A&A 493, 907-911 (2009)
DOI: 10.1051/0004-6361:200810993
R. S. Bachev
Institute of Astronomy, Bulgarian Academy of Sciences, 72 Tsarigradsko Chausse Blvd., 1784 Sofia, Bulgaria
Received 19 September 2008 / Accepted 28 November 2008
Abstract
Aims. The main purpose of this paper is to study time delays between the light variations in different wavebands for a sample of quasars. Measuring a reliable time delay for a large number of quasars may help constraint the models of their central engines. The standard accretion disk irradiation model predicts a delay of the longer wavelengths behind the shorter ones, a delay that depends on the fundamental quasar parameters. Since the black hole masses and the accretion rates are approximately known for the sample we use, one can compare the observed time delays with the expected ones.
Methods. We applied the interpolation cross-correlation function (ICCF) method to the Giveon et al. sample of 42 quasars, monitored in two (B and R) colors, to find the time lags represented by the ICCF peaks. Different tests were performed to assess the influence of photometric errors, sampling, etc., on the final result.
Results. We found that most of the objects show a delay in the red light curve behind the blue one (a positive lag), which on average for the sample is about +4 days (+3 for the median), although the scatter is significant. These results are broadly consistent with the reprocessing model, especially for the well-sampled objects. The normalized time-lag deviations do not seem to correlate significantly with other quasar properties, including optical, radio, or X-ray measurables. On the other hand, many objects show a clear negative lag, which, if real, may have important consequences for the variability models.
Key words: galaxies: quasars: general - accretion, accretion disks
Although variability is an extensively studied and rather common feature of quasars, little is currently known about the exact nature of the processes driving the flux changes. Variations are observed in practically all energy bands, often with time delays between them. This fact suggests a common cause (process) connecting otherwise spatially separated regions (presumably parts of an accretion disk), where most of the corresponding wavelengths come from. Since the time lags are rather short for the expected distances, it is the speed of light that is perhaps the only way to casually connect these separate regions. Several competing ideas, often leading to different signs of the time lags between the bands have been discussed in the literature (Czerny et al. 2008):
Sergeev et al. (2005) studied the light curves of 14 nearby Seyfert galaxies, observed on 60-150 epochs in 4 broad-band filters and found positive delays for most of the cases, varying between a fraction of a day and a few days. Their results are broadly consistent with the reprocessing model. Recently, similar results were reported by Liu et al. (2008) and Arévalo et al. (2008). Here we extend their works, applying a similar technique to a larger sample of quasars, optically monitored at the Wise observatory (Giveon et al. 1999) in two colors for several years. The sample is described in more detail in the next section. In Sect. 3 we describe the method we used to find the time delay between the bands, i.e. the interpolation cross-correlation function (ICCF) method. Next, the results for the time lags are presented and compared with the predictions of the reprocessing model. Finally, we discuss the reliability of the lag estimates and different implications for the central engine models of quasars, by comparing the deviations from the reprocessing model predictions with various quasar characteristics.
This work analyses publicly available light curve data for a sample of 42 Palomar-Green (Schmidt & Green 1983), mostly radio-quiet quasars, monitored at the Wise observatory in two observers-frame colors (B and R-bands), Giveon et al. (1999). This sample was chosen mostly because of the high accuracy of the CCD photometry, typically around 0.01 mag, in comparison with earlier, photographic plate based monitoring campaigns (Giveon et al. 1999, and the references therein). The time span of the monitoring was about 7 year, with a typical average monitoring interval of 40 days, though ranging significantly. The best sampled objects were observed on about 80 separate epochs, while the least sampled - on only about 25 epochs (see Sect. 5.1.1 for a discussion on sampling issues). All the objects are nearby, typically of , which insures that the analysis applies to almost the same rest-frame wavelength region. As an additional argument for using this sample is that many of the objects have reverberation-mapping central mass estimates (and respectively - Eddington ratios), so one can study possible relations between the time lags and the accretion parameters. For the rest of the objects, due to the good optical spectra available, the ``size-luminosity'' (Kaspi et al. 2005) relation can be applied for the same purpose. The sample is presented in Table 1. The object name, the red shift and the number of observational epochs are given in the first three columns, followed by the measured time lags between B and R-bands, (see Sect. 4 for details). Next columns show the black hole mass, the accretion rate (in Eddington units) and the expected lag for the simple reprocessing model (Sect. 4).
