PTF11kx: A Type Ia Supernova with Hydrogen Emission Persisting after 3.5 Years
Abstract
The optical transient PTF11kx exhibited both the characteristic spectral features of Type Ia supernovae (SNe Ia) and the signature of ejecta interacting with circumstellar material (CSM) containing hydrogen, indicating the presence of a nondegenerate companion. In this paper, we present an optical spectrum at 1342 days after peak from Keck Observatory, in which the broad component of Hα emission persists with a similar profile as in early-time observations. We also present Spitzer IRAC detections obtained 1237 and 1818 days after peak, and an upper limit from Hubble Space Telescope ultraviolet imaging at 2133 days. We interpret our late-time observations in the context of published results—and reinterpret the early-time observations—in order to constrain the CSM's physical parameters and to compare to theoretical predictions for recurrent-nova systems. We find that the CSM's radial extent may be several times the distance between the star and the CSM's inner edge, and that the CSM column density may be two orders of magnitude lower than previous estimates. We show that the Hα luminosity decline is similar to other SNe with CSM interaction and demonstrate how our infrared photometry is evidence for newly formed, collisionally heated dust. We create a model for PTF11kx's late-time CSM interactionmore »
- Authors:
-
[1];
[2];
[3];
[2];
[5];
[4]
- Univ. of Washington, Seattle, WA (United States); Univ. of California, Berkeley, CA (United States)
- Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
- Space Telescope Science Inst., Baltimore, MD (United States)
- Univ. of California, Berkeley, CA (United States)
- Univ. of Texas, Austin, TX (United States)
- Publication Date:
- Research Org.:
- Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
- Sponsoring Org.:
- USDOE; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF)
- OSTI Identifier:
- 1379907
- Grant/Contract Number:
- AC02-05CH11231; NAS5-26555; AST-1211916; AST-1302771
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 843; Journal Issue: 2; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; supernovae; PTF11kx
Citation Formats
Graham, M. L., Harris, C. E., Fox, O. D., Nugent, P. E., Kasen, D., Silverman, J. M., and Filippenko, A. V. PTF11kx: A Type Ia Supernova with Hydrogen Emission Persisting after 3.5 Years. United States: N. p., 2017.
Web. doi:10.3847/1538-4357/aa78ee.
Graham, M. L., Harris, C. E., Fox, O. D., Nugent, P. E., Kasen, D., Silverman, J. M., & Filippenko, A. V. PTF11kx: A Type Ia Supernova with Hydrogen Emission Persisting after 3.5 Years. United States. https://doi.org/10.3847/1538-4357/aa78ee
Graham, M. L., Harris, C. E., Fox, O. D., Nugent, P. E., Kasen, D., Silverman, J. M., and Filippenko, A. V. Tue .
"PTF11kx: A Type Ia Supernova with Hydrogen Emission Persisting after 3.5 Years". United States. https://doi.org/10.3847/1538-4357/aa78ee. https://www.osti.gov/servlets/purl/1379907.
@article{osti_1379907,
title = {PTF11kx: A Type Ia Supernova with Hydrogen Emission Persisting after 3.5 Years},
author = {Graham, M. L. and Harris, C. E. and Fox, O. D. and Nugent, P. E. and Kasen, D. and Silverman, J. M. and Filippenko, A. V.},
abstractNote = {The optical transient PTF11kx exhibited both the characteristic spectral features of Type Ia supernovae (SNe Ia) and the signature of ejecta interacting with circumstellar material (CSM) containing hydrogen, indicating the presence of a nondegenerate companion. In this paper, we present an optical spectrum at 1342 days after peak from Keck Observatory, in which the broad component of Hα emission persists with a similar profile as in early-time observations. We also present Spitzer IRAC detections obtained 1237 and 1818 days after peak, and an upper limit from Hubble Space Telescope ultraviolet imaging at 2133 days. We interpret our late-time observations in the context of published results—and reinterpret the early-time observations—in order to constrain the CSM's physical parameters and to compare to theoretical predictions for recurrent-nova systems. We find that the CSM's radial extent may be several times the distance between the star and the CSM's inner edge, and that the CSM column density may be two orders of magnitude lower than previous estimates. We show that the Hα luminosity decline is similar to other SNe with CSM interaction and demonstrate how our infrared photometry is evidence for newly formed, collisionally heated dust. We create a model for PTF11kx's late-time CSM interaction and find that X-ray reprocessing by photoionization and recombination cannot reproduce the observed Hα luminosity, suggesting that the X-rays are thermalized and that Hα radiates from collisional excitation. In conclusion, we discuss the implications of our results regarding the progenitor scenario and the geometric properties of the CSM for the PTF11kx system.},
doi = {10.3847/1538-4357/aa78ee},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 843,
place = {United States},
year = {Tue Jul 11 00:00:00 EDT 2017},
month = {Tue Jul 11 00:00:00 EDT 2017}
}
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