The Astrophysical Journal (Jan 2024)

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

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

DOI
https://doi.org/10.3847/1538-4357/ad3c43
Journal volume & issue
Vol. 967, no. 1
p. 50

Abstract

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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 Δ t _ab = $-{116.6}_{-9.3}^{+10.8}$ observer-frame days and Δ t _cb = $-{48.6}_{-4.0}^{+3.6}$ observer-frame days relative to the last image to arrive (image 2b; all uncertainties are 1 σ ), 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.

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