Examinando por Autor "Bechtol K."

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    Designing an Optimal Kilonova Search Using DECam for Gravitational-wave Events
    (Institute of Physics, 2024-02) Bom C.R.; Annis J.; Garcia A.; Palmese A.; Sherman N.; Soares-Santos M.; Santana-Silva L.; Morgan R.; Bechtol K.; Davis T.; Diehl H.T.; Allam S.S.; Bachmann T.G.; Fraga B.M.O.; García-Bellido J.; Gill M.S.S.; Herner K.; Kilpatrick C.D.; Makler M.; Olivares E. F.; Pereira M.E.S.; Pineda J.; Santos A.; Tucker D.L.; Wiesner M.P.; Aguena M.; Alves O.; Bacon D.; Bernardinelli P.H.; Bertin E.; Bocquet S.; Brooks D.; Carrasco Kind M.; Carretero J.; Conselice C.; Costanzi M.; da Costa L.N.; De Vicente J.; Desai S.; Doel P.; Everett S.; Ferrero I.; Frieman J.; Gatti M.; Gerdes D.W.; Gruen D.; Gruendl R.A.; Gutierrez G.; Hinton S.R.; Hollowood D.L.; Honscheid K.; James D.J.; Kuehn K.; Kuropatkin N.; Melchior P.; Mena-Fernández J.; Menanteau F.; Pieres A.; Plazas Malagón A.A.; Raveri M.; Rodriguez-Monroy M.; Sanchez E.; Santiago B.; Sevilla-Noarbe I.; Smith M.; Suchyta E.; Swanson M.E.C.; Tarle G.; To C.; Weaverdyck N.
    We address the problem of optimally identifying all kilonovae detected via gravitational-wave emission in the upcoming LIGO/Virgo/KAGRA observing run, O4, which is expected to be sensitive to a factor of ∼7 more binary neutron star (BNS) alerts than previously. Electromagnetic follow-up of all but the brightest of these new events will require >1 m telescopes, for which limited time is available. We present an optimized observing strategy for the DECam during O4. We base our study on simulations of gravitational-wave events expected for O4 and wide-prior kilonova simulations. We derive the detectabilities of events for realistic observing conditions. We optimize our strategy for confirming a kilonova while minimizing telescope time. For a wide range of kilonova parameters, corresponding to a fainter kilonova compared to GW170817/AT 2017gfo, we find that, with this optimal strategy, the discovery probability for electromagnetic counterparts with the DECam is ∼80% at the nominal BNS gravitational-wave detection limit for O4 (190 Mpc), which corresponds to an ∼30% improvement compared to the strategy adopted during the previous observing run. For more distant events (∼330 Mpc), we reach an ∼60% probability of detection, a factor of ∼2 increase. For a brighter kilonova model dominated by the blue component that reproduces the observations of GW170817/AT 2017gfo, we find that we can reach ∼90% probability of detection out to 330 Mpc, representing an increase of ∼20%, while also reducing the total telescope time required to follow up events by ∼20%. © 2024. The Author(s). Published by the American Astronomical Society.