Hard Emission from Cen A

The hard X-ray continuum of Cen A observed with INTEGRAL SPI

Mark J. Burke11affiliation: CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France , Elisabeth Jourdain11affiliation: CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France , Jean-Pierre Roques11affiliation: CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France , and Daniel A. Evans22affiliation: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 mburke@irap.omp.eu
Abstract

We revisit the average hard X-ray spectrum from the AGN of Centaurus A (Cen A) using ten years worth of observations with INTEGRAL SPI. This source has the highest flux observed from any AGN in the SPI bandpass (23 keV–8 MeV). The 10 year lightcurve of Cen A is presented, and hardness ratios confirm that the spectral shape changes very little despite the luminosity varying by a factor of a few.

Primarily, we establish the presence of a reflection component in the average spectrum by demonstrating an excess between keV, from extending the spectral shape observed at low energy to the SPI regime. The excess in Chandra HETGS and INTEGRAL SPI data is well described by reflection of the dominant power law spectrum from a neutral, optically-thick atmosphere. We find that the reprocessed emission contributes of the keV flux.

The existence of a cut-off at tens to hundreds of keV remains controversial. Using simulated spectra, we demonstrate that a high energy cut off reproduces the observed spectral properties of Cen A more readily than a simple power law. However, we also show that such a cut-off is probably underestimated when neglecting (even modest) reflection, and for Cen A would be at energies keV, with a confidence of . This is atypically high for thermal Comptonizing plasmas observed in AGN, and we propose that we are in fact modelling the more gradual change in spectral shape expected of synchrotron self-Compton spectra.

Subject headings:
galaxies: elliptical and lenticular, cD — galaxies: individual (Centaurus A, NGC 5128) — X-rays: galaxies

1. Introduction

The radio galaxy Centaurus A (Cen A, NGC 5128), at a distance of 3.8 Mpc (Harris et al., 2010) is our nearest large early-type galaxy and one of the most studied active galactic nuclei (AGN). Despite this, we are still able to say comparatively little about the spectral properties of the AGN in the hard X-ray to -ray regime. Outstanding questions relate to the presence of reprocessed emission in the 20-100 keV spectrum and the existence of a high energy downturn in the spectral shape at a few hundred keV.

In the soft X-ray, Chandra and XMM Newton grating observations have been used to demonstrate that a moderately absorbed () power law component dominates the keV spectrum. However, inspection of the fit residuals indicated the need for extra components, the most prominent of which was a narrow ( eV) emission line consistent with neutral Fe (Evans et al., 2004). It is feasible that the excess emission above the power law arises from reflection of the central X-ray source from surrounding material (George & Fabian, 1991). Indeed, the absence of more highly-ionised iron (i.e. Fe XXV, Fe XXVI) and the narrowness of the Fe line profile is indicative that reflection is occurring far from the innermost portions of the accretion disk (Evans et al., 2004). The presence of reflection in the spectrum should lead to an apparent excess keV (the so-called ‘Compton hump’, George & Fabian, 1991).

The existence of a high energy cut-off at would have profound implications for the accretion mechanism of the Cen A AGN, and is the subject of controversy. Fundamentally it would inform on the origin of the primary emission component; whether it is produced in the jet (Maraschi et al., 1992; Bloom & Marscher, 1996) by synchrotron self-Compton (SSC) (Ginzburg & Syrovatskii, 1969) or near to the accretion disc from thermal comptonisation (Dermer & Schlickeiser, 1993; Sikora et al., 1994). For the case of thermal comptonisation, a high energy cut-off in the spectrum will exist at times the temperature of the plasma (Petrucci et al., 2001; Molina et al., 2009), whereas for SSC the narrow-band spectral shape changes more gradually between the keV and GeV regimes. Molina et al. (2013) show that a reasonable upper-limit to the average for all AGN corresponds to keV, based on cosmic diffuse background measurements (Gilli et al., 2007). The SSC scenario is not new in the context of Cen A (Chiaberge et al., 2001), and describes the spectral energy distribution (SED) well at soft X-rays (observed by SWIFT) and the GeV (Abdo et al., 2010). Cen A is an FR I radio galaxy (Fanaroff & Riley, 1974), which are believed to be misaligned BL Lac objects, i.e. the jet is not aligned with the line-of-sight. However, FR I galaxies are more luminous in -rays than expected for blazars viewed off-axis, suggesting emission from a slower moving region of the jet (either at a greater distance from the nucleus (Georganopoulos & Kazanas, 2003), or in a so-called ‘sheath’ around a faster-moving inner-jet (Chiaberge et al., 2000)), as the beaming angle is inversely proportional to the bulk Lorentz factor. The SED of some other FR I galaxies are also well-described by SSC emission (Abdo et al., 2009a, b).

