Field |
Value |
Language |
dc.contributor.author |
Anderson, GE |
|
dc.contributor.author |
Hancock, PJ |
|
dc.contributor.author |
Rowlinson, A |
|
dc.contributor.author |
Sokolowski, M |
|
dc.contributor.author |
Williams, A |
|
dc.contributor.author |
Tian, J |
|
dc.contributor.author |
Miller-Jones, JCA |
|
dc.contributor.author |
Hurley-Walker, N |
|
dc.contributor.author |
Bannister, KW |
|
dc.contributor.author |
Bell, ME |
|
dc.contributor.author |
James, CW |
|
dc.contributor.author |
Kaplan, DL |
|
dc.contributor.author |
Murphy, T |
|
dc.contributor.author |
Tingay, SJ |
|
dc.contributor.author |
Meyers, BW |
|
dc.contributor.author |
Johnston-Hollitt, M |
|
dc.contributor.author |
Wayth, RB |
|
dc.date.accessioned |
2022-03-27T23:29:22Z |
|
dc.date.available |
2022-03-27T23:29:22Z |
|
dc.date.issued |
2021-06-10 |
|
dc.identifier.citation |
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA, 2021, 38 |
|
dc.identifier.issn |
1323-3580 |
|
dc.identifier.issn |
1448-6083 |
|
dc.identifier.uri |
http://hdl.handle.net/10453/155619
|
|
dc.description.abstract |
<jats:title>Abstract</jats:title>
<jats:p>Here we present stringent low-frequency (185 MHz) limits on coherent radio emission associated with a short-duration gamma-ray burst (SGRB). Our observations of the short gamma-ray burst (GRB) 180805A were taken with the upgraded Murchison Widefield Array (MWA) rapid-response system, which triggered within 20s of receiving the transient alert from the <jats:italic>Swift</jats:italic> Burst Alert Telescope, corresponding to 83.7 s post-burst. The SGRB was observed for a total of 30 min, resulting in a <jats:inline-formula>
<jats:alternatives>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S1323358021000151_inline1.png" />
<jats:tex-math>
$3\sigma$
</jats:tex-math>
</jats:alternatives>
</jats:inline-formula> persistent flux density upper limit of 40.2 mJy beam<jats:sup>–1</jats:sup>. Transient searches were conducted at the <jats:italic>Swift</jats:italic> position of this GRB on 0.5 s, 5 s, 30 s and 2 min timescales, resulting in <jats:inline-formula>
<jats:alternatives>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S1323358021000151_inline2.png" />
<jats:tex-math>
$3\sigma$
</jats:tex-math>
</jats:alternatives>
</jats:inline-formula> limits of 570–1 830, 270–630, 200–420, and 100–200 mJy beam<jats:sup>–1</jats:sup>, respectively. We also performed a dedispersion search for prompt signals at the position of the SGRB with a temporal and spectral resolution of 0.5 s and 1.28 MHz, respectively, resulting in a <jats:inline-formula>
<jats:alternatives>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S1323358021000151_inline3.png" />
<jats:tex-math>
$6\sigma$
</jats:tex-math>
</jats:alternatives>
</jats:inline-formula> fluence upper-limit range from 570 Jy ms at DM <jats:inline-formula>
<jats:alternatives>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S1323358021000151_inline4.png" />
<jats:tex-math>
$=3\,000$
</jats:tex-math>
</jats:alternatives>
</jats:inline-formula> pc cm<jats:sup>–3</jats:sup> (<jats:inline-formula>
<jats:alternatives>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S1323358021000151_inline5.png" />
<jats:tex-math>
$z\sim 2.5$
</jats:tex-math>
</jats:alternatives>
</jats:inline-formula>) to 1 750 Jy ms at DM<jats:inline-formula>
<jats:alternatives>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S1323358021000151_inline6.png" />
<jats:tex-math>
$=200$
</jats:tex-math>
</jats:alternatives>
</jats:inline-formula> pc cm<jats:sup>–3</jats:sup> (<jats:inline-formula>
<jats:alternatives>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S1323358021000151_inline7.png" />
<jats:tex-math>
$z\sim 0.1)$
</jats:tex-math>
</jats:alternatives>
</jats:inline-formula>, corresponding to the known redshift range of SGRBs. We compare the fluence prompt emission limit and the persistent upper limit to SGRB coherent emission models assuming the merger resulted in a stable magnetar remnant. Our observations were not sensitive enough to detect prompt emission associated with the alignment of magnetic fields of a binary neutron star just prior to the merger, from the interaction between the relativistic jet and the interstellar medium (ISM) or persistent pulsar-like emission from the spin-down of the magnetar. However, in the case of a more powerful SGRB (a gamma-ray fluence an order of magnitude higher than GRB 180805A and/or a brighter X-ray counterpart), our MWA observations may be sensitive enough to detect coherent radio emission from the jet-ISM interaction and/or the magnetar remnant. Finally, we demonstrate that of all current low- frequency radio telescopes, only the MWA has the sensitivity and response times capable of probing prompt emission models associated with the initial SGRB merger event.</jats:p> |
|
dc.language |
English |
|
dc.publisher |
CAMBRIDGE UNIV PRESS |
|
dc.relation.ispartof |
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA |
|
dc.relation.isbasedon |
10.1017/pasa.2021.15 |
|
dc.rights |
info:eu-repo/semantics/closedAccess |
|
dc.subject |
0201 Astronomical and Space Sciences, 0299 Other Physical Sciences |
|
dc.subject.classification |
Astronomy & Astrophysics |
|
dc.title |
Murchison Widefield Array rapid-response observations of the short GRB 180805A |
|
dc.type |
Journal Article |
|
utslib.citation.volume |
38 |
|
utslib.for |
0201 Astronomical and Space Sciences |
|
utslib.for |
0299 Other Physical Sciences |
|
pubs.organisational-group |
/University of Technology Sydney |
|
pubs.organisational-group |
/University of Technology Sydney/Faculty of Science |
|
pubs.organisational-group |
/University of Technology Sydney/Faculty of Science/School of Mathematical and Physical Sciences |
|
utslib.copyright.status |
closed_access |
* |
dc.date.updated |
2022-03-27T23:29:17Z |
|
pubs.publication-status |
Published |
|
pubs.volume |
38 |
|