In order to study the wavelength - time delay dependence we performed a linear-interpolation cross-correlation (ICCF) analysis (Gaskell & Sparke 1986) between the light curves of the two bands. The maximum of is assumed to give the time delay between the bands. The interpolation between the photometric points is necessary due to the unevenly sampled data and is one of the frequently used methods. In our particular case, the magnitude values for every second day of the interpolated light curve were later on used for the cross-correlation analysis. This time interval of 2 days seems like a reasonable choice, since it is shorter than the majority of the real data intervals, but is not too short so a huge number of ``artificial'' data points to influence the analysis. Such a 2-day interval leads to an additional (rms) uncertainty of days in the peak position, which however is generally smaller than the expected errors of other nature (see Sect. 5.1).
Other methods described in the literature (e.g. discrete CCF, Edelson & Krolik 1988; z-transformed CCF, Alexander 1997) do not seem to give significantly different results when applied to the same data (White & Peterson 1994; see also Fig. 3). The weighted delays of the top 80% of the ICCF are typically 1.5-2 times larger for this sample (see also Sergeev et al. 2005, for similar results). They correlate significantly (0.93) with the peak values, which are used throughout this paper.
Figure 1: Interpolation cross-correlation functions of B and R-band light curves as functions of the time delays (in days). A positive time delay indicates B-band leading the R-band. The scale is the same for all objects. | |
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Figure 1 shows on the same scale the ICCFs around the zero lag for all 42 objects. The ICCF peak there is typically the most prominent one, except for a few cases where additional (similar or even higher) maxima are present at significant distances from (e.g. PG 1012+008). For such peculiar cases, only the ``central'' maximum is used for the analysis.
Figure 2 presents the distribution of the rest frame time delays for all the objects from the sample. When all of them are included, the average is +3.2 days ( at 95% confidence interval) with a standard deviation of 13.2 days, and the median is +2.7 days. The t-test gives for the null hypothesis (assuming that the mean value for the parent population is zero) gives a p-value of 0.13, so the null hypothesis cannot be rejected at a significant enough level (meaning that the average time delay for the sample cannot be statistically distinguished from zero). However, the situation changes if one takes into account the presence of highly deviating delay values in the distribution (e.g. PG 1012+008 with days, Fig. 2). Two more tests, based on the median value, reject the idea that the median delay is zero at least at 95% level. First, the sign test, based on counting the number of values above and below the median, gives a p-value of 0.02. Second, very similar are the results from the signed rank test, which is based on comparing the average ranks of values above and below the median. These contradicting results from the mean and the median tests indicate that omitting deviating values is perhaps justified. Once one such value is omitted (PG 1012+008, see above), the sample mean becomes +4.6 ( at 95% conf. interval) days (p=0.006), and the median - +3.5 (p=0.012 and 0.006 for the tests mentioned above, respectively). The remaining objects' distribution resembles Gaussian (shown in Fig. 2), although the K-S test rejects the idea, strictly speaking.
Figure 8: Distribution of the time delays (ICCF peak positions) between B and R-bands. A positive time lag means the blue-band light curve leads the red one. A Gaussian fit to the distribution is shown (one deviating object omitted). The shaded area shows the distribution of the well-sampled (N>35) objects only (see the text). | |
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Table 1: The quasar sample.
In a case that the reprocessing from a standard accretion disk is primarily responsible for the optical variations and
respectively - for the interband time lags, one would expect a wavelength dependent
delay between the bands, which can be expressed (following Frank et al. 2002) as follows:
[days],
where is the accretion rate in Eddington units, is the central mass in 10^{8} Solar masses, and , are the average wavelengths of the bands, measured in units of 5000 Å^{}. This expression is obtained under the assumption that the disk emits mostly due to a viscous heating and the reprocessed radiation is only a small addition to the emitted flux. Thus, the disk rings will reprocess most effectively radiation of a wavelength close to the maximum of their Planck curves. Therefore, knowing the disk radial temperature distribution (Frank et al. 2002), one can approximately assess the wavelength dependence of the time lag. Another important assumption is that the reprocessed hard (X-ray) radiation comes from a location very close to the center. If this were not the case, but the X-rays come from e.g. a jet base elevated high above the disk instead, an additional geometrical factor of shortens the lag between B and R-bands, due to the decrease of the path difference. Table 1 (the last column) presents the expected time lags, calculated based on the accretion parameters (M and ) from the previous two columns, adopted from Kaspi et al. (2005).
