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An investigation of the origin of soft X-ray excess emission from Narrow-line Seyfert 1 galaxies Akn564 and Mrk1044

We investigate the origin of the soft X-ray excess emission from narrow-line Seyfert 1 galaxies Akn564 and Mrk1044 using XMM-Newton observations. We find clear evidence for time delays between the soft and hard X-ray emission from Akn564 based on a 100ks long observation. The variations in the 4-10keV band lag behind that in the 0.2-0.5keV band by 1768+/-122s. The full band power density spectrum (PDS) of Akn~564 has a break at ~1.2e-3Hz with power-law indices of ~1 and ~3 below and above the break. The hard (3-10keV) band PDS is stronger and flatter than that in the soft (0.2-0.5keV) band. Based on a short observation of Mrk1044, we find no correlation between the 0.2-0.3keV and 5-10keV bands at zero lag. These observations imply that the soft excess is not the reprocessed hard X-ray emission. The high resolution spectrum of Akn564 obtained with the RGS shows evidence for a highly ionized and another weakly ionized warm absorber medium. The smeared wind and blurred ionized reflection models do not describe the pn data adequately. The spectrum is consistent with a complex model consisting of optically thick Comptonization in a cool plasma for the soft excess and a steep power-law, modified by two warm absorber media as inferred from the RGS data and the foreground Galactic absorption. The smeared wind and optically thick Comptonization models both describe the spectrum of Mrk1044 satisfactorily, but the ionized reflection model requires extreme parameters. The data suggest two component corona -- a cool, optically thick corona for the soft excess and a hot corona for the power-law component. The existence of a break in the soft band PDS suggests a compact cool corona that can either be an ionized surface of the inner disk or an inner optically thick region coupled to a truncated disk.


Introduction
A significant fraction of type 1 active galactic nuclei (AGN) show 'soft X-ray excess emission' above a power-law continuum, usually identified as the steepening of the X-ray continuum below ∼ 2 keV. This soft excess emission was first observed by HEAO-1 (Pravdo et al. 1981), and EX-OSAT (Arnaud et al. 1985;Singh et al. 1985). Boller, Brandt, & Fink (1996) showed that AGN with the steepest soft X-ray spectra tend to lie at the lower end of the Hβ line width distribution. These AGN with FWHM Hβ < ∼ 2000 km s −1 are classified as the narrow-line Seyfert 1 galaxies (NLS1; Osterbrock & Pogge 1985), and are distinguished from the bulk of the Seyfert 1 galaxies. In addition to the strong soft X-ray excess below 2 keV and narrower permitted lines, NLS1 also show a number of extreme properties e.g., steep 2 − 10 keV power-law continuum, extreme X-ray variability and strong Fe II emission. These properties are all related and one suggestion is that NLS1 are the supermassive black hole analogue of stellar mass black hole X-ray binaries (BHB) in their 'high/soft' state.
However, the origin of the soft X-ray excess emission has remained a major problem in AGN research over the past two decades. The soft excess emission is a smooth continuum component rather than a blend of emission/absorption features as revealed by Chandra and XMM-Newton grating observations (e.g., Turner et al. 2001a;Collinge et al 2001). When described as a thermal component, the soft excess emission has a remarkably constant temperature (∼ 100−200 eV) across AGN with a wide range of black hole masses (Czerny et al. 2003;Gierlinski & Done 2004;Crummy et al. 2006). There are a number of ideas that have been proposed to explain the origin of the soft excess component. Pounds, Done & Osborne (1995) pointed out the similarity of the X-ray spectrum of NLS1 and Cyg X-1 in its high state (HS) and suggested that the soft excess could be the optically thick emission from an accretion disk. However, the observed soft excess emission is too hot for a disk around a supermassive black hole. One possibility is that there is a cool, optically thick Comptonizing region in addition to a hot (∼ 100 keV), optically thin (τ ∼ 1) region producing the high energy power-law emission. The cool region can Comptonize the disk photons and smoothly connect the disk emission up to soft X-ray energies (Magdziarz et al. 1998). Gierlinski & Done (2004) tested this model using high quality XMM-Newton spectra of 26 radio-quiet PG quasars. Although the spectra are well described by the Comptonization model, the temperature of the cool Comptonizing region is remarkably constant despite a large range in the black hole masses. They proposed that the observed soft excess is an artifact of heavily smeared, strong partially ionized absorption (see also Gierlinski & Done 2006;Schurch & Done 2006). Another possibility is that the emission is dominated by ionized Compton reflection. This can happen if the disk is clumpy at high accretion rates, thus hiding the hard X-ray source among many clumps. The ionized reflection can explain the observed soft excess emission . The last two models, based on relativistically smeared absorption and ionized reflection, relate the soft excess emission to atomic processes and therefore provide a natural explanation for its constant temperature for AGN with a wide range in their black hole masses.
The three models, cool Comptonization, ion-ized reflection and heavily smeared absorption, all result in statistically equally good fits. The fitting criteria are not sufficient to discriminate among them (Sobolewska & Done 2005). Variability properties of the soft and hard X-ray emission and the relationship between them may provide strong constraints on the above models for the soft excess emission. A 35 day long ASCA monitoring observation of the NLS1 galaxy Akn 564 revealed a distinction in the variability of the soft excess and power-law components on a time scale of weeks, with the soft excess emission varying by a factor of ∼ 6 compared to a factor of ∼ 4 in the power-law component (Turner et al. 2001b). Similarly, a long ∼ 10 days ASCA observation of the NLS1 galaxy IRAS 13224-3809 suggested that the soft excess component dominates the observed variability on a time scale of ∼ a week, but on shorter time scales (∼ 20000 s), the power-law component appears to dominate the variability (Dewangan et al. 2002). A 12 day long ASCA observation of another NLS1 galaxy Ton S180 suggested that the soft excess and the power-law fluxes are not well correlated on time scales of ∼ 1000 s (Romano et al. 2002). These long ASCA observations suggest two separate continuum component unlike the heavily smeared, ionized absorption model based on a single continuum component. Gallo et al. (2004) found evidence for alternate leads and lags between the 0.3 − 0.8 keV and 3 − 10 keV band emission from the NLS1 galaxy IRAS 13224-3809. Dasgupta & Rao (2006) reported energy dependent delay between the soft and hard X-ray emission in Mrk 110. These observations suggest different emitting regions for the soft excess and the power-law component from NLS1 galaxies. In this paper, we use XMM-Newton observations of two NLS1 galaxies Akn 564 and Mrk 1044 to study the variability properties of the soft and hard X-ray emission and investigate the origin of the soft excess emission. In Section 2, we outline the XMM-Newton observations of Akn 564 and Mrk 1044. We describe the temporal analysis in Section 3 and spectral analysis in Section 4 and discuss the results in Section 5. served by XMM-Newton on 2002 July 23 (ObsID: 0112600301) for 8 ks. The EPIC-pn and MOS cameras (Strüder et al. 2001;Turner et al. 2001a) were operated in the small window mode using the medium filter during both the observations. The data were reduced using version 6.5.0 of the SAS software. Examination of the background rate above 10 keV showed that the observation of Akn 564 was partly affected by the flaring particle background before an elapsed time of 7.5 ks and this early period was therefore excluded to obtain a continuous exposure with steady background. For temporal analysis, we used all the pn and MOS events with patterns ≤ 12 and a continuous exposure of 91.3 ks during which both the pn and MOS cameras operated simultaneously. There were three short duration (< 1000 s), small amplitude background flares (maximum count rate ∼ 2 counts s −1 above 10 keV) during the observation of Mrk 1044. The varying background contribution to the source was corrected by subtracting the background rate. For spectral analysis, we chose a count rate cut-off criterion to exclude the high particle background. In case of Akn 564, the MOS data are affected with photon pile-up. In order to achieve the best possible spectral resolution and to have the best spectral calibration, we chose the EPIC-pn data and used the good X-ray events (FLAG=0) with pattern zero (single pixel events) for Akn 564. For Mrk 1044, we used the good EPIC-pn events with pattern 0 − 4 (single and double pixel events). We used circular regions with radii of 40 ′′ , centered at the peak position of Akn 564 and Mrk 1044, to extract the source spectra. We also extracted background spectra from appropriate nearby circular regions, free of sources.

