Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of LGRBs

Abstract

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 < 1 host galaxies of the BAT6 LGRB sample and determine their stellar masses (M ) 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 < 1 star-forming galaxy population; and (iii) with dedicated numerical simulations of LGRB hosts having different metallicity thresholds for the progenitor star environment. Results. We find that at z < 1, LGRBs tend to avoid massive galaxies and are very powerful for selecting a population of faint low-mass star-forming galaxies, partly below the completeness limits of galaxy surveys. The stellar mass distribution of the hosts is not consistent with that of the UltraVISTA star-forming galaxies weighted by their star formation rate (SFR). This implies that, at least at z < 1, LGRBs are not unbiased tracers of star formation. To make the two distributions consistent, a much steeper faint end of the mass function would be required or a very shallow SFR-mass relation for the low-mass galaxy population. The comparison with the GRB host galaxy simulations indicates that, to reproduce the stellar mass distribution, a metallicity threshold of the order of Z th = 0.3−0.5 Z is necessary to form a LGRB. Models without a metallicity threshold or with an extreme threshold of Z th = 0.1 Z are excluded at z < 1. Under a very basic assumption, we estimate that the LGRB rate can directly trace the SFR starting from z ∼ 4 and above. Conclusions. GRB hosts at z < 1 have lower luminosities and stellar masses than expected if LGRBs were unbiased star formation tracers. The use of the Swift/BAT6 complete sample keeps this result from being affected by possible biases that could have influenced past results based on incomplete samples. The preference for low metallicities (Z 0.5 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.Key words. gamma-ray burst: general -galaxies: star formation -galaxies: photometry Appendix A is available in electronic form at http://www.aanda.orgArticle published by EDP Sciences A102, page 1 of 13 A&A 581, A102 (2015)

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

“…Vergani et al (2015) found that z < 1 LGRBs preferentially select faint, low-mass star-forming galaxies and are not unbiased tracers of star formation at z < 1. To better understand the interdependency of key properties of galaxies hosting LGRBs, here we expand the work of Vergani et al (2015) by studying the emission line spectra of the hosts in the complete sample. Using the emission line fluxes, we measure the star formation rates and metallicities of the BAT6 sample hosts (Sect.…”

“…Our sample is the same as presented in Vergani et al (2015) and is composed of 14 z < 1 LGRBs of the Swift/BAT6 sample . Because it is difficult to maintain a high level of GRB host data completeness at high redshifts A129, page 2 of 15 Notes.…”

“…LGRB hosts at z < 1 are also found to be fainter and of lower stellar mass than a field star-forming galaxy population (see also Vergani et al 2015;Perley et al 2013Perley et al , 2016b. Because the stellar mass and metallicity of star-forming galaxies are correlated (stellar massmetallicity relation, Tremonti et al 2004), the low-metallicity preference could provide the explanation for the differences in observed stellar masses between populations.…”

“…The selection requirements do not depend on the brightness of optical afterglows, ensuring that the sample contains the entire LGRB population, including dark LGRBs (Melandri et al 2012). Vergani et al (2015) found that z < 1 LGRBs preferentially select faint, low-mass star-forming galaxies and are not unbiased tracers of star formation at z < 1. To better understand the interdependency of key properties of galaxies hosting LGRBs, here we expand the work of Vergani et al (2015) by studying the emission line spectra of the hosts in the complete sample.…”

“…Recently, Vergani et al (2015) presented a study on the photometry and stellar masses of the z < 1 LGRB host galaxies of the Swift/BAT6 complete sample of bright LGRBs. The Swift/BAT6 sample ) is selected according to favourable observing conditions (Jakobsson et al 2006) to avoid a biased selection.…”