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GW170817: Swift UV detection of a blue kilonova, and improving the search in O3

Published online by Cambridge University Press:  29 January 2019

Aaron Tohuvavohu
Affiliation:
Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: [email protected]
Jamie A. Kennea
Affiliation:
Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: [email protected]
the <span class='italic'>Swift</span> gravitational wave follow-up group
Affiliation:
Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: [email protected] Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: [email protected]
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Abstract

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Swift’s rapid slewing, flexible planning, and multi-wavelength instruments make it the most capable space-based follow-up engine for finding poorly localized sources. During O1 and O2 Swift successfully tiled hundreds of square-degrees of sky in the LVC localization regions, searching for, and identifying, possible X-ray and UV/O transients in the field. Swift made important contributions to the discovery and characterization of the kilonova AT 2017gfo, discovering the UV emission and providing the deepest X-ray upper limits in the first 24 hours after the trigger, strongly constraining the dynamics and geometry of the counterpart. Swift tiled 92% of the galaxy convolved error region down to average X-ray flux sensitivities of 10−12 erg cm−2 s−1, significantly increasing our confidence that AT 2017gfo is indeed the counterpart to GW 170817 and sGRB 170817. However, there remains significant room for improvement of Swift’s follow-up in preparation for O3. This will take the form of both revised observation strategy based on detailed analysis of the results from O2, and significant changes to Swift’s operational capabilities. These improvements are necessary both for maximizing the likelihood that Swift finds a counterpart, and minimizing the impact that follow-up activities have on other Swift science priorities. We outline areas of improvement to the observing strategy itself for optimal tiling of the LVC localization regions. We also discuss ongoing work on operational upgrades that will decrease latency in our response time, and minimize impact on pre-planned observations, while maintaining spacecraft health and safety.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2019 

References

Abbott, B. et al. 2017, ApJ 848, 2.Google Scholar
Coulter, D. et al. 2017, Gamma Ray Coordinates Network Circular 21529.Google Scholar
D’Avanzo, P. et al. 2014, MNRAS 442, 2342.Google Scholar
Evans, P. et al. 2012, ApJS 203, 28.Google Scholar
Evans, P. et al. 2016, MNRAS 462, 1591.Google Scholar
Evans, P. et al. 2017, Science, DOI: 10.1126/science.aap9580.Google Scholar
Gehrels, N. et al. 2004, ApJ 611, 1005Google Scholar
Kasliwal, M. et al. 2017, Science, DOI: 10.1126/science.aap9455.Google Scholar
Smartt, S. et al. 2017, Nature, DOI: 10.1038/nature24303.Google Scholar
The LIGO Scientific Collaboration, the Virgo Collaboration 2017, Gamma Ray Coordinates Network Circular 21505.Google Scholar
The LIGO Scientific Collaboration, the Virgo Collaboration 2017, Gamma Ray Coordinates Network Circular 21513.Google Scholar
Tohuvavohu, A. 2017, IOP: Proc. ACAT, submitted.Google Scholar
van der Horst, A. J. et al. 2009, ApJ 699 1087.Google Scholar