Gaia 18dvy: A New FUor in the Cygnus OB3 Association

Abstract

MARTON, George Iuliu/0000-0003-2469-4900; Ziolkowska, Oliwia/0000-0002-0696-2839; Wyrzykowski, Lukasz/0000-0002-9658-6151; Gromadzki, Mariusz/0000-0002-1650-1518; Zielinski, Pawel/0000-0001-6434-9429; Kiss, Csaba/0000-0002-8722-6875 ; WOS: 000563107500001 ; We present optical-infrared photometric and spectroscopic observations of Gaia 18dvy, located in the Cygnus OB3 association at a distance of 1.88 kpc. Gaia 18dvy was noted by the Gaia alerts system when its light curve exhibited a greater than or similar to 4 mag rise in 2018-2019. the brightening was also observable at mid-infared wavelengths. the infrared colors of Gaia 18dvy became bluer as the outburst progressed. Its optical and near-infrared spectroscopic characteristics in the outburst phase are consistent with those of bona fide FU Orionis-type young eruptive stars. the progenitor of the outburst is probably a low-mass K-type star with an optical extinction of similar to 3 mag. A radiative transfer modeling of the circumstellar structure, based on the quiescent spectral energy distribution, indicates a disk with a mass of 4 x 10(-3)M. Our simple accretion disk modeling implies that the accretion rate had been exponentially increasing for more than 3 yr until mid-2019, when it reached a peak value of 6.9 x 10(-6)M yr(-1). in many respects, Gaia 18dvy is similar to the FU Ori-type object HBC 722. ; European Research Council (ERC) under the European UnionEuropean Research Council (ERC) [716155]; Hungarian Academy of SciencesHungarian Academy of Sciences [LP2018-7/2019, KEP-7/2018]; Hungarian National Research, Development and Innovation Office [GINOP 2.3.2-15-2016-00003, PD-128360]; Polish NCN DAINA [2017/27/L/ST9/03221]; European CommissionEuropean CommissionEuropean Commission Joint Research Centre [730890]; Polish MNiSWMinistry of Science and Higher Education, Poland [DIR/WK/2018/12]; Research Council of LithuaniaResearch Council of Lithuania (LMTLT) [S-LL-19-2]; Ministry of Education, Science and Technological Development of the Republic of Serbia [176011]; DFGGerman Research Foundation (DFG) [SPP 1992, WA 1047/11-1]; MINECO (Spanish Ministry of Economy) [RTI2018-095076-B-C21]; Polish NCN MAESTRO [2014/14/A/ST9/00121] ; We thank the anonymous referee, whose questions and comments significantly improved the paper. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program under grant agreement No. 716155 (SACCRED), Lendulet LP2018-7/2019 and KEP-7/2018 of the Hungarian Academy of Sciences, GINOP 2.3.2-15-2016-00003 and PD-128360 of the Hungarian National Research, Development and Innovation Office, Polish NCN DAINA grant 2017/27/L/ST9/03221, European Commission's Horizon 2020 OPTICON grant 730890, Polish MNiSW grant DIR/WK/2018/12, grant No.S-LL-19-2 of the Research Council of Lithuania, Project No.176011 "Dynamics and kinematics of celestial bodies and systems" of the Ministry of Education, Science and Technological Development of the Republic of Serbia, DFG priority program SPP 1992 "Exploring the Diversity of Extrasolar Planets" (WA 1047/11-1), the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). the Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and is operated by the Institute for Space Studies of Catalonia (IEEC). MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. We acknowledge ESA Gaia, DPAC, and the Photometric Science Alerts Team. We thank Christina Conner, Megan Davis, Alessandro Dellarovere, Hannah Gallamore, Mira Ghazali, Aaron Kruskie, Dylan Mankel, Jesse Leahy-McGregor, Brandon McIntyre, Barrett Ross, Courtney Wicklund, and Evan Zobel for observing Gaia 18dvy at the Michigan State University Observatory. Based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Based on observations obtained with telescopes of the University Observatory Jena, which is operated by the Astrophysical Institute of the Friedrich-Schiller-University.