April
2025
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2025PASP..137d4203D
Authors
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Das, Kaustav K.
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Kasliwal, Mansi M.
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Fremling, Christoffer
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Sollerman, Jesper
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Perley, Daniel A.
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De, Kishalay
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Tzanidakis, Anastasios
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Sit, Tawny
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Adams, Scott
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Anand, Shreya
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Ahumuda, Tomas
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Andreoni, Igor
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Brennan, Seán
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Brink, Thomas
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Bruch, Rachel J.
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Chen, Ping
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Chu, Matthew R.
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Cook, David O.
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Covarrubias, Sofia
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Dahiwale, Aishwarya
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Earley, Nicholas
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Ho, Anna Y. Q.
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Gal-Yam, Avishay
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Gangopadhyay, Anjasha
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Hammerstein, Erica
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Hinds, K. -Ryan
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Karambelkar, Viraj
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Kong, Yihan
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Kulkarni, S. R.
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Jegou du Laz, Theophile
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Liu, Chang
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Meynardie, William
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Miller, Adam A.
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Nir, Guy
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Patra, Kishore C.
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Pessi, Priscila J.
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Rich, R. Michael
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Rehemtulla, Nabeel
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Rose, Sam
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Rusholme, Ben
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Schulze, Steve
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Sharma, Yashvi
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Singh, Avinash
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Smith, Roger
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Stein, Robert
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Mandigo-Stoba, Milan Sharma
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Strotjohann, Nora L.
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Qin, Yu-Jing
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Wise, Jacob
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Wold, Avery
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Yan, Lin
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Yang, Yi
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Yao, Yuhan
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Zimmerman, Erez
Abstract
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We present the luminosity function and volumetric rate of a sample of Type IIP supernovae (SNe) from the Zwicky Transient Facility Census of the Local Universe survey (CLU). This is the largest sample of Type IIP SNe from a systematic volume-limited survey to-date. The final sample includes 330 Type IIP SNe and 36 low-luminosity Type II (LLIIP) SNe with Mr,peak > ‑16 mag, which triples the literature sample of LLIIP SNe. The fraction of LLIIP SNe is of the total CLU Type IIP SNe population ( of all core-collapse SNe). This implies that while LLIIP SNe likely represent the fate of core-collapse SNe of 8–12 M⊙ progenitors, they alone cannot account for the fate of all massive stars in this mass range. To derive an absolute rate, we estimate the ZTF pipeline efficiency as a function of the apparent magnitude and the local surface brightness. We derive a volumetric rate of for Type IIP SNe and for LLIIP SNe. Now that the rate of LLIIP SNe is robustly derived, the unresolved discrepancy between core-collapse SN rates and star formation rates cannot be explained by LLIIP SNe alone.
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