We report on TOO BeppoSAX observations af the superluminal galactic source GRS1915+105 in its high flux state. The TOO mas triggered by the Wide Field Cameras, and the source mas then followed up for about a month with a long (100 ksec) observation and a set of nine 10 ksec snapshots. The source exhibited strong flux and spectral variability over the whole energy range (0.1-300 keV). We present here the spectral analysis carried out on a portion of the longer observation. The low energy (0.1-10 keV) spectrum taken in a phase of lack of spectral variability can be reasonably well fitted with an absorbed power law plus a multicolor blackbody. Clear evidence for a Fe K alpha emission line at 6.7 keV is also found, which an intensity that may be not directly correlated with continuum flux variation.
Feroci, M., Costa, E., Matt, G., Belloni, T., Tavani, M. (1999). BeppoSAX observation of the superluminal galactic source GRS1915+105. NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS, 69(1-3), 336-339 [10.1016/S0920-5632(98)00235-7].
BeppoSAX observation of the superluminal galactic source GRS1915+105
MATT, Giorgio;
1999-01-01
Abstract
We report on TOO BeppoSAX observations af the superluminal galactic source GRS1915+105 in its high flux state. The TOO mas triggered by the Wide Field Cameras, and the source mas then followed up for about a month with a long (100 ksec) observation and a set of nine 10 ksec snapshots. The source exhibited strong flux and spectral variability over the whole energy range (0.1-300 keV). We present here the spectral analysis carried out on a portion of the longer observation. The low energy (0.1-10 keV) spectrum taken in a phase of lack of spectral variability can be reasonably well fitted with an absorbed power law plus a multicolor blackbody. Clear evidence for a Fe K alpha emission line at 6.7 keV is also found, which an intensity that may be not directly correlated with continuum flux variation.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
