TESS photometry of the nova eruption in V606 Vul: asymmetric photosphere and multiple ejections?

Kirill V. Sokolovsky, Elias Aydi, Konstantin Malanchev, Colin J. Burke, Koji Mukai, J. L. Sokoloski, Brian D. Metzger, Kirill E. Atapin, Aleksandre A. Belinski, Yu-Ching Chen, Laura Chomiuk, Pavol A. Dubovsky, Claude-Andre Faucher-Giguere, Rebekah A. Hounsell, Natalia P. Ikonnikova, Vsevolod Yu. Lander, Junyao Li, Justin D. Linford, Amy J. Mioduszewski, Isabella Molina, Ulisse Munari, Sergey A. Potanin, Robert M. Quimby, Michael P. Rupen, Simone Scaringi, Nicolai I. Shatsky, Yue Shen, Elad Steinberg, Zachary Stone, Andrey M. Tatarnikov, Indrek Vurm, Montana N. Williams, Antonio Agudo Azcona, David Boyd, Stewart Bean, Horst Braunwarth, John Blackwell, Simone Bolzoni, Ricard Casas, David Cejudo Fernandez, Franky Dubois, James Foster, Rafael Farfan, Charles Galdies, John Hodge, Jose Prieto Gallego, David J. Lane, Magnus Larsson, Peter Lindner, Ludwig Logie, Andrea Mantero, Mario Morales Aimar, Kenneth Menzies, Keith Nakonechny, Jerry Philpot, Antonio Padilla Filho, Brian Ramey, Steve Rau, Esteban Reina, Filipp D. Romanov, Nello Ruocco, Jeremy Shears, Marc Serreau, Richard Schmidt, Yuri Solomonov, Bob Tracy, Gord Tulloch, Ray Tomlin, Tamas Tordai, Siegfried Vanaverbeke, Klaus Wenzel

Published 2023-11-08Version 1

Lightcurves of many classical novae deviate from the canonical "fast rise - smooth decline" pattern and display complex variability behavior. We present the first TESS-space-photometry-based investigation of this phenomenon. We use TESS Sector 41 full-frame images to extract a lightcurve of the slow Galactic nova V606 Vul that erupted nine days prior to the start of the TESS observations. The lightcurve covers the first of two major peaks of V606 Vul that was reached 19 days after the start of the eruption. The nova reached its brightest visual magnitude V=9.9 in its second peak 64 days after the eruption onset, following the completion of Sector 41 observations. To increase the confidence level of the extracted lightcurve, we performed the analysis using four different codes implementing the aperture photometry (Lightkurve, VaST) and image subtraction (TESSreduce, tequila_shots) and find good agreement between them. We performed ground-based photometric and spectroscopic monitoring to complement the TESS data. The TESS lightcurve reveals two features: periodic variations (0.12771d, 0.01mag average peak-to-peak amplitude) that disappeared when the source was within 1mag of peak optical brightness and a series of isolated mini-flares (with peak-to-peak amplitudes of up to 0.5mag) appearing at seemingly random times. We interpret the periodic variations as the result of azimuthal asymmetry of the photosphere engulfing the nova-hosting binary that was distorted by and rotating with the binary. Whereas we use spectra to associate the two major peaks in the nova lightcurve with distinct episodes of mass ejection, the origin of mini-flares remains elusive.