1. Figure 1. Three light curves of IRAS 13224–3809 in 600-s bins
Figure 1. Three light curves of IRAS 13224–3809 in 600-s bins. The energy bands (and average count rates) are (from top-down): 0.3–10 (1.74), 0.3–0.8 (1.30) and 3–10 (0.03) keV. 0 s on the time axis marks the start of the observation at 03:15:02 on 2002 January 19. The region of high background flaring has been omitted.
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

2. Figure 2. The EPF as a function of bin width calculated for IRAS 13224–3809. The dotted line is the estimated level of the EPF expected from Poisson noise. The faint, solid line is a power-law fit to the 85–1000 s (1.2 × 10⁻²−10⁻³ Hz) region, with a normalization of 0.013<sup arrange="stack">+0.003</sup><sub arrange="stack">−0.002</sub> and an index of ± This measured index is related to the power-law index of the power spectrum (α), and consistent with α=−1.619 (see Yaqoob et al for a detailed explanation).
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

3. Figure 3. Six of the CCFs calculated from the light curves with 600-s binning. The energy bands being cross-correlated are shown in the top left of each window. The calculations were conducted such that a positive shift in time would indicate a lag of the second energy band.
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

4. Figure 4. The lag measured between the 3–10 keV and 0. 3–0
Figure 4. The lag measured between the 3–10 keV and 0.3–0.8 keV light curves, in 4500-s intervals, over the duration of the observation. The lag alternates in such a way that at times the soft band leads the hard (positive lag), and at other times, the hard leads the soft (negative lag). The time interval during which the background flare occurs has been omitted.
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

5. Figure 5. A typical hardness ratio variability curve
Figure 5. A typical hardness ratio variability curve. In this example, H= 1.5–10 keV and S= 0.3–1.5 keV (see text for details). 0 s on the time axis marks the start of the observation at 03:15:02 on 2002 January 19. The region of high background flaring has been omitted.
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

6. Figure 6. Four normalized X-ray light curves in various energy bands, and in 10-ks bins. After ∼40 ks, the amplitude of the fluctuations becomes greater in the 3–10 keV band than in the softer energy bands. Note that although the count rate error bars are plotted, they are too small to see in some of the light curves.
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

7. Figure 7. ƒ_var calculated in nine energy bins between 0.2 and 10 keV. The light curves used were in bins of 200 s.
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

8. Figure 8. Four hardness ratios correlated with count rates
Figure 8. Four hardness ratios correlated with count rates. The bands used are show in the upper left of each panel. The count rates used are the summation of H and S.
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

9. Figure 9. The cross-correlation of the H= 0. 8–1. 5 keV and S= 0. 3–0
Figure 9. The cross-correlation of the H= 0.8–1.5 keV and S= 0.3–0.8 keV light curve and hardness ratio variability curve. The CCF indicates a short delay between the two curves, such that the hardness ratio curve lags behind the light curve.
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS

10. Table 1. Comparison of the blackbody and power-law unabsorbed fluxes in the 0.8–1.5 keV band. Fluxes are in units of 10⁻¹³ erg s⁻¹ cm⁻². The associated uncertainty in the fluxes is derived from the uncertainty in the count rates, and it is shown in brackets. The fourth column is the ratio of power-law flux over blackbody flux (column 3/column 2).
From: The X-ray variability of the narrow-line type 1 Seyfert galaxy IRAS from an XMM-Newton observation
Mon Not R Astron Soc. 2004;347(1): doi: /j x
Mon Not R Astron Soc | © 2004 RAS