منابع مشابه
XMM - NEWTON High Resolution Spectroscopy of NGC 5548
We analyze a 137 ks exposure X-ray spectrum of the Seyfert 1 galaxy NGC 5548 obtained with the XMM-Newton Reflection Grating Spectrometer. Due to the long exposure time, the spectrum is of higher statistical quality than the previous observations of this AGN. Therefore, we detect for the first time in NGC 5548 inner-shell transitions from O III to O VI ions, and the Unresolved Transition Array ...
متن کاملObservations of Ngc 5548
We present simultaneous observations by EUV E, ASCA, and RXT E of the type 1 Seyfert galaxy NGC 5548. These data indicate that variations in the EUV emission (at D0.2 keV) appear to lead similar modulations in higher energy keV) X-rays by D10È30 ks. This is contrary to popular (Z1 models which attribute the correlated variability of the EUV, UV and optical emission in type 1 Seyferts to reproce...
متن کاملThe Soft and Medium–energy X–ray Variability of Ngc 5548: a Reanalysis of Exosat Observations
We present a detailed cross–correlation (CCF) and power spectrum re–analysis of the X–ray light curves of the bright Seyfert 1 galaxy NGC5548 obtained with EXOSAT. The 0.05–2 keV and 1–4 keV light curves are cross–correlated with the 1–9 keV and 4–9 keV light curves respectively. We discuss how spurious time lags can be introduced by systematic effects related to detector swapping as well as th...
متن کاملBeppoSAX spectroscopy of the NGC 7078 ( M 15 ) globular cluster X - ray source X 2127 + 119
Results of a 1999 November 16–17 BeppoSAX observation of the low-mass X-ray binary X 2127+119 located in the globular cluster M15 are presented. The system is believed to be one where the central neutron star is normally obscured by the accretion disk, and only X-rays scattered into our line of sight by an extended accretion disk corona (ADC) are observed. The 0.1–10 keV lightcurve is energy de...
متن کاملPhysical properties of the BLR of NGC 5548 3
We investigate the variability of physical parameters in the Broad Line Region (BLR) of NGC 5548 using the Boltzmann plot (BP) method. We apply the method on the Balmer lines observed from 1996 to 2004, and find that variability earlier detected in the lines, is also present in the temperature. We find that the average temperature for the considered period was T≈ 10000 K, and that varies from 6...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2002
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20020235