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Published July 11, 2018 | Published + Accepted Version
Journal Article Open

Discovery of an old nova shell surrounding the cataclysmic variable V1315 Aql


Following our tentative discovery of a faint shell around V1315 Aql reported in Sahman et al., we undertook deep Hα imaging and intermediate-resolution spectroscopy of the shell. We find that the shell has its geometric centre located on V1315 Aql. The mass, spectral features, and density of the shell are consistent with other nova shells, rather than planetary nebulae or supernova remnants. The radial velocity of the shell is consistent with the systemic velocity of V1315 Aql. We believe this evidence strongly suggests that the shell originates from an earlier nova event. This is the first nova shell discovered around a nova-like and supports the theory of nova-induced cycles in mass transfer rates (hibernation theory) first proposed by Shara et al.

Additional Information

© 2018 The Author(s) Published by Oxford University Press on behalf of the 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/about_us/legal/notices) Accepted 2018 April 12. Received 2018 March 29; in original form 2018 March 19. We would like to thank the referee for his helpful comments and for pointing out the latest AAVSO light curve of BK Lyn demonstrating Z Cam-like behaviour. We acknowledge with thanks the variable star observations from the AAVSO International Database, contributed by observers worldwide and used in this research. VSD and SPL were supported under grants from the Science and Technology Facilities Council (STFC). This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported from the Spanish Ministerio de Ciencia e Innovacion through grant AyA2011-24052. The INT is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. 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.

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