Spectro-photometric follow-up of the outbursting AM CVn system ASASSN-21br

• Published in: Monthly notices of the Royal Astronomical Society Vol. 532; no. 4; pp. 4205 - 4216
• Main Authors: Painter, S, Aydi, E, Motsoaledi, M, Sokolovsky, K V, Strader, J, Buckley, D A H, Kochanek, C S, Maccarone, T J, Mukai, K, Shappee, B J, Stanek, K Z
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 06-08-2024
• Subjects: Absorption; Accretion disks; Background noise; Emission spectra; Gravitational waves; Line spectra; Orbits; Outbursts; Photometry; Sky surveys (astronomy); Spectrum analysis; cataclysmic variables; binaries; white dwarf
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stae1726

ABSTRACT
We report on spectroscopic and photometric observations of the AM Canum Venaticorum (AM CVn) system ASASSN-21br, which was discovered in outburst by the All-Sky Automated Survey for Supernovae in 2021 February. The outburst lasted for around three weeks, and exhibited a pronounced brightness dip for $\approx$4 d, during which the spectra showed a sudden transition from emission- to absorption-line dominated. Only $\approx$60 AM CVn systems with derived orbital periods are found in the Galaxy, therefore increasing the sample of AM CVn systems with known orbital periods is of tremendous importance to (1) constrain the physical mechanisms of their outbursts and (2) establish a better understanding of the low-frequency background noise of future gravitational wave surveys. Time-resolved photometry taken during the outburst of ASASSN-21br showed modulation with a period of around 36.65 min, which is likely the superhump or orbital period of the system. Time-resolved spectroscopy taken with the Southern African Large Telescope did not show any sign of periodicity in the He i absorption lines. This is possibly due to the origin of these lines in the outbursting accretion disc, which makes it challenging to retrieve periodicity from the spectral lines. Future follow-up spectral observations during quiescence might allow us better constrain the orbital period of ASASSN-21br.