The Compton hump from reflection was first detected in Seyfert galaxies using the Ginga satellite (Nandra & Pounds, 1994), but its discovery in the Cen A spectrum remains tentative. Markowitz et al. (2007) used Suzaku observations to claim a non-detection, while Fukazawa et al. (2011) demonstrated a residual excess in the continuum between keV but were not able to compensate for this in their reflection modelling (their figure 5), neither do they adequately model the emission above 20 keV. Beckmann et al. (2011) used INTEGRAL IBIS and SPI data to claim a detection of the reflection component. However, their approach merely assessed the consistency of the flux from a best-fit reflection component with zero, which is not a valid method to test for the presence of a spectral component (see the discussion in Protassov et al., 2002). Moreover, the Compton hump must be consistent with the inferred reflection properties observed in the soft X-ray bandpass and with the input spectrum being from the central source.

Observations of Cen A with Fermi-LAT have shown that the GeV spectrum follows a much steeper power law ( Abdo et al., 2010) than is measured in the X-ray regime (, Evans et al., 2004; Beckmann et al., 2011; Rothschild et al., 2011; Fukazawa et al., 2011). This difference in spectral shape between the keV and GeV regime might indicate the presence of a high energy cut-off, as would be expected for the thermal Compton scenario, or it could be the case that the spectrum evolves gradually between low and high energy, as is expected for SSC spectra. Previous work by Kinzer et al. (1995) used OSSE data to claim a high energy cut-off with inversely proportional to intensity over the 120-700 keV band. Rothschild et al. (2011) used the highest quality datasets from 12 years of RXTE HEXTE data to constrain MeV during the brightest epochs, while Beckmann et al. (2011) used INTEGRAL JEM-X/IBIS/SPI/PICsIT data to fit an absorbed cut-off power law with a best-fit keV, and subsequently re-fit the spectrum with a thermal comptonisation model (compPS), finding keV.

The present paper makes use of 10 years worth of data obtained with the primary spectrometer, SPI (Vedrenne et al., 2003; Roques et al., 2003), on-board the International Gamma Ray Astrophysics Laboratory (INTEGRAL, Winkler et al., 2003). At present SPI is the optimal instrument for studying both AGN reflection and cut-off components simultaneously, as it is sensitive over the 20 keV – 8 MeV range with an excellent spectral resolution (2.5 keV at 1.3 MeV). In this paper we study the average Cen A spectra, and present evidence of the reflection component in the SPI data based on extending the best-fit continuum of Chandra grating observations to higher energies. Subsequently, we use simulated spectra to carry out a robust statistical test for the existence of a high-energy cut-off. Finally, we investigate the extent to which we can accurately recover with simple models when reflection is also present in the spectra of AGN.

2. Preparation and Analysis

2.1. Data Reduction

We select only SPI observations where the Cen A nucleus is inside the FoV. These data are further reduced by excluding science windows with a high background activity due to passage of the observatory through the Earth’s radiation belts or increased solar activity. The source flux extraction for each energy band is performed through a model fitting procedure which compares the source and background fluxes convolved with the instrument transfer matrix with the count rates recorded in the detector plane (as outlined by Jourdain & Roques, 2009). We model the sky based on a point source at the location of Cen A, and assume the flux to be constant over one revolution ( days, or less if multiple targets were observed during that revolution) of the spacecraft. Each revolution is comprised of numerous ‘science windows’, lasting ks, which commence as the observatory is re-pointed as part of the dithering strategy. We model the background as an empty field that is variable on a timescale of 5 science windows for a given revolution. This reduction was carried out using the SPI Data Analysis Interface (SPIDAI111http://sigma-2.cesr.fr/integral/spidai).

