Physics and Astronomy Faculty Publications and Presentations
Document Type
Article
Publication Date
3-2025
Abstract
The discovery of the optical/infra-red counterpart (AT2017gfo) to the binary neutron star gravitational-wave detection (GW170817), which was followed by a short gamma-ray burst (GRB 170817), marked a groundbreaking moment in multi-messenger astronomy. To date, it remains the only confirmed joint detection of its kind. However, many experiments are actively searching for similar fast-fading electromagnetic counterparts, known as kilonovae. Fortunately, the Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST) provides excellent prospects for identifying kilonova candidates either from, or independent of, gravitational-wave and GRB triggers. Cadence choices for LSST surveys are especially important for maximising the likelihood of kilonovae detections. In this work, we explore the possibility of optimizing Rubin Observatory's ability to detect kilonovae by implementing a fast transient metric shown to be successful with an existing wide field survey, e.g., the Zwicky Transient Facility. We study existing LSST cadences, how detection rates are affected by filter selections, the return timescales for visits of the same area in the sky, and other relevant factors. Through our analysis, we have found that employing baseline cadences and utilizing triplet families like presto_gap produced the highest likelihood of kilonova detection.
Recommended Citation
Andrade, Cristina, Raiyah Alserkal, Luis Salazar Manzano, Emma Martin, Igor Andreoni, Michael W. Coughlin, Nidhal Guessoum, and Liliana Rivera Sandoval. "The Effect of Vera C. Rubin Observatory Cadence Selections on Kilonova Detectability." Publications of the Astronomical Society of the Pacific 137, no. 3 (2025): 034102. https://doi.org/10.1088/1538-3873/adbfbc
Creative Commons License
This work is licensed under a Creative Commons Attribution 4.0 International License.
Publication Title
Publications of the Astronomical Society of the Pacific
DOI
10.1088/1538-3873/adbfbc
Comments
© 2025. The Author(s)
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