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      GW190814 follow-up with the optical telescope MeerLICHT

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      Creators
      Wet, S. de
      Groot, P.J.
      Bloemen, S.
      Poole, R. Le
      Klein-Wolt, M.
      Körding, E.
      McBride, V.
      Paterson, K.
      Pieterse, D.L.A.
      Vreeswijk, P.M.
      Woudt, P.
      Date of Archiving
      2021
      Archive
      ViZieR
      Related links
      http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/649/A72
      Related publications
      GW190814 follow-up with the optical telescope MeerLICHT⋆  
      Publication type
      Dataset
      Access level
      Open access
      Please use this identifier to cite or link to this item: https://hdl.handle.net/2066/234447   https://hdl.handle.net/2066/234447
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      Organization
      Astrophysics
      Audience(s)
      Astronomy, astrophysics
      Key words
      gravitational waves; stars: black holes; stars: neutron
      Abstract
      The Advanced LIGO and Virgo gravitational wave observatories detected a signal on 2019 August 14 during their third observing run, named GW190814. A large number of electromagnetic facilities conducted follow-up campaigns in the search for a possible counterpart to the gravitational wave event, which was made especially promising given the early source classification of a neutron star-black hole merger. Aims. We present the results of the GW follow-up campaign taken with the wide-field optical telescope MeerLICHT, located at the South African Astronomical Observatory Sutherland site. We use our results to constrain possible kilonova models. Methods. The MeerLICHT telescope observed more than 95% of the probability localisation each night for over a week in three optical bands (u, q, i) with our initial observations beginning almost two hours after the GW detection. We describe the search for new transients in MeerLICHT data and investigate how our limiting magnitudes can be used to constrain an AT2017gfo-like kilonova. Results. A single new transient was found in our analysis of MeerLICHT data, which we exclude from being the electromagnetic counterpart to GW190814 owing to the existence of a spatially unresolved source at the coordinates of the transient in archival data. Using our limiting magnitudes, the confidence with which we can exclude the presence of an AT2017gfo-like kilonova at the distance of GW190814 was low (<10–4).
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