BeppoSAX observed 8 times the gamma-ray bright blazar PKS 0528+134 in Feb. and Mar. 1997, during a multiwavelength campaign involving EGRET, onboard CGRO, and ground based telescopes. The source was in its faintest X-ray state observed so far, with an unabsorbed [2-10] keV flux of 2.5 x 10(-12) erg cm(-2) s(-1). The spectrum can be fitted with a power law, with energy index alpha(X) = 0.49 +/- 0.07 between 0.1 and 10 keV. The high energy instrument PDS detected a flux in the 15-100 keV band which appears disconnected from the lower X-ray energies, most likely due to a contaminating source. We consider our findings in the context of the overall spectral energy distribution and discuss their implications for synchrotron and inverse Compton models.

The blazar PKS 0528+134: new results from BeppoSAX observations / Ghisellini, G.; Tagliaferri, G.; Costamante, L.; Maraschi, L.; Celotti, Anna Lisa; Fossati, G.; Bassani, L.; Cappi, M.; Frontera, F.; Pian, E.; Comastri, A.; Cavallone, M.; DE FRANCESCO, G.; Lanteri, L.; Raiteri, C. M.; Sobrito, G.; Villata, M.; Giarrusso, S.; Sacco, B.; Glass, I. S.; Grandi, P.; Molendi, S.; Padovani, P.; Palumbo, G. G. C.; Perola, C.; Salvati, M.; Treves, A.. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 348:1(1999), pp. 63-70.

The blazar PKS 0528+134: new results from BeppoSAX observations

Celotti, Anna Lisa;
1999-01-01

Abstract

BeppoSAX observed 8 times the gamma-ray bright blazar PKS 0528+134 in Feb. and Mar. 1997, during a multiwavelength campaign involving EGRET, onboard CGRO, and ground based telescopes. The source was in its faintest X-ray state observed so far, with an unabsorbed [2-10] keV flux of 2.5 x 10(-12) erg cm(-2) s(-1). The spectrum can be fitted with a power law, with energy index alpha(X) = 0.49 +/- 0.07 between 0.1 and 10 keV. The high energy instrument PDS detected a flux in the 15-100 keV band which appears disconnected from the lower X-ray energies, most likely due to a contaminating source. We consider our findings in the context of the overall spectral energy distribution and discuss their implications for synchrotron and inverse Compton models.
1999
348
1
63
70
Ghisellini, G.; Tagliaferri, G.; Costamante, L.; Maraschi, L.; Celotti, Anna Lisa; Fossati, G.; Bassani, L.; Cappi, M.; Frontera, F.; Pian, E.; Comastri, A.; Cavallone, M.; DE FRANCESCO, G.; Lanteri, L.; Raiteri, C. M.; Sobrito, G.; Villata, M.; Giarrusso, S.; Sacco, B.; Glass, I. S.; Grandi, P.; Molendi, S.; Padovani, P.; Palumbo, G. G. C.; Perola, C.; Salvati, M.; Treves, A.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/16180
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