Spatially Resolved Properties of the GRB 060505 Host: Implications for the Nature of the Progenitor

Christina C. Thöne, Johan P. U. Fynbo, Göran Östlin, Bo Milvang-Jensen, Klaas Wiersema, Daniele Malesani, Desiree Della Monica Ferreira, Javier Gorosabel, D. Alexander Kann, Darach Watson, Michal Michalowski, Andrew S. Fruchter, Andrew J. Levan, Jens Hjorth, Jesper Sollerman

Research output: Contribution to journalArticlepeer-review

Abstract / Description of output

GRB 060505 was the first well-observed nearby possible long-duration gamma-ray burst (GRB) that had no associated supernova. Here we present spatially resolved spectra of the host galaxy of GRB 060505, an Sbc spiral, at redshift z=0.0889. The GRB occurred inside a star-forming region in the northern spiral arm at 6.5 kpc from the center. From the position of the emission lines, we determine a maximum rotational velocity for the galaxy of v~212 km s-1, corresponding to a mass of 1.14×1011 Msolar within 11 kpc from the center. By fitting single-age spectral synthesis models to the stellar continuum, we derive a very young age for the GRB site, confirmed by photometric and Hα line measurements, of around ~6 Myr, which corresponds to the lifetime of a 32 Msolar star. The metallicity derived from several emission-line measurements varies throughout the galaxy and is lowest at the GRB site. Using the Two Degree Field Galaxy Redshift Survey we can locate the host galaxy in its large-scale (~Mpc) environment. The galaxy lies in the foreground of a filamentary overdensity, extending southwest from the galaxy cluster Abell 3837 at z=0.0896. The properties of the GRB site are similar to those found for other long-duration GRB host galaxies with high specific star formation rate and low metallicity, which is an indication that GRB 060505 originated from a young, massive star that died without making a supernova. Based on ESO-ToO proposal 077.D-0661 and ESO-LP proposal 177.A-0591.
Original languageEnglish
Pages (from-to)1151-1161
JournalAstrophysical Journal
Publication statusPublished - 1 Apr 2008


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