A comparison between short GRB afterglows and KN170817: shedding light on kilonovae properties. (arXiv:1901.05792v1 [astro-ph.HE])

A comparison between short GRB afterglows and KN170817: shedding light on kilonovae properties. (arXiv:1901.05792v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rossi_A/0/1/0/all/0/1">A. Rossi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stratta_G/0/1/0/all/0/1">G. Stratta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maiorano_E/0/1/0/all/0/1">E. Maiorano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spighi_D/0/1/0/all/0/1">D. Spighi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masetti_N/0/1/0/all/0/1">N. Masetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palazzi_E/0/1/0/all/0/1">E. Palazzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gardini_A/0/1/0/all/0/1">A. Gardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melandri_A/0/1/0/all/0/1">A. Melandri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nicastro_L/0/1/0/all/0/1">L. Nicastro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pian_E/0/1/0/all/0/1">E. Pian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Branchesi_M/0/1/0/all/0/1">M. Branchesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dadina_M/0/1/0/all/0/1">M. Dadina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Testa_V/0/1/0/all/0/1">V. Testa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brocato_S/0/1/0/all/0/1">S. Brocato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benetti_S/0/1/0/all/0/1">S. Benetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciolfi_R/0/1/0/all/0/1">R. Ciolfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Covino_S/0/1/0/all/0/1">S. Covino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DElia_V/0/1/0/all/0/1">V. D'Elia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grado_A/0/1/0/all/0/1">A. Grado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Izzo_L/0/1/0/all/0/1">L. Izzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perego_A/0/1/0/all/0/1">A. Perego</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piranomonte_S/0/1/0/all/0/1">S. Piranomonte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salvaterra_R/0/1/0/all/0/1">R. Salvaterra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Selsing_J/0/1/0/all/0/1">J. Selsing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tomasella_L/0/1/0/all/0/1">L. Tomasella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_S/0/1/0/all/0/1">S. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vergani_D/0/1/0/all/0/1">D. Vergani</a>

Multi-messenger astronomy started with the discovery of kilonova AT2017gfo,
the optical counterpart of GW170817 and of the short GRB 170817A. This was also
the first time that a kilonova could be followed up spectroscopically. In this
work, we aim at searching the fingerprints of AT2017gfo-like kilonova emissions
in the optical/NIR light curves of selected short GRBs. We used the
spectroscopic and photometric data-set of AT2017gfo to build rest-frame
spectral templates of the kilonova. Afterwards we compared these templates with
light curves of 39 short GRBs with known redshift. We could establish empirical
constraints on the existence of AT2017gfo-like kilonovae in previously observed
short GRBs posing limits to the kilonova emission mechanism. Moreover, we find
further supporting evidence to all claimed kilonova detections and seven new
possible kilonovae associated with short GRBs.

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