Figure 10: Various realizations of ICCF as functions of the time delay (in days) for PG 0804+761, obtained by adding appropriate random noise to the light curves (simulating the photometric errors) - the left panel and using a random sub sample of the original sample (simulating scarcely observed cases) - 50% ( the middle panel) and 25% ( the right panel). One sees that both effects, although influential, do not significantly alter the final result. For that particular case, the photometric error effect appears to be responsible for 0.4 days uncertainty in the ICCF peak position, while the reduction of the original sample by a half - for 1.3 days and by 75% - for 3.3 days. In order to check the compatibility, the discrete cross-correlation method was also applied to the PG 0804+761 light curves (open symbols with error bars; the left panel). Here the peak cannot be defined so clearly, but the general shape of the curve is very similar. The slight vertical offset between the ICCF and the DCCF is perhaps a binning artifact (the time over which the DCCF is averaged is 20 days) and does not seem to affect the peak position. | |
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In order to get an idea about how much different uncertainties affect the time lags (the position of the ICCF peak), we performed two tests to the light curve data of a well sampled object, PG 0804+761, with a clearly defined positive lag, to see if the photometric errors associated with the data points and the sampling can alter significantly the result. Figure 3 (left panel) shows a number of ICCFs of the light curves with a random noise, appropriately added to mimic the expected photometric error. One sees that the effect is not significant, leading to a days uncertainty of the peak position. The sampling, as expected, can affect more significantly the peak position. This object is observed on N=88 epochs, while many others - in less than 30. In order to study the effects of the scarce sampling, we randomly retrieved a sub sample of the original data points, which was further used for the interpolation and the cross-correlation analysis. The results for a number of simulations are shown in Fig. 3, middle and right panels for 50% and 25% sub samples, respectively. One may get the impression of a significant scatter of the peak position, although it is due mostly to the different peak values (the maxima of the ICCFs are not normalized); the peak position itself varies a little - 1.3 days (rms) for the 50%th sub sample and 3.3 days for the 25%th one. Therefore, the photometric error and the sampling effects cannot alter significantly the lag results, at least for the well-sampled objects. Yet, for the very scarcely observed objects, the uncertainties of the peak position might be significant. Based on the simulations described above, we found appropriate a very tentative error assessment approach, taking into account all sources of errors: , where we adopt (Sect. 3) and days. This expression may work reasonably well for our sample (where N<100), but should by no means be considered universal; see Gaskell & Peterson (1987) for more details on the error issues.
Figure 14: Normalized difference between the observed and the expected time lags as functions of different quasar properties. The figure shows the influence of the number of the observations, N ( top-left panel, objects are separated by their black hole masses) and radio-loudness (Kellermann index, middle-left; Kellermann et al. 1989); (B-R) color ( bottom-left); H line width (in km s^{-1}, top-right); soft X-ray spectral index ( middle-right); red shift ( bottom-right) - all they shown with different symbols, separated by the number of the observations. As the top-left panel shows, the scatter between the observed and the expected times is significant only for N<35, so this value is further used in the remaining panels as a separation criterion between the well-sampled and the under-sampled objects. | |
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Note, that the statistical errors of the cross-correlation functions are very small due to the large number of interpolated magnitude values used and their effect on the peak position is negligible. If the observed time lags are as a result of reprocessing, the errors estimated above, following this simple approach, appear to be significantly underestimated for a number of reasons in comparison with the observed scatter (Fig. 4, see also Sect. 5.2).
