The effect of dust obscuration in RR Telescopii on optical and IR long-term photometry and Fe II emission lines

¹ Physics Department, Faculty of Arts and Sciences, Omladinska 14, 51000 Rijeka, Croatia e-mail: dubravka.karuza-kotnik@ri.htnet.hr
² Institut d'Astrophysique de Paris UMR7075 CNRS, Université Pierre & Marie Curie, 98 bis Boulevard Arago, 75014 Paris, France e-mail: friedjung@iap.fr
³ South African Astronomical Observatory, Observatory, South Africa and national Astrophysics and Space Science Programme, University of Cape Town, 7701 Rondebosch, South Africa e-mail: paw@saao.ac.za
⁴ Instituto de Astrofisica de Canarias, La Laguna (Tenerife), Spain e-mail: katrina@iac.es
⁵ Dept. of pure and applied physics, Queens University, Belfast, Northern Ireland e-mail: F.Keenan@qub.ac.uk

Received: 12 September 2005
Accepted: 19 January 2006

Abstract

Aims.Infrared and optical photometric and spectroscopic observations of the symbiotic nova RR Tel are used to study the effects and properties of dust in symbiotic binaries containing a cool Mira component, as well as showing “obscuration events” of increased absorption, which are typical for such Miras.

Methods.A set of photometric observations of the symbiotic nova RR Tel in different wavelength bands – visual from 1949 to 2002 and near-infrared () from 1975 to 2002 – are presented. The variability due to the normal Mira pulsation was removed from the JHKL data, which were then compared with the American Association of Variable Star Observers' () visual light curve. The changes of the Fe II emission line fluxes during the 1996-2000 obscuration episode were studied in the optical spectra taken with the Anglo-Australian telescope.

Results.We discuss the three periods during which the Mira component was heavily obscured by dust as observed in the different wavelength bands. A change in the correlations of J with other infrared magnitudes was observed with the colour becoming redder after JD 2 446 600. Generally, was comparable, while was larger than typical values for single Miras. A distance estimate of 2.5 kpc, based on the IR data, is given. A larger flux decrease for the permitted than for the forbidden Fe II lines, during the obscuration episode studied, has been found. There is no evidence for other correlations with line properties, in particular with wavelength, which suggests obscuration due to separate optically thick clouds in the outer layers.