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    Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes

    Access Status
    Fulltext not available
    Authors
    Anderson, Gemma
    Bland, Philip
    Booler, Tom
    Crosse, Brian
    Cupák, Martin
    de Gois, J.S.
    Devillepoix, Hadrien
    Emrich, David
    Franzen, Thomas
    Hancock, Paul
    Hartig, Ben
    Horsley, L.
    Howie, Robert
    Kenney, David
    Paxman, Jonathan
    Sansom, Eleanor
    Shannon, Ryan
    Sokolowski, Marcin
    Steele, K.
    Tingay, Steven
    Towner, Martin
    Trott, Cathryn
    Walker, Mia
    Wayth, Randall
    Williams, Andrew
    Date
    2017
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Andreoni, 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.
    Source Title
    Publications of the Astronomical Society of Australia
    DOI
    10.1017/pasa.2017.65
    ISSN
    1323-3580
    School
    Curtin Institute of Radio Astronomy (Physics)
    Remarks

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

    URI
    http://hdl.handle.net/20.500.11937/61575
    Collection
    • Curtin Research Publications
    Abstract

    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.

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