JWST Photometric Time-delay and Magnification Measurements for the Triply Imaged Type Ia "SN H0pe" at z = 1.78

Pierel, J. D. R.; Frye, B. L.; Pascale, M.; Caminha, G. B.; Chen, W.; Dhawan, S.; Gilman, D.; Grayling, M.; Huber, S.; Kelly, P.; Thorp, S.; Arendse, N.; Birrer, S.; Bronikowski, M.; Cañameras, R.; Coe, D.; Cohen, S. H.; Conselice, C. J.; Driver, S. P.; DŚilva, J. C. J.; Engesser, M.; Foo, N.; Gall, C.; Garuda, N.; Grillo, C.; Grogin, N. A.; Henderson, J.; Hjorth, J.; Jansen, R. A.; Johansson, J.; Kamieneski, P. S.; Koekemoer, A. M.; Larison, C.; Marshall, M. A.; Moustakas, L. A.; Nonino, M.; Ortiz, R.; Petrushevska, T.; Pirzkal, N.; Robotham, A.; Ryan, R. E.; Schuldt, S.; Strolger, L. G.; Summers, J.; Suyu, S. H.; Treu, T.; Willmer, C. N. A.; Windhorst, R. A.; Yan, H.; Zitrin, A.; Acebron, A.; Chakrabarti, S.; Coulter, D. A.; Fox, O. D.; Huang, X.; Jha, S. W.; Li, G.; Mazzali, P. A.; Meena, A. K.; Pérez-Fournon, I.; Poidevin, F.; Rest, A.; Riess, A. G.
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The Astrophysical Journal

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Supernova (SN) SN H0pe is a gravitationally lensed, triply imaged, Type Ia SN (SN Ia) discovered in James Webb Space Telescope imaging of the PLCK G165.7+67.0 cluster of galaxies. Well-observed multiply imaged SNe provide a rare opportunity to constrain the Hubble constant (H 0), by measuring the relative time delay between the images and modeling the foreground mass distribution. SN H0pe is located at z = 1.783 and is the first SN Ia with sufficient light-curve sampling and long enough time delays for an H 0 inference. Here we present photometric time-delay measurements and SN properties of SN H0pe. Using JWST/NIRCam photometry, we measure time delays of Δt ab = $-{116.6}_{-9.3}^{+10.8}$ observer-frame days and Δt cb = $-{48.6}_{-4.0}^{+3.6}$ observer-frame days relative to the last image to arrive (image 2b; all uncertainties are 1σ), which corresponds to a ∼5.6% uncertainty contribution for H 0 assuming 70 km s‑1 Mpc‑1. We also constrain the absolute magnification of each image to μ a = ${4.3}_{-1.8}^{+1.6}$ , μ b = ${7.6}_{-2.6}^{+3.6}$ , μ c = ${6.4}_{-1.5}^{+1.6}$ by comparing the observed peak near-IR magnitude of SN H0pe to the nonlensed population of SNe Ia.