On the nature of V2282 Sgr
Abstract
The star V2282 Sgr is positionally consistent with a strong Chandra X-ray and a Spitzer/IRAC MIR source. We derived its long term -band light curve from the photographic archives of the Asiago and Catania Observatories, covering the years from 1965 to 1984. CCD photometry in Summer 2009 was re-analyzed. Optical spectra were secured at Loiano Observatory in 2011 and 2012. J H K photometry, obtained from several experiments in different epochs was compared and the Spitzer images were re-analyzed. V2282 Sgr was found to be irregular variable in all wavelengths. Spectroscopically, it shows strong emission features (H Balmer lines, [NII]6584 AA and [OIII]5007/4959 AA) while the Na D doublet is very strong, indicating a circumstellar envelope. A single thermal energy distribution cannot reproduce the observed SED, while it can be explained as the sum of a G-type star plus a variable circumstellar disc, which mimics a class 0/I object. Most likely, V2282 Sgr is a 1-2 mass pre main sequence star with an accretion disk.
Keywords
Cite
@article{arxiv.1312.0085,
title = {On the nature of V2282 Sgr},
author = {Roberto Nesci and Corinne Rossi and Antonio Frasca and Ettore Marilli and Paolo Persi},
journal= {arXiv preprint arXiv:1312.0085},
year = {2018}
}
Comments
13 pages, 7 figure, in press on Baltic Astronomy