After data reduction the average SPI spectrum of Cen A has an effective exposure time of 1.355 Ms.

Observations between keV using the Chandra ACIS instrument have shown that the inner of Cen A boasts a wealth of X-ray features besides the bright nucleus, such as the extended jet (Worrall et al., 2008), hot gas (Kraft et al., 2008), shock-lobes (Croston et al., 2009) and a large population of X-ray binaries (Voss et al., 2009; Burke et al., 2013). These other features are potentially problematic for studying the high-energy emission of the nucleus with SPI, which has an angular resolution of . However, Suzaku observations of Cen A have shown that the contribution to the keV flux of Cen A from X-ray binaries is (Fukazawa et al., 2011), less than of the AGN emission, while the bright extended () jet (Worrall et al., 2008) only contributes . As we expect the contribution of other X-ray features to diminish at higher energy, we are confident that the emission detected by SPI comes overwhelmingly from the nucleus. In this paper we make use of reduced and processed Chandra spectra presented by Evans et al. (2004).

Figure 1.— Lightcurve of Cen A observed by INTEGRAL SPI (upper panel) and hardness residuals after subtraction of the weighted mean (lower panel).

2.2. Analysis

2.2.1 Intensity and Hardness

Rothschild et al. (2011) established that the shape of the high-energy spectrum of Cen A does not change with time over the RXTE bandpass, despite the flux varying by a factor of a few. We tested this over the wider bandpass of the SPI data, by calculating hardness ratios and judging their consistency with a constant value. The keV lightcurve of the Cen A nucleus is presented in the top panel of figure 1, beneath which we show the residuals of two hardness ratios subtracted from their weighted means. These support the conclusion of Rothschild et al. (2011), i.e. that in the hard X-rays the spectral shape is unchanged despite significant variation in flux. This consistency of spectral shape allows us to examine the average spectrum of Cen A over all observations.

2.2.2 Spectral Fitting

Using XSPEC 12.7 we find that the average INTEGRAL spectrum of Cen A fitted with an absorbed powerlaw with absorption fixed at is adequately described () by a power law of photon index . All spectral fitting uncertainties in this paper are quoted at the level.

As a further test of spectral consistency, and to demonstrate the validity of using the average Cen A spectrum, we extracted spectra from high and low intensity regimes, defined as being above or below (see figure 1). We found nearly identical power law fits, barring a change in normalisation, with , ; within the uncertainty of associated with each measurement.

Figure 2.— The residuals from the dominant power law component found by Evans et al. (2004) using the Chandra gratings data, with normalisation free. On the left are these same Chandra data, while the right panel shows the residuals of the average spectrum observed by INTEGRAL SPI. The SPI residuals correspond to having the cross-calibration factor fixed (, the value found from fitting a single absorbed power law to both datasets), and as a free parameter (). For clarity, these instances are offset in .

To evaluate the existence of other model components we assess the consistency of the spectral shape between low and high energy, particularly because low energy data is comparatively good quality. We revisit the Chandra METGS and HETGS spectra of the Cen A core (obsID 1600) presented in Evans et al. (2004) with the same spectral grouping ( counts per bin). They found the continuum to be dominated by a power law. We fitted an absorbed power law (phabs powerlaw in XSPEC) to the Chandra spectrum with , with the normalisation free to vary. We then introduced the SPI spectrum to gauge how well the spectral shape extended to high energies. To account for calibration and non-simultaneity between the Chandra and INTEGRAL observations, we allow a multiplicative factor to the INTEGRAL portion of the model. To determine a reasonable value for C, we first fit the Chandra data with an absorbed power law, with a Gaussian to account for the narrow emission in the vicinity of the Fe K complex. Freezing all key parameters except normalisation prior to adding the SPI data, i.e. such that only the normalisation and may vary, finding . Subsequently, we free the photon index to vary as well, recovering (with ). In figure 2 we present the residuals after fitting the simple power law model with fixed at 0.78 and (the main power law component found by Evans et al., 2004). In the right-hand panel – the INTEGRAL SPI residuals – we also present residuals for .