Although the observed and the calculated lags appear to be broadly consistent for the well-sampled objects (Sect. 5.2), the scatter is significant. Except for the errors, described inSect. 5.1.1, there are also several other factors that may contribute to the scatter:
Except for the uncertainties of different nature (see above), the scatter between the expected and the observed lags can also be attributed to the possibility that the reprocessing may not be the primary driver of the optical variability for some of the objects. As mentioned before, a weak blazar component can also play a role, in addition to other (possibly unknown) mechanisms. If so, one may expect to be able to differentiate between the quasars, for which the reprocessing is responsible for the observed lags from those, for which this mechanism is different, based on other quasar properties, such as radio loudness, X-ray spectral index, continuum colors, optical spectra, etc. The idea is that these different mechanisms may leave their signatures on the observed quasar appearance. We tested the normalized time lag difference against various quasar observables, including luminosity, accretion rate, equivalent widths of H and [OIII] lines and their ratio, FeII/H ratio, radio power, X-ray to optical continuum index^{}, as well as CIV1549 equivalent width and shift^{}, but found no significant correlations, except for some tendencies. The most interesting cases are shown in Fig. 4. The top-left panel shows the influence of the number of observational epochs - one sees that for the scatter reduces significantly, meaning that for many objects, the number of the observations may be simply not high enough to reveal the true time lags. Based on this observation, all the remaining panels of this figure show separately the objects for which N>35 (as filled squares) from the remaining, undersampled objects (as crosses). Interestingly, this tendency is not that strong for the higher-mass objects ( ), for which the scatter appears to be generally small for all N (only in the top-left panel the separation is based on ). The radio-loudness does not seem to play a significant role in the scatter (middle-left), meaning probably that a possible blazar component does not contribute significantly to the optical variability for this sample. A weak tendency for the bluer object to have a delay between the bands shorter than expected, even for the well-sampled objects, is shown in the bottom-left panel (Fig. 4). It is not clear how to explain this effect, if real at all, but it may be connected to the way continuum is generated (i.e. the exact accretion disk structure and properties, being perhaps different from the standard model). The top-right panel shows the influence of the of the width of the broad lines (H). The scatter appears to be most significant for the narrower-line ( km s^{-1}) objects, which may have implications for possible quasar population differences (e.g. Sulentic et al. 2000). The soft X-ray spectral index panel (middle-right) reveals an interesting possibility that the optical variations of the harder ( ) objects are perhaps less likely to be attributed to reprocessing in a standard accretion disk, which may have implications for the origin of the soft X-ray excess. Finally, the bottom-right panel demonstrates that, indeed, the emission lines around may also play a role in the continuum time lags, as the scatter appears to be the largest there (see Sect. 5.1.2 for more details).
If we take into account only the best sampled objects (), the average normalized difference between the observed and the expected time lags, , is -0.32, slightly less than the expected value of zero. Should there be no systematic errors involved in the estimation of , and in a case that the reprocessing is mainly responsible for the lags, another possibility emerges, i.e. the irradiating source is located above the disk, as mentioned previously. The value of -0.32 corresponds roughly to an elevation angle of 45 deg, meaning a height above the disk in order of the distances at which the optical continuum is generated, i.e. 100-1000 gravitational radii (Arévalo et al. 2008), raising the possibility that the jet base is the primary source of irradiating X-rays (see however Czerny & Janiuk 2007, for a warm absorber interpretation). This interpretation, however, due to the large scatter, cannot be justified statistically with the available optical data, so it has to be considered only as an interesting possibility.
In this paper we analyze the light curves and study the time lags between the optical continuum bands for a large sample of quasars. In spite of the significant scatter, we show that the lags are broadly consistent with the reprocessing model, according to which the optical variations are largely due to the reprocessing of the central X-ray radiation in a surrounding thin accretion disk. There are also some indications that the central X-ray irradiating source may be located at some height (a few hundred Schwarzschild radii) above the disk plane, representing perhaps a (failed) jet base. The deviations of the observed lags from the expectations, assuming the reprocessing model, do not seem to correlate significantly with any other quasar properties and are probably due mostly to the scarce sampling. The paper also demonstrates that the broad-band optical monitoring of quasars could be a powerful tool to study the central engines, provided the light curve is well sampled. A small robotic telescope (e.g. 0.4-0.6 m), dedicated to monitoring a large sample of brighter quasars once every 2-3 days, with an accuracy of 0.02 mag or better in 3 filters, might be able to clarify the role of reprocessing in quasar variability.