Observation and Data Reduction
We also processed the RGS data obtained from the long observation of Akn 564. We extracted the first order source and the background spectra by making the spatial, order selections on the processed event files, and calibrated by applying the most recent calibration data. We also used a temporal filter to exclude the high particle background based on a count rate cut-off criterion. We have used the ISIS (version 1.4.7) spectral fitting environment (Houck & Denicola 2000;Houck 2002) for power and energy spectral analysis. Unless otherwise stated, all errors are quoted at 90% confidence level.

Akn 564
For temporal analysis, we combined the pn and MOS data to increase the signal-to-noise ratio. In order to study cross-correlation between different energy bands, we extracted light curves in several energy bands 0.2 − 0.3, 0.2 − 0.5, 0.2 − 1, 0.2 − 2, 2−10, 3−10, 4−10 and 5−10 keV with time bins of 64 s. Figure 1 shows the light curves of Akn 564 in the 0.2 − 0.3 and 5 − 10 keV bands rebinned to 512 s. X-ray emission from Akn 564 is highly variable. The 0.2−0.3 keV band light curve shows a trough-to-peak variations by a factor of ∼ 3.3, while the hard band (5 − 10 keV) shows a troughto-peak variation by a factor of ∼ 3.6. Although the 0.2 − 0.3 keV and 5 − 10 keV band light curves appear to be correlated, the most rapid variability is seen in the hard band. A visual comparison of the light curves suggests that variations in the hard band appear to lag those in the soft band.
To investigate further, we have performed crosscorrelation and power spectral analysis.

