High Metallicity LGRB Hosts

J. F. Graham; A. S. Fruchter; E. M. Levesque; L. J. Kewley; N. R. Tanvir; A. J. Levan; S. K. Patel; K. Misra; K. -H. Huang; D. E. Reichart; M. Nysewander; P. Schady

arXiv · 1511.00667

High Metallicity LGRB Hosts

J. F. Graham·A. S. Fruchter·E. M. Levesque·L. J. Kewley·N. R. Tanvir·A. J. Levan·S. K. Patel·K. Misra·K. -H. Huang·D. E. Reichart·M. Nysewander·P. Schady

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Abstract

We present our imaging and spectroscopic observations of the host galaxies of two dark long bursts with anomalously high metallicities, LGRB 051022 and LGRB 020819B, which in conjunction with another LGRB event with an optical afterglow comprise the three LGRBs with high metallicity host galaxies in the Graham & Fruchter (2013) sample. In Graham & Fruchter (2013), we showed that LGRBs exhibit a strong and apparently intrinsic preference for low metallicity environments (12+log(O/H) < 8.4 in the KK04 scale) in spite of these three cases with abundances of about solar and above. These exceptions however are consistent with the general star-forming galaxy population of comparable brightness & redshift. This is surprising: even among a preselected sample of high metallicity LGRBs, were the metal aversion to remain in effect for these objects, we would expect their metallicity to still be lower than the typical metallicity for the galaxies at that luminosity and redshift. Therefore we deduce that it is possible to form an LGRB in a high metallicity environment although with greater rarity. From this we conclude that there are three possible explanations for the presence of the LGRBs observed in high metallicity hosts as seen to date: (1) LGRBs do not occur in high metallicity environments and those seen in high metallicity hosts are in fact occurring in low metallicity environments that have become associated with otherwise high metallicity hosts but remain unenriched. (2) The LGRB formation mechanism while preferring low metallicity environments does not strictly require it resulting in a gradual decline in burst formation with increasing metallicity. (3) The typical low metallicity LGRBs and the few high metallicity cases are the result of physically different burst formation pathways with only the former affected by the metallicity and the later occurring much more infrequently.

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J. F. Graham, A. S. Fruchter, E. M. Levesque, L. J. Kewley, N. R. Tanvir, A. J. Levan, S. K. Patel, K. Misra, K. -H. Huang, D. E. Reichart, M. Nysewander, P. Schady. 2015-11-02. High Metallicity LGRB Hosts. https://arxiv.org/abs/1511.00667

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