Details

Autor(en) / Beteiligte

• Angelini, L
• Burrows, D. N
• Holland, S. T
• Starling, R
• Hill, J. E
• Willingale, R
• Cominsky, L. R
• Moretti, A
• de Pasquale, M
• Wijers, R. A. M. J
• Nakazawa, K
• Marshall, F. E
• Sarazin, C. L
• Meszaros, P
• Hurkett, C. P
• Kobayashi, S
• White, N. E
• Goad, M
• Palmer, D. M
• Chester, M. M
• Krimm, H. A
• Sato, G
• Tagliaferri, G
• Tueller, J
• Perri, M
• Gronwall, C
• Smale, A. P
• Page, K
• Levan, A
• Markwardt, C. B
• Barthelmy, S. D
• Barbier, L
• Mason, K. O
• Klose, S
• Kouveliotou, C
• Still, M
• Poole, T
• Rol, E
• Page, M
• O'Brien, P. T
• Hinshaw, D
• Fenimore, E. E
• Zhang, B
• Norris, J. P
• Romano, P
• Suzuki, M
• Cummings, J. R
• Chincarini, G
• Boyd, P. T
• Sakamoto, T
• Giommi, P
• Blustin, A
• Mushotzky, R. F
• Tashiro, M
• Patel, S
• Roming, P. W. A
• McGowan, K
• Parsons, A. M
• Grupe, D
• Mangano, V
• Hullinger, D
• Nousek, J. A
• Sollerman, J
• Hurley, K. C
• Campana, S
• Wells, A. A
• Osborne, J. P
• Schady, P
• Beardmore, A
• Rosen, S
• Gehrels, N
• Takahashi, T
• Breeveld, A
• Cannizzo, J
• Kennea, J. A
• Cusumano, G
• Hjorth, J

Titel

A short γ-ray burst apparently associated with an elliptical galaxy at redshift z = 0.225

Ist Teil von

• Nature, 2005-10, Vol.437 (7060), p.851-854

Ort / Verlag

London: Nature Publishing

Erscheinungsjahr

2005

Quelle

Psychology and Behavioral Sciences Collection

Beschreibungen/Notizen

• Gamma-ray bursts (GRBs) come in two classes: long (> 2 s), soft-spectrum bursts and short, hard events. Most progress has been made on understanding the long GRBs, which are typically observed at high redshift (z 1) and found in subluminous star-forming host galaxies. They are likely to be produced in core-collapse explosions of massive stars. In contrast, no short GRB had been accurately (< 10″) and rapidly (minutes) located. Here we report the detection of the X-ray afterglow from-and the localization of-the short burst GRB 050509B. Its position on the sky is near a luminous, non-star-forming elliptical galaxy at a redshift of 0.225, which is the location one would expect if the origin of this GRB is through the merger of neutron-star or black-hole binaries. The X-ray afterglow was weak and faded below the detection limit within a few hours; no optical afterglow was detected to stringent limits, explaining the past difficulty in localizing short GRBs.