The Hydrogen-poor Superluminous Supernovae from the Zwicky Transient Facility Phase I Survey. I. Light Curves and Measurements

Z. H. Chen, Lin Yan, T. Kangas, R. Lunnan, S. Schulze, J. Sollerman, D. A. Perley, T. W. Chen, K. Taggart, K. R. Hinds, A. Gal-Yam, X. F. Wang, I. Andreoni, E. Bellm, J. S. Bloom, K. Burdge, A. Burgos, D. Cook, A. Dahiwale, K. DeR. Dekany, A. Dugas, S. Frederik, C. Fremling, M. Graham, M. Hankins, A. Ho, J. Jencson, V. Karambelkar, M. Kasliwal, S. Kulkarni, R. Laher, B. Rusholme, Y. Sharma, F. Taddia, L. Tartaglia, B. P. Thomas, A. Tzanidakis, J. Van Roestel, R. Walter, Y. Yang, Y. H. Yao, O. Yaron

研究成果: 雜誌貢獻期刊論文同行評審

14 引文 斯高帕斯(Scopus)

摘要

During the Zwicky Transient Facility (ZTF) Phase I operations, 78 hydrogen-poor superluminous supernovae (SLSNe-I) were discovered in less than 3 yr, constituting the largest sample from a single survey. This paper (Paper I) presents the data, including the optical/UV light curves and classification spectra, while Paper II in this series will focus on the detailed analysis of the light curves and modeling. Our photometry is primarily taken by ZTF in the g, r, and i bands, and with additional data from other ground-based facilities and Swift. The events of our sample cover a redshift range of z = 0.06 − 0.67, with a median and 1σ error (16% and 84% percentiles) of z med = 0.265 − 0.135 + 0.143 . The peak luminosity covers −22.8 mag ≤ M g,peak ≤ −19.8 mag, with a median value of − 21.48 − 0.61 + 1.13 mag. The light curves evolve slowly with a mean rest-frame rise time of t rise = 41.9 ± 17.8 days. The luminosity and timescale distributions suggest that low-luminosity SLSNe-I with a peak luminosity ∼−20 mag or extremely fast-rising events (<10 days) exist, but are rare. We confirm previous findings that slowly rising SLSNe-I also tend to fade slowly. The rest-frame color and temperature evolution show large scatters, suggesting that the SLSN-I population may have diverse spectral energy distributions. The peak rest-frame color shows a moderate correlation with the peak absolute magnitude, i.e., brighter SLSNe-I tend to have bluer colors. With optical and UV photometry, we construct the bolometric luminosity and derive a bolometric correction relation that is generally applicable for converting g, r-band photometry to the bolometric luminosity for SLSNe-I.

原文???core.languages.en_GB???
文章編號41
期刊Astrophysical Journal
943
發行號1
DOIs
出版狀態已出版 - 1 1月 2023

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