Y Gem, a symbiotic star outshone by its asymptotic giant branch primary component

¹ Instituto de Astrofísica de Andalucía, IAA-CSIC, Glorieta de la Astronomía S/N, Granada 18008, Spain
² Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, Mexico
³ Escola de Artes, Ciências e Humanidades, USP, Av. Arlindo Bettio 1000, 03828-000 São Paulo, Brazil

^⋆ Corresponding author; mar@iaa.es

Received: 30 July 2024
Accepted: 21 November 2024

Abstract

Context. A considerable number of asymptotic giant branch (AGB) stars exhibit UV excess and/or X-ray emission that indicates a binary companion. AGB stars are so bright that they easily outshine their companions. This almost prevents their identification. Y Gem has been known for some decades to be an AGB star that is bright in the far-UV and X-rays, but it is unclear whether its companion is a main-sequence star or a white dwarf (WD) in a symbiotic system (SySt).

Aims. Our goal is to uncover the true nature of Y Gem, which will help us to study the possible misidentified population of SySts.

Methods. Multiwavelength IR, optical, UV, and X-ray observations were analyzed to investigate the properties of the stellar components and the accretion process in Y Gem. In particular, an optical spectrum of Y Gem is presented here for the first time, while X-ray data are interpreted by means of reflection models produced by an accretion disk and material in its vicinity.

Results. The optical spectrum exhibits the typical sawtooth-shaped features of molecular absorptions in addition to narrow recombination and forbidden emission lines. The emission lines and the analysis of the extinction-corrected UV spectrum suggest a hot component with T_eff ≈ 60 000 K, L = 140 L_⊙, and R = 0.11 R_⊙ that very likely is an accreting WD. The late component is found to be an 1.1 M_⊙ AGB star with T_eff = 3350 K and R = 240 R_⊙.

Conclusions. Using IR, optical, UV, and X-ray data, we found that Y Gem is an S-type SySt whose compact component is accreting at an estimated mass-accretion rate of Ṁ_acc = 2.3 × 10⁻⁷ M_⊙ yr⁻¹. At this accretion rate, the accreting WD has reached the stable and steady burning phase in which no recurrent events are expected.