Cross Correlation Analysis
We have computed cross-correlation function (CCF) using the XRONOS program crosscor. We used the slow direct Fourier algorithm to compute the CCF between the soft and hard band light curves with 64 s bins. Figure 2 shows the CCFs as a function of time delay between the energy bands (a) 0.2 − 2 keV and 2 − 10 keV, (b) 0.2 − 1 keV and 3 − 10 keV, (c) 0.2 − 0.5 keV and 4 − 10 keV and (d) 0.2 − 0.3 keV and 5 − 10 keV. The 0.2 − 2 keV and 2 − 10 keV band light curves are strongly correlated without any time delay as indicated by the sharp peak at zero lag. However, the strength of the sharp peak decreases with the increase in the separation between the soft and hard bands. In the CCF of 0.2 − 1 keV and 3−10 keV band light curves, the sharp peak weakens and another broad peak at positive time lags becomes relatively stronger. The broad peak dominates the CCF for the 0.2−0.5 keV and 4−10 keV band light curves and only a weaker sharp peak is seen. The sharp peak is not clearly seen in the CCF between 0.2 − 0.3 keV and 5 − 10 keV bands, only the broad peak is seen. Thus the hard 4 − 10 keV or 5 − 10 keV band clearly lags the soft 0.2 − 0.5 keV or 0.2 − 0.3 band.
It is hard to assess the statistical significance of the time lag based on model fitting to the CCF using the traditional χ 2 minimization technique. The reasons are (i) the shape of the CCF is generally complex, (ii) the CCF data points are not independent and (iii) the errors are not normally distributed. Therefore, we have adopted a model independent way, following Peterson et al. (1998), to measure the time lag. The principal source of uncertainty in the time lag between two long, continuous light curves is the uncertainty in the observed count rates. To account for this uncertainty, we have performed Monte Carlo simulations using IDL (version 6.3). We simulated 1000 pairs of soft and hard band lightcurves by modifying the observed count rates by random Gaussian deviates assuming that the errors on the observed count rates are normally distributed. We calculated the time lag between each pair of the simulated soft and hard band light curves as the centroid of the CCF based on all points with cor-  Figure 3 shows the distribution of time lags between the 0.2 − 0.5 keV and 4 − 10 keV bands. We calculated the time lag between the observed soft and hard bands as the centroid of the CCF and the errors on the time lag by directly integrating the time-lag distribution over a range to obtain 68%, 90% or 99% confidence level. Thus we measured the time lag between the 0.2 − 0.5 and 4 − 10 keV bands to be 1768 ± 92 s (68%), ±122 s (90%) or ±191 s (99%). A similar procedure resulted in the time lag between the 0.2 − 0.3 and 5 − 10 keV to be 1767 ± 196 s (68%), ±320 s (90%) or ±462 s (99%).
We have also searched for variations in the CCF or time delay. For this purpose, we divided both 0.2 − 0.5 keV and 4 − 10 keV light curves into nine equal segments with lengths 10.1 ks and computed the CCFs for each segment. The nine CCFs are plotted in Figure 4. The CCFs are not similar. There is no or weak correlation between the soft and hard band light curves in the segments II-VI and VIII. In segment IV, the soft and hard band appear to be weakly anti-correlated with a soft band lead of ∼ 1200 s. The two bands are strongly correlated without any lag for the segments I & IX, while for the segments VII and VIII, the hard band lags behind the soft band. For these segments, the time lag varies from ∼ 900 − 2900 s. In segment VII, the soft and hard band appear to anticorrelate at a lag of ∼ −3000 s. Brinkmann, Papadakis & Raeth (2007) have employed the sliding window technique to study the cross-correlation properties of Akn 564 between the 0.3 − 1 keV and 3 − 10 keV bands using the same data. There results are similar to the presented here if we note that the first 7.5 ks of data were excluded from our analysis. The leads and lags in the X-ray emission from Akn 564 are also similar to the alternate leads and lags in 4500 s intervals found between the 0.3 − 0.8 keV and 3 − 10 keV band X-ray emission from IRAS 13224-3809 by . The contribution due to the Poisson noise has not been subtracted. Right: Power density spectra in the soft (0.2 − 0.5 keV) and hard (3 − 10 keV) bands, derived from the combined EPIC-pn and MOS data. The constant power expected from the Poisson errors have been subtracted. The best-fitting broken power-law models are also shown. The soft band power density spectrum is clearly steeper and weaker than the hard band power density spectrum.

The power density spectra
To make a further study of the variability properties of Akn 564, we have calculated power density spectra (PDS) of Akn 564 from the combined pn+MOS lightcurves in the full (0.2−10 keV), soft (0.2 − 0.5 keV) and hard (3 − 10 keV) bands, sampled at 16 s. We used the slow algorithm implemented in the XRONOS program 'powspec'. Following Papadakis & Lawrence (1993), we rebinned the PDS in logarithmic space with a binsize of 20 and performed the fitting within the ISIS (version 1.4.5) spectral fitting environment. We converted the PDS to equivalent energy spectra (power → counts/bin; Hz → keV) using the sitar timing package. We fitted the PDS with a simple powerlaw model. We also used a constant to account for the power arising from the Poisson noise. The simple power-law model resulted in an unacceptable fit (minimum χ 2 = 225.2 for 139 degrees of freedom (dof)). We then replaced the power-law with a broken power-law model. This model resulted in the minimum χ 2 = 169.2 for 137 dof. The broken power-law model provided an improved fit at a statistical significance level of > 99.99% compared to the power-law model according to the maximum likelihood ratio test. Thus we conclude that the PDS of Akn 564 has a break at (1.2±0.3)×10 −3 Hz with power-law indices 1.3 +0.1 −0.2 below the break and 3.2 +0.5 −0.4 above the break. The break frequency reported here is similar to the high frequency break at ∼ 2 × 10 −3 Hz discovered by Papadakis et al. (2002) based on ASCA data (see also Alevaro et al. 2006) The constant power due to Poisson noise is 0.024±0.0012 (rms/mean) 2 Hz −1 . The PDS and the best-fit broken power-law plus constant model are plotted in Figure 5. The power arising from the Poisson errors have not been subtracted.
We also fitted the power-law and broken powerlaw models to the soft (0.2−0.5 keV) and hard (3− 10 keV) PDS of Akn 564. The power-law model resulted in an unacceptable fit to the PDS in the soft band (χ 2 = 193.2 for 139 dof) with powerlaw index of 1.7 ± 0.1. The broken power-law model provided a better fit (χ 2 /dof = 160.9/137) with power-law indices 1.4 +0.1 −0.2 and 4.0 +1.8 −1.3 before and after the break frequency 1.1 +0.2 −0.6 × 10 −3 Hz. This is an improvement over the power-law fit at a significance level of > 99.99% based on the maximum likelihood ratio test. The power-law model provided an acceptable fit to the hard band PDS (χ 2 = 138.4 for 139 dof) with an index of 1.2 ± 0.1. The broken power-law model resulted in an improved fit (χ 2 /dof = 127.2/137) with indices < 1.0 (90% upper limit) and 1.8 +0.5 −0.4 before and after the break frequency < 1.2 × 10 −3 Hz (90% upper limit). This is an improvement over the power-law model at a level of 99.6% significance level. However, the parameters are not well determined. We have plotted the soft and hard band PDS and the best-fit broken power-law models in Fig. 5 (right panel). Clearly the soft band PDS is steeper than the hard band PDS. This implies that the X-ray emission in the hard band varies more than that in the soft band on shorter time scales.

