6533b7d9fe1ef96bd126c1fe
RESEARCH PRODUCT
Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of the Swift/BAT6 complete sample of LGRBs
Patrick PetitjeanStefano CovinoJochen GreinerE. Le Floc'hSergio CampanaSamuel BoissierL. K. HuntS. D. VerganiAndrew J. LevanP. D'avanzoAlberto Fernández-sotoAlberto Fernández-sotoThomas KrühlerA. MelandriJ. JapeljMathieu PuechAndreja GombocDaniel A. PerleyTommaso VinciF. HammerHector FloresG. TagliaferriRuben SalvaterraF. Mannuccisubject
Stellar massMetallicityAstrophysics::High Energy Astrophysical PhenomenaPopulationgamma-ray burst: generalAstrophysicsAstrophysics::Cosmology and Extragalactic Astrophysics01 natural sciences0103 physical sciencesAstrophysics::Solar and Stellar Astrophysicseducation010303 astronomy & astrophysicsQCAstrophysics::Galaxy AstrophysicsQBPhysicseducation.field_of_study010308 nuclear & particles physicsStar formationAstronomy and AstrophysicsGalaxyStarsgalaxies: photometrySpace and Planetary Sciencegalaxies: star formationSpectral energy distributionAstrophysics::Earth and Planetary AstrophysicsGamma-ray burst[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]description
Aims: Long gamma-ray bursts (LGRBs) are associated with massive stars and are therefore linked to star formation. However, the conditions needed for the progenitor stars to produce LGRBs can affect the relation between the LGRB rate and star formation. By using the power of a complete LGRB sample, our long-term aim is to understand whether such a bias exists and, if it does, what its origin is. Methods: To reach our goal we use the Swift/BAT6 complete sample of LGRBs. In this first paper, we build the spectral energy distribution (SED) of the 14 z ⋆) from SED fitting. To investigate the presence of a bias in the LGRB-star formation relation we compare the stellar mass distribution of the LGRB host galaxies (i) with star-forming galaxies observed in deep surveys (UltraVISTA) within the same redshift limit; (ii) with semi-analytical models of the z th = 0.3-0.5 Z☉ is necessary to form a LGRB. Models without a metallicity threshold or with an extreme threshold of Zth = 0.1 Z☉ are excluded at z Conclusions: GRB hosts at z ☉) inferred by the comparison with the simulations can be a consequence of the particular conditions needed for the progenitor star to produce a GRB. Appendix A is available in electronic form at http://www.aanda.org
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2015-09-01 |