sylvio Klose (Thüringer Landessternwarte Tautenburg, Germany), Jean-Baptiste Marquette (Institut d'Astrophysique de Paris, France), Enrico Ramirez-Ruiz (Institute for Advanced Study, Princeton and Department of Astronomy and Astrophysics, University of California, Santa Cruz, USA), Paul M. Vreeswijk (ESO and Departamento de Astronomia, Universidad de Chile, Santiago, Chile), and Ralph A. M. Wijers (Astronomical Institute 'Anton Pannekoek', University of Amsterdam, The Netherlands).



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