The star V2282 Sgr is positionally consistent with a strong Chandra X-ray and a Spitzer/IRAC mid-infrared source. We derived its long-term I-band light curve from the photographic archives of the Asiago and Catania Observatories, covering the years from 1965 to 1984. Also, CCD R-c photometry of 2009 was re-analyzed. Optical spectra were collected at the Loiano Observatory in 2011 and 2012. J,H,K-s photometry, obtained from several sources 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] 6584A and [OIII] 5007/4959A) while the Na I 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 disk, which mimics YSO of class 0/I. Most likely, V2282 Sgr is a 1-2 M circle dot mass pre-main-sequence star with an accretion disk.
ON THE NATURE OF V2282 SGR / Nesci, Roberto; Rossi, Corinne; A., Frasca; E., Marilli; P., Persi. - In: BALTIC ASTRONOMY. - ISSN 1392-0049. - STAMPA. - 22:(2013), pp. 259-271.
ON THE NATURE OF V2282 SGR
NESCI, Roberto;ROSSI, Corinne;
2013
Abstract
The star V2282 Sgr is positionally consistent with a strong Chandra X-ray and a Spitzer/IRAC mid-infrared source. We derived its long-term I-band light curve from the photographic archives of the Asiago and Catania Observatories, covering the years from 1965 to 1984. Also, CCD R-c photometry of 2009 was re-analyzed. Optical spectra were collected at the Loiano Observatory in 2011 and 2012. J,H,K-s photometry, obtained from several sources 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] 6584A and [OIII] 5007/4959A) while the Na I 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 disk, which mimics YSO of class 0/I. Most likely, V2282 Sgr is a 1-2 M circle dot mass pre-main-sequence star with an accretion disk.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
