The Zwicky Transient Facility phase I sample of hydrogen-rich superluminous supernovae without strong narrow emission lines

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Acknowledgement

We thank the anonymous referee for suggestions that helped to improve the paper.

This study is based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the ZTF project. ZTF is supported by the National Science Foundation under grants no. AST-1440341 and AST-2034437 and a collaboration including current partners Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University of Warwick, Ruhr University Bochum, Northwestern University and former partners the University of Washington, Los Alamos National Laboratories, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. SED Machine is based upon work supported by the National Science Foundation under grant no. 1106171. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant #12540303 (PI: Graham). This work uses the GROWTH Followup Marshal (Kasliwal et al. 2019) and was supported by the GROWTH project funded by the National Science Foundation under grant no. 1545949.

This study is based partially on observations made with the NOT, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku, and the University of Oslo, representing Denmark, Finland, and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofísica de Canarias. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofísica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT. The LT 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 Astrofísica de Canarias with financial support from the UK Science and Technology Facilities Council. The WHT is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias.

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. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.

TK acknowledges support from the Swedish National Space Agency and the Swedish Research Council. SS acknowledges support from the Gravitational Radiation and Electromagnetic Astrophysical Transients (GREAT) research environment, funded by Vetenskapsrådet, the Swedish Research Council, project number 2016-06012. RL acknowledges support from a Marie Skłodowska-Curie Individual Fellowship within the Horizon 2020 European Union (EU) Framework Programme for Research and Innovation (H2020- MSCA-IF-2017-794467). TWC acknowledges EU funding under Marie Skłodowska-Curie grant H2020-MSCA-IF-2018-842471. LT acknowledges support from Ministero dell'Istruzione (MIUR); Progetti di Ricerca di Interesse Nazionale (PRIN) 2017 grant 20179ZF5KS. AGY’s research is supported by the EU via European Research Council (ERC) grant no. 725161, the Israel Science Foundation (ISF) gravitational wave (GW) excellence center, an Isreal Ministry of Science (IMOS) space infrastructure grant and Binational Science Foundation (BSF)/Transformative and Global Innovation Fund (GIF) grants, as well as the André Deloro Institute for Advanced Research in Space and Optics, the Schwartz/Reisman Collaborative Science Program and the Norman E Alexander Family M Foundation ULTRASAT Data Center Fund, The Kimmel center for Planetary Sciences, Minerva and Yeda-Sela; AGY is the incumbent of the The Arlyn Imberman Professorial Chair.

Data Availability

The photometry data used in this study are included as supplementary material; raw images used in ZTF photometry are publicly available through ZTF Data Release 10 at https://www.ztf.caltech.edu/ztf-public-releases.html. All output corner plot files and figures from light-curve modelling are also included as supplementary material. Reduced spectra used in this study are publicly available through WISEREP (https://www.wiserep.org/). The derived data generated in this research will be shared on reasonable request to the corresponding author.

Optical/UV Swift photometry data used in this paper are available publicly on the NASA Swift Data Archive (https://heasarc.gsfc.nasa.gov/). X-ray count rates are publicly available on Swift XRT website (https://www.swift.ac.uk/user_objects/). Similarly, the host galaxy data used in this paper were obtained from public data repositories as described in Section 6.

Supplemental Material

Supplementary data (ZIP)