A search for radio emission from double-neutron star merger GW190425 using Apertif
Journal article, 2021
Context
Detection of the electromagnetic emission from coalescing binary neutron stars (BNS) is important for understanding the merger and afterglow. Aims. We present a search for a radio counterpart to the gravitational-wave (GW) source GW190425, a BNS merger, using Apertif on the Westerbork Synthesis Radio Telescope (WSRT).
Methods
We observed a field of high probability in the associated localisation region for three epochs at ΔTâ€., =â€., 68, 90, 109 d post merger. We identified all sources that exhibit flux variations consistent with the expected afterglow emission of GW190425. We also looked for possible transients. These are sources that are only present in one epoch. In addition, we quantified our ability to search for radio afterglows in the fourth and future observing runs of the GW detector network using Monte Carlo simulations.
Results
We found 25 afterglow candidates based on their variability. None of these could be associated with a possible host galaxy at the luminosity distance of GW190425. We also found 55 transient afterglow candidates that were only detected in one epoch. All of these candidates turned out to be image artefacts. In the fourth observing run, we predict that up to three afterglows will be detectable by Apertif.
Conclusions
While we did not find a source related to the afterglow emission of GW190425, the search validates our methods for future searches of radio afterglows.
Detection of the electromagnetic emission from coalescing binary neutron stars (BNS) is important for understanding the merger and afterglow. Aims. We present a search for a radio counterpart to the gravitational-wave (GW) source GW190425, a BNS merger, using Apertif on the Westerbork Synthesis Radio Telescope (WSRT).
Methods
We observed a field of high probability in the associated localisation region for three epochs at ΔTâ€., =â€., 68, 90, 109 d post merger. We identified all sources that exhibit flux variations consistent with the expected afterglow emission of GW190425. We also looked for possible transients. These are sources that are only present in one epoch. In addition, we quantified our ability to search for radio afterglows in the fourth and future observing runs of the GW detector network using Monte Carlo simulations.
Results
We found 25 afterglow candidates based on their variability. None of these could be associated with a possible host galaxy at the luminosity distance of GW190425. We also found 55 transient afterglow candidates that were only detected in one epoch. All of these candidates turned out to be image artefacts. In the fourth observing run, we predict that up to three afterglows will be detectable by Apertif.
Conclusions
While we did not find a source related to the afterglow emission of GW190425, the search validates our methods for future searches of radio afterglows.
Stars: neutron
Gravitational waves
Radio continuum: stars
Author
O. M. Boersma
Netherlands Institute for Radio Astronomy (ASTRON)
University of Amsterdam
J. van Leeuwen
University of Amsterdam
Netherlands Institute for Radio Astronomy (ASTRON)
E. A.K. Adams
Netherlands Institute for Radio Astronomy (ASTRON)
University of Groningen
B. Adebahr
Ruhr-Universität Bochum
A. M. Kutkin
Russian Academy of Sciences
Netherlands Institute for Radio Astronomy (ASTRON)
T. Oosterloo
University of Groningen
Netherlands Institute for Radio Astronomy (ASTRON)
W.J.G. de Blok
University of Cape Town
Netherlands Institute for Radio Astronomy (ASTRON)
University of Groningen
R. H. Van Den Brink
Tricas Industrial Design & Engineering
Netherlands Institute for Radio Astronomy (ASTRON)
A. H.W.M. Coolen
Netherlands Institute for Radio Astronomy (ASTRON)
L. Connor
California Institute of Technology (Caltech)
University of Amsterdam
Sieds Damstra
Netherlands Institute for Radio Astronomy (ASTRON)
H. Dénes
Netherlands Institute for Radio Astronomy (ASTRON)
K. M. Hess
Netherlands Institute for Radio Astronomy (ASTRON)
University of Groningen
J. M. van der Hulst
University of Groningen
B. Hut
Netherlands Institute for Radio Astronomy (ASTRON)
Marianna Ivashina
Chalmers, Electrical Engineering, Communication, Antennas and Optical Networks
G. M. Loose
Netherlands Institute for Radio Astronomy (ASTRON)
D. M. Lucero
Virginia Polytechnic Institute and State University
Y. Maan
Netherlands Institute for Radio Astronomy (ASTRON)
Mika
Netherlands Institute for Radio Astronomy (ASTRON)
V. A. Moss
Netherlands Institute for Radio Astronomy (ASTRON)
The University of Sydney
Commonwealth Scientific and Industrial Research Organisation (CSIRO)
H. Mulder
Netherlands Institute for Radio Astronomy (ASTRON)
L. C. Oostrum
University of Amsterdam
Netherlands Institute for Radio Astronomy (ASTRON)
Mark Ruiter
Netherlands Institute for Radio Astronomy (ASTRON)
D. Van Der Schuur
Netherlands Institute for Radio Astronomy (ASTRON)
R. Smits
Netherlands Institute for Radio Astronomy (ASTRON)
N. Vermaas
Netherlands Institute for Radio Astronomy (ASTRON)
D. Vohl
Netherlands Institute for Radio Astronomy (ASTRON)
J. Ziemke
University of Groningen
Netherlands Institute for Radio Astronomy (ASTRON)
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 650 A131Subject Categories
Subatomic Physics
Meteorology and Atmospheric Sciences
Astronomy, Astrophysics and Cosmology
DOI
10.1051/0004-6361/202140578