@article{bdc1141301674ee79f2a35f327ab43fb,
title = "LensWatch. I. Resolved HST Observations and Constraints on the Strongly Lensed Type Ia Supernova 2022qmx (“SN Zwicky”)",
abstract = "Supernovae (SNe) that have been multiply imaged by gravitational lensing are rare and powerful probes for cosmology. Each detection is an opportunity to develop the critical tools and methodologies needed as the sample of lensed SNe increases by orders of magnitude with the upcoming Vera C. Rubin Observatory and Nancy Grace Roman Space Telescope. The latest such discovery is of the quadruply imaged Type Ia SN 2022qmx (aka, “SN Zwicky”) at z = 0.3544. SN Zwicky was discovered by the Zwicky Transient Facility in spatially unresolved data. Here we present follow-up Hubble Space Telescope observations of SN Zwicky, the first from the multicycle “LensWatch (www.lenswatch.org)” program. We measure photometry for each of the four images of SN Zwicky, which are resolved in three WFC3/UVIS filters (F475W, F625W, and F814W) but unresolved with WFC3/IR F160W, and present an analysis of the lensing system using a variety of independent lens modeling methods. We find consistency between lens-model-predicted time delays (≲1 day), and delays estimated with the single epoch of Hubble Space Telescope colors (≲3.5 days), including the uncertainty from chromatic microlensing (∼1-1.5 days). Our lens models converge to an Einstein radius of θ E = ( 0.168 − 0.005 + 0.009 ) ″ , the smallest yet seen in a lensed SN system. The “standard candle” nature of SN Zwicky provides magnification estimates independent of the lens modeling that are brighter than predicted by ∼ 1.7 − 0.6 + 0.8 mag and ∼ 0.9 − 0.6 + 0.8 mag for two of the four images, suggesting significant microlensing and/or additional substructure beyond the flexibility of our image-position mass models.",
author = "Pierel, {J. D.R.} and N. Arendse and S. Ertl and X. Huang and Moustakas, {L. A.} and S. Schuldt and Shajib, {A. J.} and Y. Shu and S. Birrer and M. Bronikowski and J. Hjorth and Suyu, {S. H.} and S. Agarwal and A. Agnello and Bolton, {A. S.} and S. Chakrabarti and C. Cold and F. Courbin and {Della Costa}, {J. M.} and S. Dhawan and M. Engesser and Fox, {Ori D.} and C. Gall and S. Gomez and A. Goobar and Jha, {S. W.} and C. Jimenez and J. Johansson and C. Larison and G. Li and R. Marques-Chaves and S. Mao and Mazzali, {P. A.} and I. Perez-Fournon and T. Petrushevska and F. Poidevin and A. Rest and W. Sheu and R. Shirley and E. Silver and C. Storfer and Strolger, {L. G.} and T. Treu and R. Wojtak and Y. Zenati",
note = "Funding Information: We would like to thank David Jones, Nao Suzuki, and Taylor Hoyt for discussions helpful to the analysis in this work. This paper is based in part on observations with the NASA/ESA Hubble Space Telescope obtained from the Mikulski Archive for Space Telescopes at STScI. The specific observations analyzed can be accessed via DOI:10.17909/gvys-q017; support was provided to J.D.R.P. and M.E. through program HST-GO-16264. S.E. and S.H.S. thank the Max Planck Society for support through the Max Planck Research Group for S.H.S. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51492 awarded to A.J.S. by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This work has also been enabled by support from the research project grant “Understanding the Dynamic Universe” funded by the Knut and Alice Wallenberg Foundation under Dnr KAW 2018.0067. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (LENSNOVA: grant agreement No. 771776). This research is supported in part by the Excellence Cluster ORIGINS which is funded by the Deutsche Forschungsgemeinschaft (DFG; German Research Foundation) under Germany{\textquoteright}s Excellence Strategy—EXC-2094—390783311. S.S. acknowledges financial support through grants PRIN-MIUR 2017WSCC32 and 2020SKSTHZ. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). J.H., C.C., and R.W. were supported by a VILLUM FONDEN Investigator grant to J.H. (project number 16599). X.H. was supported in part by the University of San Francisco Faculty Development Fund. G.L. and Y.S. acknowledge the support from the China Manned Spaced Project (CMS-CSST-2021-A12). Funding Information: F.P. acknowledges support from the Spanish State Research Agency (AEI) under grant No. PID2019-105552RB-C43. S.D. acknowledges support from the European Union{\textquoteright}s Horizon 2020 research and innovation program Marie Skodowska-Curie Individual Fellowship (grant agreement No. 890695), and a Junior Research Fellowship at Lucy Cavendish College, Cambridge. T.P. acknowledges the financial support from the Slovenian Research Agency (grants I0-0033, P1-0031, J1-8136 and Z1-1853). This work was supported by a collaborative visit funded by the Slovenian Research Agency (ARRS, travel grant number BI-US/22-24-006). I.P.-F. acknowledges support from the Spanish State Research Agency (AEI) under grant number PID2019-105552RB-C43. C.G. is supported by a VILLUM FONDEN Young Investigator Grant (project number 25501). C.L. acknowledges support from the National Science Foundation Graduate Research Fellowship under grant No. DGE-2233066. Funding Information: We would like to thank David Jones, Nao Suzuki, and Taylor Hoyt for discussions helpful to the analysis in this work. This paper is based in part on observations with the NASA/ESA Hubble Space Telescope obtained from the Mikulski Archive for Space Telescopes at STScI. The specific observations analyzed can be accessed via DOI: 10.17909/gvys-q017 ; support was provided to J.D.R.P. and M.E. through program HST-GO-16264. S.E. and S.H.S. thank the Max Planck Society for support through the Max Planck Research Group for S.H.S. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51492 awarded to A.J.S. by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This work has also been enabled by support from the research project grant “Understanding the Dynamic Universe” funded by the Knut and Alice Wallenberg Foundation under Dnr KAW 2018.0067. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (LENSNOVA: grant agreement No. 771776). This research is supported in part by the Excellence Cluster ORIGINS which is funded by the Deutsche Forschungsgemeinschaft (DFG; German Research Foundation) under Germany{\textquoteright}s Excellence Strategy—EXC-2094—390783311. S.S. acknowledges financial support through grants PRIN-MIUR 2017WSCC32 and 2020SKSTHZ. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). J.H., C.C., and R.W. were supported by a VILLUM FONDEN Investigator grant to J.H. (project number 16599). X.H. was supported in part by the University of San Francisco Faculty Development Fund. G.L. and Y.S. acknowledge the support from the China Manned Spaced Project (CMS-CSST-2021-A12). Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",
year = "2023",
month = may,
day = "1",
doi = "10.3847/1538-4357/acc7a6",
language = "English (US)",
volume = "948",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",
}