The case of AT2022wtn: a Tidal Disruption Event in an interacting galaxy

Abstract

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Acknowledgement

This work is dedicated to my daughter Delia, who was with(-in) me all the time, during the data analysis, interpretation, and writing phases that led to the birth of this manuscript.

We thanks the anonymous referee for the useful comments that contribute to the improvement of the manuscript. We thank Daniel Perley for his contribution to the spectroscopic data set with the LT data. This work makes use of observations from the Las Cumbres Observatory global telescope network. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. These results made use of the Lowell Discovery Telescope (LDT) at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the LDT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects Survey). ePESSTO + observations were obtained under ESO programs ID 111.24PR and 112.25JQ. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. We wish to recognize and acknowledge the cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. The SED machine is based upon work supported by the National Science Foundation under grant no. 1106171. ATLAS is primarily funded to search for near earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575. Science products are made possible by grants Kepler/K2 J1944/80NSSC19K0112, HST GO-15889, and STFC grants ST/T000198/1 and ST/S006109/1 and contributions form University of Hawaii Institute for Astronomy, the Queen’s University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and The Millennium Institute of Astrophysics (MAS), Chile. Pan-STARRS telescopes are supported by the National Aeronautics and Space Administration under grants NNX12AR65G and NNX14AM74G, from the Near-Earth Object Observations Program. Data are processed at Queen’s University Belfast enabled through the STFC grants ST/P000312/1 and ST/T000198/1. This work was funded by ANID, Millennium Science Initiative, ICN12_009. The material is based upon work supported by NASA under award number 80GSFC21M0002. FO acknowledges support from MIUR, PRIN 2020 (grant 2020KB33TP) ‘Multimessenger astronomy in the Einstein Telescope Era (METE)’ and from INAF-MINIGRANT (2023): ‘SeaTiDE–Searching for Tidal Disruption Events with ZTF: the Tidal Disruption Event population in the era of wide field surveys’. MB, EC, and TP acknowledge the financial support from the Slovenian Research Agency (grants I0-0033, P1-0031, J1-8136, J1-2460, and Z1-1853) and the Young Researchers program. TWC acknowledges the Yushan Fellow Program by the Ministry of Education, Taiwan for the financial support (MOE-111-YSFMS-0008-001-P1). PC was supported by the Science & Technology Facilities Council [grants ST/S000550/1 and ST/W001225/1]. CPG acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Programme of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 programme, from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. TEMB acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Union Next Generation EU/PRTR funds under the 2021 Juan de la Cierva program FJC2021-047124-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. TR acknowledges support from the Research Council of Finland project 350458 and the Cosmic Dawn Center (DAWN) which is funded by the Danish National Research Foundation under grant DNRF140. SM acknowledges support from the Research Council of Finland project 350458. RS acknowledges support from grants by the National Science Foundation (AST 2206730) and the David and Lucille Packard Foundation (PI: Kasliwal). MN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 948381) and by UK Space Agency grant no. ST/Y000692/1. IA acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement no. 852097), from the Israel Science Foundation (grant no. 2752/19), from the United States–Israel Binational Science Foundation (BSF; grant no. 2018166), and from the Pazy foundation (grant no. 216312). LM acknowledges support through a UK Research and Innovation Future Leaders Fellowship (grant no. MR/T044136/1). SGG acknowledges support from the ESO Scientific Visitor Programme.

Data Availability

The photometric data from I:IO/LT, LCOGT and UVOT underlying this article are available in the article itself. The PS1, ATLAS, and ZTF are publicity available. The NTT spectra are publicity available through the PESSTO SSDR4 ESO Phase 4 Data Release (see the ESO archive search and retrieve interface) and on the The Weizmann Interactive Supernova Data Repository (https://www.wiserep.org) The remaining processed spectroscopic data underlying this article are made available as online Supporting Information. All the data set will be also shared on request to the corresponding author.

Supplemental Material

staf746_Supplemental_Files - zip file