Spectroscopy of the first resolved strongly lensed Type Ia supernova iPTF16geu
Abstract
We report the results from spectroscopic observations of the multiple images of the strongly lensed Type Ia supernova (SN Ia), iPTF16geu, obtained with ground-based telescopes and the Hubble Space Telescope (HST). From a single epoch of slitless spectroscopy with HST, we resolve spectra of individual lensed supernova images for the first time. This allows us to perform an independent measurement of the time-delay between the two brightest images, Δt = 1.4 ± 5.0 d, which is consistent with the time-delay measured from the light curves. We also present measurements of narrow emission and absorption lines characterizing the interstellar medium in the SN Ia host galaxy at z = 0.4087, as well as in the foreground lensing galaxy at z = 0.2163. We detect strong Na ID absorption in the host galaxy, indicating that iPTF16geu belongs to a subclass of SNe Ia displaying 'anomalously' large Na ID column densities compared to dust extinction derived from light curves. For the lens galaxy, we refine the measurement of the velocity dispersion, σ = 129 ± 4 km s⁻¹, which significantly constrains the lens model. We use ground-based spectroscopy, boosted by a factor ∼70 from lensing magnification, to study the properties of a high-z SN Ia with unprecedented signal-to-noise ratio. The spectral properties of the supernova, such as pseudo-Equivalent widths of several absorption features and velocities of the Si II-line, indicate that iPTF16geu is a normal SN Ia. We do not detect any significant deviations of the SN spectral energy distribution from microlensing of the SN photosphere by stars and compact objects in the lensing galaxy.
Additional Information
© 2020 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2020 December 8. Received 2020 November 24; in original form 2020 April 23. Published: 16 December 2020. We thank E. Zackrisson and A. Adamo for helpful discussions. We thank T. Brink, R. Bruch, Cooper, S. Goldwasser, A. Ho, I. Irani, B. Jain, Y. Sharma, A. Tzanidakis, Q. Ye, and W. Zheng for performing observations. AG acknowledges support from the Swedish National Space Agency and the Swedish Research Council. RL is supported by a Marie Skłodowska-Curie Individual Fellowship within the Horizon 2020 European Union (EU) Framework Programme for Research and Innovation (H2020-MSCA-IF-2017-794467). ASC acknowledges support from the G.R.E.A.T research environment, funded by Vetenskapsrådet, the Swedish Research Council. The Intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee (USA), the Oskar Klein Center at Stockholm University (Sweden), the Weizmann Institute of Science, the TANGO Program of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the Universe. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. These results made use of the Lowell Discovery Telescope at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale and by a grant from the Mt. Cuba Astronomical Foundation. Data Availability: All our spectra are available from the WISeREP archive (Yaron & Gal-Yam 2012).Attached Files
Published - staa3829.pdf
Submitted - 2004.10164.pdf
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Additional details
- Eprint ID
- 103707
- Resolver ID
- CaltechAUTHORS:20200604-151427243
- Swedish National Space Agency
- Swedish Research Council
- Marie Curie Fellowship
- H2020-MSCA-IF-2017-794467
- G.R.E.A.T. Research Environment
- W. M. Keck Foundation
- John and Ginger Giovale
- Mt. Cuba Astronomical Foundation
- Created
-
2020-06-05Created from EPrint's datestamp field
- Updated
-
2021-05-28Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department, Palomar Transient Factory, Division of Geological and Planetary Sciences (GPS)