@article {23936, title = {M31N 2005-09c: a fast Fe II nova in the disk of M 31}, volume = {464}, year = {2007}, month = {2007/03/1}, pages = {1075 - 1079}, abstract = {Context: Classical novae are quite frequent in M 31. However, very few spectra of M 31 novae have been studied to date, especially during the early decline phase.
Aims: Our aim is to study the photometric and spectral evolution of a M 31 nova event close to outburst.
Methods: Here, we present photometric and spectroscopic observations of M31N 2005-09c, a classical nova in the disk of M 31, using the 1.3 m telescope of the Skinakas Observatory in Crete (Greece), starting on the 28th September, i.e. about 5 days after outburst, and ending on the 5th October 2005, i.e. about 12 days after outburst. We also have supplementary photometric observations from the La Sagra Observatory in Northern Andaluc{\'\i}a, Spain, on September 29 and 30, October 3, 6 and 9 and November 1, 2005. The wavelength range covered by the spectra is from 3565 {\r A} to 8365 {\r A}. The spectra are of high S/N allowing the study of the evolution of the equivalent widths of the Balmer lines, as well as the identification of non-Balmer lines.
Results: The nova displays a typical early decline spectrum that is characterized by many weak Fe II multiplet emissions. It is classified as a Pfe nova. From the nova light curve, we have also derived its speed class, t_2=14{\textpm}2.5 days. As the nova evolved the Balmer lines became stronger and narrower. The early decline of the expansion velocity of the nova follows a power law in time with an exponent of ≃-0.2.}, keywords = {Astrophysics, CATACLYSMIC VARIABLES, galaxies: individual: M 31, STARS: NOVAE}, isbn = {0004-6361}, url = {https://ui.adsabs.harvard.edu/abs/2007A\&A...464.1075H}, author = {Hatzidimitriou, D. and Reig, P. and Manousakis, A. and Pietsch, W. and Burwitz, V. and Papamastorakis, I.} }