In the Chandra panel of figure 2 the known (unmodelled) reflection component can clearly be seen as an excess in the spectrum at keV. The systematic shape of the residuals in the right-hand panel, from the SPI data, shows that the power law alone is an inadequate representation of the spectrum at high energy, and we suggest that the apparent excess of the data in the 20-50 keV range and excess of the model at higher energies is the result of the unmodelled reflection component, consistent with the excess at 6.4 keV.

The reflionx model (Ross & Fabian, 2005) describes the reflection of a power law spectrum from an optically thick atmosphere. The key parameters of reflionx are the photon index of the ionising continuum (thus should be tied to the of the a separate power law component during fitting), ionisation parameter and the abundance of iron in the reprocessing medium. Neutral reflection in a distant absorber is a nearly ubiquitous feature of AGN spectra, and Walton et al. (2013) successfully modelled this using reflionx for a sample of high-quality Suzaku observations of AGN (with fixed to the minimal value, as required of neutral material). They found that their reflection treatment had the required flexibility to reproduce all of the broadband spectra consistently over their sample. Therefore we chose to use reflionx in the current work as our preferred model of reflection from AGN.

In figure 3 we present our best-fit model and residuals for the absorbed power law plus reflection model to the Chandra and INTEGRAL SPI data (see table 1). During the fitting process we tied the photon index of the reflection component to that of the power law, to be consistent between input and reflected spectrum. In the first instance, we left free to vary, with and frozen at the default values (solar and zero, respectively) and found that it tended towards low values between 10 (the lowest ionisation state) and an upper-limit of 55, as expected for reflection from a distant surface. We subsequently followed the treatment of Walton et al. (2013) and fixed .

We also probed the sensitivity of the fit to and . Letting these parameters vary yielded best-fit values of and . This value of redshift is fully consistent with that found in the catalogue (, Lavaux & Hudson, 2011), and henceforth we fixed to the catalogue value during fitting. As an inset to figure 3, we include residuals of the keV for both and at the best-fit value. For the model is excessive over the measured flux in one channel between keV, and only allowing to take positive values has the effect of slightly skewing the Fe emission in the model to more closely match the measured spectrum.

The parameters of the power law are constant, with ; consistent with the dominant power law found from fitting the Chandra data. Finally, we obtained a best-fit with , and the cross-calibration constant fixed, which we show with residuals in figure 3 and present the corresponding parameters in table 1. The model describes the SPI data well, with . Over the range keV, the flux of the power law component , while the reprocessed emission contributes a flux , i.e. of the total emission. An important caveat to this is that there is degeneracy between and the normalisation , and refitting with showed the flux fraction is consistently between of the total emission over keV.

To translate this result to a form consistent with the literature, we fit the SPI spectra using the model pexrav (Magdziarz & Zdziarski, 1995), which describes the reflection of a seed cut-off power law spectra from a neutral accretion disc. This has the key parameter , which is an expression of the solid angle of the reflecting material illuminated by the central source (, normalised to 1). We fix the and parameters to the dominant power law of the Chandra spectra and also fix the inclination parameter to 0.82 (corresponding to the cosine of , Neumayer et al., 2007). We also varied between values keV (see § 2.2.4), finding that has negligible sensitivity to this parameter when is above a few hundred keV. We recover a value of , which is consistent with previous attempts to measure the extent of reflection in Cen A with INTEGRAL (, Beckmann et al., 2011).

Note. – We fix , and the multiplicative calibration constant (see text). and represent the normalisations of the power law and reflection components.

Table 1Best-fit parameters of phabs(powerlaw+reflionx)
Figure 3.— Spectral model including reflection component (top panel), together with the best fit residuals (bottom panels, as in figure 2. Inset we show the effect on the residuals of leaving fixed to 0 and then having it as a free parameter.