Mrk 1044
As stated above, the observation of Mrk 1044 was affected by short-duration, weak flares. Therefore, the source light curves were corrected for background contribution using appropriate background light curves extracted from blank sky regions. The combined pn+MOS and background corrected light curves of Mrk 1044 are shown in Fig. 1 (right). X-ray emission from Mrk 1044 is variable with trough-to-peak variations of ∼ 2 (0.2 − 0.5 keV) and ∼ 3 (4 − 10 keV). However, the 0.2 − 0.5 keV and 4 − 10 keV light curves do not appear to be strongly correlated.
The cross correlations between the soft and hard bands are plotted in Figure 6. Similar to Akn 564, the 0.2 − 2 keV and 2 − 10 keV bands are strongly correlated without any delay and the strength of this correlation decreases with the interval between the soft and hard bands. There is no correlation between the 0.2 − 0.3 keV and 5 − 10 keV bands at zero lag. There is a weak anti-correlation at a positive delay of ∼ 1000 s and a weak correlation at positive delays of 3000− 5000 s. As the CCF for Mrk 1044 is based on a short 7.9 ks observation, the CCF is likely only one representation of many possible cross correlations similar to that seen for Akn 564.

Spectral Analysis
We have performed spectral modeling of Akn 564 and Mrk 1044. We present the results based on the high signal-to-noise pn data for both Akn 564 and Mrk 1044 and the high resolution RGS data for Akn 564. We note that Papadakis et al. (2007) have performed a detailed spectral analysis of Akn 564 using the same observation. The purpose here is to investigate the alternative models for the origin of the soft X-ray excess emission. All the spectra were analyzed with the Interactive Spectral Interpretation System (ISIS, version 1.4.5). The pn data were grouped to a minimum of 100 and 20 counts per spectral channel for Akn 564 and Mrk 1044, respectively. We consider a model fit as statistically unacceptable if the the null hypothesis can be rejected at more than 95% significance. The errors on the best-fit spectral parameters are quoted at a 90% confidence level. Below we use narrow Gaussian line components with their widths fixed at σ = 10 eV that are unresolved by the EPIC-pn data.
4.1. The soft X-ray excess emission NLS1 galaxies are known to show strong soft Xray excess emission below ∼ 2 keV. To show this soft excess, first we fitted a simple absorbed power law (PL) model to the EPIC-pn spectra above 3 keV (3 − 10 keV for Mrk 1044 and 3 − 11 keV for Akn 564). The simple PL model resulted in minimum χ 2 = 527.4 for 519 dof and 119.0 for 127 dof for Akn 564 and Mrk 1044, respectively, thus providing good fits to the 3− 10 keV pn data. We have plotted the ratio of the pn data and the best-fit PL model in Figure 7 after extrapolating the model to low energies. The plots clearly show strong soft excess emission below ∼ 2.5 keV and possible iron Kα lines near ∼ 6.4 keV in the spectra of both the NLS1. The soft X-ray excess emission from NLS1 are usually well described by a simple blackbody or a multicolor disk blackbody (MCD). Addition of the MCD component to the absorbed PL improved the fit. The fit was reasonably good for Mrk 1044 (χ 2 /dof = 628.0/541). Addition of a narrow Gaussian line at ∼ 6.4 keV further improved the fit (χ 2 /dof = 611.7/539). The best-fit parameters of the MCD+PL model for Mrk 1044 are listed in Table 1 and the EPIC-pn data, the best-fit model and residuals are plotted in Figure 9. The MCD+PL model was a poor fit for Akn 564 (χ 2 /dof = 1494.1/913). Examination of the residuals showed broad emission/absorption features below ∼ 1 keV in the spectrum of Akn 564. To verify and investigate these features, we have analyzed the high resolution soft X-ray spectra of Akn 564 obtained with the two RGS simultaneously with the EPIC-pn data. We used the Cash statistic to fit the low count RGS data. We fitted a simple PL model, modified with the neutral absorption, jointly to RGS1 and RGS2 data in the 0.35−1.9 keV band. This resulted in a steep spectrum (Γ ∼ 3.0) and N H = 7.6 × 10 20 cm −2 . Addition of an MCD component improved the fit (C/dof = 2575.9/1572; ∆C = −225.4 for two parameters). The best-fit parameters are N H ∼ 5.2 × 10 20 cm −2 , Γ ∼ 2.44 and the MCD kT in ∼ 165 eV. Examination of the ratio of the data and model revealed a strong absorption feature at ∼ 0.5 keV and additional weak and narrow absorption features in the 0.5 − 1 keV band, suggesting the presence of a warm absorber medium in Akn 564.

