Designing an Optimal Kilonova Search Using DECam for Gravitational-wave Events

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dc.contributor.authorBom C.R.
dc.contributor.authorAnnis J
dc.contributor.authorGarcia A.
dc.contributor.authorPalmese A.
dc.contributor.authorSherman N.
dc.contributor.authorSoares-Santos M.
dc.contributor.authorSantana-Silva L
dc.contributor.authorMorgan R.
dc.contributor.authorBechtol K
dc.contributor.authorDavis T.
dc.contributor.authorDiehl H.T.
dc.contributor.authorAllam S.S.
dc.date.accessioned2025-04-10T17:01:25Z
dc.date.available2025-04-10T17:01:25Z
dc.date.issued0024
dc.descriptionINDEXACION SCOPUS
dc.description.abstractWe 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
dc.identifier.issn0004637X
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/64126
dc.language.isoen
dc.publisherInstitute of Physics
dc.subjectNeutron Stars; Gravitational Wave; Circumstellar Disk
dc.titleDesigning an Optimal Kilonova Search Using DECam for Gravitational-wave Events
dc.typeArtículo
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