@article{489e9f2fcec94fc79dc45c5238516908,
title = "North Ecliptic Pole merging galaxy catalogue",
abstract = "Aims. We aim to generate a catalogue of merging galaxies within the 5.4 sq. deg. North Ecliptic Pole over the redshift range 0:0 ≤ z ≤ 0:3. To do this, imaging data from the Hyper Suprime-Cam are used along with morphological parameters derived from these same data. Methods. The catalogue was generated using a hybrid approach. Two neural networks were trained to perform binary merger nonmerger classifications: one for galaxies with z ≤ 0:15 and another for 0:15 ≤ z < 0:30. Each network used the image and morphological parameters of a galaxy as input. The galaxies that were identified as merger candidates by the network were then visually checked by experts. The resulting mergers will be used to calculate the merger fraction as a function of redshift and compared with literature results. Results. We found that 86.3% of galaxy mergers at z ≤ 0:15 and 79.0% of mergers at 0:15 ≤ z < 0:30 are expected to be correctly identified by the networks. Of the 34 264 galaxies classified by the neural networks, 10 195 were found to be merger candidates. Of these, 2109 were visually identified to be merging galaxies. We find that the merger fraction increases with redshift, consistent with literature results from observations and simulations, and that there is a mild star-formation rate enhancement in the merger population of a factor of 1:102 ± 0:084.",
keywords = "Catalogs, Galaxies: evolution, Galaxies: interactions, Galaxies: statistics, Methods: data analysis",
author = "Pearson, {W. J.} and Suelves, {L. E.} and Ho, {S. C.C.} and N. Oi and S. Brough and Holwerda, {B. W.} and Hopkins, {A. M.} and Huang, {T. C.} and Hwang, {H. S.} and Kelvin, {L. S.} and Kim, {S. J.} and L{\'o}pez-S{\'a}nchez, {A. R.} and {Ma{\aa}{\~A} {\^A} Ek}, K. and C. Pearson and A. Poliszczuk and A. Pollo and V. Rodriguez-Gomez and H. Shim and Y. Toba and L. Wang",
note = "Funding Information: Acknowledgements. We would like to thank the referee for their thorough and thoughtful comments that helped improve the quality and clarity of this paper. We would like to thank C. Conselice, A. Graham, A. Nanni and D. J. D. Santos for helpful discussions on this paper. W.J.P. has been supported by the Polish National Science Center project UMO-2020/37/B/ST9/00466. K.M. has been supported by the Polish National Science Center project UMO-2018/30/E/ST9/00082. This research was conducted under the agreement on scientific cooperation between the Polish Academy of Sciences and the Ministry of Science and Technology in Taipei and supported by the Polish National Science Centre grant UMO-2018/30/M/ST9/00757 and by Polish Ministry of Science and Higher Education grant DIR/WK/2018/12. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST programme from the Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org This paper is based [in part] on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center (ADC) at National Astronomical Observatory of Japan. Data analysis was in part carried out with the cooperation of Center for Computational Astrophysics (CfCA), National Astronomical Observatory of Japan. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 177.A-3016. Publisher Copyright: {\textcopyright} 2022 American Institute of Physics Inc.. All rights reserved.",
year = "2022",
month = may,
day = "1",
doi = "10.1051/0004-6361/202141013",
language = "English",
volume = "661",
journal = "Astronomy and astrophysics",
issn = "0004-6361",
publisher = " EDP Sciences",
}