Warm absorber model for Akn 564
To describe the weak absorption features seen in the RGS data, we have created a warm absorber model for Akn 564 using the spectral simulation code CLOUDY version 7.02.01 (last described by Ferland et al. 1998). We used a multicomponent ionizing continuum similar to that observed from Akn 564. We used the 'agn' continuum available within CLOUDY. This continuum has four parameters: the temperature of the big blue bump emission, the slope of the high energy X-ray continuum, X-ray to UV ratio (α ox ) and the UV spectral index. We set the temperature of the big blue bump component and the slope of the high energy continuum to be similar to the temperature of the soft X-ray excess emission and the slope of the hard power law, respectively, derived from the EPIC-pn data. For Akn 564, α ox = 0.941 (Gallo 2006) and we used a typical value of −0.5 for the UV spectral index (Elvis et al. 1994;Francis 1993). The X-ray power law is assumed to fall as ν 3 above 100 keV and the big blue bump component is assumed to have an infra-red exponential cut-off at kT IR = 0.01 Ryd or 0.136 eV. We also included the cosmic microwave background radiation so that the incident continuum has nonzero intensity at very long wavelengths. We assumed a plane parallel geometry and calculated grids of models by varying the ionization parameter and the total hydrogen column density. We also included UTA features from Gu et al. (2006) in our calculation. The grid of models were imported to ISIS in the form of an XSPEC-style multiplicative table model as described in Porter et al. (2006).
To describe the weak absorption features in the RGS spectra of Akn 564, we multiplied the CLOUDY warm absorber model to the MCD+PL model. The model was also modified by neutral absorption along the line of sight as before. The addition of the warm absorber component improved the fit (C/dof = 2469.3/1569; ∆C = −106.6 for three additional parameters) with warm absorber column, N W ∼ 4×10 20 cm −2 , ionization parameter (logξ ∼ 2) and the out-   Table 2. We note that the best-fit neutral absorption column density derived from the RGS data is N H = 5.24 +0.13 −0.03 × 10 20 cm −2 which is less than the Galactic column of 6.40 × 10 20 cm −2 derived from the HI map of Dickey & Lockman (1990). The best-fit column, however, is consistent with the Galactic column of 5.34 × 10 20 cm −2 derived from the Leiden/Argentine/Bonn ( −1 ×10 20 cm −2 using the Chandra high energy transmission grating observations of Akn 564. Given the above uncertainties in the measurement of cold N H , we fix the cold absorption at the bestfit RGS value of N H = 5.24 × 10 20 cm −2 in all the subsequent fits for Akn 564. The above analysis clearly shows the presence of a two phase warm absorber medium in Akn 564. Some or all of the emission/absorption features resulting in the poor quality of the fit to the EPICpn, described above in section 4.1 are likely due to the presence of warm absorbers. However, it is difficult to determine accurately the parameters of the warm absorber based on the lower resolution EPIC-pn data alone. Therefore, we used the bestfit warm absorber components derived from the RGS data to model the EPIC-pn data. We used the two component warm absorber model with the fixed parameters along with the MCD+PL model and fitted the EPIC-pn data. The addition of the warm absorber components improved the fit, providing χ 2 /dof = 1654.1/912. However, the fit is still not acceptable mainly due to a strong absorption feature near 0.5 keV and slight excess of  emission below 0.5 keV. The absorption feature is stronger by a factor of ∼ 2.5 in the EPIC-pn data than that derived from the RGS data. Also the excess emission below 0.5 keV is not evident in the RGS data. Thus EPIC-pn and RGS do not agree well below 0.6 keV. Therefore we ignore the EPIC-pn data below 0.6 keV in the fits for Akn 564 described below. After excluding the data below 0.6 keV, the MCD+PL model modified with the two component warm absorber and neutral absorption along the line of sight provided a much better fit (χ 2 /dof = 941.2/856). Adding a narrow Gaussian line at ∼ 6.6 keV further improved the fit (∆chi 2 /dof = −21.9 for two parameters). Figure 10 shows the EPIC-pn data, the best-fit model and the χ-residuals and the best-fit parameters are listed in Table 1. The parameters of the MCD and PL components are similar to that derived from the RGS data (see Table 2 and 2). The MCD component used above to describe the soft X-ray excess emission is physically inappropriate. The inner accretion disk temperatures, kT in = 179±2 eV for Akn 564 and 138±3 eV for Mrk 1044 are much higher than that expected from a disk around a black hole of mass 10 6 − 10 7 M ⊙ . For this reason, the origin of the soft excess emission has remained unsolved for more than two decades.

Relativistically blurred ionized reflection
One possibility is that the reflected emission from a partially ionized accretion disk could be strong below 1 keV and can account for the strong soft excess emission (see e.g., Crummy et al. 2005). Though there is no clear evidence for a broad iron Kα line, such a line from an accretion disk could be hidden in the strong X-ray continuum. To test whether the strong soft Xray excess emission from Akn 564 and Mrk 1044 could be produced by the ionized reflection emission arising from the reprocessing of the primary X-ray emission in the disk, we have fitted the relativistically blurred ionized reflection model to the EPIC-pn spectra of both the NLS1. We used the table model reflion (Ross & Fabian 2005;Ross, Fabian & Young 1999) for the ionized reflection and blur the ionized reflection emission relativisti- Fig. 9.-Observed EPIC-pn data and the best-fit models for Mrk 1044 corresponding to the best-fit models and their parameters listed in Table 1. cally by convolving with a LAOR kernel (kdblur) to obtain the relativistically broaden ionized reflection from the inner regions of an accretion disk. The parameters of reflion model are ionization parameter (ξ), iron abundance relative to solar (A F e ), photon index of the illuminating powerlaw and the normalization of reflected spectrum. The parameters of the convolution model kdblur are the inner and outer radii of the disk (r in and r out ), emissivity index (β) and the disk inclination (i). We fixed the outer radius at r out = 400r g where r g = GM/c 2 is the gravitational radius. We used the power-law component for the continuum. We also used a narrow Gaussian to describe the unresolved iron Kα line from distant matter. We also used the two component warm absorber model with the parameters fixed at the values derived from the RGS data. We refer the full model as the blurred reflection model. The best-fit parameters of this model are listed in Table 1. The observed data and the best-fit reflection models are shown in Figure 9 (Mrk 1044) and Figure 10 (Akn 564). The model resulted in poorer fit than the MCD+PL model for both the NLS1 (χ 2 /dof = 954.2/837 for Akn564 and 671.6/535 for Mrk 1044). Also the emissivity index is unphysically large (β ≥ 10) and the inner radius is very small for both the AGN, suggesting that the model cannot account for the observed smoothness of the soft excess X-ray emission. The very steep emissivity indices and the small inner radii of the LAOR kernel were required to smooth the recombination features sufficiently to produce the featureless soft X-ray excess emission from both the NLS1s.

