Discovery of an Apparent Red, High-velocity Type Ia Supernova at z = 2.9 with JWST
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jats:titleAbstract</jats:title> jats:pWe present the James Webb Space Telescopejats:italic </jats:italic>(JWST) discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS+53.13485−27.82088 with a host spectroscopic redshift of 2.903 ± 0.007. The transient was identified in deep (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic follow-up with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (jats:italicc</jats:italic> ∼ 0.9) despite a host galaxy with low extinction and has a high Ca jats:scii</jats:sc> velocity (19,000 ± 2000 km sjats:sup−1</jats:sup>) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-jats:italicz</jats:italic> Ca-rich population. Although such an object is too red for any low-jats:italicz </jats:italic>cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (≲1jats:italicσ</jats:italic>) with ΛCDM. Therefore unlike low-jats:italicz</jats:italic> Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high jats:italicz</jats:italic> truly diverge from their low-jats:italicz</jats:italic> counterparts and to confirm that standardized luminosities nevertheless remain constant with redshift.</jats:p>
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Acknowledgements: We would like to thank Erin Hayes, Saurabh Jha, and Rick Kessler for the useful discussion. We thank the DDT and JWST/HST scheduling teams at STScI for the extraordinary effort in getting the DDT observations used here scheduled quickly. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #1180 and 6541. Part of the JWST data used in this Letter can be found in MAST (Rieke et al. 2023; JADES DR1). Additionally, this work made use of the lux supercomputer at UC Santa Cruz, which is funded by NSF MRI grant AST 1828315, as well as the High Performance Computing (HPC) resources at the University of Arizona, which is funded by the Office of Research Discovery and Innovation (ORDI), Chief Information Officer (CIO), and University Information Technology Services (UITS). A.J.B. acknowledges funding from the “FirstGalaxies” Advanced Grant from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 789056). P.A.C., E.E., D.J.E., and B.D.J. are supported by a JWST/NIRCam contract to the University of Arizona, NAS5-02015. D.J.E. is also supported as a Simons Investigator. R.M. acknowledges support by the Science and Technology Facilities Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH,” and by the UKRI Frontier Research grant RISEandFALL. R.M. also acknowledges funding from a research professorship from the Royal Society. B.E.R. acknowledges support from the NIRCam Science Team contract to the University of Arizona, NAS5-02015, and JWST Program 3215. JDRP is supported by NASA through a Einstein Fellowship grant No. HF2-51541.001 awarded by the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555.
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2041-8213