GWOPS: A VO-technology Driven Tool to Search for the Electromagnetic Counterpart of Gravitational Wave Event. (arXiv:2009.03497v2 [astro-ph.IM] UPDATED)

GWOPS: A VO-technology Driven Tool to Search for the Electromagnetic Counterpart of Gravitational Wave Event. (arXiv:2009.03497v2 [astro-ph.IM] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Xu_Y/0/1/0/all/0/1">Yunfei Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_D/0/1/0/all/0/1">Dong Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cui_C/0/1/0/all/0/1">Chenzhou Cui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fan_D/0/1/0/all/0/1">Dongwei Fan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_Z/0/1/0/all/0/1">Zipei Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yu_B/0/1/0/all/0/1">Bangyao Yu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_C/0/1/0/all/0/1">Changhua Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Han_J/0/1/0/all/0/1">Jun Han</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mi_L/0/1/0/all/0/1">Linying Mi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_S/0/1/0/all/0/1">Shanshan Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+He_B/0/1/0/all/0/1">Boliang He</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tao_Y/0/1/0/all/0/1">Yihan Tao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_H/0/1/0/all/0/1">Hanxi Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_S/0/1/0/all/0/1">Sisi Yang</a>

The search and follow-up observation of electromagnetic (EM) counterparts of
gravitational waves (GW) is a current hot topic of GW cosmology. Due to the
limitation of the accuracy of the GW observation facility at this stage, we can
only get a rough sky-localization region for the GW event, and the typical area
of the region is between 200 and 1500 square degrees. Since GW events occur in
or near galaxies, limiting the observation target to galaxies can significantly
speedup searching for EM counterparts. Therefore, how to efficiently select
host galaxy candidates in such a large GW localization region, how to arrange
the observation sequence, and how to efficiently identify the GW source from
observational data are the problems that need to be solved. International
Virtual Observatory Alliance has developed a series of technical standards for
data retrieval, interoperability and visualization. Based on the application of
VO technologies, we construct the GW follow-up Observation Planning System
(GWOPS). It consists of three parts: a pipeline to select host candidates of GW
and sort their priorities for follow-up observation, an identification module
to find the transient from follow-up observation data, and a visualization
module to display GW-related data. GWOPS can rapidly respond to GW events. With
GWOPS, the operations such as follow-up observation planning, data storage,
data visualization, and transient identification can be efficiently
coordinated, which will promote the success searching rate for GWs EM
counterparts.

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