Smeared absorption from partially ionized material
The observed soft excess emission could be an artifact of smeared absorption from partially ionized material as described by Gierlin'ski & Done (2004). To test this scenorio, we have fitted the EPIC-pn data with the smeared absorption model. We used the XSPEC local model swind1 for the smeared absorption from a partially ionized wind from an accretion disk and the simple PL model for the continuum. Again we used a Gaussian Fig. 10.-Observed EPIC-pn data and the best-fitting MCD+PL, blurred ionized reflection, smeared absorption from partially ionized wind and optically thick thermal Comptonization models for Akn 564. The best-fit parameters are listed in Table 1. for the narrow iron Kα line and the two component warm absorber model with fixed parameters derived from the RGS data. The parameters of the smeared wind model are absorption column density, the ionization parameter (ξ = L/nr 2 ) and the Gaussian sigma for velocity smearing in units of v/c. The smeared absorption model provided a good fit to the spectrum of Mrk 1044 (χ 2 /dof = 592.4/538) but fails to describe the spectrum of Akn 564 (χ 2 /dof = 1147.1/842). This model requires unphysically large smearing velocity (∼ 0.8c) for Akn 564 to smooth sufficiently the absorption lines in order to produce the observed smooth soft excess emission (see Table 1 and Fig. 10).

Optically-thick, thermal Comptonization
The strong and smooth soft excess emission from NLS1 can also be described as arising from thermal Comptonization in an optically thick corona. To test such a scenario, we used the thermal Comptonization model (ThComp) described by Zdziarski et al (1996). The free parameters of ThComp model are the asymptotic power-law index (Γ thcomp ), electron temperature (kT e ) and the seed photon temperature (kT bb ). The electron scattering optical depth (τ ) can be calculated from the asymptotic power-law photon index (Γ compth ) and electron temperature (kT e ) as follows α = 9 4 + 1 (kT e /m e c 2 )τ (1 + τ /3) with Γ thcomp = α+1 (Sunyaev & Titarchuk 1980). We also used the PL model to describe the hard PL for the hot Comptonized component. We fixed the temperature of the seed photons for the optically thick Comptonization at 30 eV. This is equivalent to assuming that the seed photons for the Comptonizations in the warm and hot plasma arise from the accretion disk. Again we used the narrow Gaussian line for the iron Kα line. This model provided good fits for both the NLS1s (χ 2 /dof = 900.2/842 for Akn 564 and χ 2 /dof = 603.0/538 for Mrk 1044). The best-fit parameters are listed in Table 1 and the EPIC-pn data and the best-fit model are plotted in Fig. 9 and Fig. 10 . The electron temperatures are low (∼ 0.18 keV for Akn 564 and ∼ 0.14 keV for Mrk 1044) and electron scattering optical depths are very high (τ ∼ 45) for both the NLS1s. We note that the thermal Comptonization model best describes the EPIC-pn data in the 0.6 − 11 keV band for Akn 564 (see Table 1). We expect that the most suitable model must provide a reasonably good fit to the full band EPIC-pn data except for the absorption feature at 0.54 keV, provided that the calibration errors at low energies (< 0.5 keV) are at a level of a few percent. We find that the thermal Comptonization model best describes the full band data with χ 2 /dof = 1164.8/911 without any significant change in the best-fit parameters listed in Table 1. Addition of an absorption line at 0.54 keV improved the fit to χ 2 /dof = 985.5/908 with line center at E = 0.54 ± 0.005, f line = −(4.44 ± 0.06) × 10 −4 ergs cm −2 s −1 and width σ < 8 eV. The ionized reflection and smeared absorption models both fail to describe the data below 0.5 keV when extended to lower energies. Refitting the reflection model with the addition of an absorption line at 0.54 keV to the full band data resulted in poor fit (χ 2 /dof = 1392.2/906) with large emissivity index (β = 9.17 +0.20 −0.03 ) and small inner radius (r in < 1.239r g ) as before. The smeared absorption model with the addition of the absorption line provided the worst fit among the four models.

Discussion
We have studied the X-ray temporal and spectral characteristics of Akn 564 and Mrk 1044. We found that the 0.2 − 2 keV and 2 − 10 keV band lightcurves are strongly correlated without any time delay. However, the strength of this correlation decreases with increasing separation between the soft and hard bands. We have found significant correlation between the soft (0.2 − 0.3 keV, 0.2 − 0.5 keV) and hard (5 − 10 keV, 4 − 10 keV) band lightcurves at positive time delays. The 4 − 10 keV band lags behind the 0.2 − 0.5 keV band by 1767 ± 122 s (at 90%) in Akn 564. We note that Arevalo et al (2006) found time delays that increase both with time scale and energy separation between the energy bands. This means that there is no single, well defined delay. Instead, the measured delay based on the cross-correlation analysis is the averaged delay between the soft and hard bands. We find no correlation at zero time lag between the 0.2 − 0.3 keV and 5 − 10 keV band emission from Mrk 1044. We confirm the presence of a break at ∼ 1.2 × 10 −3 Hz in the power density spectrum of Akn 564, earlier detected by Papadakis et al. (2002) based on ASCA observations. We also find that the PDS of Akn 564 is energy dependent. The hard band (3−10 keV) PDS, consistent with a simple power law, is flatter and stronger than the soft band (0.2 − 0.5 keV) PDS that shows clear evidence for the break. These observations strongly suggest that different variability process dominate the soft and hard band emission. This may suggest physically distinct spectral components for the soft excess and the power-law components.

