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Seyfert galaxy NGC5548 emits X-rays in quasi-periodic oscillations (QPOs). Analysis of data obtained by the Exosat satellite shows that NGC5548 is the first object with an active galactic nuclei (AGN) known to produce X-ray QPOs. Similar findings from compact galaxy X-ray binaries indicate that QPOs result from material being absorbed within a dense object, probably a black hole. However, the low estimated mass for the black hole that may exist within NGC5548's AGN may be hard to reconcile with current theories of AGN structure.

A 130-day hydroponic experiment was carried out in a glasshouse to examine whether manganese (Mn) concentration in the nutrient solution affects the nutritional status of olive plants and to find out whether the chlorophyll fluorescence technique is suitable to assess Mn toxicity and/or deficiency stress in olive plants prior to the appearance of these two nutritional disorders. For this purpose, chlorophyll fluorescence parameters (Fv/Fm and Fv/F0 ratios) were recorded every 40 days in the leaves of 'Kothreiki' and 'FS-17' olive cultivars, which were irrigated with Hoagland's nutrient solutions containing various Mn concentrations. In parallel the elongation of the main shoot of all experimental plants, as well as the concentrations of Mn, iron (Fe), zinc (Zn), boron (B), phosphorus (P), calcium (Ca), magnesium (Mg), and potassium (K) in their leaves were recorded. The following Mn treatments were applied: 0 μM Mn (to induce Mn deficiency), 40 μM Mn (to promote normal growth), and 640 μM Mn (to induce Mn toxicity). Our results indicated that not only the rate of shoot elongation but also the fluctuation with time of the leaf concentrations of all determined mineral elements (except for Mn) was not significantly affected by the Mn concentration in the nutrient solution, irrespectively of the cultivar. This was not observed with regard to the time variation of the Fv/Fm and Fv/F0 ratios, where the values of these parameters were significantly reduced in the 640 μM Mn treatment at the 80th and 130th day of the experiment in both olive cultivars, compared to the relevant previous ones (those of the days 0 and 40th), something which did not happen in the other two Mn treatments (0 and 40 μM). However, in none of the two cultivars tested and in any of the three Mn treatments (0, 40 and 640μM) the Fv/Fm and Fv/F0 ratios did not drop below the critical values of 0.8 and 4, respectively, even at the end of the experiment, where high Mn concentrations were found in the leaves of both cultivars treated with 640 μM Mn (616 μg g-1 d.w. in 'FS-17' and 734 μg g-1 d.w. in 'Kothreiki'). Symptoms of Mn toxicity (curling and brown speckles) were observed in the top leaves of both cultivars, after the 90th day of the experiment. At the same time, the final leaf Mn concentrations (those of the 130th day of the experiment) in plants grown under 0 μM Mn were 23 μg g-1 d.w. in 'FS-17' and 20 μg g-1 d.w. in 'Kothreiki', i.e., a little above of the deficiency range (<20 μg g-1 d.w.). At the 130th day, Mn concentration in nutrient solution, as well as Mn concentration in the leaves of both olive cultivars was negatively correlated with the leaf concentration of Fe and the values of the Fv/Fm and Fv/F0 ratios, and positively with the concentrations of Zn and P in the leaves. Finally, the periodical measurement of the Fv/Fm and Fv/F0 ratios was proved to be a non-reliable means to predict the appearance of the visible symptoms of Mn toxicity in olive leaves (although their values declined significantly at the 80th and 130th day of the experiment in both olive cultivars). [ABSTRACT FROM AUTHOR]

We present a comprehensive examination of the X-ray variability of the narrow-line Seyfert 1 (NLS1) galaxy NGC 4051, one of the most variable active galactic nuclei (AGN) in the sky. We combine over 6.5 years of frequent monitoring observations by RXTE with a >100-ks continuous observation by XMM–Newton and so present an overall 2–10 keV power spectral density (PSD) covering an unprecedented frequency range of over 6.5 decades from <10−8 to >10−2 Hz. The combined RXTE and XMM–Newton PSD is a very good match to the PSD of the galactic black-hole binary system (GBH) Cygnus X-1 when in a ‘high’, rather than ‘low’, state, providing the first definite confirmation of an AGN in a ‘high’ state. We also find that a bending power law, rather than a sharply broken power law, besides being more physical, is a much better description of the high-state PSD of Cygnus X-1 and is also a better description of the PSD of NGC 4051. At low frequencies the PSD of NGC 4051 has a slope of −1.1 bending, at a frequency Hz, to a slope of . Although does not depend on photon energy, is steeper at lower energies. If scales with mass, we imply a black-hole mass of in NGC 4051, which is consistent with the recently reported reverberation value of . Hence NGC 4051 is emitting at ∼30 per cent . NGC 4051 follows the same rms–flux relationship as GBHs, consistent with higher Fourier frequencies being associated with smaller radii. From the cross-power spectra and cross-correlation functions between XMM–Newton light curves in different energy bands, we note that the higher-energy photons lag the lower-energy ones. We also note that the lag is greater for variations of longer Fourier period and increases with the energy separation of the bands. Variations in different wavebands are very coherent at long Fourier periods but the coherence decreases at shorter periods and as the energy separation between bands increases. This behaviour is again similar to that of GBHs, and of MCG-6-30-15, and suggests a radial distribution of frequencies and photon energies with higher energies and higher frequencies being associated with smaller radii. Combining our observations with observations from the literature we find it is not possible to fit all AGN to the same linear scaling of break time-scale with black-hole mass. However, broad-line AGN are consistent with a linear scaling of break time-scale with mass from Cygnus X-1 in its low state and NLS1 galaxies scale better with Cygnus X-1 in its high state. We suggest that the relationship between black-hole mass and break time-scale is a function of at least one other underlying parameter which may be accretion rate or black-hole spin or both. [ABSTRACT FROM AUTHOR]

Presents the results from a study of the timing properties and the energy spectrum of the radio-quiet quasar PG 0804+761, based on monitoring RXTE/PCA observations that lasted for a year. Study of the X-ray variations on time-scales of weeks/months of the most luminous radio-quiet quasar studied so far; Significant variations in the 2 to 10 keV band of an average amplitude of ˜15 per cent; Power spectrum estimation at higher frequencies.

We present a series of RXTE observations of the nearby obscured Seyfert galaxies ESO103-G35, IC5063, NGC 4507 and NGC 7172. The period of monitoring ranges from seven days for NGC 7172 up to about seven months for ESO103-G035. The spectra of all galaxies fit well with a highly obscured (N[sub H]>10[sup 23] cm[sup -2]) power-law and an Fe line at 6.4 keV. We find strong evidence for the presence of a reflection component in ESO103-G35 and NGC 4507. The observed flux presents strong variability on day time-scales in all objects. Spectral variability is also detected in the sense that the spectrum steepens with increasing flux similar to the behaviour witnessed in some Seyfert 1 galaxies. [ABSTRACT FROM AUTHOR]

We present a flux variability study of simultaneous RXTE and EUVE observations of the highly variable Seyfert galaxy NGC 4051. We find a strong correlation between variability in the EUV and medium-energy X-ray bands, indicating that both are sampling the same power-law continuum. The lag between the two bands is less than 20 ks and, depending on model assumptions, may be <1 ks. We examine the consequences of such a small lag in the context of simple Comptonization models for the production of the power-law continuum. A lag of <1 ks implies that the size of the Comptonizing region is less than 20 Schwarzschild radii for a black hole of mass >10[sup 6] M[sub ⊙]. [ABSTRACT FROM AUTHOR]