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Yan, H.Ma, Z.
Sun, B.
Wang, L.
Kelly, P.
Diego, J.M.
Cohen, S.H.
Windhorst, R.A.
Jansen, R.A.
Grogin, N.A.
Beacom, J.F.
Conselice, C.J.
Driver, S.P.
Frye, B.
Coe, D.

Marshall, M.A.
Koekemoer, A.

Willmer, C.N.A.
Robotham, A.
D’Silva, J.C.J.
Summers, J.
Nonino, M.
Pirzkal, N.
Ryan, R.E., Jr.
Ortiz, R., III
Tompkins, S.
Bhatawdekar, R.A.
Cheng, C.
Zitrin, A.

Willner, S.P.
Affiliation
Steward Observatory, University of ArizonaIssue Date
2023-11-22
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American Astronomical SocietyCitation
Haojing Yan et al 2023 ApJS 269 43Rights
© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
With its unprecedented sensitivity and spatial resolution, the James Webb Space Telescope (JWST) has opened a new window for time-domain discoveries in the infrared. Here we report observations in the only field that has received four epochs (spanning 126 days) of JWST NIRCam observations in Cycle 1. This field is toward MACS J0416.1−2403, which is a rich galaxy cluster at redshift z = 0.4 and is one of the Hubble Frontier Fields. We have discovered 14 transients from these data. Twelve of these transients happened in three galaxies (with z = 0.94, 1.01, and 2.091) crossing a lensing caustic of the cluster, and these transients are highly magnified by gravitational lensing. These 12 transients are likely of a similar nature to those previously reported based on the Hubble Space Telescope (HST) data in this field, i.e., individual stars in the highly magnified arcs. However, these 12 could not have been found by HST because they were too red and too faint. The other two transients are associated with background galaxies (z = 2.205 and 0.7093) that are only moderately magnified, and they are likely supernovae. They indicate a demagnified supernova surface density, when monitored at a time cadence of a few months to a ∼3-4 μm survey limit of AB ∼28.5 mag, of ∼0.5 arcmin−2 integrated to z ≈ 2. This survey depth is beyond the capability of HST but can be easily reached by JWST. © 2023. The Author(s). Published by the American Astronomical Society.Note
Open access journalISSN
0067-0049Version
Final Published Versionae974a485f413a2113503eed53cd6c53
10.3847/1538-4365/ad0298
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Except where otherwise noted, this item's license is described as © 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.