Implications of the observed time delays
The observed hard band delays from Akn 564 demonstrate that the soft excess emission cannot be the reprocessed emission of the primary X-ray emission. Fabian et al. (2002) presented the reflection dominated ionized accretion disk model and successfully reproduced the strong soft excess emission from the NLS1 galaxy 1H 0707-495. In this model, the strong soft excess is caused by the multiple reflections of mostly hidden hard X-ray continuum by the clumpy disk and the stronger reflectivity of the partially ionized material below ∼ 0.7 keV, associated with an abrupt change in the opacity (Ross, Fabian & Ballantyne 2002;Fabian et al. 2004). The soft X-ray excess emission is the reprocessed emission in this model, hence it is unlikely that the soft X-rays lead the hard X-ray emission. This is, however, not a strong constraint on the ionized reflection model. Many of the soft X-ray lines expected from the accretion disk are excited by soft X-ray photons with energies slightly greater than the line energies as the photoelectric absorption cross section varies as ∼ E −3 . The ionizing soft X-ray photons can lead the hard (3 − 10 keV) band emission due to the Compton delay of hard photons in the Comptonization process. Since the life times of excited states, responsible for the line photons, are very short compared to the expected Compton delay between the soft and hard photons, the line photons as well as the scattered soft X-ray emission can still lead the hard band primary emission. However, in this case, the soft X-ray excess emission is not expected to show rapid and large amplitude variability as the reflection component and broad iron line are known to show little variability in MCG-6-30-15 (Miniutti et al. 2007). Moreover, the blurred ionized reflection model with physically plausible parameters cannot reproduce the observed soft X-ray excess emission from Akn 564 and Mrk 1044.
Gierlinski & Done (2004) presented an alternative model for the origin of the soft excess emission. In this model, the soft excess emission is mainly due to the strong and smeared absorption near ∼ 0.7 keV. The soft excess and the hard power law are part of the same and single continuum component except for the small contribution from smeared emission lines. This means the soft and hard band emission arise from the same continuum component or physical process -Comptonization. The time delay is a natural outcome of the Comptonization process. A general prediction of Comptonization models is that the hard X-ray variations should lag behind those in softer bands (Payne 1980). Therefore it is natural to attribute the observed time delays between hard and soft photons to this process. The time lag represents the difference in the photon escape times between the soft and hard bands. The hard band photons tend to have undergone more scattering events, therefore travel longer and escape the corona later than the soft band photons. Thus the observed time lag is consistent with a single continuum component and hence with the smeared absorption model. However, there are three problems with the smeared wind model. (i) This model (XSPEC local model swind1; Gierliński & Done 2004) does not describe the X-ray spectrum of Akn 564 satisfactorily. (ii) The 3 − 10 keV band shows more variability power on short time scales than the 0.2−0.5 keV band, which is not expected in the simple Comptonization models in which the variability is caused by the variations in the seed photons alone. (iii) The smearing velocity for Akn 564 suggested by the swind1 model is very large (v ∼ 0.8c) for disk winds. Hydrodynamical simulations show that the line driven winds do not have the required smearing velocity (N. J. Schurch, private communication). It remains to be seen if the magnetically driven winds can provide the required smearing.
The two component model, Comptonization in two separate regions, is a viable option. In this model, the soft excess emission arises from the Comptonization in the low temperature (warm), optically thick plasma while the hard power-law is produced by the Comptonization in the hot plasma. Indeed the EPIC-pn spectra of Akn 564 and Mrk 1044 are both well described by the two component model. The temperature of the warm plasma is ∼ 175 eV for Akn 564 and ∼ 135 eV for Mrk 1044. This region, giving rise the soft excess emission, is optically thick (τ ∼ 45). Physically, this component could be the warm skin on the accretion disk surface or a region between the disk and an optically thin inner flow (Magdziarz et al. 1998) or an optically thick corona coupled with a truncated disk (Done & Kubota 2006). Depending on the geometry of the disk and the two component corona system, there can be delay between the soft excess and high energy power-law components.
However, the two component Comptonization model has difficulty in explaining the constancy of the temperature of the Comptonizing region producing the soft excess emission. Gierlinski & Done (2004) derived the temperature of the putative Comptonizing region in the range 0.1 − 0.2 keV which is remarkably constant for 26 different PG quasars. They concluded that the constancy of the temperature is inconsistent with that expected from the span of the asymptotic power-law index (Γ thcomp ∼ 1.5 − 2.5). However, the 0.3 − 10 keV XMM-Newton band only includes the high energy tail of the optically thick Comptonized emission. Both the peak of the soft excess component (kT ∼ 0.1 − 0.2 keV) and the asymptotic power-law component fall below 0.3 keV. Using such data, it may be difficult to measure accurately both the temperature and the asymptotic photon index, particularly in the presence of line of sight neutral absorption and complex warm absorber, both modifying the soft X-ray spectrum below 1 keV. NLS1 galaxies show a large diversity in their soft X-ray ROSAT photon indices (Γ ∼ 1.5 − 5.0), suggesting varying shape of the soft excess component (Boller, Brandt & Fink 1996). The constancy of the temperature for the soft excess emission is required to be investigated using a sample of NLS1 galaxies similar to that used by Boller, Brandt & Fink (1996). Another possibility is that the disk/corona geometry is different in NLS1 galaxies as they are accreting close to the Eddington rate. In such situations, the inner disk is likely thick and hotter. It remains to be seen if such thick structure can have uniform temperatures across AGN with a large range in their luminosity and black hole masses.

