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

Abstract

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.

Time-Delay Cosmography: Measuring the Hubble Constant and Other Cosmological Parameters with Strong Gravitational Lensing

“…2024 ; Pierel et al. 2024a ) were compared to the predictions of seven independently constructed cluster lens models to measure a value for the Hubble constant. In combination with the standardizable magnification of the type Ia nature of the SN, this resulted .…”

“…( 2024 ) discovered another lensed supernovae in a cluster, this time of type Ia, which even allows for a standardization of the lensing magnification (Pierel et al. 2024a ), and (Pierel et al. 2024b ) discovered for the first time a second supernovae in the same host galaxy, with the initial supernovae discovered in archival data by (Rodney et al.…”

Lensed Type Ia Supernova “Encore” at z = 2: The First Instance of Two Multiply Imaged Supernovae in the Same Host Galaxy

“…While the most precise time-delay measurements come from lensed SNe observed before peak brightness, a lensed SN Ia observed roughly in the phase of images A and B in multiple filters should still provide a time-delay-measurement uncertainty of ∼5 observer-frame days (Pierel & Rodney 2019). Image C was observed well after peak brightness in the nebular phase of SNe Ia, where the slow and uncertain evolution will likely result in a lower time-delay precision of 10 observerframe days (Pierel et al 2024). Initial expectations from lens models of the MACS J0138.0−2155 cluster and SN Encore photometry suggest the delay between images A and B will be 1 month, while the delay between images A and C will be ∼1 yr.…”

“…Precise measurements of this "time delay" yield a direct distance measurement to the lens system that constrains the Hubble constant (H 0 ) in a single step (e.g., Refsdal 1964;Paraficz & Hjorth 2009;Linder 2011;Treu & Marshall 2016;Grillo et al 2018Grillo et al , 2020Grillo et al , 2024Birrer et al 2022b;Treu et al 2022;Kelly et al 2023a;Suyu et al 2024). While this has been accomplished with quasars (e.g., Kundić et al 1997;Schechter et al 1997;Burud et al 2002;Hjorth et al 2002;Vuissoz et al 2008;Suyu et al 2010;Tewes et al 2013;Bonvin et al 2017Bonvin et al , 2018Bonvin et al , 2019Birrer et al 2019Birrer et al , 2020Chen et al 2019;Shajib et al 2020Shajib et al , 2023Wong et al 2020), there is much discussion about the advantages of using supernovae (SNe) instead to leverage a variety of valuable characteristics such as predictable evolution, simplicity of observations, standardizable brightness (for Type Ia SNe, SNe Ia), and mitigated microlensing effects (e.g., Foxley-Marrable et al 2018;Goldstein et al 2018;Pierel & Rodney 2019;Ding et al 2021;Huber et al 2021;Pierel et al 2021Pierel et al , 2024Birrer et al 2022a;Chen et al 2024;Pascale et al 2024). The sample of strongly lensed SNe has grown over the last decade to include two galaxy-scal...…”

“…While this has been accomplished with quasars (e.g., Kundić et al 1997;Schechter et al 1997;Burud et al 2002;Hjorth et al 2002;Vuissoz et al 2008;Suyu et al 2010;Tewes et al 2013;Bonvin et al 2017Bonvin et al , 2018Bonvin et al , 2019Birrer et al 2019Birrer et al , 2020Chen et al 2019;Shajib et al 2020Shajib et al , 2023Wong et al 2020), there is much discussion about the advantages of using supernovae (SNe) instead to leverage a variety of valuable characteristics such as predictable evolution, simplicity of observations, standardizable brightness (for Type Ia SNe, SNe Ia), and mitigated microlensing effects (e.g., Foxley-Marrable et al 2018;Goldstein et al 2018;Pierel & Rodney 2019;Ding et al 2021;Huber et al 2021;Pierel et al 2021Pierel et al , 2024Birrer et al 2022a;Chen et al 2024;Pascale et al 2024). The sample of strongly lensed SNe has grown over the last decade to include two galaxy-scale systems (Goobar et al 2017(Goobar et al , 2023Pierel et al 2023) and five cluster-scale systems (Kelly et al 2015;Rodney et al 2021;Chen et al 2022;Kelly et al 2022;Frye et al 2024) though only SN Refsdal (Kelly et al 2023a, 2023b and SN H0pe (Chen et al 2024;Frye et al 2024;…”