Spectroscopic and Photometric Development of T Pyxidis (2011) from 0.8 to 250 Days After Discovery

TL;DR

This study provides a detailed analysis of T Pyxidis's 2011 nova outburst, combining high-cadence optical photometry and spectroscopy to reveal phases of mass loss, spectral evolution, and correlations with X-ray and radio emissions.

Contribution

It offers the first high-cadence SMEI light curve analysis of T Pyxidis, identifying distinct phases and stages of mass loss, and correlates spectral features with multi-wavelength observations.

Findings

Detected a 1.44-day periodicity before maximum brightness.

Identified two stages of mass loss with different characteristics.

Correlated spectral evolution with X-ray and radio light curves.

Abstract

We investigated the optical light curve of T Pyx during its 2011 outburst through compiling a database of SMEI and AAVSO observations. The SMEI light curve, providing unprecedented detail with high cadence data during t=1.5-49 days post-discovery, was divided into four phases based on the idealised nova optical light curve; the initial rise, the pre-maximum halt (or the 'plateau'), the final rise, and the early decline. Variation in the SMEI light curve reveals a strongly detected period of 1.44\pm0.04 days before the visual maximum. The spectra from the LT and SMARTS telescopes were investigated during t=0.8-80.7 and 155.1-249.9 days. The nova was observed very early in its rise and a distinct high velocity ejection phase was evident. A marked drop and then gradual increase in derived ejection velocities were present. Here we propose two different stages of mass loss, a short-lived phase occurring immediately after outburst followed by a more steadily evolving and higher mass loss phase. The overall spectral development follows that typical of a Classical Nova and comparison to the photometric behaviour reveals consistencies with the simple evolving pseudo-photosphere model of the nova outburst. The optical spectra are also compared to X-ray and radio light curves. Weak [Fe X] 6375A emission was marginally detected before the rise in X-ray emission. The middle of the plateau in the X-ray light curve is coincident with the appearance of high ionization species detected in optical spectra and the peak of the high frequency radio flux.