The disk-corona geometry
Inverse Compton scattering by thermal electrons provides the best possible explanation for the observed smooth soft X-ray excess emission from Akn 564 and Mrk 1044. Our spectral analysis favors two physically distinct corona: high optical depth, low temperature corona and high temperature, low optical depth corona. There are two possible geometries with two component corona. The cool, optically thick corona may be similar to the coupled disk corona geometry proposed by Done & Kubota (2006) for the very high state of black hole binaries. In this geometry, the inner accretion disk is truncated and is coupled to an optically thick corona, and gravitational energy release powers both the disk and the optically-thick corona. Comptonization of the disk photons in this corona may give rise to the broad soft excess component. In addition to the optically thick corona, a hot corona is responsible for the powerlaw component. The hot corona could be the same as the patchy corona above the disk and is likely powered by magnetic flares in the disk similar to the solar flares (Haardt, Maraschi, & Ghisellini 1994;Stern et al. 1995;Poutanen & Svensson 1996;Poutanen & Fabian 1999;Merloni & Fabian 2001). The seed photons could either be the soft photons from the disk or those arising from the cool, optically thick corona. Since the disk is coupled to the optically thick corona, appreciable time lag between the disk photons and the soft excess photons are not expected. The variability of the disk flux and the soft excess emission is governed by the variations in the accretion rate, while the variability of the power-law component is governed both by the variation in the soft photons as well as any variability process intrinsic to the corona such as that related to variation in the electron population. The flatter power density spectrum of Akn 564 in the hard band may be related to the additional variability of the power-law component due to the changes in electron population on short time scales e.g., caused by magnetic flares above the accretion disk.
Another possible geometry is the ionized surface of a disk acting as an optically thick and cool corona with a temperature of ∼ 0.1 − 0.3 keV (e.g, Magdziarz et al. 1998;see also O'Brian et al. 2001;Page et al. 2002;Vaughan et al. 2002). In this case, thermal Comptonization of disk photons by thermal electrons in the hot surface of the disk will produce the smooth soft excess. The steep power-law extending to high energies can be produced in another purely hot thermal/nonthermal or in a hybrid thermal-nonthermal plasma.
It is difficult to distinguish the two geometries described above. The different power spectra of the soft and hard band X-ray emission may constrain the two geometries. Recently  have shown a strong correlation between the break frequency, black hole mass and the bolometric luminosity for black hole binaries and AGN. If the break frequencies are related to the characteristic radii from the central source, their result suggests a characteristic size that appears to decrease with increasing accretion rate or luminosity. The clear evidence for a break in the soft band PDS of Akn 564 suggests a characteristic size associated with the soft X-ray excess emission which can be the size of the optically thick corona or the radius of the inner truncated disk in the model suggested by Done & Kubota (2006). It is also possible that the disk surface below an inner radius is ionized and the temperature of the inner disk surface is higher than that expected from the standard disk. The inner disk surface may then be responsible for the soft excess emission. The lack of a clear break in the hard band PDS of Akn 564 may suggest that power-law emission is probably not associated with a characteristic size and it arises from an extended corona similar to a patchy corona above an accretion disk. Future long observations of Akn 564 are required to clearly demonstrate the presence or absence of a break in the hard band PDS.

Conclusions
We have presented temporal and spectral study of XMM-Newton observations of Akn 564 and Mrk 1044. The main results are as follows: 1. The 0.2 − 2 keV and 2 − 10 keV band Xray emission from both the NLS1 galaxies are strongly correlated without any time delay. However, the variations in the 0.2 − 0.5 keV band are found to lead those in the 4 − 10 keV band by 1768 ± 122 s (90%) in Akn 564. We do not find any correlation between the 0.2−0.3 keV and 5−10 keV X-ray emission from Mrk 1044 at zero time delay. The two bands appear to anti-correlate at a positive lag of ∼ 1000 s and likely correlated at a lag of ∼ 3000 − 5000 s. Long observations of Mrk 1044 are required to confirm the time delay.
2. The full band power density spectrum of Akn 564 has a break at (1.2±0.3)×10 −3 Hz, corresponding to a time scale of ∼ 1000 s, similar to the delay between 0.2 − 0.5 and 4 − 10 keV bands. It is not clear if there is any physical relation between the two time scales. There is a clear evidence of a break in the soft band PDS but the hard band does not show a clear evidence for the break.
3. The soft (0.2 − 0.5 keV) band PDS of Akn 564 is significantly steeper and weaker than the hard (3 − 10 keV) band PDS. This implies that the power-law component is more variable than the soft excess component on shorter time scales. The implication of this result on the Comptonization models is that the variations in the power-law component are not only caused by the variations in the seed photons but also by the variations in the hot electron population. Thus electron injection on short time scales ( 1000 s) are required. This could be evidence for magnetic flares thought to power the corona above the accretion disk.
4. The soft excess emission from Mrk 1044 is featureless in the EPIC-pn data and is well described by the smeared absorption or optically thick Comptonization. The RGS data show evidence for warm absorbers in Akn 564. The EPIC-pn spectrum of Akn 564 is well described by a complex model consisting of optically thick thermal Comptonization in a low temperature (∼ 0.15 keV) plasma and a steep power-law, modified by two phase warm absorber medium and the Galactic absorption. The ionized reflection and smeared wind models fail to describe the data satisfactorily.
5. The temporal and spectral characteristics of Akn 564 and Mrk 1044 are consistent with a two component corona -a compact low temperature, optically thick corona and an extended hot corona. The compact corona could be an inner optically thick region coupled to a truncated disk or the ionized surface of an inner untruncated disk. The soft excess emission can be produced in the inner, optically thick corona and the power-law component is produced in the hot corona.