2.2.3 Testing for a high-energy cut-off in SPI data

To test for the presence of a high-energy cut-off, we first defined a test statistic ; the difference in photon indices found from fitting an absorbed power law to the keV and keV ranges ( always fixed at ). The motivation for this is to detect a change in spectral shape between low and high energy, as we would expect if there is a cut-off at a few hundred keV. For the average Cen A spectrum, we calculate . We then judge the unusualness of our test statistic based upon simulated spectra produced using the XSPEC command fakeit.

In the first instance, we simulate 1000 spectra based on the absorbed power law fit to the Cen A spectrum () and calculated for each of the spectra. Only of spectra had a more negative than observed. The Poisson uncertainty associated with a bin containing 32 counts is , and so we can confidently state that the Cen A spectrum lies outside of the distribution. This is statistical evidence that the power law alone is not the correct description of the spectral shape.

The next stage was to simulate thousands of cut-off power law spectra with a range of covering several plausible values for thermal Compton spectra; keV in steps of 100 keV. We found that is sensitive to our choice of . For keV, we find that only of simulated spectra have as negative as observed, and this increases to ,, for to keV. This suggests that a change in the spectral shape at high energy is a reasonable explanation for our observed .

Finally, we checked the sensitivity of to the presence of reflection in the spectrum, by simulating spectra as above, but with a reflionx component contributing of the 23-60 keV flux. Our testing showed that distribution of varied very little with increased reflection flux, and even at contribution could only produce a result as the measured in fewer than of simulated spectra.

2.2.4 Recoverability of

To further investigate the location of a high energy rollover in the spectrum, we must first understand our ability to retrieve the true cut-off energy from fitting simplified spectral models. This is of particular interest because all AGN observed with INTEGRAL have lower quality data than Cen A, and fitting simple parameter models is the standard method of phenomenologically parametrising the data (some or all sources in e.g. Soldi et al., 2005; Malizia et al., 2008; Beckmann et al., 2009).

For a range of we simulated spectra based on our best-fit for Cen A (table 1), but with a cut-off present in the spectrum and with reflection contributing of the keV flux. We then fit the simulated spectra with an absorbed cut-off power law model (phabs cutoffpl). In figure 4 we present and confidence bars based on the distribution of recovered against the actual values. We present the two confidence bars to illustrate the skewed nature of the distributions. In XSPEC, the maximum possible value of allowed was set to 5 MeV, and the fits would occasionally ‘peg’ at this value for the higher values of . It is clear that the fits systematically underestimate when there is reflection present in the spectrum but ignored in the spectral fitting process. We indicate the recovered from fitting the average Cen A spectrum with an absorbed cut-off power law (dashed horizontal line), keV. This measurement lies outside of the main of the distribution when the actual keV.

To estimate a lower-limit to the energy of a possible cut-off in the Cen A spectrum, we compare the measured from fitting with an absorbed cut-off power law to the spectra simulated with keV. By computing the confidence region in the plane (figure 5), we find that the measured excludes a cut-off energy of 700 keV with confidence.

Figure 4.— The ranges of recovered found from fitting an absorbed cut-off power law (phabs(cutoffpl)) to simulated spectra. We also indicate the inner confidence to highlight the skewed natured of the distribution. The simulated spectra possess a weak reflection component similar to that found in the Cen A average spectrum (such that the combined simulated model is phabs[cutoffpl+reflionx]). The recovered values are systematically lower than the true values used in the simulations. The green dashed line indicates the measured found from fitting the average spectrum of Cen A with an absorbed cut-off power law.
Figure 5.— The , and confidence regions in the plane found from fitting simulated spectra that possess a 700 keV cut-off. Note that for the best-fits from of simulations ‘pegged’ at the maximal value permitted, 5000 keV. For clarity, these data are not shown, but were factored into the calculation of each confidence region. The red cross denotes the phabs(cutoffpl) best-fit value for the average spectrum from Cen A.

3. Discussion

We analysed the average hard X-ray to soft -ray spectrum of Cen A observed with INTEGRAL SPI, with an aim to saying more about the contribution of reprocessed emission to the spectrum and the existence of an high-energy cut-off. These features have important implications for the geometry and accretion physics of the source. This study makes use of 10 years of observations, and we present the lightcurve of this period in figure 1. The most striking feature of the lightcurve is the systematic increase in intensity between MJD 54000 and MJD 55000. Contemporaneous RXTE observations also recorded such an increase (Rothschild et al., 2011). Based on the SPI lightcurve, the hard X-ray emission from the Cen A nucleus can vary in intensity by as much as a factor of four on timescales of years, and by a factor of two over a period of a few months, while the spectral shape remains constant, consistent with the RXTE results.

