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dc.contributor.authorAnderson, Gemma
dc.contributor.authorBland, Philip
dc.contributor.authorBooler, Tom
dc.contributor.authorCrosse, Brian
dc.contributor.authorCupák, Martin
dc.contributor.authorde Gois, J.S.
dc.contributor.authorDevillepoix, Hadrien
dc.contributor.authorEmrich, David
dc.contributor.authorFranzen, Thomas
dc.contributor.authorHancock, Paul
dc.contributor.authorHartig, Ben
dc.contributor.authorHorsley, L.
dc.contributor.authorHowie, Robert
dc.contributor.authorKenney, David
dc.contributor.authorPaxman, Jonathan
dc.contributor.authorSansom, Eleanor
dc.contributor.authorShannon, Ryan
dc.contributor.authorSokolowski, Marcin
dc.contributor.authorSteele, K.
dc.contributor.authorTingay, Steven
dc.contributor.authorTowner, Martin
dc.contributor.authorTrott, Cathryn
dc.contributor.authorWalker, Mia
dc.contributor.authorWayth, Randall
dc.contributor.authorWilliams, Andrew
dc.identifier.citationAndreoni, I. and Ackley, K. and Cooke, J. and Acharyya, A. and Allison, J. and Anderson, G. and Ashley, M. et al. 2017. Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes. Publications of the Astronomical Society of Australia. 34: Article ID e069.

The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (~2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor.

dc.publisherCambridge University Press
dc.titleFollow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes
dc.typeJournal Article
dcterms.source.titlePublications of the Astronomical Society of Australia

Lists Curtin authors only - please see the published version for a complete list of authors.

curtin.departmentCurtin Institute of Radio Astronomy (Physics)
curtin.accessStatusFulltext not available

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