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MIKE High Resolution Spectroscopy of Raman-scattered O VI and C II Lines in the Symbiotic Nova RR Telescopii

Published online by Cambridge University Press:  30 December 2019

Jeong-Eun Heo
Department of Physics and Astronomy, Sejong University, Seoul, Korea email:
Hee-Won Lee
Department of Physics and Astronomy, Sejong University, Seoul, Korea email:
Rodolfo Angeloni
Departamento de Física y Astronomía, Universidad de La Serena, La Serena, Chile
Tali Palma
Observatorio Astronómico, Universidad Nacional de Córdoba, Córdoba, Argentina
Francesco Di Mille
Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
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We present a high-resolution optical spectrum of the symbiotic nova RR Tel obtained with MIKE at Magellan-Clay telescope. RR Tel is a wide binary system of a hot white dwarf and a Mira with an orbital period of a few decades, where the white dwarf is accreting through gravitational capture of some fraction of material shed by the Mira. We find broad emission features at 6825, 7082, 7023, and 7053 Å, which are formed through Raman scattering of far-UV O VI ⋋⋋ 1032 and 1038 Å, C II ⋋⋋ 1036 and 1037 Å with atomic hydrogen. Raman O VI features exhibit clear double-peak profiles indicative of an accretion flow with a characteristic speed ∼ 30 km s−1, whereas the Raman C II features have a single Gaussian profile. We perform a profile analysis of the Raman O VI by assuming that O VI emission traces the accretion flow around the white dwarf with a fiducial scale of 1 AU. A comparison of the restored fluxes of C II ⋋⋋ 1036 and 1037 from Raman C II features with the observed C II ⋋ 1335 multiplet is consistent with the distance of RR Tel ∼ 2.6 kpc based on interstellar extinction of C II.

Contributed Papers
© International Astronomical Union 2019 


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