JWST Photometric Time-delay and Magnification Measurements for the Triply Imaged Type Ia “SN H0pe” at z = 1.78
Justin Pierel, Brenda Frye, Massimo Pascale, G. B. Caminha, W. Chen, Suhail Dhawan, Daniel Gilman, Matthew Grayling, S. Huber, Pat Kelly, S. Thorp, Nikki Arendse, Simon Birrer, M. Bronikowski, R. Cañameras, Dan Coe, Seth H. Cohen, Christopher J. Conselice, Simon P. Driver, Jordan C. J. D’Silva, Michael Engesser, Nicholas Foo, C. Gall, Nikhil Garuda, C. Grillo, Norman A. Grogin, Jaimie M. Henderson, J. Hjorth, Rolf A. Jansen, J. Johansson, Patrick S. Kamieneski, Anton M. Koekemoer, Conor Larison, Madeline A. Marshall, Leonidas A. Moustakas, M. Nonino, Rafael Ortiz, T. Petrushevska, Nor Pirzkal, A. S. G. Robotham, Jr. Ryan, S. Schuldt, Louis-Gregory Strolger, Jake Summers, S. H. Suyu, Tommaso Treu, Christopher N. A. Willmer, Rogier A. Windhorst, Haojing Yan, Adi Zitrin, Ana Acebrón, Sukanya Chakrabarti, D. A. Coulter, Ori D. Fox, Xiaosheng Huang, Saurabh W. Jha, G. Li, P. A. Mazzali, Ashish Kumar Meena, I. Pérez‐Fournon, F. Poidevin, A. Rest, Adam G. Riess
Abstract
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 Δ t ab = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>116.6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>9.3</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>10.8</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> observer-frame days and Δ t cb = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>48.6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>4.0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>3.6</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> 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 = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>4.3</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.6</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> , μ b = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>7.6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2.6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>3.6</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> , μ c = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>6.4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.5</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.6</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> by comparing the observed peak near-IR magnitude of SN H0pe to the nonlensed population of SNe Ia.