We revisit the earlier Chandra grating spectra from Cen A. This was motivated by the need to model the Fe complex consistently with the energy range of the Compton hump. We examine the consistency between these low and high energy datasets by fitting the normalisations of the dominant power law reported by Evans et al. (2004), and show that this inadequately models the high-energy spectrum (figure 3), the shape of the residuals indicating an excess between keV. We propose that this excess is physical evidence of the so-called Compton hump, resulting from a reprocessing of the central X-ray emission. To model the excess at keV and 6-7 keV in a consistent way as reflection from a neutral, distant absorber we employed the model reflionx, first to demonstrate the low ionisation state of the reflecting medium, as expected for neutral material before fixing the ionisation parameter to the minimal value in subsequent fitting. In this way, we obtain a good description of the low- and high-energy spectra (figure 3). The best-fit model parameters (table 1) suggest that reflection may account for as much as of the keV flux, and that the reflecting may have sub-solar abundances (). The photon index dominant power law component is consistent with , as was found by Evans et al. (2004), and so fitting the reflection component directly describes the excess in spectral shape demonstrated in figure 2.

It is well-established that the spectral shape of Cen A changes between the X-ray and hard -ray regime (Abdo et al., 2010), with some authors proposing that this takes the form of a cut-off defined by the characteristic temperature of a thermal Comptonizing plasma (e.g. Beckmann et al., 2011) or more gradual spectral curvature as would be expected for SSC emission, as evidenced from the broader SED (Chiaberge et al., 2001; Abdo et al., 2010). The lack of ionised or broadened emission lines indicates that there is not a significant emission component arising from the disk (Marconi et al., 2000; Evans et al., 2004), which is in agreement with our conclusion that the jet is the principal emitter.

The statistic, which we defined as the difference in spectral slope between low ( keV) and high ( keV) energy, is very sensitive to the presence of a cut-off. Based on we show that a simple power law is an unlikely description of the spectrum at high-energy (despite an acceptable , § 2.2.2), and the measured value of can be reproduced from a cut-off at a few hundred keV. Absorbed cut-off power law fits to the average spectrum recovered keV. By simulating spectra dominated by a cut-off power law with a comparatively small reflection component, over a range of and then fitting a simple cut-off power law recovers parameters that lie outside of confidence region for (figure 5), all the more so for smaller (figures 4). Recalling that for a thermal Comptonizing plasma (Sunyaev & Titarchuk, 1980), this suggests keV, and even a conservative keV leads to keV. Molina et al. (2013) suggest a reasonable upper-limit of keV for average thermal Compton emission from all AGN, based on cosmic diffuse background measurements (Gilli et al., 2007), and we suggest that this argues against this being the primary source of hard X-rays in Cen A. Our results support the picture of Cen A where the broad SED can be described by SSC emission (Chiaberge et al., 2001; Abdo et al., 2010), consistent with other FR I galaxies that are considered to be BL Lac objects observed along a line-of-sight that is not aligned to the jet axis (Abdo et al., 2009a, b).

Finally, our results from fitting a solitary absorbed cut-off power law to spectra that are dominated by a cut-off power law but also contain a modest amount of reflection shows that is systematically underestimated. This effect increases with increased reflection. As it is often the case that studying AGN with INTEGRAL requires fitting an absorbed cut-off power law to the data to try to obtain a general picture of the thermal plasma in AGN, we believe that the inferred will have been over-estimated for many sources where reflection has not been taken into account.

We thank the anonymous referee for their careful reading of the manuscript and for many helpful comments that greatly improved the readability of this paper.

The INTEGRAL SPI project is supported under the responsibility and leadership of CNES. We are grateful to ASI, CEA, CNES, DLR, ESA, INTA, NASA, and OSTC for support.

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