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A comparison between short GRB afterglows and AT2017gfo: shedding light on kilonovae properties

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arxiv 1901.05792 v3 pith:FAY37NPT submitted 2019-01-17 astro-ph.HE

A. Rossi , G. Stratta , E. Maiorano , D. Spighi , N. Masetti , E. Palazzi , A. Gardini , A. Melandri
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L. Nicastro E. Pian M. Branchesi M. Dadina V. Testa S. Brocato S. Benetti R. Ciolfi S. Covino V. D'Elia A. Grado L. Izzo A. Perego S. Piranomonte R. Salvaterra J. Selsing L. Tomasella S. Yang D. Vergani L. Amati J. B. Stephen
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keywords kilonovashortat2017gfoat2017gfo-likegrbsafterglowsbluefirst
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Multi-messenger astronomy received a great boost following the discovery of kilonova AT2017gfo, the optical counterpart of the gravitational wave source GW170817 associated with the short gamma-ray burst GRB 170817A. AT2017gfo was the first kilonova that could be extensively monitored in time both photometrically and spectroscopically. Previously, only few candidates have been observed against the glare of short GRB afterglows. In this work, we aim to search the fingerprints of AT2017gfo-like kilonova emissions in the optical/NIR light curves of 39 short GRBs with known redshift. For the first time, our results allow us to study separately the range of luminosity of the blue and red components of AT2017gfo-like kilonovae in short GRBs. In particular, the red component is similar in luminosity to AT2017gfo, while the blue kilonova can be more than 10 times brighter. Finally, we find further evidence to support all the claimed kilonova detections and we exclude an AT2017gfo-like kilonova in GRBs 050509B and 061201.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Gamma-ray burst progenitors revisited

    astro-ph.HE 2026-07 conditional novelty 6.0 of 10

    About 30–40% of long gamma-ray bursts at z<0.3 lack supernova emission and likely arise from compact object mergers, at rates comparable to short GRBs.

  2. Diversity of kilonova light curves

    astro-ph.HE 2019-08 conditional novelty 6.0 of 10

    Radiative transfer simulations show that kilonova peak brightness and time in optical and near-infrared bands can distinguish prompt-collapse, magnetar-accelerated, and black hole-neutron star merger ejecta.

  3. Electromagnetic counterparts of black hole-neutron star mergers: dependence on the neutron star properties

    astro-ph.HE 2019-08 conditional novelty 5.0 of 10

    Predictions of BHNS kilonova and afterglow light curves show that low-mass neutron stars produce brighter EM counterparts and that the blue B-band deficit can distinguish BHNS from NSNS mergers.

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