학술논문
JWST Photometric Time-Delay and Magnification Measurements for the Triply-Imaged Type Ia 'Supernova H0pe' at z = 1.78
Document Type
Working Paper
Author
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.; Canameras, R.; Coe, D.; Cohen, S. H.; Conselice, C. J.; Driver, S. P.; Dsilva, 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 Iii, R.; Petrushevska, T.; Pirzkal, N.; Robotham, A.; Ryan, Jr., 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.; Perez-Fournon, I.; Poidevin, F.; Rest, A.; Riess, A. G.
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Subject
Language
Abstract
Supernova (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 $\Delta t_{ab}=-116.6^{+10.8}_{-9.3}$ and $\Delta t_{cb}=-48.6^{+3.6}_{-4.0}$ observer-frame days relative to the last image to arrive (image 2b; all uncertainties are $1\sigma$), which corresponds to a $\sim5.6\%$ uncertainty contribution for $H_0$ assuming $70 \rm{km s^{-1} Mpc^{-1}}$. We also constrain the absolute magnification of each image to $\mu_{a}=4.3^{+1.6}_{-1.8}$, $\mu_{b}=7.6^{+3.6}_{-2.6}$, $\mu_{c}=6.4^{+1.6}_{-1.5}$ by comparing the observed peak near-IR magnitude of SN H0pe to the non-lensed population of SNe Ia.
Comment: Accepted in ApJ
Comment: Accepted in ApJ