R.Cutter (1); K.Ackley (2); B.P.Gompertz (1); J.Lyman (1);�� G.Ramsay
(5); K.Ulaczyk (1); D.K.Galloway (2); E.Stanway (1); T.Killestein(1);
K.Wiersema (1); M.Kennedy (10); D.Steeghs (1); M.Dyer (3); V.Dhillon
(3); P.O'Brien (4); D.Pollacco (1); E.Thrane (2);S.Poshyachinda (6);
S.Mattila (7); L.Nuttall (8); E.Palle (9); A.Levan (1); T.Marsh (1);
R.West (1); Y.-L.Mong (2); A.Casey (2); M.Brown(2); B.Muller (2);
J.Mullaney (3); E.Daw (3); S.Littlefair (3); J.Maund (3); L.Makrygianni
(3); R.Starling (4); R.Eyles (4); S.Tooke(4); S.Aukkaravittayapun (6);
U.Sawangwit (6); S.Awiphan (6); D.Mkrtichian (6); P.Irawati (6); R.Kotak
(7); T.Heikkila (7); E.Rol (2)
(1) Warwick University, (2) Monash University, (3) University of
Sheffield, (4) University of Leicester, (5) Armagh Observatory &
Planetarium, (6) National Astronomical Research Institute of Thailand,
(7) University of Turku, (8) University of Portsmouth, (9) Instituto de
Astrofisica de Canarias), (10) Univ. of Manchester.
report on behalf of the GOTO collaboration:
We report on optical observations with the Gravitational-wave Optical
Transient Observer prototype in response to S200213t (GCN #27042).
Targeted observations started shortly after the preliminary event
notification was received. These spanned 47 unique tile pointings, with
image subtraction, containing 54.2% of the source location probability
(based on the initial BAYESTAR skymap) and were acquired between 04:15
UT Feb 13 2020 and 06:44 UT Feb 14 2020 (starting 3 minutes after the
event trigger). No new transients that could be credibly associated with
S200213t were detected.
Each pointing spans 4.9x3.7 square degrees and consisted of 3x60s
exposures in our L-band filter (400-700nm passband similar to g+r) with
a median 5-sigma photometric depth equivalent to g=18.4 for an
individual pointing (median moon illumination of 71.7% and some variable
cloud coverage was present). Limits are based on a photometric
calibration against PS1 sources. Most pointings were observed multiple
times, typically 2-3 times.
Images are processed immediately after acquisition using the GOTOphoto
pipeline. Difference imaging was performed on the median of each triplet
of exposures using recent survey observations of the same pointings.
Source candidates were initially filtered using a classifier and
cross-matched against a variety of catalogs, including the MPC and PS1.
Human candidate vetting was performed following data acquisition and
automated classifier cuts.
GOTO is operated at the La Palma observing facilities of the University
of Warwick on behalf of a consortium including the University of
Warwick, Monash University, Armagh Observatory, the University of
Leicester, the University of Sheffield, the National Astronomical
Research Institute of Thailand (NARIT), The University of Portsmouth,
the University of Turku and the Instituto de Astrofisica de Canarias