@article{88471484733b4c9185acc3354841b48d,
title = "A search for optical and near-infrared counterparts of the compact binary merger GW190814",
abstract = "We report on our observing campaign of the compact binary merger GW190814, detected by the Advanced LIGO and Advanced Virgo detectors on 2019 August 14. This signal has the best localization of any observed gravitational wave (GW) source, with a 90 per cent probability area of 18.5 deg2, and an estimated distance of ≈240 Mpc. We obtained wide-field observations with the Deca-Degree Optical Transient Imager (DDOTI) covering 88 per cent of the probability area down to a limiting magnitude of w = 19.9 AB. Nearby galaxies within the high probability region were targeted with the Lowell Discovery Telescope (LDT), whereas promising candidate counterparts were characterized through multicolour photometry with the Reionization and Transients InfraRed (RATIR) and spectroscopy with the Gran Telescopio de Canarias (GTC). We use our optical and near-infrared limits in conjunction with the upper limits obtained by the community to constrain the possible electromagnetic counterparts associated with the merger. A gamma-ray burst seen along its jet's axis is disfavoured by the multiwavelength data set, whereas the presence of a burst seen at larger viewing angles is not well constrained. Although our observations are not sensitive to a kilonova similar to AT2017gfo, we can rule out high-mass (>0.1 M☉) fast-moving (mean velocity ≥0.3c) wind ejecta for a possible kilonova associated with this merger.",
author = "Thakur, {A. L.} and S. Dichiara and E. Troja and Chase, {E. A.} and R. S{\'a}nchez-Ram{\'i}rez and L. Piro and Fryer, {C. L.} and Butler, {N. R.} and Watson, {A. M.} and Wollaeger, {R. T.} and E. Ambrosi and {Becerra Gonz{\'a}lez}, J. and Becerra, {R. L.} and G. Bruni and Cenko, {S. B.} and G. Cusumano and A. D'A{\`i} and J. Durbak and Fontes, {C. J.} and P. Gatkine and Hungerford, {A. L.} and O. Korobkin and Kutyrev, {A. S.} and Lee, {W. H.} and S. Lotti and G. Minervini and G. Novara and {la Parola}, V. and M. Pereyra and R. Ricci and A. Tiengo and S. Veilleux",
note = "Funding Information: ALT, RSR, and LP acknowledge support from the European Union's Horizon 2020 Programme under the AHEAD2020 project (grant agreement n. 871158) and by ASI (Italian Space Agency) through the Contract no. 2019-27-HH.0. SD and ET acknowledge support for this work under NASA grant 80NSSC18K0429. JBG acknowledges the support of the Viera y Clavijo program funded by ACIISI and ULL. GB acknowledges financial support under the INTEGRAL ASI-INAF agreement 2019-35-HH.0 and from MIUR (PRIN 2017 grant 20179ZF5KS). We thank Charlie Hoy for his help in accessing and loading the finalized GW190814 skymap. We thank the staff of the Observatorio Astron{\'o}mico Nacional. Some of the data presented in this paper were acquired with the DDOTI instrument of the Observatorio Astron{\'o}mico Nacional on the Sierra de San Pedro M{\'a}rtir. DDOTI is funded by CONACyT (LN 260369, LN 271117, and 277901), NASA Goddard space Flight center, the University of Maryland (NNX17AK54G), and the Universidad Nacional Aut{\'o}noma de M{\'e}xico (CIC and DGAPA/PAPIIT IT102715, IG100414, AG100317, and IN109418) and is operated and maintained by the Observatorio Astron{\'o}mico Nacional and the Instituto de Astronom{\'i}a of the Universidad Nacional Aut{\'o}noma de M{\'e}xico. We acknowledge the contribution of Neil Gehrels to the development of DDOTI. Some of the data used in this paper were acquired with the RATIR instrument, funded by the University of California and NASA Goddard Space Flight Center, and the 1.5-m Harold L. Johnson telescope at the Observatorio Astron{\'o}mico Nacional on the Sierra de San Pedro M{\'a}rtir, operated and maintained by the Observatorio Astron{\'o}mico Nacional and the Instituto de Astronom{\'i}a of the Universidad Nacional Aut{\'o}noma de M{\'e}xico. We acknowledge the contribution of Leonid Georgiev and Neil Gehrels to the development of RATIR. The spectroscopic data presented in this work were reduced using standard routines of PyRAF. PyRAF is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. This research made use of ccdproc, an Astropy package for image reduction (Craig et al. 2017). This work made use of the data products generated by the NYU SN group, and released under DOI:10.5281/zenodo.58766, available at https://github.com/nyusngroup/SESNtemple/. Publisher Copyright: {\textcopyright} 2020 The Author(s)",
year = "2020",
month = dec,
day = "1",
doi = "10.1093/mnras/staa2798",
language = "English (US)",
volume = "499",
pages = "3868--3883",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "3",
}