Optical spectroscopic follow up of the classical nova V606 Vul (TCP J20210770+2914093)
ATel #14832; E. Aydi, K. V. Sokolovksy, J. Strader, L. Chomiuk, A. Kawash (MSU), Kwan-Lok Li (NCKU), N. Ikonnikova, K. E. Atapin, A. A. Belinski, M. A. Burlak, A. V. Dodin, N. A. Maslennikova, K. A. Postnov, S. A. Potanin, B. S. Safonov, N. I. Shatsky, and A. M. Tatarnikov (SAI Moscow State University)
on 6 Aug 2021; 19:45 UT
Credential Certification: Elias Aydi (aydielia@msu.edu)
Subjects: Optical, Binary, Cataclysmic Variable, Nova, Star, Transient, Variables
We report on spectroscopic follow up of the classical nova V606 Vul (TCP J20210770+2914093), which was discovered by Seiichiro Kiyota (Kamagaya, Japan) on 2021-07-16.56 UT, and classified spectroscopically as a classical nova by Munari et al. (ATel #14793).
We obtained several low- and medium-resolution spectra on 2021-07-29/30 using the Goodman spectrograph (Clemens et al. 2004, SPIE, 5492, 331) on the 4.1-m SOAR telescope (Cerro Pachon, Chile) and the 2.5-m SAI Moscow State University telescope (Kislovodsk, Russia). We also obtained low resolution spectra on 2021-08-05 using the 2.5-m SAI telescope. The spectra taken on July 29 and 30 show P Cygni profiles of Balmer, Fe II, and O I, with absorption troughs at blueshifted velocities of around 300 km/s. The spectra are consistent with that of a classical nova before optical peak. The spectra obtained on August 05, almost a week later, show the same lines but with multiple spectral components: P Cygni profiles with absorption troughs at blueshifted velocities of around 350 km/s superimposed on top of broad emissions with a FWZI of around 3200 km/s. These features are that of a classical nova after optical peak. This is consistent with the AAVSO optical light curve, which peaked at around 2021-08-02. The spectral evolution of nova V606 Vul is consistent with the paradigm of early spectral evolution of novae presented by Aydi et al. (2020; ApJ, 905, 62), which suggests the presence of two physically distinct outflows, a slow and fast one, during the early weeks of a nova event.
This ATel is based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes do Brasil (MCTIC/LNA), the U.S. National Science Foundation's National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).
